BEGIN:VCALENDAR VERSION:2.0 CALSCALE:GREGORIAN PRODID:-//SabreDAV//SabreDAV//EN X-WR-CALNAME:ANU Astronomy & Astrophysics Colloquia and Seminars (Mount Str omlo) REFRESH-INTERVAL;VALUE=DURATION:PT4H X-PUBLISHED-TTL:PT4H BEGIN:VEVENT DTSTART:20221122T000000Z DTEND:20221122T010000Z DTSTAMP:20261011T152429Z UID:s7slf2g38vh4ni2ato78un818g@google.com CREATED:20220926T013814Z DESCRIPTION:Most massive stars are found in binaries (and higher multiplici ty systems) that interact over the course of their evolution. Mass transfe r plays a key role in understanding phenomena as diverse as supernovae\, X -ray binaries\, gamma ray bursts\, kilonovae\, tidal disruption events\, n ovae\, intermediate luminosity optical transients\, and gravitational-wave mergers. I will discuss recent 3-d (hydrodynamics)\, 1-d (spherical stell ar models)\, and 0-d (rapid binary population synthesis) efforts to explor e mass transfer\, including common-envelope evolution\, and constrain it w ith observations. LAST-MODIFIED:20221120T033907Z LOCATION:DLT & ZOOM (host: Neco Kriel) \nZoom: https://anu.zoom.us/j/997853 41005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ilya Mandel (Monash University) "Interactions in massive stellar bi naries" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240313T000000Z DTEND:20240313T013000Z DTSTAMP:20261011T152430Z UID:esnh3iaraud9l3m6fc7q6oe4bg@google.com CREATED:20240220T233617Z DESCRIPTION:Most of the stars in today’s Universe were formed >8 billion years ago\, but we still have a poor understanding of the sites and condit ions under which they formed\, as well as how their formation shaped the g alaxies they reside in. Conventional wisdom – from decades of optical/NI R studies of stars and ionised gas – says that the star-forming gas in t hese early galaxies was more “clumpy” and turbulent than in local star -forming galaxies\, supporting the most widely accepted theories of disk g alaxy evolution and star-formation regulation. Yet\, what leads up to star formation is the availability of its fuel\, molecular gas\, which has bee n revealed for 100s of z>1 galaxies over the last decade thanks to new sub -/mm facilities\, especially the Atacama Large Millimetre/Submillimetre Ar ray (ALMA). In this talk\, I will discuss what we have learnt over the las t decade by observing and modelling molecular gas at Cosmic Noon (z=1–3) . I will highlight how some of these results appear to be in tension with current models of star-formation regulation and disk settling and will sho w how we can (literally) resolve this apparent tension with new observatio ns and simulations of both molecular and ionised gas at Cosmic Noon. Looki ng to the future\, I will discuss how we can better understand the process es leading up to and following star formation all the way up to Cosmic Daw n with next-generation facilities\, especially the Square Kilometre Array and Extremely Large Telescope. LAST-MODIFIED:20240308T100611Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Stu Wyithe) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Melanie Kaasinen (ESO) "Unravelling the History of Star Formation a nd Galaxy Assembly" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170921T010000Z DTEND:20170921T020000Z DTSTAMP:20261011T152429Z UID:498ma3pndncgp0ltfh9hjbmtlo@google.com CREATED:20170912T035608Z DESCRIPTION:Strongly gravitationally lensed galaxies are veritable gems for our understanding of high-redshift galaxy evolution\, allowing us (at lea st in the few most fortuitous cases) to study dust\, gas\, and star format ion even in the most intense starbursts on scales of individual star-formi ng regions. On these scales\, below one to few 100 pc in the source plane\ , kpc-scale rotational support no longer dominates\, and star formation is regulated by the local gas and stellar mass surface densities and energy injection from turbulence and winds driven by star formation and AGN. In recent years\, wide-field far-infrared and sub-millimeter surveys carried out with Herschel and the South Pole Telescope have drastically increased our samples of such starburst galaxies. The brightest such sources known\, however\, come from another\, even larger survey\, which was certainly no t built to study high-redshift galaxies: The Planck all-sky survey. In spi te of 5' beam size and a confusion limit of 600 mJy (corresponding to a FI R luminosity of about 5x10^13 Lsun at z~2)\, Planck has provided us with a small\, exquisite set of the brightest\, strongly gravitationally lensed\ , dusty\, high-z starburst galaxies known\, 'Planck's Dusty GEMS'. I will report on our follow-up work that was necessary to identify and characteri ze these galaxies\, including ALMA interferometry at 0.1'' beam size\, and discuss the first surprising lessons which they have already taught us\, from the signatures of winds to diffuse cold neutral gas to the delicate b alance between turbulence and gravity\, which does not seem so different f rom that in giant molecular clouds in the Milky Way. I will also discuss t he first direct observational constraint for a (bottom-heavy) stellar init ial mass function from gravitational lensing in the galaxy-formation epoch \, which is consistent with those of massive low-redshift early-type galax ies\, but defies the standard assumptions of most cosmological models. LAST-MODIFIED:20170915T054110Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Nicole Nesvadba (IAS Orsay) "Probing individual star-forming region s in maximal starbust galaxies at redshifts z=2-3: Planck's Dusty GEMS." TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181207T030000Z DTEND:20181207T040000Z DTSTAMP:20261011T152429Z UID:43ag2jl9gu0s64s88slmugqem0@google.com CREATED:20181022T011623Z DESCRIPTION:For more than 50 years\, the rate and distribution of positron (anti-electron) annihilation in the Milky Way has puzzled astronomers. Pos itrons with low (~MeV) initial energies are predominantly produced by beta + unstable radioactive elements\, however\, the observed rate of positron annihilation in the Milky Way far exceeds the predicted rate of positron p roduction by 'conventional sources' such as core-collapse and Type Ia supe rnovae. Moreover\, the observed distribution of positron annihilation in the Milky Way appears to trace the older stellar populations of the Galaxy (the Galactic bulge and a thick\, truncated disk)\, while radioactive mat erial is predominantly synthesised in the thin disk of the Galaxy. Over th e past four years of my PhD candidature\, I have constrained scenarios for positron injection and transport in energetic outflows of the Milky Way\, investigated positron annihilation sites in the Milky Way beyond annihila tion with electrons bound to hydrogen and helium atoms\, as well as invest igating in detail the possibility that positrons are born in the ejecta of subluminous thermonuclear supernovae that concentrate in old stellar popu lations. I will present highlights of this theoretically-focussed work in my talk\, along with emphasis on the implications of this work beyond high -energy astrophysics. Please join my collaborators and I for an antimatter -themed cake in the CSO common room following the talk. LAST-MODIFIED:20181123T050113Z LOCATION:CSO Common Room (host: Moller) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Fiona Panther (RSAA) "Positron annihilation in the Milky Way: Searc hing for a source of Galactic antimatter (End-of-thesis colloquium)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220601T010000Z DTEND:20220601T013000Z DTSTAMP:20261011T152429Z UID:n713blinprp8op9rs9p8q004mg@google.com CREATED:20220517T030109Z DESCRIPTION:Free space optical communications with satellites are affected by atmospheric turbulence\, typically using adaptive optics to correct for the resulting signal errors. This can be done using laser guide stars as a reference signal for the wavefront signal\, with the exception of tip-ti lt\, which up to date cannot be reliably measured with laser guide stars. Proposed solutions utilise the downlink signal (sent from satellite to gro und station) as a reference source with which to pre-compensate for tip-ti lt in the uplink signal. However\, the point ahead angle due to the orbita l motion of the satellites results in the signals propagating through diff erent regions of the atmosphere. Due to atmospheric anisoplanatism\, there is a degree of tip-tilt decorrelation between the laser links. The purpos e of this study is to determine if the tip-tilt is sufficiently correlated such that the downlink can still be used as a reference source for adapti ve optics applied to the uplink signal. This project developed methods to measure the tip-tilt of double stars and analyse the correlation of these effects between the two component stars\, equivalent to the downlink and u plink signals. Observational data of double stars at Mount Stromlo Observa tory (Canberra\, Australia) at different elevations and separations are an alysed to obtain statistics of the atmospheric tip-tilt. Different methods of each element of the analysis are evaluated in order to optimise the al gorithm. These tools enable an assessment of the feasibility of using the downlink as a reference to improve the performance of the uplink signal. T his work aims to assess the feasibility of using the downlink as a referen ce signal for atmospheric tip tilt sensing with the goal of improving the performance in the uplink communications. LAST-MODIFIED:20220517T030109Z LOCATION:DLT & ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Monique Cockram (RSAA) "Developing methods to use observational dat a of double stars to assess the feasibility of tip-tilt retrieval on the d ownlink signal for uplink pre-compensation in free space optical communica tions (Master's thesis presentation)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231012T000000Z DTEND:20231012T013000Z DTSTAMP:20261011T152429Z UID:gpkv66onhscpo1li43l58dfuh4@google.com CREATED:20231011T103106Z DESCRIPTION:This will be a quick overview of the phenomenology of accreting supermassive black holes and their jets. The understanding that has emerg ed from their systematics at multiple frequencies\, combined with the resu lts from computational simulations and connections with properties of thei r host galaxies and their evolution will be discussed. LAST-MODIFIED:20231011T103106Z LOCATION:Duffield Lecture Theatre (host: TBC) \nZoom: https://anu.zoom.us/j /83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Prajval Shastri (Raman Research Institute) "Different Angles on Acc reting Supermassive Black Holes" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161111T030000Z DTEND:20161111T032000Z DTSTAMP:20261011T152429Z UID:4ne3kpi90vdavs8s3jlo8sr24s@google.com CREATED:20161031T233108Z DESCRIPTION:In this talk\, I'll present an inside view of ESO and Paranal O bservatory from my UT-4 Fellow's perspective. I'll talk about clear skies and lasers and smog and 8.2m mirrors\, but not necessarily in this order. LAST-MODIFIED:20161109T043105Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Frederic Vogt (ESO) "Life as an ESO Fellow: 1yr on" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161118T033000Z DTEND:20161118T035000Z DTSTAMP:20261011T152429Z UID:btc918j9pf9cdpmg5hg7tqk0lo@google.com CREATED:20161114T004105Z DESCRIPTION:Presently an over 3sigma tension exists between values of the H ubble constant H0 derived from analysis of fluctuations in the Cosmic Micr owave Background by Planck and local measures of the expansion using calib rators of type Ia supernovae (SNe Ia). Calibration of SNe Ia requires a se ries of often subtle choices\, and the need to preclude human bias is more compelling that ever before. We perform a blind reanalysis of Riess et al . (2011) to measure the H0 using SNe Ia from CfA3 and LOSS\, calibrated by Cepheid variables and the geometric distance to NGC 4258. We obscure the value of H0 throughout our analysis and the referee process. Our analysis departs from that of Riess et al. (2011) by incorporating the covariance m atrix method adopted in SNLS and JLA to quantify SN Ia systematics\, and i ncludes a simultaneous fit of all SN Ia and Cepheid data using MultiNest\, thus capturing the full dependences and interactions of all parameters. T he measured value of H0 is yet to be revealed\; however\, we find a relati ve uncertainty in H0 marginally larger than the errors in Riess et al. (20 11) and in the Efstathiou (2014) reanalysis. Our error budget is dominated by statistical noise in the supernova data\, whilst the systematic contri bution to the error in H0 is dominated by uncertainties in the host galaxy mass dependence and Malmquist bias. LAST-MODIFIED:20161115T021107Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Bonnie Zhang (RSAA) "A blinded determination of the Hubble constant from supernovae'" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141118T000000Z DTEND:20141118T010000Z DTSTAMP:20261011T152430Z UID:j5an0fhl4cpod1ver4c5g3h648@google.com CREATED:20141117T060335Z DESCRIPTION:Deviations in chemical abundances that are found amongst the Ga lactic field stars and dwarf galaxies suggest a rich diversity of conditio ns in the early Universe and in events thereafter. High resolution spectro scopy for many RGB stars in dwarf galaxies over a range of masses show how each has had a unique chemical evolution. While these stars do not clearl y resemble those in the Galaxy\, we can use them to study variations in th e physical processes of galaxy assembly and evolution. Early results in th e search for metal-poor stars in the Galactic Centre are also providing a fresh approach to studying galaxy formation scenarios. LAST-MODIFIED:20250925T231018Z LOCATION:Duffield Lecture Theatre (host: David Nataf) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kim Venn (University of Victoria\, British Columbia) "Stellar abund ances in dwarf galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210323T000000Z DTEND:20210323T010000Z DTSTAMP:20261011T152429Z UID:9klnmt5uddq30tsabb8fmsni5c@google.com CREATED:20210215T211114Z DESCRIPTION:The new Australian SKA pathfinder (ASKAP) radio telescope is no w ramping up towards its full survey mode. In the process\, it has conduct ed several pilot surveys\, each of which is a major survey in its own righ t. Here I will talk about the new results from the EMU Pilot survey\, such as the discovery of new giant radio galaxies\, and starburst rings in nea rby spiral galaxies\, and finding that we detect almost all the galaxies i n 6dfGS. The biggest surprise was the discovery of a number of circles of radio emission (dubbed Odd Radio Circles) about 1 arcminute in diameter. After discounting the obvious explanations (artefacts\, supernova remnants \, starburst rings\, gravitational lenses\, etc) we still have no good exp lanation of the physical mechanism that is causing them. Our best evidence \, from Meerkat and other telescopes\, is that they surround galaxies at a redshift of ~0.3\, and have a typical diameter of ~1 Mpc\, and also show internal structure. The most promising hypothesis is that they result fro m a spherical shock\, perhaps from a cataclysmic event or starburst wind i n the central galaxy\, but so far we have only circumstantial evidence to support this hypothesis\, and so the hunt for an explanation continues. LAST-MODIFIED:20210319T071606Z LOCATION:ZOOM (host: Amit Seta) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ray Norris (CSIRO) "Invited Colloquium: Charting the uncharted radi o sky with ASKAP: new results from Evolutionary Map of the Universe" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160701T040000Z DTEND:20160701T042000Z DTSTAMP:20261011T152429Z UID:96f3v2uiemf22ucb4c13argotk@google.com CREATED:20160610T060108Z DESCRIPTION:Settling for a set of lockpicks as one of the more likely “il legal” things I’d be able to sneak back into Australia while visiting the US\, I’ve embarked on a fascinating journey of locks\, how they work and the often false sense of security they provide. In this talk I’ll explain just what lock picking is\, how it differs from what Hollywood por trays – and some personal experiences. I’ll describe how you can make your own keys\, picks\, what constitutes a ‘good’ lock and introduce you to the growing hobby of “locksport”\, while reassuring you that th ese techniques won’t be used on your home (lifting roof tiles is much fa ster)! LAST-MODIFIED:20160624T125107Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:James Webb (EOS) "Locks\, schmocks. Lockpicking and tales of (mis) adventure of an amateur locksmith." TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221216T020000Z DTEND:20221216T024500Z DTSTAMP:20261011T152429Z UID:794c35qo1u7tbqhgvomcuvqjj4@google.com CREATED:20221212T012908Z DESCRIPTION:Phylogenetic methods are widely applied in evolutionary studies in biology and are meant to reconstruct history\, as long as there are he ritable traits to trace evolution. Galaxies evolve and it turns out that a tracer for evolution are the chemical abundances because chemical element s are made in stars and passed from generation to generation. I will prese nt our recent progress in using chemical abundances in low-mass long-lived stars as heritable traits\,  how can we use these traits to build and in terpret phylogenetic trees\, and how are we using trees to learn about the evolutionary history of the Milky Way. LAST-MODIFIED:20221212T021109Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Callum Lynn) \nZoom: https ://anu.zoom.us/j/99785341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Paula Jofre (University Diego Portales) "Understanding the evoluti on of the Milky Way with phylogenetic trees" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260908T010000Z DTEND:20260908T020000Z DTSTAMP:20261011T152430Z UID:9iki7a8ffmuk2fvlcupa87kh64@google.com CREATED:20260605T021622Z DESCRIPTION:The centres of galaxies are among the most extreme environments in the Universe\, where millions of stars and black holes can be packed into remarkably compact regions around a supermassive black hole. In some galaxies\, these environments are further shaped by massive and luminous d iscs of gas\, creating a rich laboratory for gravitational interactions. T he resulting dynamics can drive extraordinary phenomena\, from black-hole mergers and gravitational waves to stellar disruptions and explosions. Yet how these processes interact and evolve over cosmic timescales remains po orly understood. I will review the governing processes that shape the dyna mics of stars and black holes in dense galactic nuclei\, including the eff ects of gas surrounding active supermassive black holes. Recent work explo res how complex gravitational interactions can shape the formation and evo lution of compact objects and produce distinctive observable signatures. I will discuss how these theoretical studies connect the dynamics of indivi dual stars and black holes to observations from current and next-generatio n facilities\, including LIGO–Virgo–KAGRA\, the Vera C. Rubin Observat ory and the future LISA mission\, providing new ways to probe the hidden l ives of stars and black holes at the hearts of galaxies. LAST-MODIFIED:20260904T010005Z LOCATION:Zoom or Duffield Lecture Theatre (host: Arunima) \nZoom: https://a nu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Evgeni Grishin (Monash U.) "Stellar Tango in the Hearts of Galaxies " TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230630T040000Z DTEND:20230630T042000Z DTSTAMP:20261011T152429Z UID:571m2e64v0vm8jhl4f85ik302g@google.com CREATED:20230626T020105Z DESCRIPTION:TBA LAST-MODIFIED:20230629T021605Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Neco) \nZoom: https://anu. zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Chris Lidman (RSAA) "New and old opportunities at SSO." TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141219T030000Z DTEND:20141219T031500Z DTSTAMP:20261011T152430Z UID:auoh678j43tkarkfn378sub09s@google.com CREATED:20250925T231028Z DESCRIPTION:The properties of the midplanes of planet-forming protostellar disks remain largely unprobed by observations due to the high optical dept h of dust and commonly observed molecules. However\, rotational emission l ines from rare molecules may have optical depths near unity in the vertica l direction\, so that the lines are strong enough to be detected\, yet rem ain transparent enough to trace the disk midplane. In this talk\, I will p resent a chemical evolution model of an MRI-active T-Tauri disk. The optic al depths of low-order rotational lines of C17O are around unity\, which s uggests it may be possible to see into the disk midplane using C17O. With our computed C17O/H2 abundance ratio\, such ALMA observations would provid e estimates of the disk masses by measuring the intensity of gas emission. LAST-MODIFIED:20250925T231028Z LOCATION:Duffield Lecture Theatre (host: Tiantian Yuan) \nZoom: https://anu .zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mo (Emma) Yu (University of Texas at Austin) "Probing planet nurser ies with rare CO isotopologues" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190321T000000Z DTEND:20190321T010000Z DTSTAMP:20261011T152429Z UID:srdl8sdcaaupcce3codt0i7lac@google.com CREATED:20190214T031117Z DESCRIPTION:Next generation galaxy surveys will be no longer either wide-fi eld shallow surveys or ultra-deep surveys with small coverage. They will h ave both very wide-field coverage and very deep depth. The goal is not onl y just to detect galaxies at high redshifts\, but also measure their large scale structures and then estimate their dark halos and their evolution a t various redshifts. Japan-Princeton Subaru HyperSuprimCam(HSC) survey is one of this kind. The HSC survey aims to perform a galaxy survey reaching the same spatial volume as SDSS but detecting galaxies at much higher red shifts\, and to provide targets for the next generation spectroscopic surv ey PFS. The CFHT Large-Area U-band Deep Survey (CLAUDS) is a deep U-band imaging in the HSC fields carried by a joint team from China\, Canada and France with 3 PIs\, each from one participating country respectively. The HSC+CLAUDS data permit studying galaxies at z=3 and below. With the U-band limiting magnitude of U=27.5 and a coverage of 15 deg^2\, we already have about 1 million LBGs at z=3 and 2 millions of BM/BX sources at z~2. This is the largest LBG/BM/BX sample\, providing a chance to explore the large scale structure at z>2. LAST-MODIFIED:20190308T010110Z LOCATION:CSO Common Room (host: Zhang) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jiasheng Huang (CASSACA/CfA) "CFHT Large-Area U-band Deep Survey (C LAUDS)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240322T030000Z DTEND:20240322T033000Z DTSTAMP:20261011T152429Z UID:0f4rvqi6nf3kv99cotcjg5i8bk@google.com CREATED:20240318T103607Z DESCRIPTION:Fast radio bursts (FRBs) are mysterious astrophysical transient s whose origin and mechanism remain unknown. Compact object mergers are a popular and intriguing theory for the progenitors of some FRBs. Neutron st ar-black hole (NSBH) mergers could power FRBs through mechanisms such as n eutron star tidal disruptions. This could present an opportunity for multi -messenger observations\, providing new insight into the nature of FRBs an d nuclear matter. Sophisticated statistical techniques are required to con fidently associate an FRB with an NSBH signal. In this talk I discuss poss ible avenues for measuring neutron star tidal disruptions and their astrop hysical implications if they are connected to FRBs. LAST-MODIFIED:20240318T103607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Neco Kriel) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Teagan Clark (Monash) "Neutron star-black hole tidal disruptions: g ravitational waves and fast radio bursts" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151110T000000Z DTEND:20151110T010000Z DTSTAMP:20261011T152429Z UID:qgavg1tsu911fe86hrjcem3oro@google.com CREATED:20151029T013607Z DESCRIPTION:Data from the VVV NIR survey of the inner Milky Way show that o ur Galaxy has a strongly peanut-shaped bulge. Extending the analysis to la rger radii with other surveys shows that the long bar is aligned with the bulge and extends to about 30 degrees longitude. The outermost parts of th e bar are dominated by a new superthin\, presumably younger component. Dyn amical models based on the 3D bulge density and the BRAVA kinematic data a llow us to determine the mass in the bulge region and to put constraints o n the mass-to-light ratio and dark matter content in the bulge as well as on the bar's pattern speed. The Milky Way bulge appears to have been mostl y formed from the disk through a bar and buckling instability\, with littl e evidence for a 'classical'\, merger-built bulge. LAST-MODIFIED:20151030T045106Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ortwin Gerhard (MPE) "The New Milky Way: Peanut Bulge and Long Bar" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190405T030000Z DTEND:20190405T033000Z DTSTAMP:20261011T152429Z UID:ddhtmtav8f9q0cfct818jt7qn0@google.com CREATED:20190331T233606Z DESCRIPTION:How do star systems form? How do planets form? What are planets made of? Can they support life? These are open questions in astronomy. To find answers we turn to exoplanet detection\, specifically direct imaging methods\, and the mid infrared region with its ability to penetrate dust clouds and provide molecular fingerprinting information. Direct imaging\, methods that use the light from the exoplanet\, has successfully imaged a number of exoplanets. A key problem in direct imaging tis the very dim lig ht from the planet compared to the very bright light from the host star. T he most widely adopted means of overcoming this is physically blocking the star with an opaque disc or a phase plate\, so called coronagraphy\, such observations however inherently favouring the detection of large exoplane ts at a great distance form their host star. Nulling interferometry uses t he light from the star itself\, from multiple telescopes\, to form an inte rferometric null over the star whilst leaving orbiting material\, like ga s or planets\, detectable. Measuring the light in the infrared spectrum al so further improves the contrast between the star and exoplanet due to the “warm” emission from forming exoplanets in particular. This project e xplores the use of photonic chips in nulling interferometry as a replaceme nt for bulk optical benches. Photonics has an inherently stability and com pactness advantage over bulk optics equivalent systems. This is especially relevant for future space missions. We report novel designs of a nulling interferometer\, in chalcogenide glass that is transparent in the infrare d up to a wavelength of 10 microns\, to create a >40 dB extinction of st ar light over a 400 nm bandwidth. LAST-MODIFIED:20190331T233606Z LOCATION:CSO Common Room (host: Zhang) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Harry-Dean Goldsmith (RSAA) "Fabricating a nulling interferometer f or exoplanet direction" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180517T010000Z DTEND:20180517T020000Z DTSTAMP:20261011T152430Z UID:1tpgelblau7vtuf96obq5pap94@google.com CREATED:20180302T000214Z DESCRIPTION:Data from the Fermi Large Area Telescope indicates that there i s an extended source of GeV gamma-ray photons coming from the Galactic Cen tre. Initially\, it was thought that this could be due to self-annihilatin g dark matter. However\, recent work shows that the spatial morphology bet ter matches the shape of the Galactic bulge rather than a spherically symm etric shape that would be expected from a dark matter signal. I will discu ss this result and also give details on the evidence that the source of th e excess is due to an unresolved population of millisecond pulsars. LAST-MODIFIED:20180511T002108Z LOCATION:Duffield Lecture Theatre (host: Panther) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Chris Gordon (University of Canterbury) "Is the Galactic Bulge shin ing in gamma rays?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230117T223000Z DTEND:20230118T010000Z DTSTAMP:20261011T152430Z UID:9pum65ji1c2hgpto0vp6gonlfc@google.com CREATED:20230111T054507Z DESCRIPTION:Schedule: 09:30 - 9:50 Alex Fan 09:50 - 10:10 Joel Montgomery 1 0:10 - 10:30 Grace Blomfield 10:30 - 11:00 Coffee break 11:00 - 11:20 Sam He 11:20 - 11:40 Luka Mijnarends 11:40 - 12:00 Jason Price LAST-MODIFIED:20230112T012108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Tony Travouillon) \nZoom: https://anu.zoom.us/j/99785341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Summer Research Student Seminar Series (RSAA) "Summer Student Semin ars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230922T043000Z DTEND:20230922T050000Z DTSTAMP:20261011T152429Z UID:t8og2svromt2gpvr5a73sbqe9g@google.com CREATED:20230823T045614Z DESCRIPTION:The Curious Minds program brings together a group of high schoo l girls with a passion for STEM subjects. I spent the last school holidays with these girls helping them deep-dive into the variety of opportunities that STEM has to offer\, and especially introduced them to engineering in a fun\, hands-on way. Come along to hear about how Curious Minds engages disadvantaged girls\, connects them with industry (including SSO) and sets them up with further learning opportunities. LAST-MODIFIED:20230823T045614Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark) \nZoom: https://anu. zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Grace McGinness (RSAA) "Meet the Next Generation of Women Scientist s" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220308T000000Z DTEND:20220308T010000Z DTSTAMP:20261011T152429Z UID:dpg5jes35tej7vld30s0q16ql0@google.com CREATED:20220228T031607Z DESCRIPTION:The relativistic cosmic ray population has long been theorized as a promising energy source for galactic winds\; however\, the details of cosmic ray propagation and influence in turbulent\, multiphase environmen ts are complex and unclear\, thereby impairing our understanding of galaxy evolution as a whole. In this talk\, I will present magnetohydrodynamic ( MHD) simulations of cosmic ray transport and impact in three instructive c ase-studies. First\, I'll present galaxy-scale simulations of cosmic ray driven winds from an LMC-like dwarf galaxy\, showing how the efficiency of supernova-driven outflows depends on cosmic ray transport. Second\, I'll zoom in on an idealized interstellar medium\, whose density inhomogeneitie s and collisional targets comprise an ''obstacle course'' for cosmic rays. I'll show how cosmic rays navigate and exchange energy and momentum with this clumpy\, highly resolved medium\, focusing on implications for wind d riving but also touching on an interesting discrepancy between galaxy evol ution simulations and multiwavelength observations. Finally\, I'll expand these zoom-in simulations to include turbulence\, probing cosmic ray energ y loss/gain in the presence of compressive turbulent motions and revising canonical equations for turbulent reacceleration. LAST-MODIFIED:20220302T120608Z LOCATION:DLT & ZOOM (host: Shyam Menon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Chad Bustard (UC Santa Barbara\, USA) "Invited Colloquium: Cosmic R ay Hydrodynamics and Galactic Wind Driving" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251104T220000Z DTEND:20251105T060000Z DTSTAMP:20261011T152430Z UID:od1ntgq8883l5ib1qmt4sv6mno@google.com CREATED:20250924T003613Z DESCRIPTION:Honours and masters end-of-thesis talks LAST-MODIFIED:20250924T003613Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Chris Wolf) \nZoom: https: //anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Honours and masters students (RSAA) "Honours and masters end-of-the sis talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200924T010000Z DTEND:20200924T013000Z DTSTAMP:20261011T152429Z UID:22ckon5eekm1uendf76lc6gdmc@google.com CREATED:20200907T060509Z DESCRIPTION:TBD LAST-MODIFIED:20200907T060509Z LOCATION:ZOOM 997 8534 1005 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dávid Guszejnov (UT Austin (USA)) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150213T032000Z DTEND:20150213T034000Z DTSTAMP:20261011T152429Z UID:o9m2lrvja48evrd4bbm9ort8ao@google.com CREATED:20150119T064110Z DESCRIPTION:TBD LAST-MODIFIED:20150622T074456Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Matthew Colless (RSAA) "The link between structure and kinematics i n early-type galaxies - the view from SAMI" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171123T000000Z DTEND:20171123T010000Z DTSTAMP:20261011T152429Z UID:s87km3fm56r2l2voln0pmnbrig@google.com CREATED:20170928T015107Z DESCRIPTION:Protoplanetary disks are the birthplaces of planets but the spa tial resolution at long wavelengths has so far been insufficient to resolv e the critical 5-30 AU region. The Atacama Large Millimeter Array (ALMA) n ow allows us to zoom in to nearby disks and determine the physical and che mical structure associated with planet formation. This talk will provide examples of recent work on observations and models of protoplanetary disks in various stages of evolution. Surveys of large numbers of disks provide insight into typical masses and sizes\, revealing surprisingly weak gas e mission. Special attention will be given to transitional disks\, which ar e a subset of disks with evidence for sharp-rimmed cavities (gaps or holes ). They are the best candidate sources for harboring just-formed giant pl anets. ALMA allows imaging of both the gas and dust in these disks\, prov iding constraints on the properties of any young planets. Some prospects f or JWST will be mentioned. LAST-MODIFIED:20171112T225109Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ewine van Dishoeck (RSAA) "Zooming in on planet-forming zones of di sks around young stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261126T000000Z DTEND:20261126T010000Z DTSTAMP:20261011T152430Z UID:g30om00omaspnjsan5sntg1iag@google.com CREATED:20260929T040014Z DESCRIPTION:TBC LAST-MODIFIED:20260929T040014Z LOCATION:Zoom or Duffield Lecture Theatre (host: TBC) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Nicholas Achilleos (University College London) "TBC" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170320T003000Z DTEND:20170320T010000Z DTSTAMP:20261011T152430Z UID:p0djdh3a202kf0hrni6kk850oo@google.com CREATED:20170316T074107Z DESCRIPTION:In 2016 I completed my PhD at the University of Sydney and left astronomy to take up a position as a Science Curator at the Powerhouse Mu seum. In this talk I will discuss a little bit about my decision to leave astronomy\, how I got my new position\, and what skills from my PhD have b een most useful in my new role. I will talk about my experience of leaving astronomy - both the upsides and the downsides. Finally\, I'll share a li ttle bit about what I've been working on since starting my new position\, and hopefully show just how much fun working in a Science Museum can be. LAST-MODIFIED:20170317T035608Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sarah Reeves (University of Sydney) "A fork in the career road: fro m astronomer to curator" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201204T030000Z DTEND:20201204T033000Z DTSTAMP:20261011T152430Z UID:kb6k7mqk736ic5lb5v6ndljhoo@google.com CREATED:20201116T003615Z DESCRIPTION:The new FoF format is like an Open Mic: Our speakers have 15 mi nutes each to talk about topics of their choice. The idea of the new FoF i s to get to know the many individuals that work under the same roof\, allo w newcomers to find friends easily\, and find new friends or colleagues wi th similar interests and hobbies. So feel free to talk about some of your most favourite adventures\, memorable Stromlo anecdotes\, your hobbies\, y our last COVID-DIY project\, your voluntary activities outside of Stromlo or whatever you are passionate about. Science talks (about a scientific to pic/question that you are interested in) are also welcome\, but be mindful of your audience (astronomers\, students\, engineers\, professional staff ). LAST-MODIFIED:20201116T215614Z LOCATION:ZOOM 997 8534 1005 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Shyam Menon and TBD (RSAA) "The amazing phenomenon of Sleep and TBD " TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181026T030000Z DTEND:20181026T033000Z DTSTAMP:20261011T152429Z UID:cl1ppplailu92o2up9t6bqcrrs@google.com CREATED:20181018T000104Z DESCRIPTION:Hickson compact group (HCG) galaxies are a prime experimental g round for learning about star formation (SF) due to their unique kinematic properties. No previously devised SF relations have been able to accurate ly describe the physics of the observed star formation rate in these HCG s ystems. In this study we extend on previous works to devise a more physica lly meaningful SF relation to better encompass the physics of these unique systems. We combine CO(1--0) data from the Combined Array from Research i n Millimeter Astronomy (CARMA) to trace the column density of molecular ga s Dgas and deep Ha imaging taken on the Southern Astrophysical Research (S OAR) Telescope tracing D_SFR to investigate star formation efficiency acro ss face-on HCG\, NGC7674. We find a lack of universality in star formation \, with two distinct sequences present in the D_gas-D_SFR plane (also know n as the Kennicutt-Schmidt (KS) plane)\; one for inside and one for outsid e the nucleus. We devise a SF relation based on the multi-freefall prescri ption of gas and the critical density\, which itself is dependant on the v irial parameter a_vir\, the ratio of turbulent to gravitational energy. We find that our modified SF relation describes the physics of this system w ell for a virial parameter of about 5--10 across the galaxy\, leading to a n order-of-magnitude reduction in SFR compared to a_vir~1 systems. LAST-MODIFIED:20181025T024604Z LOCATION:Duffield Lecture Theatre (host: Moller) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Diane Salim (RSAA) "Turbulence in Hickson Compact Group NGC7674" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160714T010000Z DTEND:20160714T020000Z DTSTAMP:20261011T152429Z UID:vb9mvfeds970tk5i3hkkqgmm48@google.com CREATED:20160517T002116Z DESCRIPTION:Recent observations have shown that the properties of the dense intracluster gas cooling in the cores of clusters of galaxies are signifi cantly affected by AGN activity in the central brightest galaxy. I will re view these observations and focus on the most nearby example of this AGN F eedback from NGC1275 at the core of the Perseus cluster. LAST-MODIFIED:20160704T074106Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alastair Edge (Durham University) "The rise and fall (and rise agai n) of NGC1275" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220331T030000Z DTEND:20220331T040000Z DTSTAMP:20261011T152429Z UID:sc4q7blscge5saqlohq6jhaqsk@google.com CREATED:20220314T000613Z DESCRIPTION:TBD LAST-MODIFIED:20220314T232614Z LOCATION:DLT & ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Markus Dirnberger (RSAA) "End-of-MPhil Talk: Dwarf galaxies in the M66 Group" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230323T000000Z DTEND:20230323T010000Z DTSTAMP:20261011T152429Z UID:4qolvl3ojm0q1magfmtmr2p8kg@google.com CREATED:20230319T034108Z DESCRIPTION:A trend in photoionization models of the Narrow Line Regions (N LR) of Seyfert 2's is to consider a wide range of cloud densities (at each NLR radius) that extends from 100 up to 1e8 cm-3 (LOC models). Such model s are relatively successful in reproducing the observed strength of most optical emission lines\, including the [OIII] lines. However\, LOC models have not considered calculating the density sensitive [ArIV] l4711/l4740 d oublet ratio. The reason is that the [ArIV] lines are very weak. In a rece nt paper on this subject\, I could rely on only 7 high excitation Seyfert 2's observed by Koski in 1978! However\, I recently had the surprise of di scovering that the SDSS S7 Survey could measure [ArIV] in about 45 nuclei! Of the 22 high excitation Seyfert 2's of the S7 sample\, the [ArIV] ratio s in 18 objects favour plasma densities that do not extend beyond ~50\,000 cm-3. Assuming such densities\, we evaluate that the temperature of the N LR must lie around 13\,500K\, which is inferred from the [OIII] l4363/l500 7 ratio that standard photoionization models have difficulty in reproducin g. We are currently exploring different solutions to the temperature probl em. LAST-MODIFIED:20230319T034108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Henry) \nZoom: https://anu .zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Luc Binette (National Autonomous University of Mexico) "Temperature issues with NLR studies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190228T003000Z DTEND:20190228T010000Z DTSTAMP:20261011T152429Z UID:obj6sbbk5nd3dkkg99bo8tvh4o@google.com CREATED:20190128T232717Z DESCRIPTION:Quiescent galaxies are on average smaller than star-forming gal axies of the same mass. This structural difference could be due either to the evolution of galaxy populations as a whole\, or to the structural evol ution of individual galaxies as they become quiescent. Gas rich mergers ar e effective at driving gas in the central region of galaxies\, where it ca n trigger both star-formation and active galactic nuclei activity: as a co nsequence\, galaxies that experienced major gas-rich mergers may both shri nk in size and become quiescent. We use 0.6 < z < 1.0 visible rest-frame s pectroscopy from the LEGA-C Survey to study the stellar population of post -starburst galaxies. In these systems\, which have recently become quiesce nt\, we find that stellar age increases with radius\, as expected after ma jor gas-rich mergers. LAST-MODIFIED:20190226T231106Z LOCATION:CSO Common Room (host: Oh) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Francesco D'Eugenio (Ghent University) "Evidence of compaction in p ost-starburst galaxies at redshift 1" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240220T000000Z DTEND:20240220T013000Z DTSTAMP:20261011T152429Z UID:fs0qtovrm9k772ernblu6uj6s0@google.com CREATED:20231212T003615Z DESCRIPTION:In this talk on the Andromeda (M31) galaxy\, I will present the results from a homogenous\, extended survey of Planetary Nebulae covering the entire disc and inner halo of M31 out to 50 kpc radius. Taken jointly with observational results from previous extensive investigations\, these findings support a recent (~2.5 Gyr)\, massive (1:4 mass ratio) accretion event from a satellite infalling along the Giant stellar stream\, in a ne arly radial orbit. This tumultuous recent past of Andromeda is very diffe rent from our own Milky Way galaxy\, that experienced a rather quiescent e volution in the last 8 Gyrs. I will present the evidence for a younger thi n and older thicker disc component in M31 and present the age-velocity dis persion relation at the corresponding radial distance of the solar neighbo urhood in M31. Then I explore the chemical composition of these discs usin g Oxygen and Argon element abundance. The two kinematically distinct discs in Andromeda are also chemically distinct\, 1) with the thin disc reachin g higher Argon abundances than the thicker disc\, 2) the thicker disc havi ng a positive Oxygen and null Argon radial gradient\, 3) while the thin di sc presents a negative radial gradient in both Oxygen and Argon. The latte r gradient is consistent with the negative Oxygen gradient previously meas ured for the HII regions. I then use the log(O/Ar) vs. (12 + log(Ar/H) ) d istribution of stars with different ages to constraint the chemical evolut ion of the parent stellar populations in the thin and thicker M31 discs. T he distributions in this plane show that the chemical and also the structu ral properties of the thin and thicker discs in M31 are remarkably differe nt from those determined for the Milky Way. I then investigate the stella r populations and kinematics of the inner halo substructures - NE and W sh elves\, Giant stellar stream and G1 clump - and compare them with the deta iled predictions from simulations of a major merger event in Andromeda. Th e goal is to understand whether it is a wet or a dry merger\, and to furt her constrain the pre-merger M31 disc population and that of the satellite as well. As part of the forward look\, I shall present the potential info rmation from the combined use of Oxygen and Argon to constrain the early p hases of star formation in z>4.0 galaxies. LAST-MODIFIED:20240208T232116Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hiep Nguyen) \nZoom: https ://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Magda Arnaboldi (ESO) "The evolution of the Giant Andromeda galaxy mapped using planetary nebulae in its disc and inner halo" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261027T040000Z DTEND:20261027T051500Z DTSTAMP:20261011T152430Z UID:ub9ksm22g6afq5s2evt8auf51c@google.com CREATED:20260503T114414Z DESCRIPTION:Our monthly Skillshare sessions provide an informal\, supportiv e\, and practical space for students and postdoctoral researchers to devel op and exchange research skills\, professional-development tools\, and eff ective workflows. The format is primarily focused on students\, in particu lar those enrolled in the ASTR8030 course Astronomy and Astrophysics Resea rch Skills. However\, everyone is very warmly invited to join and contribu te.\n\nSessions are held on selected Tuesdays from approximately 3:00-4:15 ish pm in the CSO Common Room. Depending on the topic\, they may include s hort introductions\, demonstrations\, panel discussions\, interactive exer cises\, or open-ended hands-on activities. LAST-MODIFIED:20260905T020013Z LOCATION:Zoom or CSO Common Room (host: Sven Buder and Melanie Kaasinen) \n Zoom: https://anu.zoom.us/j/89544552112?pwd=Bdoo5fgMVS2Ls6e3Fs0NSNk9OMpaXn .1 SEQUENCE:2 STATUS:CONFIRMED SUMMARY:RSAA Skillshare (RSAA) "How to write an academic application" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210709T040000Z DTEND:20210709T043000Z DTSTAMP:20261011T152429Z UID:s7osgmmpk7np5qn005760pqmeo@google.com CREATED:20210622T060112Z DESCRIPTION:The Feast-of-Facts are an informal open-mic format from RSAA me mbers for RSAA members. LAST-MODIFIED:20210706T020607Z LOCATION:ZOOM and Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Noelia Martinez (RSAA) "4000km of mud\, ice\, rock\, and (mis)adven tures" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151215T000000Z DTEND:20151215T010000Z DTSTAMP:20261011T152429Z UID:8g5ja5907aa4fciathf9brtlbk@google.com CREATED:20150915T003615Z DESCRIPTION:Following the East Asian Observatory assuming operations of the James Clerk Maxwell Observatory in March 2015\, the Observatory has had a n extremely successful and productive year. The JCMT is the premier submil limeter facility in the northern hemisphere for wide-field continuum and h eterodyne observations\, and maintains a suite of instrumentation that off ers high-impact science opportunities well into the next decade. The EAO i ntends to accelerate these achievements by embarking on an ambitious progr am of instrument upgrades and additions that will further extend the JCMT' s capabilities. An overview of the East Asian Observatory and its vision w ill be described\, and the JCMT operations and capabilities will be presen ted. The merits of the new organisation will be presented with reference t o how and why Australian astronomy would benefit from joining this new par tnership and this premier observing facility. LAST-MODIFIED:20151214T010104Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jessica Dempsey (JCMT operations manager) "JCMT: submillimeter oppo rtunities for Australia with the East Asian Observatory" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241122T030000Z DTEND:20241122T033000Z DTSTAMP:20261011T152429Z UID:ibel7qu5h9qasqhg6b6propvp4@google.com CREATED:20241017T044118Z DESCRIPTION:MAVIS is an Australian-led adaptive optics instrument being des igned for ESO's VLT Unit Telescope 4. In September a delegation from the M AVIS Consortium\, including five staff from AITC\, had a very successful t rip to the Paranal Observatory to visit the VLT (and ELT!) to discuss a br oad range of technical topics. This talk will discuss some of the outcomes of the trip\, and is bound to include many photos of large telescopes and the Atacama Desert. LAST-MODIFIED:20241017T044118Z LOCATION:Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.zoom.us/j /83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:David Brodrick & Dionne Haynes & Jennifer Burgess (RSAA/AITC) "MAVI S Paranal visit report" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160927T010000Z DTEND:20160927T020000Z DTSTAMP:20261011T152429Z UID:1innjardrkfvl3sob5tgbhmsdc@google.com CREATED:20160629T211115Z DESCRIPTION:In galaxy evolution studies\, the galaxies and their central su per-massive black holes are commonly linked together through bulge growth scenario's. The evidence is the tight correlation between the black hole m ass and the bulge mass in early-type galaxies. Surprisingly\, the total ma ss of the galaxy does not correlate well with black holes mass. In this ta lk\, I will show how black hole masses are measured with stellar kinematic s. And I will show how the host galaxy properties correlate to black hole mass. Global processes appear to be most significant. LAST-MODIFIED:20160926T065105Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Remco van den Bosch (MPIA) "Galaxies and their Super-Massive Black Holes" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170605T010000Z DTEND:20170605T012000Z DTSTAMP:20261011T152429Z UID:l3gj7lhk8puit5e01v18ai31i0@google.com CREATED:20170605T000103Z DESCRIPTION:Space assets such as communication satellites and the Internati onal Space Station are at serious risk from collision with over 300 000 it ems of space debris in orbit. Currently\, only a fraction of these objects can be monitored by space debris tracking stations. To enable more accura te tracking from the EOS Laser Tracking Station\, a Guide Star Laser (GSL) will be installed to allow for adaptive optics (AO) corrections of the in fra-red laser beam. The focus of this project was to develop a system to i nterface three different GSL models on the EOS 1.8m telescope. Over the la st four months\, a team of engineering students from the ANU have worked t o determine technical requirements for this interface using a systems engi neering approach. We have analysed over 150 requirements and developed a c omprehensive verification and validation scheme to address system conflict s. In addition\, a conceptual design in the form of a CAD model has been p roduced. This presentation will cover what the team has achieved\, as well as the individual contributions each team member. LAST-MODIFIED:20170605T000103Z LOCATION:Duffield Lecture Theatre (host: Celine d'Orgeville) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:ANU/SERC students (ANU/SERC) "ANU Guide Star Laser Interface Projec t" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250109T030000Z DTEND:20250109T040000Z DTSTAMP:20261011T152429Z UID:214aa8apmonogrh35cfl1qti4o@google.com CREATED:20250107T045707Z DESCRIPTION:Never before have we had such precise control of photon creatio n\, manipulation\, and detection. In this talk\, I will describe the Roche ster Institute of Technology's Future Photon Initiative that seeks to leve rage state-of-the art understanding of photonic devices for a broad range of applications\, spanning astrophysics\, quantum information science and technology\, energy\, and operation in high radiation environments. In par ticular\, I will discuss our efforts to advance single photon counting ima ging detectors for future missions\, such as the Habitable World Observato ry. LAST-MODIFIED:20250107T045707Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Jenny Jiang) \nZoom: https ://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Don Figer (Rochester Institute of Technology) "The Future Photon In itiative and Detecting Habitable Worlds" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220315T030000Z DTEND:20220315T033000Z DTSTAMP:20261011T152429Z UID:bn1auqkkrttcfgnl8vbd298vk0@google.com CREATED:20220309T023606Z DESCRIPTION:The lambda CDM model predicts that some part of the stellar hal o were formed by minor mergers of dwarf galaxies and therefore should cont ain the debris of those systems. Also\, galaxies with different masses hav e different star formation history (SFH) and therefore different chemical evolution. This project aims to find a relationship between the stellar ma ss of the accreted structures and chemical abundances. LAST-MODIFIED:20220313T235307Z LOCATION:DLT & ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anne Xie (RSAA) "ASC project: Estimation of stellar mass of the acc reted structures based on chemical abundances from GALAH" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170317T030000Z DTEND:20170317T032000Z DTSTAMP:20261011T152429Z UID:3tcm94ifsn97tsjigrl64o6di8@google.com CREATED:20170210T050112Z DESCRIPTION:Direct imaging of exoplanets is limited by the optics of the te lescope which need to be removed by deconvolution or subtraction of point spread functions (PSFs). In this project\, existing methods of image analy sis are tested with a large sample of stars imaged by Keck to search for c ompanions. I hope to improve on these analysis methods to help establish n ew sensitivity limits for planet detection and\, in the event of any clear detections\, improve our understanding of planet formation. LAST-MODIFIED:20170310T025105Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alex Wallace (RSAA) "Searching for Young Exoplanets with High-Contr ast Imaging in the Near Infrared - Thesis Proposal" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230502T010000Z DTEND:20230502T020000Z DTSTAMP:20261011T152430Z UID:bd4o92tvcsr399cb8fbuq3bpmc@google.com CREATED:20230429T232306Z DESCRIPTION:Monitoring and management of inland and coastal water quality i s essential for safe drinking water\, for recreational and agricultural us es\, and for preserving freshwater and marine ecosystems. Satellite data a re often used for inland and coastal water observations but with severe li mitations: current space-based sensors have insufficient spatial resolutio n to capture many inland and near-coastal waters\, or insufficient spectra l resolution or signal-to-noise ratio to discern several water quality var iables that are important to end-users. CSIRO and NASA JPL are collaborati ng on an 18-month feasibility study for the AquaSat-1 mission concept\, wh ich aims to demonstrate measurement of optical water quality indicators fr om space for a set of key inland and coastal waters in Australia and weste rn USA. The proposed AquaSat-1 payload is a state-of-the-art visible to ne ar-infrared Dyson imaging spectrometer developed by JPL\, with a design ba sed on JPL's EMIT instrument currently operating from the International Sp ace Station. In this presentation\, I'll give an overview of the feasibili ty study\, results so far\, and next steps. LAST-MODIFIED:20230429T232306Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Neco Kriel) \nZoom: https: //anu.zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Courtney Bright (CSIRO) "The CSIRO-JPL AquaSat-1 Feasibility Study" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250408T010000Z DTEND:20250408T020000Z DTSTAMP:20261011T152429Z UID:eue7c38e0te69ssl0ba26maa34@google.com CREATED:20250106T230124Z DESCRIPTION:Many domains of contemporary astrophysics drive escalating dema nds for measurement precision from data. Witnessing intrinsically subtle phenomena\, such as the faint mote of light betraying an exoplanet against the glare of its host star\, often mandates breakthrough performance in several domains simultaneously. For this example\, the extreme contrast be tween the planet and star must be delivered while probing angular scales a t or beyond the diffraction limit of the largest contemporary telescopes. Accomplishing such tasks requires an integrated approach spanning the enti re workflow from instrument to data products\, bringing innovative hardwar e and principled approaches to optimisation and data analysis. Founded in novel interferometric and photonic technologies\, a handful of new instru ments led from my group (at Subaru\, Keck\, LBT\, VLT and CHARA) push to o vercome the observational limits. The commissioning of my AMI-interferomet er mode flying aboard JWST/NIRISS instrument has provided a springboard fo r interferometric technologies onto space platforms. A next step in bringi ng precision interferometric measurement to space\, my team are now in the final construction phase of the TOLIMAN mission\, which will fly a 12.5cm aperture space telescope (Australia's largest to date). TOLIMAN targets a n audacious outcome in planetary astrophysics: an exhaustive search for te mperate-orbit rocky planets in Alpha Cen\, our nearest neighbour star syst em\, by performing narrow-angle astrometric monitoring of the binary at ex treme precision. While spanning a diverse range of instruments\, this talk will distil the key thread of principled ideas that enable them. LAST-MODIFIED:20250316T231609Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Peter Tuthill (U. Sydney) "A coherent revolution: interferometry an d photonics for precision astrophysics" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191101T033000Z DTEND:20191101T040000Z DTSTAMP:20261011T152429Z UID:7pshld2q0ot878br4sqjllc94g@google.com CREATED:20191004T042614Z DESCRIPTION:What the heck are FPGAs and what are they doing in space? This talk will lead you on the exciting journey of FPGAs\; state-of-the-art ele ctronic devices that are taking space missions to the next level. Not only will you learn how these devices work\, but you'll also hear how they are being applied to cutting-edge space missions and technologies including R SAA's very own 'Emu' 1.4 micrometer space-telescope. LAST-MODIFIED:20191029T091607Z LOCATION:Duffield Lecture Theatre (host: Zhang) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Shanae King (RSAA/AITC) "AITC Series - FPGAs in space!" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150529T040000Z DTEND:20150529T044000Z DTSTAMP:20261011T152429Z UID:onk6040n42j6p0a7vbqu0n1nc4@google.com CREATED:20150513T084609Z DESCRIPTION:This talk provides a handy guide on what one can do in the real world after obtaining a PhD in Astronomy (and after the postdocs run out and no tenured positions available). It focusses on the various types of s kills\, knowledge and application gained during a PhD that actually makes one quite employable across a range of areas and positions/roles. This is based on my own experience (and other ex-astro bodies) to provide case stu dy examples covering a wide array of project and technology types and the range of different roles over the years. This talk provides important awar eness raising for young students – noting that one may not stay in one ’s chosen field and that a 'multi-career' is more than likely\, along wi th the numerous opportunities possible out there. LAST-MODIFIED:20150513T085608Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Peter Teague (Vipac Engineers & Scientists Ltd) "How can a PhD in A stronomy prepare you for doing other things in the Real World" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200924T010000Z DTEND:20200924T013000Z DTSTAMP:20261011T152430Z UID:r20kt69lojst0aqs55ltpq6834@google.com CREATED:20200912T030209Z DESCRIPTION:TBD LAST-MODIFIED:20200912T030209Z LOCATION:ZOOM 997 8534 1005 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dávid Guszejnov (UT Austin (USA)) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160401T030000Z DTEND:20160401T032000Z DTSTAMP:20261011T152429Z UID:3e3rfsdienr87snveh03gcqk2g@google.com CREATED:20160317T065107Z DESCRIPTION:The standard cosmological model currently fits a wide range of data spectacularly well. In fact so well that much attention is focussed on finding any small deviations from this model. In terms of the cosmic m icrowave background such features are often referred to as "anomalies" - t here are several of them described in the literature. They might represen t smoking guns for fundamental changes in our picture of high energy physi cs\, or they might just be statistical flukes. I will describe some of th e debate about assessing the statistical significance of such anomalies. LAST-MODIFIED:20160328T150107Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Douglas Scott (University of British Columbia) "Modern cosmology: a nomalies\, damned anomalies and statistics" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150703T042000Z DTEND:20150703T044000Z DTSTAMP:20261011T152430Z UID:hg2mo4vjpnntn8ef5o3ohggkko@google.com CREATED:20150623T070608Z DESCRIPTION:TBD LAST-MODIFIED:20150625T044109Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Christopher Nolan (RSAA) "Annual Thesis Talk" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190627T010000Z DTEND:20190627T020000Z DTSTAMP:20261011T152430Z UID:m7qhksq813f0nnq5e4msmdek2g@google.com CREATED:20190619T054604Z DESCRIPTION:The Gravity Recovery and Climate Experiment (GRACE) space gravi ty mission has been one of the most successful missions ever\, impacting t he disciplines of hydrology\, geophysics\, oceanography and cryospheric sc ience. For the first time\, it was possible to quantify changes in broad-s cale water resources\, measure directly the mass loss of ice sheets in pol ar regions\, observe the mass increase of the oceans due to polar melting and watch the process of uplift and subsidence of continents due to meltin g of ice sheets over the past 20\,000 years. The key instrumental observat ion that makes all this possible was the inter-satellite measurement of ch ange in distance between the two GRACE satellies\, flying in tandem orbits at 300-500 km altitude above Earth. Decommissioned in 2017\, the GRACE mi ssion was succeeded by the GRACE Follow On mission which was launched in M ay 2018. We have developed software at the Research School of Earth Scien ces to use the instrument measurements (so-called 'Level-1B data') to esti mate changes in mass on Earth. In this presentation I will take the lid of f the black box of data processing and show the incredible feats of engine ering that make it possible\, describe how it works and highlight some of the strengths and weaknesses of analysis from the GRACE and GRACE Follow O n missions. Results from GRACE Follow On allow us to compare the state of the current drought compared to the end of the Millenium Drought in 2009 a nd show the concerning increase in mass loss in Antarctica\, especially in the Totten Glacier region near Australia’s Casey Station. LAST-MODIFIED:20190620T234105Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Paul Tregoning (RSES) "GRACE and GRACE Follow On space gravity miss ions: how to get from um/s measurements to Gt/year ice melting rates" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240927T043000Z DTEND:20240927T050000Z DTSTAMP:20261011T152429Z UID:fca5tc1dk4u4vjfpv5qjo0qos4@google.com CREATED:20240925T040110Z DESCRIPTION:Turbulent motions perturb magnetic field lines and produce magn etic fluctuations. The perturbations leave imprints of turbulence statisti cs on magnetic field. Observation of synchrotron radiation is one of the e asiest ways to study turbulent magnetic field. First\, we obtained the spa tial spectrum of synchrotron polarization so that shows how the spectrum i s affected by Faraday rotation and how to recover the statistics of underl ying turbulence magnetic field. Since polarized synchrotron intensity aris ing from magnetized turbulence are anisotropic along the direction of mean magnetic field. Secondly\, we studied quadrupole ratio to quantitatively describe the degree of anisotropy introduced by magnetic field at multi-wa velengths. This work demonstrated that the spectrum and quadrupole ratio o f synchrotron polarization can be very informative tools to get detailed i nformation about the statistical properties of MHD turbulence from radio o bservations of diffuse synchrotron polarization. LAST-MODIFIED:20240925T040110Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Cameron van Eck) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Hyeseung Lee (UNIST (Republic of Korea)) "Statistical study of turb ulence from polarized synchrotron radiation" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260522T040000Z DTEND:20260522T043000Z DTSTAMP:20261011T152430Z UID:ee1crkn12hm36oiqsu4ltrfkm8@google.com CREATED:20260503T113516Z DESCRIPTION:Not all roads lead to an academic life. Three tech consultants from Vivanti Consulting will share their experience on careers that can le verage your research skills in solving problems with big data. Elise Hampt on is a Mt Stromlo Alum (2017) and has been working as a Data Scientist fo r the past 9 years. Elise will take you through a recent project where she created a Neural Network for frog species classifications. Shir Erez-rein is a software engineer with 5 years of experience in IT Consulting. Shir will take you through graph databases and the amazing analysis you can do with them. Michael Brightwood has a PhD in evolutionary biology and now wo rks as a data scientist. He'll discuss the mental and professional metamor phosis from academia to industry. This presentation will give you a taste of the work you can do outside of academia and give you an idea of how the transition works. LAST-MODIFIED:20260527T014042Z LOCATION:Zoom or Duffield Lecture Theatre (host: Brad Tucker) \nZoom: https ://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Elise Hampton (Vivanti) "Thinking of careers beyond research?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250612T010000Z DTEND:20250612T020000Z DTSTAMP:20261011T152429Z UID:kol5228mvtph9vcd0gcug20eg0@google.com CREATED:20250515T000611Z DESCRIPTION:Wide field Adaptive Optics (AO) is the branch of AO that aims t o deliver compensation of atmospheric turbulence for ground-based optical telescope over patches of sky larger than the isoplanatic patch imposed by the nature of turbulence - typically 10 to 20" - delivered by the so-call ed Single-Conjugate AO. In this talk - a rehash of a keynote talk delivere d at the Wide-Field AO workshop in Tokyo earlier this year - I will review Wide-Field AO (WFAO) systems\, and explain their principles and how they beat fundamental limitations on both wavefront sensing and phase compensat ion. I will also review the various type of WFAO breeds\, including GLAO\, MCAO and MOAO\, with some illustrating example systems. LAST-MODIFIED:20250515T000611Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Francois Rigaut (RSAA) "Wide Field Adaptive Optics" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160414T010000Z DTEND:20160414T020000Z DTSTAMP:20261011T152429Z UID:b3o7a3daaeaejsfe966mug84s0@google.com CREATED:20160228T234114Z DESCRIPTION:The Murchison Widefield Array is conducting an all-sky low-freq uency radio survey across 70-230 MHz. The GaLactic and Extragalactic All-s ky MWA (GLEAM) Survey comprises of over 300\,000 catalogued components and represents a huge leap forward in our understanding of the low frequency radio sky. I will present the early science results from GLEAM probing the local to distance Universe. Highlights will include improved understandin g of the star formationm of local star forming galaxies\, searching for cl usters at high redshift around radio-loud active galactic nuclei and sear ching for the first black holes. This work also has implications for the s cience from continuum surveys from SKA_LOW which may not be as confusion l imited as previously feared. LAST-MODIFIED:20160411T013106Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Nick Seymour (Curtin Institute of Radio Astronomy) "Exploring the E xtra-galactic Low Frequency Universe with MWA" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220414T010000Z DTEND:20220414T020000Z DTSTAMP:20261011T152429Z UID:4v99jopiqsd2rqj81qmp8mpr98@google.com CREATED:20220405T002110Z DESCRIPTION:Cool stars are fossils from the history of the universe and the ir properties can provide unique insights on the formation and evolution o f the Milky Way. I show how the chrono-chemo-dynamic narrative of the Milk y Way can be unravelled by combining stellar parameters derived from diffe rent surveys and methodologies across stellar evolutionary phases. We are now systematically studying stellar populations in the broader Galactic co ntext\, and thanks to transformational facilities we will soon be able to bridge between the Milky Way and other galaxies. Measuring the chemistry o f resolved stellar populations up to a few Mpc will open up science cases that so far could only be addressed with nearby stars\, and transform our ability to test and to use the Milky Way as a template to study other gala xies. I review some of the main results obtained in this quest\, present o ngoing efforts and highlight future directions with upcoming observational facilities. LAST-MODIFIED:20220412T004110Z LOCATION:DLT & ZOOM (host: Ioana Ciuca) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Luca Casagrande (RSAA) "Invited Colloquium: Stars in the Milky Way and the next frontier" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170320T000000Z DTEND:20170320T003000Z DTSTAMP:20261011T152430Z UID:ql8ei2sf3n56ufkariq71dm9gs@google.com CREATED:20170316T074107Z DESCRIPTION:The radio sky is an extremely dynamic place. Many transients in cluding gamma-ray bursts\, supernovae\, X-ray binaries\, tidal disruption events and flare stars produce bright radio emission. This radio emission is important to observe as it traces relativistic ejecta and non-thermal p rocesses\, allowing us to study shocks and particle acceleration\, while p robing magnetic fields and the ISM. However\, the most interesting physics takes place at the very beginning of the transient event but it is diffic ult to get a prompt follow-up response in the radio band. We are now enter ing the era of rapid-response radio telescopes that are capable of trigger ing on transient events detected by missions such as Swift\, Fermi and aLI GO. I will discuss results obtained using the rapid-response systems on th e Arcminute Microkelvin Imager (AMI\; a radio telescope based in the UK) a nd the Murchison Widefield Array (MWA\; based in Western Australia). These experiments are inspiring other telescopes to install similar capabilitie s\, including the Australia Telescope Compact Array (ATCA). I will explain how I plan to use Australian radio telescope to obtain the ealiest observ ations of short-duration gamma-ray bursts. Such observations will provide vital insight into the early-time radio signatures of gravitational wave e vents and contribute invaluable knowledge towards optimising transient sci ence condicted with the Square Kilometre Array. LAST-MODIFIED:20170317T035606Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Gemma Anderson (Curtin University) "Probing extreme astrophysics wi th rapid-response radio telescopes in the SKA era" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20211130T000000Z DTEND:20211130T010000Z DTSTAMP:20261011T152429Z UID:7lgmsva1rpui7lggqmk1ara9ko@google.com CREATED:20211129T012205Z DESCRIPTION:The binary neutron star merger GW170817 was a golden event for multi-messenger astronomy made possible by gravitational wave detection. I t allowed us to gleam an insight into short gamma-ray bursts\, jet formati on and topology\, and r-process nucleosynthesis - but information about th e merger and post-merger phases still remains unbeknown to us. A gravitati onal wave detector with significantly improved sensitivity between 1 - 3 k Hz would allow us to probe the exotic nuclear physics that govern the insi des of neutron stars from their signature in the merger signal. The Austra lian gravitational wave detector concept NEMO builds on the 4 km long dual recycled Fabry-Perot Michelson design of the Advanced LIGO detectors but employs key upgrades to address the need for higher circulating laser powe r. Cryogenically cooled silicon test masses and suspensions\, a longer las er wavelength\, and a long signal recycling cavity are key changes that le ad to a strain sensitivity comparable to third generation GW observatories in the frequency band from 1 to 3 kHz. This talk gives a general overview of gravitational wave detection\, key technological concepts\, the astrop hysical motivation for a kHz-band detector\, and discusses select implemen tation details for NEMO. LAST-MODIFIED:20211129T022609Z LOCATION:ZOOM (host: Lilli Sun\, Sven Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Johannes Eichholz (CGA) "RSAA/CGA Seminar: NEMO: A Kilohertz-Band G ravitational Wave Detector and 3G Pathfinder" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230217T020000Z DTEND:20230217T030000Z DTSTAMP:20261011T152429Z UID:nbf8cnig3v9veostf15350f0o4@google.com CREATED:20230126T012112Z DESCRIPTION:In this seminar I will present some of the results I have obtai ned so far during the course of my PhD. First\, I'll discuss the current b imodal paradigm of galaxy evolution (i.e. star-forming vs passive)\, and w hether galaxies form two physically distinct groups in terms of stellar ma ss and specific star formation rate. Actually\, the existence of a quiesce nt population of galaxies is related to the question: do galaxies (complet ely) stop forming stars? I'll show that observational and theoretical appr oaches might offer different answers. The bimodal picture is often explain ed by means of 'quenching' processes\, that drive the star formation histo ry of galaxies to a halt. The last section of my talk will be devoted to p resent an observational method to discriminate between those systems under going secular (i.e. ageing) and fast evolution (i.e. quenching)\, and its connection with other physical properties. I'll finish the talk providing a summary of the main conclusions and some future prospects. LAST-MODIFIED:20230205T000116Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Pablo Corcho Caballero (Macquarie University) "Ageing and quenching in the local Universe." TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150220T032000Z DTEND:20150220T034000Z DTSTAMP:20261011T152429Z UID:ccc4kqfavg6dfcgij8k1p3liv8@google.com CREATED:20150119T064112Z DESCRIPTION:Dwarf galaxies are amongst the most dark matter dominated stell ar systems in the universe. Our observations of this however\, are based o n kinematic measurements that assume dynamic equilibrium. In this talk I w ill present the results of my first paper\; a detailed analysis of the ste llar substructure surrounding the Hercules dwarf spheroidal galaxy\, demon strating that Hercules is a strongly tidally disrupted system and therefor e not in dynamic equilibrium. LAST-MODIFIED:20150215T230607Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tammy Roderick (RSAA) "Stellar substructures around the Hercules dw arf spheroidal galaxy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250311T000000Z DTEND:20250311T010000Z DTSTAMP:20261011T152429Z UID:lutgv1r7kakh2cdcvrakhaclg4@google.com CREATED:20250106T225616Z DESCRIPTION:The accretion flow onto the 4 million solar mass black hole Sgr A* is fed by the winds of massive stars in the central few parsecs of the Galaxy. As the captured material flows towards the event horizon it emits across the electromagnetic spectrum from radio and sub-millimetre through infrared into X-rays. The emission is variable on time scales from minute s to years (and longer)\, providing valuable information on the physical processes at work in the accretion flow. JWST observations of SgrA* at sev eral epochs in 2023 and 2024 have yielded simultaneous light curves at 2.1 and 4.8 micron with unprecedented sensitivity\, allowing accurate charact erisation of the spectral evolution during flaring events in the infrared. In addition NuSTAR observed a very bright X-ray flare simultaneous with f laring observed in the infrared by JWST. I shall present these new observa tions and the implications for models of the accretion flow. LAST-MODIFIED:20250206T224122Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hiep Nguyen) \nZoom: https ://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mark Wardle (Macquarie U.) "Infrared and X-ray flaring of the Galac tic Centre supermassive black hole Sgr A*" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190801T010000Z DTEND:20190801T020000Z DTSTAMP:20261011T152429Z UID:c50hvqngoci373braj2hkncr38@google.com CREATED:20190702T060508Z DESCRIPTION:TBD LAST-MODIFIED:20190702T060508Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Troels Haugbølle "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251022T023000Z DTEND:20251022T034500Z DTSTAMP:20261011T152430Z UID:6kds950b4ikilhfkmc9n111p0g@google.com CREATED:20251019T225106Z DESCRIPTION:Program: 1:30-1:45pm: Charleze Girdler (supervisor: Luca Casagr ande): Developing a Metallicity Calibration for SkyMapper System using Gai a 1:45-2:00pm Shihai Zhu (supervisor: Yuxiang Qin): Impact on galaxy forma tion considering the bulk velocity between baryons and dark matter 2:00-2: 15pm Sif Svendsgaard (supervisor: Rob Sharp): Reverberation Mapping of AGN 2:15-2:30pm: Alannah Falco (supervisors: Chris Lidman\, Bailey Martin): S earching for Intrinsic Correlations between the Spectral Features of Type Ia Supernovae and Hubble Residuals 2:30-2:45pm: Baochen Tian (supervisor: ChongChong He): A Python Pipeline for Post-processing QUOKKA Radiation-MHD Simulations Abstracts: Title: Developing a Metallicity Calibration for SkyMapper System using Gaia Abstract: This project tested the quality of SkyMapper DR4 uvgriz photometry at deriving stellar metallicities by explo ring metallicity calibration of this data\, leveraging on Gaia photometry \, to derive stellar metallicities and benchmark its performances against spectroscopic surveys. In the end a functional form for metallicity calibr ation was done for giant stars and dwarf stars separately. Title: Impact on galaxy formation considering the bulk velocity between baryons and dark matter Abstract: Bulk streaming between baryons and cold dark matter (vcb ) imprints a spatially varying pressure floor that delays the formation of the first galaxies. We present a reproducible pipeline that constructs co llisionless N-body field and vcb field by compute the linear matter power spectrum and component transfer functions with CAMB and adopted 2LPT initi al conditions via PySCo to improve early-time accuracy. Using a Lbox = 500 Mpc/h volume\, redshifts z = 5-30\, and smoothing scales R = {3\, 20\, 10 0} Mpc\, we compare a global-RMS model to a local patch-wise treatment of vcb. The local model yields coherent\, smoothing scale-dependent\, and red shift-dependent fluctuations in collapsed fraction\, with stronger streami ng velocity induced suppression at larger R and earlier times\, while late r dominated by thermal suppression. The Halo Mass Function (HMF) shows the same result\; suppression in HMF by vcb is ~ 20% - 40% for low mass halo end and insignificant for high mass halo\; and later vanishes at low redsh ift\, which is consistent with our expectation. These results emphasize th at resolving the local structure of vcb is essential for predicting the fo rmation of early galaxies. Title: Reverberation Mapping of AGN Abstract: Reverberation mapping is the technique of measuring the continuum spectrum of an Active Galactic Nuclei and the echoed spectra. This method can be u sed to estimate the masses of the AGN\, however it requires multiple measu rements which can span weeks to months or years. The AGN\, J1910 has been measured since 2023 to study the reverberation. For this project\, an accu rate and more efficient method to handle the spectra has been tested using the PyQSOFit software. Title: Searching for Intrinsic Correlations betwe en the Spectral Features of Type Ia Supernovae and Hubble Residuals Abstra ct: Investigating sources of intrinsic scatter in the distance modulus res iduals following standardisation of Type Ia Supernovae (SNe Ia) is key to improving their precision as distance indicators in observational cosmolog y. In this talk\, I will discuss the findings from the investigation into intrinsic correlations between the Si II velocity of SNe Ia and Hubble Res iduals\, using data from the Dark Energy Bedrock All-Sky Supernovae (DEBAS S) program. In particular\, I will explore the presence of such a correlat ion when applying standard corrections for SN colour and light curve width as well with an additional correction for the correlation between Hubble Residuals and host galaxy mass. Title: A Python Pipeline for Post-process ing QUOKKA Radiation-MHD Simulations Abstract: This project introduces a n ew Python pipeline designed to post-process simulation data from the GPU-a ccelerated radiation-magnetohydrodynamics code\, QUOKKA. The primary goal is to bridge the gap between theoretical simulations and astronomical obse rvations by generating synthetic observational data from the simulation ou tputs. Our pipeline uses the yt library for handling large datasets and th e DESPOTIC package to calculate the gas's chemical and thermal state. This tool will enable direct comparisons with real-world telescope data\, prov iding a powerful method to validate the physical models used in the simula tions. LAST-MODIFIED:20251019T225106Z LOCATION:Duffield Lecture Theatre and ZOOM (host: Helmut Jerjen) \nZoom: ht tps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:ASTR3005 Students "ASTR3005 Individual Research Projects Seminar" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160526T010000Z DTEND:20160526T020000Z DTSTAMP:20261011T152429Z UID:j6smqc3cqkk6msvae7gkhv14mk@google.com CREATED:20160324T071120Z DESCRIPTION:Unconscious or implicit bias is proliferating as a topic of int erest within scholarly research and social policy\, and within public disc ourse. Unconscious bias has been linked with a wide range of social issues including employment\, policing and criminal justice\, education\, health and healthcare\, housing and public transport\, and to experiences and ou tcomes for a diverse range of groups related to gender\, age\, sexual orie ntation\, ethnicity\, migration status\, socioeconomic position\, disabili ty. However\, despite its growing popularity\, measuring unconscious bias and its resultant effects remains less well understood\, with knowledge of effective interventions to counter unconscious bias even more limited. Th is seminar will provide an overview of the best available evidence regardi ng measuring and addressing unconscious bias and explore implications for de-biasing initiatives at individual and organisational levels. There will be opportunity for discussion of implications of this evidence for univer sity and research contexts. LAST-MODIFIED:20160517T045606Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Naomi Priest (ANU) "Understanding and addressing unconscious bias: Complexities\, challenges and opportunities" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190829T010000Z DTEND:20190829T020000Z DTSTAMP:20261011T152429Z UID:o7jmunk38o3tet11otqh4782lo@google.com CREATED:20190801T043614Z DESCRIPTION:Magnetic fields pervade the interstellar medium (ISM) of the Mi lky Way. These fields interact with various components within the ISM\, l ocking in to the ionised phases of the ISM\, forming the magneto-ionic med ium. This medium is responsible for a significant input of energy into the ISM. The study of magnetic fields in the ISM of the Milky Way is therefor e critical to understanding the energetics and evolution of the Galaxy. My thesis investigates magnetic fields in the Galaxy\, and how they interact with a variety of ISM structures. I will present results of all-sky diffu se radio polarimetry made with the Parkes 64m Telescope. Considerable effo rt has recently been made in the observation of diffuse polarized emission across the entire sky. Polarized radio emission carries a wealth of infor mation on the magneto-ionic medium. Linearly polarized waves experience Fa raday rotation as they propagate through the magneto-ionic medium of the M ilky Way. Further\, the Galaxy itself is a significant source of polarized emission via synchrotron radiation. In combination with measurements of a dditional ISM tracers\, I have used these observations to unravel the magn eto-ionic properties of the Galactic ISM. As we enter the SKA era\, unders tanding how to best utilise and understand these data will be key to solvi ng the mysteries of cosmic magnetism. LAST-MODIFIED:20190823T033609Z LOCATION:Duffield Lecture Theatre (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alec Thomson (RSAA) "Unravelling the magneto-ionic fabric of the Mi lky Way Galaxy (End-of-Thesis Colloquium)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240913T040000Z DTEND:20240913T043000Z DTSTAMP:20261011T152429Z UID:p6i25qj3g4c9fess1dgk903850@google.com CREATED:20240709T235624Z DESCRIPTION:Update on the current status of Astronomy Australia Ltd. LAST-MODIFIED:20240709T235624Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Stu Wyithe (RSAA) "AAL update" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191024T000000Z DTEND:20191024T010000Z DTSTAMP:20261011T152430Z UID:4t2sa86vgvuvm094n64eh1aua0@google.com CREATED:20191017T013108Z DESCRIPTION:In the unified model of active galactic nuclei (AGNs)\, blazars are of a special subclass whose relativistic jets point towards us\, cha racterized by its violent variation. The variation mechanism of blazars is still in debate. In this talk\, I will present a case study on PKS 1502+1 06. For this target\, we obtained the correlations between light curves at different frequencies. The time lag estimation enables us to derive the l ocation of optical and gamma-ray emission regions relative to the radio in jet. A significant correlation between polarization and fluxes is also ob tained. We also proposed that the curved jet model can explain the variati on in flux\, spectral index and polarization in a unified manner. Then\, I will present the theoretical frame work\, and discussed the scaling law of spectral index\, and its application in GRB etc. LAST-MODIFIED:20191023T060604Z LOCATION:Duffield Lecture Theatre (host: Francis) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Yunguo Jiang (Shandong University) "A study on the emitting regions and the variation mechanism of blazars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200924T010000Z DTEND:20200924T013000Z DTSTAMP:20261011T152429Z UID:q1a9pqr7cc503gofpik4hjkt7c@google.com CREATED:20200906T090609Z DESCRIPTION:TBD LAST-MODIFIED:20200906T090609Z LOCATION:ZOOM 997 8534 1005 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dávid Guszejnov (UT Austin (USA)) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210813T040000Z DTEND:20210813T043000Z DTSTAMP:20261011T152430Z UID:tmggeamh2ratittv5pmrbqlq2c@google.com CREATED:20210713T033610Z DESCRIPTION:The Feast-of-Facts are an informal open-mic format from RSAA me mbers for RSAA members. LAST-MODIFIED:20210730T033108Z LOCATION:DLT and ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Phil Taylor (RSAA) "Sustainability Myths and Misconceptions" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160506T040000Z DTEND:20160506T042000Z DTSTAMP:20261011T152429Z UID:8m5musdf3j58tcm0rco1tvolps@google.com CREATED:20160228T234118Z DESCRIPTION:Next week the 61st Eurovision Song Contest will be held in Stoc kholm! This is something very close to my heart and I thought that I would talk about the history of Eurovision and how important it is for European cultural dynamics. I will then briefly summarise three sociological paper s that deal with concepts of "European" identity\, presenting national ide ntity through the contest\, LGBTIQ+ rights and movements\, and perception of the east/west divide within Europe - all through the lens of the Eurovi sion Song Contest. I will also be holding a Eurovision party this year on Friday 13th May. Everyone is invited. Bring some food or drink from your f avourite country. Address will be announced at my talk or email me later. LAST-MODIFIED:20160506T022105Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rajika Kuruwita (RSAA) "Political Science through the lens of Eurov ision" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250211T000000Z DTEND:20250211T010000Z DTSTAMP:20261011T152429Z UID:f240f3fs5p5nh1q5v2mshusrdk@google.com CREATED:20250106T225608Z DESCRIPTION:Understanding dark matter and dark energy\, which make up 95% o f the Universe\, requires cosmological surveys to achieve percent-level pr ecision. Yet\, this precision reveals tensions between observations and th e standard cosmological model\, potentially stemming from systematic biase s. CLONES (Constrained LOcal & Nesting Environment Simulations) are digita l twins of the local Universe designed to replicate our cosmic environment and tackle these challenges. Highlighting key cosmological tensions and s howcasing a few example studies of these CLONES will demonstrate how they can offer a powerful framework for bias-free analyses\, advancing our unde rstanding of galaxy evolution and large-scale structure formation. LAST-MODIFIED:20250119T225110Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Matthew Colless) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jenny Sorce (CNRS-Lille) "CLONES: Digital Twins of the Local Univer se for Bias-Free Inference" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20211028T003000Z DTEND:20211028T020000Z DTSTAMP:20261011T152429Z UID:flpss1i0cl1cihv5eqa8v124fk@google.com CREATED:20211018T005106Z DESCRIPTION:Schedule: 11:30-11:45am: Erin Holdorf Title: Searching for Gia nt Planets in Wide Orbits Within 30 pc Abstract: This speech will describ e how planetary orbits were simulated for FGK stars to determine the numbe r of expected detections of exoplanets in wide orbits and was then compare d to the number of stars that have excess proper motion in Gaia EDR3. --- -------- 11:45-12:00am: Jennifer Jang Title: Studying the impact of weat her on the DREAMS survey Abstract: The Dynamic REd All-Sky Monitoring Su rvey (DREAMS) is the Infrared time-domain telescope to be examining the So uthern hemisphere for the first time\, built by ANU astronomers. In this p roject\, we have studied the weather impact of the DREAMS telescope and sa w if there exists a way to optimize the survey. Examining behaviors of cad ence plots\, through the prioritization method alternation\, we have concl uded that there is indeed a possibility. And furthermore\, if the cadence plot behaviors are studied and well understood\, the DREAMS surveys can be more optimized from where it is now. ----------- 12:00-12:15pm: Isaac K anowski Title: Spectroscopic Identification of Strong Gravitationally Len sed Images Abstract: This talk will describe the process of locating high redshift\, strong gravitationally lensed images in MAGPI data. To be able to identify these galaxy-like emission sources within the data cubes\, th e foreground galaxies which acts as lenses must first be modelled and remo ved. The method used for this removal and identification of sources will b e discussed\, as will the galaxies that have been detected as a result. - ---------- 12:15-12:30pm: Hannah Loiterton Title: Quantifying properties of planet-host stars using a catalogue of stellar parameters from SkyMapp er and Gaia DR2. Abstract: The properties of exoplanets and their correla tions with host stars are known to be critical in gaining more informed in sights on the process of planet formation. In this study\, I have cross-ma tched stellar parameters derived from the SkyMapper survey against the NAS A exoplanet archive\, with the goal of exploring how exoplanet frequency a nd properties vary across stars with different stellar parameters. Some pr eliminary results are presented. ----------- 12:30-12:45pm: Bailey Marti n Title: Influences on the Line-by-Line Elemental Abundance Measurements of the GALAH Survey Abstract: To unravel the mysteries of our Milky Way d own to the small details\, we need stellar measurements\, such as elementa l abundances\, with outstanding accuracy and precision. The measurement of elemental abundances from spectra is subject to a variety of parameters. Previously these influences have been analysed independently. We provide a n analysis of these parameters in a combined fashion\, to determine whethe r there are any inherent correlations between them. Our analysis covers th e correlations of microturbulence and Barium abundance as well as the infl uence of technical parameters like spectral resolution\, spectrum normalis ation and the mapping of CCD pixels to wavelengths. ----------- 12:45-13 :00pm: Holly Robinson Title: ISM Temperature and Density of a Single Star HII Region Abstract: Using data from the KOALA integral field unit on th e Anglo-Australian Telescope\, we calculate the ISM temperature and densit y of a single star HII region\, N81\, located in the Small Magellanic Clou d. We utilize PyNeb to perform these measurements for an individually reso lved HII region. We then compare the expected flux from strong emission li nes such as hydrogen alpha to measure the radial temperature and density s tructure within an HII region. LAST-MODIFIED:20211027T233110Z LOCATION:ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:ASTR 3005 Students (RSAA) "ASTR 3005 presentations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261117T000000Z DTEND:20261117T010000Z DTSTAMP:20261011T152430Z UID:ini59bhe28m8ql40jbsng73of0@google.com CREATED:20260615T020029Z DESCRIPTION:TBC LAST-MODIFIED:20260716T070027Z LOCATION:Zoom or Duffield Lecture Theatre (host: Emily Wisnioski) \nZoom: h ttps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Benedetta Vulcani (INAF) "TBC" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241217T000000Z DTEND:20241217T010000Z DTSTAMP:20261011T152429Z UID:rrskunfsr5vn1qd5sce06lurp0@google.com CREATED:20241017T015119Z DESCRIPTION:In this colloquium I will cover two topics: (1) The first part of the talk will cover the measurement of optical emission lines in multip le locations across the Large and Small Magellanic Clouds using the Austra lian National University 2.3-metre telescope and the WiFeS integral field spectrograph. From these measurements maps of the gas phase metallicity\, extinction\, Halpha radial velocity\, and Halpha velocity dispersion have been made for both Clouds. The optical radial velocity and velocity disp ersion maps have been compared to neutral atomic hydrogen (HI) gas maps of the Clouds. The maps provided in this work show details not accessible i n the study of more distant dwarf galaxies. (2) The second part of the tal k will deal with giant low surface brightness galaxies (gLSBs). These are galaxies that have extremely extended\, faint\, optical disks and high tot al dark matter masses. The existence of such galaxies is problematic for the current model of galaxy formation\, since the major mergers responsibl e for the large total mass would likely have destroyed the large optical d isk. A pilot sample of optically selected gLSBs have been observed in the radio to quantify various properties from their neutral atomic hydrogen g as\, including their HI mass and asymmetry. These observations shed light on the formation mechanisms for these galaxies. LAST-MODIFIED:20241216T010607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Matthew Colless) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Philip Lah (NYU Abu Dhabi) "Emission Line Maps of the Large and Sma ll Magellanic Clouds\, and HI Observations of Giant Low Surface Brightness Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231024T000000Z DTEND:20231024T013000Z DTSTAMP:20261011T152429Z UID:bc3uutpdtncc10rhcvq1uqit0s@google.com CREATED:20230917T235114Z DESCRIPTION:Understanding how chemical elements are distributed in time and space across the universe is a major question in Astrophysics\, and one o f the key goals of the ARC Centre of Excellence ASTRO 3D. I'll summarise m y team's recent efforts in tracing the elements in the early universe usin g ESO/VLT via the XQR-30 survey of intervening metal absorbers towards z~6 quasars. With the benefit of the long lever arm from z=1.9 to 6.4\, high sensitivity\, resolution and significant number statistics\, we can make i nroads. Strong MgII absorbers trace the global star formation rate density \, in contrast to the incidence of weak MgII in the Circumgalactic Medium (CGM) that remains remarkably flat across cosmic time. Metals ions trace b oth chemical enrichment and the ionization state of the CGM. I'll show how a decline in CIV\, coupled with a rise in CII and OI complements current evidence for a late reionization continuing to occur in metal-enriched and therefore biased regions of the Universe. Finally\, in direct comparison with JWST\, I will demonstrate why medium resolution ground-based spectros copy is essential for a complete census of the high z CGM. LAST-MODIFIED:20231019T131106Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hiep Nguyen) \nZoom: https ://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Emma Ryan-Weber (Swinburne U.) "The Chemical Evolution and Reioniza tion of Galaxy Halos" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230613T010000Z DTEND:20230613T020000Z DTSTAMP:20261011T152429Z UID:655brhh8snfvbqlg8ka3pdggk8@google.com CREATED:20230605T005608Z DESCRIPTION:Star-forming galaxies are a copious source of non-thermal radia tion which spans over 20 dex in energy\, from ultra-high energy gamma-rays at PeV scale down to radio emission at ueV energies. Most of this emissio n derives from energy losses of cosmic rays that pervade the interstellar medium. In this work we show how a galaxy model that requires only few inp ut parameters that are easily observed\, even for high redshift objects\, and some basic\, run-of-the-mill\, assumptions is sufficient to reproduce their non-thermal spectra. We then utilise this knowledge to derive the co ntribution star-forming galaxies make to the diffuse isotropic gamma-ray b ackground\, explain the origin of the far-infrared radio correlation and s imultaneously obtain radio spectral indices that match observation. LAST-MODIFIED:20230611T225106Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Takafumi) \nZoom: https:// anu.zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Matt Roth (RSAA) "Non-thermal emission from star-forming galaxies ( End of Thesis Talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171116T000000Z DTEND:20171116T010000Z DTSTAMP:20261011T152430Z UID:ahotdu59q6cgahadi5vmsti8jk@google.com CREATED:20170919T011111Z DESCRIPTION:A key missing piece in a predictive theory of star formation is the link between scales of individual stars and star clusters up to the s cales of entire galaxies. LEGUS\, a HST Treasury program of 50 nearby gala xies imaged at UV and optical wavelengths\, is now providing us the inform ation to test the overall organization and spatial evolution of star forma tion. I will present my latest findings of using star clusters from LEGUS combined with millimeter observations to trace the hierarchy of the entire star-forming process to improve our understanding of the evolution of sta r formation\, stellar populations\, and the natal molecular gas in galaxie s. LAST-MODIFIED:20171024T175114Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kathryn Grasha (UMass) "Hierarchical Star Formation Across Space an d Time with Star Clusters" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190517T040000Z DTEND:20190517T043000Z DTSTAMP:20261011T152429Z UID:isppmhsb4sgembqr5l84vhnoes@google.com CREATED:20190429T035107Z DESCRIPTION:At 2010\, the presence of two red clumps (RCs) has been discove red in the high-latitude fields of the Milky Way bulge from 2MASS and OGLE surveys. This double RCs are widely accepted as evidence for a giant X-sh aped structure originated from the bar instability. We suggested\, however \, a drastically different interpretation based on the multiple stellar po pulation phenomenon as is observed in globular clusters (GCs)\, where the bright RC is from He and Na enhanced second-generation stars\, while the f aint RC is representing first-generation stars with normal abundances. Bec ause these two scenarios imply very different pictures of the formation of the bulge\, understanding the origin of the double RC is of crucial impor tance. As supporting evidence for multiple population scenario\, here we r eport our discovery that the stars in the two RCs show a significant diffe rence in CN-band strength. In addition\, we found that the red giant branc h stars in the outer bulge ( > 5.5° from the Galactic center) are divided into two groups according to Na abundance in the [Na/Fe] - [Fe/H] plane. Since these chemical patterns and characteristics are only explained by st ars originated in GCs\, this is evidence that the double RC is due to the multiple population phenomenon\, and that the outer bulge was mostly assem bled from disrupted proto-GCs in the early history of the Milky Way. LAST-MODIFIED:20190509T011105Z LOCATION:Duffield Lecture Theatre (host: Oh) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dongwook Lim (Yonsei University) "The origin of the double red clum p in the Milky Way bulge" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191212T000000Z DTEND:20191212T010000Z DTSTAMP:20261011T152429Z UID:oh2d20bq01g46v8na4qggcrvi0@google.com CREATED:20191022T041213Z DESCRIPTION:We have used two methods to search for surviving companions of Type Ia SN progenitors in five Balmer-dominated SN remnants (SNRs) in the Large Magellanic Cloud: 0509-67.5\, 0519-69.0\, N103B\, DEM L71\, and 0548 -70.4. In the first method\, we use the Hubble Space Telescope photometric measurements of stars to construct color-magnitude diagrams (CMDs)\, and compare positions of stars in the CMDs with those expected from theoretica l post-impact evolution of surviving main sequence or helium star companio ns. In the second method\, we use Multi-Unit Spectroscopic Explorer (MUSE) observations to carry out spectroscopic analyses of stars in order to use large peculiar radial velocities as diagnostics of surviving companions. In both methods\, we find stars with unexpected behaviors that could be ca ndidates of surviving companions of the SN progenitors. LAST-MODIFIED:20191210T032604Z LOCATION:Duffield Lecture Theatre (host: Tang) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Chuan-Jui Li (ASIAA) "Search for Surviving Companions of Progenitor s of Young LMC Type Ia Supernova Remnants" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250604T033000Z DTEND:20250604T054500Z DTSTAMP:20261011T152429Z UID:u86328smtalqs6u13o9i9kqhck@google.com CREATED:20250603T021106Z DESCRIPTION:End of thesis talks by honours and masters students LAST-MODIFIED:20250622T062708Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Chris Wolf) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Honours and Masters Students (RSAA) "Honours and Masters End-of-The sis Talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150717T042000Z DTEND:20150717T044000Z DTSTAMP:20261011T152429Z UID:qm3lgg2n03l8bkrjb2mhq0q7a8@google.com CREATED:20150703T070108Z DESCRIPTION:TBD LAST-MODIFIED:20150709T092607Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Bonnie Zhang (RSAA) "Annual Thesis Talk" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260827T010000Z DTEND:20260827T020000Z DTSTAMP:20261011T152430Z UID:or0p4i1chl8k4c63nf5re8nst0@google.com CREATED:20260503T114413Z DESCRIPTION:Adaptive optics is a technology used in fields such as astronom y to mitigate the effects of atmospheric turbulence. To achieve this\, the phase of the incoming wavefront is corrected in real time. Two key compon ents in this correction are the wavefront sensor and guide star. The wavef ront sensor generates a signal that allows for the phase of the wavefront to be estimated. In strong scintillation conditions\, commonly used slope- based wavefront sensors have a large degradation in performance. The guide star is the source used to estimate the phase of the science target. Lase r guide stars were developed to increase the fraction of the sky where ada ptive optics can be used. However\, due to laser guide star tip-tilt indet ermination\, 100% sky coverage is still not achievable. In this EoT talk I will investigate the use of an interferometric wavefront sensor with mach ine learning in the high scintillation regime in simulations and lab bench testing. I will also investigate the use of non-homogeneities in the sodi um layer as a potential methodology for laser guide star tip-tilt estimati on. LAST-MODIFIED:20260820T020008Z LOCATION:Zoom or Duffield Lecture Theatre (host: Noelia Martinez) \nZoom: h ttps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Erin Holdorf (RSAA) "Machine Learning Enhanced Wavefront Sensing fo r Laser Guide Stars in Strong Scintillation (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240926T010000Z DTEND:20240926T020000Z DTSTAMP:20261011T152429Z UID:15tvrmcm65rvh0pfmb642d3rkg@google.com CREATED:20240305T110642Z DESCRIPTION:My research centers on understanding the origin of the initial mass function (IMF)\, which is the mass distribution of stars in a young c luster. I perform a comprehensive parameter study of the IMF using magneto hydrodynamical (MHD) simulations of star cluster formation. The simulation s incorporate gravity\, turbulence\, magnetic fields\, protostellar heatin g\, and mechanical feedback via jets and outflows. With my work\, I conclu sively demonstrate that integrating all these mechanisms simultaneously in simulations is crucial since each of them has an individual effect on the characteristics of the IMF. I show that the inclusion of protostellar out flows in simulations increases the number of stars formed\, while lowering the median mass and star formation rate by a factor of ~ 2. Furthermore\, I observe that the mode of turbulence driving has a key part in shaping t he form of the IMF\, where a purely compressive turbulence driving (curl-f ree) produces a higher fraction of low mass stars as compared to a purely solenoidal driving (divergence-free). My work also reveals that the IMF ex hibits a weak dependence on the cloud virial parameter\, the ratio of the kinetic energy to potential energy\, which is another important cloud prop erty related to turbulence. I propose that the scatter in the IMF characte ristics observed in the Milky Way is a consequence of the variations in th e environmental conditions like the turbulence driving and the virial para meter. The large suite of simulations I conducted also provided substantia l data to analyse various binary properties of stars with robust statistic al significance. I find that the turbulence properties such as the mode of driving have a considerable impact on the stellar multiplicity and orbita l eccentricity. LAST-MODIFIED:20240918T130108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Christoph Federrath) \nZoo m: https://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sajay Mathew (RSAA) "The Turbulent Origin of the Initial Mass Funct ion (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171030T000000Z DTEND:20171030T010000Z DTSTAMP:20261011T152429Z UID:k2e7pecl2hh0cdoakq8p75ls5c@google.com CREATED:20171019T064608Z DESCRIPTION:The orbital parameters of binary stars at intermediate periods (100-1000 d) are difficult to measure with conventional methods and are ve ry incomplete. For the past couple of years I’ve been developing a metho d that uses stellar pulsations to determine the orbital parameters of bina ry stars\, which is particularly suited to intermediate periods and can de tect objects down to planetary masses. It has tripled the number of interm ediate-mass stars with fully solved binary orbits. The detected companions include planets\, brown dwarfs\, and main sequence stars with masses betw een 0.1 and 2.5 Msun\; over 20% are white dwarfs in blue straggler systems \, and a few companions could be neutron stars or black holes. Some system s are clear triples\, and many will become Type Ia supernovae and related phenomena. Statistically robust mass-ratio and eccentricity distributions will be presented\, and I will explain what they tell us about binary star formation. LAST-MODIFIED:20171024T163608Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Simon Murphy (University of Sydney) "An exciting haul of planetary\ , binary and triple systems from pulsation timing" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170406T010000Z DTEND:20170406T020000Z DTSTAMP:20261011T152430Z UID:6i7raa9trv8lbsnh7lq77vud2s@google.com CREATED:20170317T020609Z DESCRIPTION:One of the most pressing issues in the Lambda cold dark matter (CDM) paradigm is the ''plane of satellite'' problem: the distribution of observed Milky Way satellite galaxies appears to form a thin polar plane\, which is largely inconsistent with the prediction of the Lambda-CDM model \, i.e. an isotropic distribution of dark matter sub-halos. This problem w as often seen as a consequence of observational biases because many of pre viously known satellite galaxies were discovered in the Sloan Digital Sky Survey whose survey footprint initially focused on the northern Galactic p ole region. Subsequent wide-field surveys to map the southern sky were thu s required for an unbiased observational assessment of the standard cosmol ogical model. I present the discovery of five new low-luminosity Milky Wa y companions from the Sloan Digital Sky Survey\, Dark Energy Survey\, and Stromlo Milky Way Satellite survey project: two dwarf spheroidal galaxies (Pegasus III & Horologium II) and three star clusters (Kim 1--3). Both Peg asus III and Horologium II\, as well as the majority of new dwarf satellit e galaxies discovered by other recent studies\, turn out tightly aligned w ith the original plane of satellites defined by previously known satellite galaxies. This result confirms the presence of the plane of satellites th roughout the whole sky\, which largely conflicts with the previous predict ion\, and thus calls for a reexamination of the current standard cosmologi cal model. LAST-MODIFIED:20170329T100106Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dongwon Kim (RSAA) "Search for Ultra-faint Milky Way Satellites - E nd of thesis colloquium" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240927T010000Z DTEND:20240927T020000Z DTSTAMP:20261011T152429Z UID:m8o08mc8107t7deubmoin35jns@google.com CREATED:20240829T011120Z DESCRIPTION:The cosmic evolution of galaxies and supermassive black holes ( SMBHs) is believed to be correlated through interlinked physical processes . However\, two aspects of the galaxy-BH correlation remain unclear: the f ueling of actively accreting black holes (called Active Galactic Nuclei or AGNs) and the physical process of AGN feedback. Previous attempts to answ er these questions using single-aperture spectra of galaxies have fallen s hort\, as they can only consider the dominant excitation source in the spe ctrum and cannot rule out the involvement of other excitation sources such as supermassive black holes\, star formation\, and shock excitations. In this thesis\, we present a novel solution to separate the mixing mechanism s in galaxy spectra analysis: a new theoretical three-dimensional (3D) dia gram that can simultaneously separate star formation\, AGN\, and shocks in galaxies with integral field spectroscopy (IFU) data. This new 3D diagram incorporates the most up-to-date and self-consistent theoretical models f or HII regions\, AGN narrow-line regions\, and the time-dependent shocks a nd precursor models. The inclusion of theoretical models in the new 3D dia gram independently constrains the parameter space for each mechanism and p rovides information on the gas metallicity\, ionization states\, and shock velocity along with the separation. By applying this new 3D diagram\, we obtain detailed maps of the mechanism distribution\, gas metallicity\, and ionization states for individual galaxies in nearby active galaxies in th e S7\, SAMI\, and MaNGA surveys. With these results\, we study how the con tribution and spatial distribution of each power source change with the en vironment\, stellar mass\, and merger stages for the galaxies in mergers. This research shines a new light on the study of galaxy evolution\, especi ally its coevolution with the growth of the central black hole. LAST-MODIFIED:20240917T005111Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Peixin Zhu (RSAA) "Separating star formation\, AGN\, and Shocks in Active Galaxies (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171130T220000Z DTEND:20171201T060000Z DTSTAMP:20261011T152429Z UID:795kro566cb2vd15ri1eimkc40@google.com CREATED:20170811T014115Z DESCRIPTION:Mt. Stromlo Student Seminars LAST-MODIFIED:20171120T233110Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mt. Stromlo Student Seminars (ANU) "Mt. Stromlo Student Seminars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160219T030000Z DTEND:20160219T032000Z DTSTAMP:20261011T152429Z UID:atsva7nr64lotrl0afi642obss@google.com CREATED:20160218T005605Z DESCRIPTION:TBD LAST-MODIFIED:20160218T040606Z LOCATION:Duffield Lecture Theatre (host: Francis Bennet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Robert Ward (ANU) "Observation by Advanced LIGO of gravitational wa ves from a binary black hole merger" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240917T010000Z DTEND:20240917T020000Z DTSTAMP:20261011T152429Z UID:brqcrfov4t3v1e3p2pmkijm8dc@google.com CREATED:20240527T020646Z DESCRIPTION:We're excited to finally be able to show the supernova cosmolog y results from the completed Dark Energy Survey. We observed for 6 years with a custom-built camera on the CTIO-4m telescope in Chile\, and followe d-up with spectra from the Anglo-Australian Telescope. This produced a br and new sample of ~1500 type Ia supernova\, which approximately quintuples the cosmology-quality high-redshift (z > 0.5) supernovae in the literatur e. We find tight constraints on dark energy and dark matter and see tantal ising hints that the equation of state of dark energy may change with time . This amazing data also allowed us to detect gravitational lensing magni fication of the supernovae (which gives information on the shape of dark m atter haloes) and make a beautifully precise measurement of time dilation due to the expansion of the Universe. LAST-MODIFIED:20240913T032109Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tamara Davis (U. Queensland) "Supernova cosmology with the complete Dark Energy Survey" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200722T230000Z DTEND:20200723T064000Z DTSTAMP:20261011T152429Z UID:v91i9ifbgb03nov5hl3gepeeu0@google.com CREATED:20200708T235208Z DESCRIPTION:James Dempsey (9:00-9:20)\, Sarah McIntyre (9:20-9:40)\, Piyush Sharda (9:40-10:00)\, Morning Tea (10:00-11:00)\, Lara Cullinane (11:00-1 1:20)\, Umang Malik (11:20-11:40)\, Josephine Munro (11:40-12:00)\, Jack L ivingston (12:00-12:20)\, Lunch Break (12:20-13:00)\, Jonah Hansen (Propos al Talk 13:00-13:30)\, Georgina Taylor (13:30-13:50)\, Tania Barone (13:50 -14:10)\, James Beattie (Proposal Talk 14:10-14:40)\, Harrison Abbot (14:4 0-15:00)\, Afternoon Tea (15:00-15:30)\, Lyla Jung (Proposal Talk 15:30-16 :00)\, Jen Kammerer (16:00-16:20)\, Arthur Puls (16:20-16:40) LAST-MODIFIED:20200722T035607Z LOCATION:ZOOM 997 8534 1005 (host: Travouillon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA HDR Students (RSAA) "HDR Student Annual Reviews" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240725T030000Z DTEND:20240725T060000Z DTSTAMP:20261011T152429Z UID:bi488nvm2t7aavgopuro2usgd4@google.com CREATED:20240708T024208Z DESCRIPTION:This town hall will be an opportunity for in-person participati on in the process of drafting the 2025 Decadal Plan for Australian Astrono my. The chair of the decadal plan committee and current president of the N ational Committee for Astronomy\, Professor Virginia Kilborn (Swinburne)\, and representatives of all of the working groups within the committee\, w ill be at Mount Stromlo in-person to provide a status update\, present som e highlights of the work completed so far\, and solicit feedback. There wi ll be ample opportunities for discussion\, and all staff and students are encouraged to attend. LAST-MODIFIED:20240708T024208Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Decadal Plan Working Groups (Various) "Decadal Plan In-Person Town Hall" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190516T010000Z DTEND:20190516T013000Z DTSTAMP:20261011T152429Z UID:mg9keu5g8s7r7i9jnn1u0hkap4@google.com CREATED:20190501T005107Z DESCRIPTION:The results from the ANU/RSAA Staff Survey will be presented. A ll staffs are encouraged to attend. LAST-MODIFIED:20190501T005107Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:ANU/RSAA Staff Survey (RSAA) "ANU/RSAA Staff Survey" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190524T040000Z DTEND:20190524T043000Z DTSTAMP:20261011T152429Z UID:69vm1tvsp13055s5s3ffupb7d0@google.com CREATED:20190408T023610Z DESCRIPTION:Future Adaptive Optics (AO) systems aim at delivering sharper a nd more uniform image quality among wider Field of View (FoV) in short wav elengths. The concept of Multi Conjugate Adaptive Optics (MCAO) makes this possible by using multiple guide stars and deformable mirrors. Generating an optimal tomography algorithm that minimizes the impact of various erro r sources is one of the most critical parts in the development of future A O systems. The first Visible band AO facility\, MCAO Assisted Visible Imag er and Spectrograph (MAVIS)\, is proposed to achieve 15% Strehl Ratio amon g 30” square FOV. In this thesis proposal talk\, I will introduce the pl anned work during my PhD on the tomography algorithm for MAVIS as well as other future MCAO systems in general. In particular\, the three stages of my thesis project are: 1.) End-to-end simulations for the estimation of MA VIS performance\, 2.) Tomography algorithm optimization with Learn and App ly method\, Predictive Control and other noise suppression methods\, 3.) D emonstrating experiments on AITC Optics Test Bench. LAST-MODIFIED:20190520T093605Z LOCATION:Duffield Lecture Theatre (host: Zhang) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Hao Zhang (RSAA) "Laser Tomography in High-order Adaptive Optics: P redictive Control and Reconstructor Optimization (Thesis proposal talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180524T010000Z DTEND:20180524T020000Z DTSTAMP:20261011T152429Z UID:jclcqujil5he7cr4asv6c6ss0s@google.com CREATED:20180410T235617Z DESCRIPTION:The birth of galaxies represents the last unexplored frontier o f cosmic history and it is commonly believed such early systems led to the transformation of neutral gas in the intergalactic medium into its presen tfully-ionized state. Some progress has been made in charting the demograp hics of early galaxies into the era when reionization is thought to occur\ , but little is known about their nature of their stellar populations\, th e possible role of active nuclei and whether galaxies are capable of gener ating sufficient ionizing radiation. Spectroscopy holds the key to address ing these questions\, targeting both individual sources at high redshiftas well as carefully-chosen analogs at intermediate redshift. I will describ e the recent progress and challenges as we anticipate the launch of JWST a nd the arrival of next-generation large telescopes. LAST-MODIFIED:20180513T082611Z LOCATION:Duffield Lecture Theatre (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Richard Ellis (UCL) "Early Galaxies and Cosmic Reionization: Progre ss and Challenges" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161124T000000Z DTEND:20161124T010000Z DTSTAMP:20261011T152429Z UID:c0b27um8lgllqclplcq8m9lcq4@google.com CREATED:20161019T230110Z DESCRIPTION:Massive galaxies at high redshift are fed gas from the cosmic w eb by narrow\, dense streams of cold gas\, penetrating supersonically thro ugh hot\, dilute halos. This source of gas is the main driver for star for mation in massive galaxies and also affects the conditions in the intergal actic medium (IGM). The interaction of the cold stream with the hot backgr ound of the halo may result in heating\, dissipation and fragmentation of the stream\, potentially affecting clumping\, accretion and SF\, as well a s producing direct observational signatures for cold streams and their bre akup. As part of a larger campaign to study these effects\, we consider th e supersonic Kelvin-Helmholtz Instability (KHI) at the stream-background b oundary. Linear analysis of the problem (https://arxiv.org/abs/1606.06289) reveals that cosmic cold streams can be susceptible to both surface and b ody modes of KHI and that perturbations are likely to become nonlinear bef ore the stream reaches the galaxy at the halo center. Hence\, we turn our attention to the nonlinear stage of KHI. In the nonlinear stage\, surface modes evolve into a turbulent shear layer. Using numeric simulations in RA MSES and simple analytic models\, we study the growth of this perturbed la yer under typical conditions for a supersonic\, cold and dense stream flow ing through a hot\, dilute background. Our preliminary results indicate th at sufficiently narrow streams\, with a diameter smaller than a few percen t of the virial radius\, can be completely disrupted by KHI before reachin g the galaxy. In this talk\, I will describe the linear and nonlinear stag es for the different modes of KHI\, and relate these general results to th e specific scenario of cold streams feeding galaxies. LAST-MODIFIED:20161123T003104Z LOCATION:Duffield Lecture Theatre (host: Enrico Di Teodoro) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dan Padnos (Hebrew University of Jerusalem) "Kelvin-Helmholtz Insta bility of Cold Streams in Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210914T010000Z DTEND:20210914T020000Z DTSTAMP:20261011T152429Z UID:fqr6qkalmkb7viaugld2g1o2u4@google.com CREATED:20210826T043108Z DESCRIPTION:The third LIGO/Virgo observational campaign was very fruitful o bservations from a gravitational wave (GW) standpoint. But from the point of view of other multi-messenger observers\, we have no plausible electrom agnetic (EM) counterparts associated with the merger of compact binaries. SkyMapper is a good example of how CGA's joint efforts work in practice an d why it is important to overcome challenges before the O4 run. In this ta lk\, as an important use-case of our robotic facility\, we describe our fo llow-up strategy and current tools that can maximize success on the upcomi ng race from early kilonova discovery to rapid EM follow-up of GW events o ut to around 200 Mpc distance. To better reflect lessons learned from the O3 run\, we present the analysis on the real SkyMapper data for the second binary neutron star merger GW190425 (known in Australia as ANZAC Day even t). We will close with an outlook to future work and the O4 run. LAST-MODIFIED:20210826T043108Z LOCATION:ZOOM (host: Sven Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Seo-Won Chang (RSAA/CGA) "Joint RSAA+CGA Seminar: Preparation for t he advanced LIGO-Virgo-KAGRA O4 Observing Run: SkyMapper Optical Follow-up of Gravitational Wave Triggers" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230321T000000Z DTEND:20230321T010000Z DTSTAMP:20261011T152429Z UID:rbg1qmqrmq6ii4m5i7vg7p3igc@google.com CREATED:20230306T033109Z DESCRIPTION:Rapidly growing black holes are surrounded by accretion discs t hat make quasars the brightest objects in the Universe. Their brightness i s known to be variable\, but the causes of this are not implied by simple disc models and still debated. Due to the small size of accretion discs an d their great distance\, there are no resolved images addressing the puzzl e. In this work\, we study the dependence of their variability on luminosi ty\, wavelength and orbital/thermal timescale. We use over 5\,000 of the m ost luminous quasars with light curves (LCs) of almost nightly cadence fro m > 5 years of observations by the NASA/ATLAS project\, which provides 2 b illion magnitude pairs for a structure function (SF) analysis. When time i s expressed in units of orbital or thermal timescale in thin-disc models i n the random walk (RW) regime\, we find a universal structure function\, i ndependent of luminosity and wavelength\, supporting the model of magneto- rotational instabilities as a main cause. Over a > 1 dex range in time\, t he fractional variability amplitude follows log(A/A0) 1/2 x log(dt/tth). Deviations from the universality in the RW regime may hold clues on the or ientation of discs. Given the anisotropic emission from quasar accretion d iscs\, their viewing angle affects estimates of the quasar luminosity\, bl ack-hole mass and Eddington ratio. Discs appear over-luminous when viewed pole-on and under-luminous when viewed at high inclination. In radio-quiet quasars\, the viewing angle is usually unknown\, although spectroscopic i ndicators have been proposed. We use the universality in the variability S F of quasar LCs to infer offsets between observed and intrinsic luminosity due to the anisotropy. We select two subsamples from the above for this w ork\, one is a sample of 183 quasars with measured H-beta lines as well as another sample of 753 quasars with CIV and MgII lines. Starting from the proposed orientation indicators\, we expect quasars with narrower H-beta l ines and with more blueshifted CIV lines to be viewed more pole-on and thu s appear over-luminous. In contrast\, our SF analysis finds that presumed pole-on discs appear under-luminous\, consistently for both line indicator s. The simplest explanation would be that quasars with highly blueshifted CIV lines have dusty outflows\, which render the accretion disc under-lumi nous\, irrespective of inclination angle. In our SF analysis\, we corrobor ate a known suppression at timescale shorter than the RW regime\, which is caused by an unknown reason. We propose that this is due to a "smearing" effect caused by the synchronized emission from different parts of the dis c reaching us after different time lags. We seperate the sample of ~5000 q uasars by their redshifts and luminosities\, fit the SFs of every groups t o find the dt breaks from the RW regime\, then investigate the relation be tween those breaks and the rest-frame wavelengths and luminosities. If our assumption is correct\, we will see a relation following the disc size pr edicted by the thin-disc models. This will be an innovative method measuri ng the disc size other than previous methods such as micro-lensing variabi lity and continuum reverberation mapping. LAST-MODIFIED:20230309T230612Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Maddie McKenzie) \nZoom: h ttps://anu.zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ji-Jia (RSAA) "Quasar Variability and its Relation to Accretion Dis c Properties (End of Thesis Talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240618T010000Z DTEND:20240618T020000Z DTSTAMP:20261011T152430Z UID:h53gvoouuuhnkd0ats377h1glc@google.com CREATED:20240415T035626Z DESCRIPTION:The Vera C. Rubin Observatory's Legacy Survey of Space & Time ( LSST) will be a 10-year optical and near infrared survey that will image t he entire visible sky every three nights. The science enabled by Rubin's L SST will be very broad\, ranging from studies of small moving bodies in th e solar system to the structure and evolution of the universe as a whole. In May this year the 3.2-Gigapixel Camera arrived at Rubin Observatory in Chile. In early 2025 it will be mounted on the telescope and on-sky scienc e validation will begin. The start of full operations and execution of the LSST is expected to follow in late 2025. Rubin/LSST will collect about 2 0 terabytes of multi-color imaging data every night\, culminating in a 500 petabyte set of images and data products after 10 years. In this talk I w ill provide an update on the current status of Rubin/LSST construction and discuss how we are preparing the scientific community to analyse and do s cience with the LSST dataset. LAST-MODIFIED:20240617T233607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Sven Buder) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Leanne Guy (Rubin Observatory) "Rubin Observatory and the Legacy Su rvey of Space and Time: Preparing for Science" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170817T010000Z DTEND:20170817T020000Z DTSTAMP:20261011T152430Z UID:als4eebck9jq4a2o0gt0mfr5t0@google.com CREATED:20170513T120613Z DESCRIPTION:Aside from being spectacular displays in their own right\, Type Ia supernova explosions have a key role in measuring the expansion histor y of the Universe and synthesizing the iron group elements. But what is th eir origin? That Type Ia supernovae arise from exploding white dwarfs is r elatively well-established but the manner in which the explosion is ignite d and how this can be determined from what we observe remain hotly debated issues. I will discuss the theoretical modelling of Type Ia supernovae w ith particular focus on how radiative transfer simulations can be used to test explosion scenarios. I will argue that understanding the diversity of thermonuclear supernovae requires us to investigate a variety of differen t progenitor scenarios. Specifically\, I will present recent results from our work on both Chandrasekhar mass white dwarf explosion scenarios and su b-Chandrasekhar mass models. LAST-MODIFIED:20170809T075608Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Stuart Sim (UQ Belfast) "Modelling thermonuclear supernovae: how to blow up a white dwarf star" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150605T040000Z DTEND:20150605T042000Z DTSTAMP:20261011T152429Z UID:k7cssnbc63k4hji75j1t3oulkg@google.com CREATED:20150603T084105Z DESCRIPTION:The most massive black holes in the nearby Universe seem to lar gely be hosted by massive central cluster galaxies. The ultra-massive blac k hole in NGC 1277\, reported by van den Bosch et al. based on a stellar k inematic measurement\, is an extreme outlier in this respect. NGC 1277 is not a central cluster galaxy\, but a lenticular galaxy in the Perseus Clus ter\, at a distance of about 3.8' from the central cluster galaxy. I will present our recent detection of CO(1-0) emission from NGC 1277 and discuss the BH mass based on constraints derived from the molecular gas kinematic s. LAST-MODIFIED:20150603T122606Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Julia Scharwaechter (Observatoire de Paris) "A close look at the ul tra-massive black hole in NGC 1277" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190304T023000Z DTEND:20190304T033000Z DTSTAMP:20261011T152429Z UID:sr57a8tord7r58rbiimnskqps0@google.com CREATED:20190220T032110Z DESCRIPTION:We present the second data release (DR2) of the SkyMapper South ern Survey\, a hemispheric survey carried out by RSAA with the SkyMapper T elescope at Siding Spring Observatory. DR2 is available to Australian astr onomers from 1 March 2019 and is the first release to go beyond the ~18 ma g (10-sigma) limit of the Shallow Survey released in DR1. It includes port ions of the sky at full survey depth that reach >21 mag in g and r filters . The DR2 photometry has a precision as measured by internal reproducibili ty of 1% in uv bands and 0.7% in griz bands. More than 21\,000 deg^2 have data in some filters (at either Shallow or Main Survey depth) and over 7\, 000 deg^2 have deep Main Survey coverage in all six filters. The release c ontains over 120\,000 images\, as well as catalogues with over 500 million unique astrophysical objects and nearly 5 billion individual detections. It also contains cross-matches with a range of external catalogues such as Gaia DR2\, Pan-STARRS1 DR1\, GALEX GUVcat\, 2MASS\, and AllWISE\, as well as spectroscopic surveys such as 2MRS\, GALAH\, 6dFGS\, and 2dFLenS. We d iscuss properties of the data including its limitations\, methods to acces s the data\, and example science investigations underway\, in order to sti mulate as many of you as possible to use SkyMapper for your own purpose. LAST-MODIFIED:20190301T033205Z LOCATION:CSO Common Room (host: Bessell) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Christopher A. Onken & Christian Wolf (RSAA) "The SkyMapper Souther n Survey Data Release 2" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240307T000000Z DTEND:20240307T013000Z DTSTAMP:20261011T152429Z UID:r7qfbn2913mu6des319i7t1ve0@google.com CREATED:20240220T233613Z DESCRIPTION:Outflows fundamentally alter the chemical composition\, structu re\, and star-formation activity of galaxies\, and are therefore one of th e most important processes shaping galaxy evolution. However\, our underst anding of outflow physics is still in its infancy\, and the role of outflo ws in quenching star-formation is a topic of ongoing debate. In this talk\ , I will highlight recent observational breakthroughs enabled by the James Webb Space Telescope (JWST)\, the Very Large Telescope (VLT) and the Atac ama Large Millimeter Array (ALMA). Specifically\, I will examine the role of AGN-driven outflows in quenching massive galaxies at cosmic noon\, and compare the mechanisms accelerating star-formation driven outflows at diff erent redshifts. Outflows are just one component of the cosmic baryon cycl e\, and I will conclude by discussing how future observations with VLT/MAV IS\, 30m-class telescopes and the Square Kilometer Array which will enable us\, for the first time\, to connect the dots between inflows\, outflows and star-formation over much of the history of the Universe. LAST-MODIFIED:20240229T220109Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Stu Wyithe) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rebecca Davies (Swinburne) "Do outflows quench star-formation?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161209T030000Z DTEND:20161209T032000Z DTSTAMP:20261011T152430Z UID:pi1bdl58re4k3ki5t8plhmirjc@google.com CREATED:20161209T010606Z DESCRIPTION:Ever looked up at the night sky during observing\, and wanted t o take photo\, but just didn't know how to take the shot ? Well\, we've al l been there. In this talk\, I will talk about why astronomers should not let good photons go to waste\, why everyone with a DSLR should get their g ears out and start taking photos. If you don't have a DSLR\, still do come along\, there will be pretty pictures. And by the end of the talk\, there is a good chance you'll be brainwashed to spend two thousand dollars. LAST-MODIFIED:20161209T010606Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dilyar Barat (RSAA) "Astrophotography\, because you're staying up a nyway" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200227T000000Z DTEND:20200227T010000Z DTSTAMP:20261011T152429Z UID:voo3tataih61mcl2npsjhn87qc@google.com CREATED:20191119T105611Z DESCRIPTION:An open discussion on culture and behaviour in astronomy. LAST-MODIFIED:20200226T085104Z LOCATION:Duffield Lecture Theatre (host: ) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Culture and Behaviour in Astronomy "Culture and Behaviour in Astron omy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160331T000000Z DTEND:20160331T010000Z DTSTAMP:20261011T152430Z UID:vh1l6ciauhft45og3d1i13hts0@google.com CREATED:20151216T054613Z DESCRIPTION:Stellar astrophysics has entered a new golden age\, thanks to w onderfully precise measurements being returned by NASA's Kepler mission. K epler is a 0.9-metre space telescope that has been monitoring the brightne ss of more than 100\,000 stars with extraordinary accuracy for more than f our years. Its main goal is to discover extra-solar planets by detecting the small dips in light as they transit their parent stars. The mission h as been spectacularly successful\, with thousands of candidates reported. Meanwhile\, Kepler's observations of oscillations in thousands of stars h ave led to a revolution in asteroseismology. Key results include detectin g gravity modes in red giant stars and characterizing stars found to host exoplanets. Upcoming results from ESA's Gaia mission will add to the exci tement\, as will the launch next year of TESS\, which is an all-sky follow -up mission to Kepler. LAST-MODIFIED:20160322T064106Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tim Bedding (University of Sydney) "A Golden Age of Asteroseismolog y with Kepler" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230420T010000Z DTEND:20230420T020000Z DTSTAMP:20261011T152429Z UID:ssq1b31511mh1019goe53mc9mo@google.com CREATED:20230313T052215Z DESCRIPTION:Located in the highest point of Antarctic inland\, Dome A has b een considered as one of the best astronomical observatory sites in the wo rld. Some survey telescopes are planning to be installed in Dome A. Unlike any other areas\, these telescopes have to be settled on the snow ground. In that case\, it is very important to analyze the Snow mechanics to keep the foundation stable. The presentation firstly introduced the analysis o f the snow strength in Dome A. Secondly\,the dynamic and statics analysis of the telescope tower and the dome tower will be shown in this presentati on. Meanwhile\, some instruments has been developed to test the snow stres s in Dome A by the NIAOT Antarctic team\,these instruments also have been used in Beijing Winter Olympic games. LAST-MODIFIED:20230418T075609Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBA) \nZoom: https://anu.z oom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Haikun Wen (Niaot\, CAS) "Snow Mechanics analysis of Dome A and its application in Beijing Winter Olympic games" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160329T000000Z DTEND:20160329T010000Z DTSTAMP:20261011T152429Z UID:i0om2rl80r130tpdrb305t2mi8@google.com CREATED:20160218T005615Z DESCRIPTION:Astrophysical jets carry energy and particles from very small u p to very large scales from the radius of the central object. From these r egions\, the highly collimated outflows propagate up to the distances so f ar away. This implies powerful stability and collimation taking into accou nt that different instabilities can affect the evolution of jets. Moreover \, their propagation is possibly changing the properties and evolution of the host galaxies and their environments through heating by shocks and/or mixing\, and removing of gas by shocks and transfer of momentum. Thus\, je t stability has been a significant research subject during the last decade s. In this talk\, I will present some recent results on the linear and non -linear stability analysis of non-relativistic magnetized jets carrying he lical magnetic fields. Specifically\, the role of Kelvin­ Helmholtz and c urrent- driven instabilities\, and their impact on the jet morphology\, je t braking and overall stability are analysed. I will discuss the non-linea r evolution of jets with the aid of three-dimensional numerical simulation s. LAST-MODIFIED:20160322T064105Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Maryam Anjiri (Ferdowsi University of Mashhad) "Instabilities of Cu rrent-Carrying MHD (non-rotating) Jets" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210121T000000Z DTEND:20210121T003000Z DTSTAMP:20261011T152429Z UID:0usspvddnjfl9bnr6eh4jm8qsg@google.com CREATED:20210104T055605Z DESCRIPTION:Most of the baryonic matter in the Universe is undergoing some form of magnetohydrodynamical (MHD) turbulence. At the scale of a few pars ecs\, in the cool\, approximately isothermal molecular hydrogen gas of sta r-forming clouds\, the turbulence is most likely driven on large scales\, with enough energy to invoke random motions that exceed the sound speed\, causing the gas to become highly compressible. However\, MHD turbulence th eory has been largely developed in the incompressible regime\, and theoris ts regularly ignore compressibility effects\, even though it is these effe cts that define the most important structures for star formation\, such as filaments. In this talk I report on the first of three (magnetic field\, density\, energy) analytical turbulent fluctuations theories that we have been developing as part of my PhD. That is\, the ubiquitous fluctuations o f the magnetic field in a supersonic turbulent medium\, including anisotro pic affects imparted upon the flow by a local coherent (mean) magnetic fie ld. We (1) derive an analytical model of the magnetic field fluctuations i n the sub-Alfvenic field limit\, (2) show how the coherent field causes an isotropic compressibility effects leading to bimodally oriented shocks in the gas\, and (3) show that fundamental assumptions about the Alfven veloc ity and velocity scaling relations in the flow are incorrect for anisotrop ic flows\, which in turn motivates a modified Chandrasekhar-Fermi method f or highly-magnetised molecular clouds. We test our models on an ensemble o f 24 MHD simulations across an order of magnitude in turbulent Mach number \, and five orders of magnitude in mean-field strength. Because we form ou r models undimensionalised we believe that these results are generally app licable for anyone seeking to understand magnetism in any supersonic\, tur bulent medium\, where the turbulence is being continuously stirred by astr ophysical energy sources. LAST-MODIFIED:20210114T070605Z LOCATION:ZOOM 997 8534 1005 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:James Beattie (RSAA) "Ubiquitous magnetic field fluctuations driven by large-scale supersonic turbulence" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210615T010000Z DTEND:20210615T020000Z DTSTAMP:20261011T152429Z UID:j9k3jnst6mrb2p4pusnmeuoa4s@google.com CREATED:20210211T041123Z DESCRIPTION:Software is now critical for modern research\, and frequently\, scientific breakthroughs are enabled by high-quality and innovative resea rch software. Consequently\, there is an increased demand for ''Research S oftware Engineers (RSEs)'' - people who are well-trained domain scientists with highly specialised software skills. However\, the existing policies for rewards and recognition within academia are insufficient to hire\, pro mote and retain these skilled RSEs. Broad community consultations are unde rway to finalise recommendations for a more sustainable research software ecosystem. These recommendations include both a top-down approach through funding\, policy and research assessment and a bottom-up approach through actions of individual research groups and institutions. Both of these appr oaches are necessary to drive change in culture around research software. I will discuss the current developments surrounding research software\, bo th nationally and in the international context. I will share various pract ices for software\, data and communities that you can adopt to promote a m ore sustainable research software ecosystem. LAST-MODIFIED:20220618T125715Z LOCATION:ZOOM and DLT (host: Amit Seta) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Manodeep Sinha (Swinburne) "Invited Colloquium: Towards Sustainable Research Software & Inclusive Communities" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240903T010000Z DTEND:20240903T020000Z DTSTAMP:20261011T152429Z UID:0pt3ujq76tsm14aashjb537mjs@google.com CREATED:20240415T235643Z DESCRIPTION:Sensitive\, high-resolution radio continuum observations are un covering details of the complex interaction between kpc-scale AGN jets and their environments. I will present theoretical results from a suite of an alytical and numerical models of AGN jets\, designed to inform interpretat ion of radio continuum observations. I will show how analytical jet models provide insights into poorly constrained physical processes\, including m echanisms responsible for jet intermittency\, and modes of AGN feedback in galaxies and clusters. I will then introduce the CosmoDRAGoN simulations\ , a large suite of simulated AGN jets in cosmological environments. CosmoD RAGoN uses 3D relativistic hydrodynamic simulations to describe jet dynami cs\, while synchrotron emissivity is calculated in post-processing using a n analytical model which fully accounts for the relevant loss processes. T he CosmoDRAGoN simulation data\, including synthetic radio images\, are be ing made available to the community via a web app. I will show how these s imulations can be used to probe galaxy and cluster-scale environments\, an d robustly classify radio galaxies in different evolutionary stages. I wil l conclude with a possible formation mechanism for Odd Radio Circles (ORCs )\, as radio galaxy remnants revived by the passage of a shock. LAST-MODIFIED:20240815T063614Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Maja Jablonska) \nZoom: ht tps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Stas Shabala (U. Tasmania) "Life\, death and rebirth of radio galax ies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250916T010000Z DTEND:20250916T020000Z DTSTAMP:20261011T152429Z UID:36dqn17ccn2b5pn446dioif48o@google.com CREATED:20250623T121114Z DESCRIPTION:About a billion years after the Big Bang\, the Epoch of Reionis ation saw the first light sources in the Universe slowly ionise the primor dial atoms of the surrounding IGM. Learning about this distant epoch has t he potential of unveiling crucial information about the formation of the f irst stars\, galaxies\, and early black holes\, which sourced it. However\ , its observation remains elusive. Attempted measurements of the 21cm sign al\, coming directly from the high-redshift neutral hydrogen\, are still p lagued with foregrounds and systematics\, whilst modelling uncertainties p revent us from extracting the reionisation signatures from large astrophys ical and cosmological data sets. In this talk\, I will describe how gigant ic radio interferometers in the most remote locations and state-of-the-art CMB telescopes can tell us about the nature and evolution of the first ev er light sources. I will give an overview of what has already been done\, and what is yet to achieve to get our answers. Despite promising results f rom the Hydrogen Epoch of Reionisation Array (HERA)\, which has recently g iven the lowest upper limits on the 21cm power spectrum at redshifts z > 7 \, I will show how a first detection of small-scale EoR signatures will li kely come from joint analyses and cross-correlations. LAST-MODIFIED:20250909T030106Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Tim Gao) \nZoom: https://a nu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Adelie Gorce (U. Paris-Saclay) "Unveiling the cosmic dawn with radi o observations of the sky" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191126T000000Z DTEND:20191126T010000Z DTSTAMP:20261011T152429Z UID:rq77an3vf8k2ibv4e9pbi0tgvg@google.com CREATED:20191029T102111Z DESCRIPTION:The Milky Way's central box/peanut bulge together with the plan ar long bar are estimated to contain one third of our Galaxy's stars. Dyna mical models based on star count and radial velocity data have also set li mits on the dark matter mass in the bulge\, and determined a fairly large corotation radius of ~6kpc\, which suggests that the Galactic bar will be important also for understanding solar neighbourhood dynamics. I will disc uss the dynamics of the Milky Way's barred components\, including recent w ork on the pattern speed based on VVV and Gaia proper motions. I will also describe new results on stellar metallicities in the long bar\, and on is olating the Galactic spiral arms in Gaia DR2. LAST-MODIFIED:20191118T054606Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ortwin Gerhard (MPE) "Structure and Dynamics of the Barred Milky Wa y" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150828T040000Z DTEND:20150828T042000Z DTSTAMP:20261011T152429Z UID:lclrg62ee8j3uoqu0b1ocljfb0@google.com CREATED:20150814T164608Z DESCRIPTION:Turbulence and magnetic fields are both ubiquitous in the Milky Way\, significantly affecting the formation of stars\, and how gas is rec ycled in the Galaxy. However\, the nature of turbulent flows in the magnet ised interstellar medium is largely unknown\, as key properties of turbule nce are poorly constrained by observations. I will discuss how observation s of synchrotron intensity fluctuations can be used to probe the sonic and Alfvenic Mach numbers of interstellar turbulence\, based on mock observat ions performed on simulations of magneto-hydrodynamic turbulence. I will a lso discuss the potential for novel polarisation analysis techniques to un iquely determine the sonic and Alfvenic Mach numbers of observed turbulenc e\, and to assist in qualitative understanding of Galactic magneto-ionic t urbulence. LAST-MODIFIED:20150816T065609Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Chris Herron (USyd) "Novel probes of magnetised interstellar turbul ence from diffuse synchrotron emission" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181114T000000Z DTEND:20181114T010000Z DTSTAMP:20261011T152430Z UID:q3febebabvfcim05ut1mdscrh8@google.com CREATED:20181013T023106Z DESCRIPTION:I will describe what is required to take spectra of ~100 nearby habitable Earth-like planets to see if they have the oxygen A-band bio-si gnature. Such a mission represents a robust and statistically significant search for exo-life. The talk will include references to proposed missions such as LUVOIR and HABEX and describe a more affordable and quicker alter native called SUPERSHARP. LAST-MODIFIED:20181105T232112Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ian Parry (University of Cambridge) "Searching for the 763nm oxygen bio-signature with direct imaging/spectroscopy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220224T000000Z DTEND:20220224T010000Z DTSTAMP:20261011T152430Z UID:0v035ev23e042700ea459nl2o0@google.com CREATED:20211210T110607Z DESCRIPTION:Please join us in the Duffield Lecture Theatre to hear what Piy ush has been working over the past years of his PhD. LAST-MODIFIED:20220221T091105Z LOCATION:DLT & ZOOM (host: Sven) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Piyush Sharda (RSAA) "PhD Thesis Talk: The role of metals from mole cular clouds to galactic discs" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150410T044000Z DTEND:20150410T050000Z DTSTAMP:20261011T152429Z UID:2cn6qsrrvoa26h57m10q1utmk8@google.com CREATED:20150405T060106Z DESCRIPTION:I would like to solicit the opinions of RSAA staff+students in the next couple of weeks as the decision whether to proceed will be taken in the near future. LAST-MODIFIED:20150405T060106Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Martin Asplund (RSAA) "Discussion on the proposed joint Keck TAC be tween ANU\, Swinburne and Australia" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231107T000000Z DTEND:20231107T010000Z DTSTAMP:20261011T152429Z UID:oeg8i2254a462flhhqtj0jdon8@google.com CREATED:20231103T011108Z DESCRIPTION:The very low-mass end of the galaxy mass function is a complica ted place\, and there are multiple ways for a stellar system to find itsel f at the present day with a small size and a low stellar mass. Globular cl usters are one type of compact low-mass stellar system\, and they are stud ied both as satellites of galaxies and as old stellar systems in their own right. I will describe some of the ways globular clusters are used in gal actic archaeology and some of the things we have learned about their role in stellar halo formation. My aim is to illuminate connections between obs ervables at high and low redshift\, the globular clusters in the Milky Way and in other galaxies\, and some of the unique opportunities for research presented by globular clusters and other very small galaxies. LAST-MODIFIED:20231103T033109Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sarah Martell (UNSW) "When are globular clusters just very small ga laxies?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250610T010000Z DTEND:20250610T020000Z DTSTAMP:20261011T152429Z UID:08tk8oinqfttiv70g0lbj1nb9k@google.com CREATED:20250121T000640Z DESCRIPTION:How do galaxies evolve from the complex\, merging systems of th e early Universe to the familiar Hubble types we see today? Tidal torques of the cosmic web impart angular momentum\, which is consequently a fundam ental property in a galaxy's evolutionary history\, affecting that galaxy' s size\, density and morphology. In this talk I will present my group's re search into the relation between specific angular momentum and galaxy evol ution from the peak of cosmic star formation to today\, including the clos e connection between the internal spatial distribution of angular momentum and visual morphology. LAST-MODIFIED:20250516T013111Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Tim Gao) \nZoom: https://a nu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sarah Sweet (U Queensland) "Linking galaxy morphology with spatiall y resolved angular momentum" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220512T010000Z DTEND:20220512T013000Z DTSTAMP:20261011T152429Z UID:qgos8jtvv73t5agu2ph94n4u4c@google.com CREATED:20220507T025106Z DESCRIPTION:Despite the fundamental nature of cosmic magnetic fields\, many questions remain regarding their origin\, evolution\, and structure. We a re able to illuminate these otherwise invisible fields through observation s of background polarised radio sources. By measuring the Faraday rotation this polarised emission experiences along the line of sight\, we are able to reconstruct the magneto-ionic structure of foreground features\, such as the Milky Way Galaxy. This technique would also be applicable to smalle r foreground objects\, such as galaxies and clusters\, however\, we are ty pically limited by the on-sky density of background sources detected by a given radio survey. On behalf of the RACS team\, I will provide an overvie w of observations from the Rapid ASKAP Continuum Survey (RACS)\; the first all-sky survey undertaken by the Australian SKA Pathfinder (ASKAP). RACS is now the state-of-the-art radio-frequency survey of the Southern sky\, w ith a noise-level of ~ 300 micro Jy/beam\, a resolution of 25 arcsec\, and 2.1 million sources detected in total intensity at 888 MHz. Through a col laboration between the observatory and the Polarisation Sky Survey of the Universes Magnetism (POSSUM) survey teams\, SPICE-RACS will catalogue line arly polarised sources from RACS and deliver a background polarised source density 3-5x higher than the current state of the art. I will present the first data release of SPICE-RACS. This catalogue contains ~6000 polarised radio sources\, imaged at 25 arcsec\, over 1300 square degrees towards th e nearby Spica HII region. I will describe our first science results deriv ed from this catalogue\, and the future plans for SPICE-RACS. LAST-MODIFIED:20220507T025106Z LOCATION:DLT & ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alec Thomson (CSIRO) "SPICE-RACS: Spectra and Polarisation In Cutou ts of Extragalactic sources from RACS" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221123T003000Z DTEND:20221123T010000Z DTSTAMP:20261011T152429Z UID:9t42h7gkurhi6acvnb9k77b3d0@google.com CREATED:20221020T054617Z DESCRIPTION:Jupiter and Saturn played important roles in sculpting the pres ent-day Solar System. Their interactions sent inward water-bearing asteroi ds\, giving Earth its ocean. However\, the Jovian planets around stars oth er than our Sun have their own complex tales. Since the launch of the Tran siting Exoplanet Survey Satellite (TESS) four years ago\, the exoplanet fi eld has had a new boom of discoveries. In this talk\, I will review the di verse population of Jovian planets discovered by the TESS Mission\, especi ally those benefited from the wide field TESS Full Frame Images. These dis coveries reveal an intriguing story of the history of these Jovian planets \, and how they acted as the chief architects of their own planetary syste ms. LAST-MODIFIED:20221120T033910Z LOCATION:DLT & ZOOM (host: Neco Kriel) \nZoom: https://anu.zoom.us/j/997853 41005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Chelsea Huang (University of Southern Queensland) "TESS's Jovian Le gacy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201014T230000Z DTEND:20201015T000000Z DTSTAMP:20261011T152429Z UID:ir9v1ecqig03puguean7k0e7jo@google.com CREATED:20201012T213105Z DESCRIPTION:Radio astronomy faces a data deluge from new radio telescopes a nd wide-area surveys in the lead-up to the Square Kilometre Array. The hop e is that machine learning\, a computer science field that designs methods for extracting useful information from data\, will provide algorithms to help process this huge amount of data. In this talk I summarise my work on applying machine learning to extragalactic sources\, including the first machine learning algorithm for radio cross-identification and an innovativ e new method for characterising the Faraday complexity of polarised source s. LAST-MODIFIED:20201012T213105Z LOCATION:DLT and ZOOM 997 8534 1005 (host: Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Matthew Alger (RSAA) "End-of-Thesis Colloquium: Learning to Identif y Extragalactic Radio Sources" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160317T000000Z DTEND:20160317T010000Z DTSTAMP:20261011T152429Z UID:jh3566nj63muov9bquuf9orh0c@google.com CREATED:20160215T055611Z DESCRIPTION:The mass of a star is arguably its most fundamental parameter a nd for red giant stars it implies a stellar evolution age. Stellar masses and ages have never been derived directly from spectra of red giants. Howe ver\, using the APOGEE Kepler sample of stars (the APOKASC sample)\, with high-quality spectra and asteroseismic masses\, we have built a data-drive n spectral model using THE CANNON (arXiv:1501.07604) to infer stellar age from spectra. THE CANNON constrains the ages from spectral regions with e lements whose surface abundances reflect mass dependent dredge-up. We deli ver a catalogue of ages for 75\,000 red giants\, which span the Milky Way disk\, from the Galactic centre out to 20kpc. I will demonstrate the new a venues we are pursuing in Galactic archeology with these ages\, and beyond . LAST-MODIFIED:20160309T002107Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Melissa Ness (MPIA) "The first stellar age map of the Milky Way and beyond." TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150319T000000Z DTEND:20150319T010000Z DTSTAMP:20261011T152429Z UID:glgdnotm66cfehvampvf418t38@google.com CREATED:20150220T003614Z DESCRIPTION:Where did Edwin Hubble get his famous tuning fork from? Every a stronomer studying galaxies uses Hubble types Sa\, Sb\, Sc\; does anyone k now the actual source of the 'Hubble classification bins'? Where did Hubbl e get the Hubble luminosity profile from? Who actually computed the rate o f expansion of the Universe\, for the first time? Who secured almost all t he spectra in 'Hubble's law' v=Hr? Following years of collaboration and de tective work together with KC Freeman\, the strategy of Edwin Hubble is ex posed and unmasked to the astronomical community. The seminar details conv ersations held with the late Dr Allan Sandage. The results are contained i n a recent book published by Springer in New York. LAST-MODIFIED:20150316T234105Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:David Block (Uni Witwatersrand) "The strategy of Edwin Hubble\; cha nging the history of galaxy morphology forever" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170919T000000Z DTEND:20170919T020000Z DTSTAMP:20261011T152429Z UID:a39g7tmqkci5ltl4oekr0qhm08@google.com CREATED:20170719T092116Z DESCRIPTION:TBD LAST-MODIFIED:20170719T092116Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:ESO Road Show (ESO) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180201T000000Z DTEND:20180201T010000Z DTSTAMP:20261011T152430Z UID:dg4i3p5tb05ljcprdghmljm9so@google.com CREATED:20171124T094116Z DESCRIPTION:Close tidal encounters among large planetesimals and moons were more common than impacts. Using a mass spring model within an N-body simu lation\, we simulate the small deformation of a surface that is caused by a close tidal encounter. We find tidal encounters can induce sufficient st ress on the surface to cause large scale brittle failure of an icy crust. Strong tidal encounters may be responsible for the formation of long grabe n complexes and chasmata in ancient terrain of icy moons such as Dione\, T ethys\, Ariel and Charon. Mass spring models\, originally developed for gr aphics and gaming applications\, can measure remarkably small deformations and so can show tidal spin down of viscoelastic objects\, directly tying simulated rheology to orbital drift and internal heat generation. The new Horizons mission discovered that Pluto and Charon's minor satellites Styx\ , Nix\, Kerberos\, and Hydra\, are rapidly spinning\, but surprisingly the y have spin axis tilted into the orbital planet (they have high obliquitie s). Long simulations of the minor satellites in a drifting Pluto-Charon bi nary system exhibit rich resonant spin dynamics\, including spin-orbit res onance capture\, tumbling resonance and spin-binary resonances. We have id entified spin-precession mean-motion resonances with Charon that can lift obliquities in the Pluto/Charon system. LAST-MODIFIED:20180129T005106Z LOCATION:Duffield Lecture Theatre (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alice Quillen (University of Rochester) "Soft astronomy: Astro-visc o-elastic dynamics" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190815T010000Z DTEND:20190815T020000Z DTSTAMP:20261011T152429Z UID:m5b1rsmkauckudg020gk8onv1o@google.com CREATED:20190712T013113Z DESCRIPTION:The final 12 minutes of the Apollo 11 moon landing were filled with problems and ample reasons to abort. I will explain what was happenin g and why\, and thus unlock the tension of those last few minutes. While t he world watched in awe of the achievement\, only Mission Control and the astronauts realised how close they were to aborting...for more than one re ason LAST-MODIFIED:20190813T033605Z LOCATION:Duffield Lecture Theatre (host: Monty) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:John Lattanzio (Monash University) "Apollo 11 After 50 Years" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261103T000000Z DTEND:20261103T010000Z DTSTAMP:20261011T152430Z UID:u6ib8sgo5m67uu6pv7c3dhuno4@google.com CREATED:20260615T020027Z DESCRIPTION:TBC LAST-MODIFIED:20260716T070023Z LOCATION:Zoom or Duffield Lecture Theatre (host: TBC) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Ian Czekala (CSIRO) "TBC" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221215T000000Z DTEND:20221215T003000Z DTSTAMP:20261011T152429Z UID:pki43dkqg4nc2oekad2iu0ah9o@google.com CREATED:20220919T025617Z DESCRIPTION:Almost all star formation is observed to occur within Giant Mol ecular Clouds (GMCs)\, making their dynamics and evolution a key part in u nderstanding the formation of stars and star clusters in our universe. On the scales of these clouds it is believed that the main process regulating how efficient the star formation process is (how much gas is turned into stars) is energy injected by massive (>8 Msun) stars that acts to disrupt the cloud and halt star formation. However\, these massive stars can injec t energy in to their surroundings in many different ways: (i) their light pushing on dust grains\, (ii) that dust re-radiating that light in the inf rared which pushes on dust more\, (iii) ionizing radiation heating the sur rounding gas\, and finally (iv) that energy being absorbed in the star's o wn atmosphere resulting in massive\, high velocity outflows from the star' s surface: stellar winds. How these mechanisms act to disperse GMCs and ho w they interact with one another\, in particular which process is dominant and in which scenario\, constitutes ongoing research and debate in the li terature. In this talk I will address how the dynamics of stellar wind-dri ven bubbles are drastically modified when you consider their expansion int o the realistic\, turbulent environments of GMCs. LAST-MODIFIED:20221207T021613Z LOCATION:DLT & ZOOM (host: TBD) \nZoom: https://anu.zoom.us/j/99785341005?p wd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Lachlan Lancaster (Columbia University) "How Turbulence Pops Stella r Wind Bubbles" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230704T010000Z DTEND:20230704T020000Z DTSTAMP:20261011T152429Z UID:rfscm85qrjpdrksa17qu5k56lc@google.com CREATED:20230626T024107Z DESCRIPTION:One of the key questions in galaxy evolution is how metals trav el in and out of galaxies and how the metal enriched gas inside galactic d isks mixes into the surrounding circumgalactic gas. An important diagnosti c for this gas flow is the gas-phase metallicity gradient. However\, measu rements of gradients are often affected by limited spatial resolution. We produce mock IFU datacubes from hydrodynamic simulations of an isolated ga laxy in order to quantify the said effect. I will present the application of our models on current IFU surveys -- MaNGA\, SAMI and CALIFA -- by corr ecting the observed metallicity gradients for the effects of spatial resol ution. However\, isolated simulations do not capture the dynamics of gas flow between the disk and the CGM. For this we turn to a suite of cosmolog ical\, zoom-in simulations with high spatial and time resolution -- FOGGIE . Using the FOGGIE simulations we demonstrate that a high cadence (~few My r) is indispensable for accurately tracking the metallicity gradient evolu tion\, particularly at high-redshift (z). FOGGIE galaxies spend ~40% of th eir time during z>2 outside the typical observational uncertainty away fro m the mean behaviour. Additionally\, we present a novel\, non-parametric m ethod of quantifying the metallicity distribution which is free from geome tric assumptions. We investigate how efficiently our new method responds t o metal-mixing stimuli\, such as star-formation\, mergers and outflows. Ou r models pave the way for interpreting upcoming JWST observations of high- z metallicity gradients. LAST-MODIFIED:20230626T033107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Neco) \nZoom: https://anu. zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ayan Acharyya (Johns Hopkins University) "Robust measurements of ga s-phase metallicity distribution" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161122T000000Z DTEND:20161122T010000Z DTSTAMP:20261011T152429Z UID:71dr4qum6086vt4412p9go6t8g@google.com CREATED:20161114T003707Z DESCRIPTION:The recent discovery of gravitational waves emitted by binary b lack holes suggests these sources will be detected in large number in the next few years. Detected signals can be used to characterize black holes\, yielding direct estimation of their masses and spins. In this talk I will report on the precision we can expect from advanced LIGO and other advanc ed detectors at characterizing black holes in binary systems. I will also consider the proposed next generation of gravitational-wave detectors\, an d show how they have the potential of detecting binary black holes from la rge redshifts\, and enable precise astrophysics and cosmology. LAST-MODIFIED:20161114T003707Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Salvatore Vitale (MIT) "Characterization of black holes with gravit ational waves" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220705T010000Z DTEND:20220705T020000Z DTSTAMP:20261011T152429Z UID:7vtcis5fj5rmlsfpf342amthmg@google.com CREATED:20220520T064111Z DESCRIPTION:The source of about half of the heaviest elements in the Univer se has been a mystery for a long time. Although the general picture of ele ment formation is well understood\, many questions about the astrophysical details remain to be answered. Here I focus on recent advances in our und erstanding of the origin of the heaviest and rarest elements in the Univer se. LAST-MODIFIED:20220602T042610Z LOCATION:DLT & ZOOM (host: TBD) \nZoom: https://anu.zoom.us/j/99785341005?p wd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Enrico Ramirez-Ruiz (iUniversity of California Santa Cruz\, USA) "I nvited Colloquium: Cosmic alchemy in the era of gravitational wave astrono my" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200925T044500Z DTEND:20200925T053000Z DTSTAMP:20261011T152429Z UID:lmiq4quj3t9eufvlp3cor7u68s@google.com CREATED:20200916T102610Z DESCRIPTION:Active galactic nuclei (AGN) are among the most luminous object s known to humans\, and are ubiquitous in the local and distant Universe. The method of reverberation mapping (RM) aims to bypass the limitations of spatial resolution of current instruments\, and infer the geometry of the central regions of AGN through the analysis of light-echoes within these regions. In my talk I present the research of my thesis\, in which I have applied statistical methods to improve RM results through stacking\, a rel atively new and unexplored area of the RM field. I use simulations and obs erved data from the OzDES RM program\, and make recommendations on the dev elopment of survey strategies for future RM programs. LAST-MODIFIED:20200922T034608Z LOCATION:DLT and ZOOM 997 8534 1005 (host: Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Nat Sommer (RSAA) "Reverberation Mapping in Bulk with OzDES RM: A S tatistical Approach to Measuring the Geometry of Active Galactic Nuclei wi th Light Echoes (End-of-MPhil)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260915T010000Z DTEND:20260915T020000Z DTSTAMP:20261011T152430Z UID:m4iucv6e344ulhqdfbs0503ifs@google.com CREATED:20260605T021624Z DESCRIPTION:Comets and asteroids from other stars are evidently ejected fro m their home planetary systems in large numbers\, around 10^16 per star. O nce ejected\, these "interstellar objects" (ISOs) orbit the Galaxy. Three such objects have been discovered as they traversed our Solar System on hy perbolic orbits\, with the Vera C. Rubin Observatory expected to find many more in the course of its survey. When a population of ISOs is ejected\, it is stretched into a thin tidal stream. The ISO streams themselves are s ubject to epicyclic caustics\, and their density structures are highly sen sitive to their internal velocity dispersions. This means that a future ob served population of interstellar objects may contain "sibling" ISOs from the same parent star\, and that these may preferentially originate in part icular parts of the population's parameter space. I will also show under w hat circumstances the Sun's own ISOs may return to the Solar System\, demo nstrating that this is not a foreground ISO imposter population about whic h we need to be concerned\, and future prospects for tracing an ISO to its host star. LAST-MODIFIED:20260904T050006Z LOCATION:Zoom or Duffield Lecture Theatre (host: Tomasz Rozanski) \nZoom: h ttps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:John Forbes (U. Canterbury) "The Galaxy's population of interstella r objects in the Rubin era" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221021T030000Z DTEND:20221021T033000Z DTSTAMP:20261011T152429Z UID:8ifdui0e3u5s3455aspu0ns1sg@google.com CREATED:20220929T030513Z DESCRIPTION:Mikhael would talk to us about solving communication bottleneck s with quantym key distribution. Tony would then talk about Ultrawide fiel d imaging in the infrared in the context of the LSST depth and cadence in the K-band. LAST-MODIFIED:20220929T030513Z LOCATION:DLT & ZOOM (host: Marcus Birch) \nZoom: https://anu.zoom.us/j/9978 5341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mikhael Sayat and Tony Travouillon (RSAA) "Satellite-to-Ground Cont inuous Variable Quantum Key Distribution and Ultrawide field imaging in th e infrared" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180216T030000Z DTEND:20180216T040000Z DTSTAMP:20261011T152429Z UID:4s5dtjv2h4uq7k73871krjg22o@google.com CREATED:20180123T002609Z DESCRIPTION:I use the gas-phase chemical abundance of star-forming galaxies to understand how the environment influences the multi-phase gas cycle as a galaxy falls into the cluster potential. Using observations with DEIMOS /Keck\, I find a cluster-scale gradient in the metallicity of star-forming galaxies and present it as a new angle to identify physical processes dri ving the chemical enrichment of cluster galaxies. I use a semi-analytic mo del of ram pressure stripping to prove that removal of low-metallicity gas is not sufficient to reproduce the metallicity gradient. Using IllustrisT NG cosmological simulations\, I find systematic signature of "chemical pre -processing" of infalling galaxies. I predict that the inflow of enriched gas (pre-enrichment) is driving the chemical evolution in the overdense en vironment. In my Ph.D. dissertation\, I combine observations\, theoretical models\, and cosmological simulations to identify drivers of the chemical evolution in the cluster environment. LAST-MODIFIED:20180213T232606Z LOCATION:Duffield Lecture Theatre (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anshu Gupta (RSAA) "Chemical evolution of star-forming cluster gala xies (End-of-Thesis Colloquium)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260421T013000Z DTEND:20260421T023000Z DTSTAMP:20261011T152430Z UID:nhk0gr1iuom6ptj87su534i8fk@google.com CREATED:20260503T120153Z DESCRIPTION:The technology that underpins machine learning - differentiable programming - is poised to revolutionise astronomy\, making it possible f or the first time to fit very high dimensional models: hierarchical models describing every star in a survey\; the sensitivity of millions of pixels in a detector\; models of images or spectra with very many free parameter s\; or neural networks that represent physics we cannot easily solve in cl osed form. It also enables fundamental information-theoretic quantities li ke the Fisher information to be calculated\, allowing for determination an d optimization of the information content of an experiment. I will give an overview of recent work applying this to astronomy and in particular exop lanet science\, giving examples from imaging and time series data. LAST-MODIFIED:20260503T120154Z LOCATION:Zoom or DLT (host: Joyce Glass) \nZoom: https://anu.zoom.us/j/8297 4980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ben Pope (Macquarie U.) "Differentiable Physical Simulations for As tronomy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190201T033000Z DTEND:20190201T040000Z DTSTAMP:20261011T152429Z UID:dvt1ihar18a2162dp9kn32bbfg@google.com CREATED:20190108T053109Z DESCRIPTION:Understanding the formation and evolution of the first stars (P opulation III) has been an outstanding issue in the physics of the Early U niverse. First stars are believed to have formed at redshifts > 15 and wer e responsible for the metal enrichment and re-ionization of the primordial Universe. Thanks to computational resources\, some progress has been made in the last two decades in simulating the formation and subsequent evolut ion of these stars. However\, most of these simulations remain restricted by physical\, numerical or resolution-based limitations. In this thesis pr oposal talk\, I will describe my plans to carry out high-resolution magnet ohydrodynamical (MHD) simulations of primordial clouds where first stars f orm. In particular\, the three key areas where I plan to contribute in the field are: 1.) inclusion and realistic treatment of turbulence and magnet ic fields in the simulations\, 2.) connecting with cosmological simulation s by extracting dark matter mini-halos as precursors of primordial clouds and 3.) radiative transfer from massive protostars and mechanical feedback by protostellar jets and outflows. This research can help advance our kno wledge of the initial mass function (IMF) of the first stars which is cruc ial to understand the nature of the high-redshift Universe. LAST-MODIFIED:20190201T002606Z LOCATION:CSO Common Room (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Piyush Sharda (RSAA) "Formation of the First Stars (Thesis Proposal Talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150331T000000Z DTEND:20150331T010000Z DTSTAMP:20261011T152429Z UID:l2htne6gdc7mobcmc0utaonqh0@google.com CREATED:20150216T223217Z DESCRIPTION:Post-Asymptotic Giant Branch (post-AGB) stars bear signatures o f the entire chemical and morphological changes that occur prior to and du ring the AGB phase of evolution. In our recent studies\, we carried out an extensive low-resolution spectroscopic survey of post-AGB candidates in t he Magellanic Clouds. In this talk\, I will present two important outcomes of this survey. Firstly\, this survey resulted in a well characterised sa mple of binary and single post-AGB stars. Detailed chemical abundance stud ies of some of these objects have shown that they are chemically much more diverse than anticipated. As expected\, some of the single post-AGB objec ts are the most s-process enriched objects known to date while others\, th e likely binary objects\, are not enriched at all. However\, some objects show peculiar chemical signatures which do not correspond to the accepted single/binary star evolution and nucleosynthesis. In this talk\, I will pr esent this chemical diversity and its implications for widely accepted ste llar evolution and nucleosynthesis theories. Secondly\, one of the most im portant results of this survey is the serendipitous discovery of a group o f 'post- Red Giant Branch (post-RGB)' stars in the LMC and SMC. These are low-luminosity\, evolved\, dusty objects and they have mid-IR excesses and stellar parameters similar to those of post-AGB stars (late-G to late-A s pectral types\, low log g values\, and low metallicities with [Fe/H]~1.0). However\, their luminosities are much lower (200 - 2200Lsun) than that ex pected for post-AGB stars. It is likely that these objects are the result of a mass-loss that occurs via binary interaction on the RGB. In this talk \, I will present our analysis on this unexplored phase in binary evolutio n via evolutionary connections between the possible precursors (Sequence-E variables) and successors (systems with white dwarf [WD] components like sub-dwarf B stars or He-WDs). LAST-MODIFIED:20150325T034608Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Devika Kamath (Institute of Astronomy\, KU Leuven) "A new perspecti ve on single/binary star evolution and nucleosynthesis based on post-AGB a nd post-RGB stars in the Magellanic Clouds" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240604T010000Z DTEND:20240604T023000Z DTSTAMP:20261011T152429Z UID:74onormhnul1vo4o91jogngank@google.com CREATED:20231212T120233Z DESCRIPTION:How do planets evolve over time? Why are some planets gaseous\, while others are barren rocks? My research group is tracing the propertie s of the young planet population to understand how these newly formed plan ets evolve into the mature-aged population found around nearly every Sun-l ike star. I will detail our young planet census conducted with the NASA TE SS mission\, highlighting differences between the young planet population and the mature-aged demographics that are indicative of early atmospheric evolution. I will also present early results from our HST programs searchi ng for signatures of active mass loss in select young planetary systems. T ogether\, these programs already have the power to distinguish between pla net formation channels that are otherwise degenerate for mature planets. I n the coming years\, we aim to identify how some star-planet environments are suitable for terrestrial planets to retain atmospheres\, while others have their atmospheres stripped away. LAST-MODIFIED:20240505T101116Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Maya Jablonska) \nZoom: ht tps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:George Zhou (U. Southern Queensland) "The evolution of planets in t heir first hundred million years" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190412T040000Z DTEND:20190412T050000Z DTSTAMP:20261011T152429Z UID:ug626fv99dqbuo7hv9f8n1rq9c@google.com CREATED:20190312T234614Z DESCRIPTION:I will present the first results of the Pristine survey\, a Fra nco-Canadian photometric survey of the Milky Way halo performed with the n ew CaHK filter on CFHT's MegaCam. Currently covering ~5\,000 deg^2\, this survey leads to an efficient metallicity decomposition of the Milky Way ha lo. In particular\, I will show how efficient Pristine is in selecting the metal-poor end of the metallicity distribution ([Fe/H]<-2.5) to hunt for the very rare extremely metal-poor stars (bearer of the chemical imprint o f the first stars). Our spectroscopic follow-up campaign shows Pristine is very efficient at selecting very metal-poor stars from our photometry alo ne. A dedicated part of the survey also focuses on the enigmatic very fain t (and therefore metal-poor) Milky Way dwarf galaxies found over the last decade. I will show that Pristine can isolating likely member stars and th at it opens a well-needed window onto the detailed study of these systems that are often used as near-field cosmological probes. LAST-MODIFIED:20190403T012107Z LOCATION:CSO Common Room (host: Monty) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Nicolas Martin (CNRS Strasbourg) "Mining and mapping the first gene rations of stars with the Pristine CaH&K survey" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180605T010000Z DTEND:20180605T020000Z DTSTAMP:20261011T152429Z UID:eef7c7o9bginfi7nsg5vtuo7fk@google.com CREATED:20180508T001112Z DESCRIPTION:The ecosystem of a galaxy is driven by the balance between outf lows from the star-forming disk and infall due to interactions with nearby galaxies and the surrounding intergalactic medium. In the case of the Mil ky Way\, the number of stars being born has long been at odds with the det ected hydrogen fuel in the halo\, raising the important question of where the Milky Way predominantly gets its gas and its relationship to the surro unding halo. I will present my work using the Parkes Galactic All Sky Surv ey in HI to catalogue and study anomalous velocity hydrogen in the Galacti c halo. As part of this work\, we combined our data with a sensitive north ern-sky survey to reveal a halo hidden from the view of most large-scale s urveys\, changing our understanding of the neutral gaseous halo. We are cu rrently following up this result with SWISH\, a deep sightline survey usin g Parkes. While the 21cm emission line is a powerful tracer of neutral ato mic hydrogen (HI) in nearby galaxies like the Milky Way\, it is too weak t o be observable in the distant universe with current telescopes. In contra st\, 21cm absorption can be observed in individual galaxies over a wide ra nge in redshift and provides insight into the cosmic evolution of gas cont ent in galaxies. As part of the First Large Absorption Survey in HI (FLASH )\, we aim to study neutral gas across the Universe to z = 1\, in order to understand the relationship between supermassive black holes and the gas reservoir of their host galaxies. I will give an overview of FLASH and the observations carried out with ASKAP so far\, my specific focus on the rel ationship between soft X-ray absorption and HI absorption near the cores o f active galaxies and our future work as part of the SEAFOG radio/X-ray co llaboration. LAST-MODIFIED:20180526T034608Z LOCATION:Duffield Lecture Theatre (host: Panther) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Vanessa Moss (ASTRON) "Galactic ecosystems: Tracing neutral hydroge n and its evolution across the Universe" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260929T010000Z DTEND:20260929T020000Z DTSTAMP:20261011T152430Z UID:goamjceec15ftb1odcbq2pm2rc@google.com CREATED:20260503T114415Z DESCRIPTION:The combination of space based astrometry (Gaia) with spectrosc opic survey data from the ground is revolutionizing the way we can look at the structure and evolution of the Milky Way. Upcoming spectroscopic sur veys like WEAVE and 4MOST will further expand the reach of these studies c overing a substantial part of the Galaxy. Combined with advanced modeling techniques these tools put us in a position to systematically decompose th e Milky Way into its structural components and to disentangle the chemo-dy namical formation history of the Galaxy. These methods also enable us to look at the Galaxy as an "outside observer“ paving the way to systematic ally comparing the Milky Way against other galaxies. LAST-MODIFIED:20260923T120005Z LOCATION:Zoom or Duffield Lecture Theatre (host: Joyce Glass) \nZoom: https ://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Matthias Steinmetz (AIP) "Decomposing the Milky Way" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191108T041500Z DTEND:20191108T043000Z DTSTAMP:20261011T152429Z UID:gs1qdvj9j7bsfhfisa1k1gicb8@google.com CREATED:20191104T120105Z DESCRIPTION:The presentation will introduce PhB project on the statistical analysis of patterns in detected exoplanets. LAST-MODIFIED:20191106T131605Z LOCATION:AITC1 Meeting Room (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Andrew Rapp (RSAA/PhB) "The statistical analysis of patterns in det ected exoplanets" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190816T040000Z DTEND:20190816T043000Z DTSTAMP:20261011T152429Z UID:8smnu3c3mn9lf2c2j6h9cldjq0@google.com CREATED:20190725T160615Z DESCRIPTION:Gaia DR2 provides an unprecedented sample of stars with full 3D position and 3D velocity measurements\, creating the need for a self-cons istent means of discovering and characterising moving groups or associatio ns which are detectable as phase-space over densities. This is a critical step in piecing together the jigsaw puzzle that is the recent (<200 Myr) s tar formation history of our solar neighbourhood (<500 pc) which will not only help answer current star formation questions\, but also promises to a ssign a precise age to all nearby\, young stars. In this talk I will prese nt Chronostar\, a new Bayesian analysis tool that meets this need. Chronos tar uses the Expectation-Maximisation algorithm to remove the circular dep endency between association membership lists and the fits to their phase-s pace distributions. I will present on Chronostar’s successful independen t (re)discovery of the Beta Pictoris Moving Group\, as well as preliminary results on the decomposition of the Scorpius Centaurus OB association. Sc o-Cen has a complex formation history (with ages spanning from 3 Myr to 20 Myr) which has resulted in kinematic substructure that\, if untangled\, w ould provide insight into how this (and other) association(s) formed. LAST-MODIFIED:20190809T025107Z LOCATION:Duffield Lecture Theatre (host: Monty) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Timothy Crundall (University of Cologne) "Chronostar: a novel tool for the unsupervised discovery and ageing of stellar associations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190314T000000Z DTEND:20190314T010000Z DTSTAMP:20261011T152429Z UID:uom2k2vrhle9km4fi522cp9mro@google.com CREATED:20190110T003819Z DESCRIPTION:Nature Astronomy\, launched in January 2017\, is a new research journal published by Springer Nature. Sitting alongside our sister journa l Nature\, we aim to publish high impact research in the fields of astrono my\, astrophysics and planetary science. In this talk I will cover the mot ivation and scope of the journal\, the types of manuscripts we publish\, t he editorial process and what we look for in papers. I will also cover com mon pitfalls of writing and submitting papers and I will share hints and t ips on how to maximize the impact of your paper\, from writing an engaging but informative title and a properly contextualized but concise abstract\ , to structuring your paper in a way that your results are communicated su ccinctly. LAST-MODIFIED:20190219T114116Z LOCATION:CSO Common Room (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Marios Karouzos (Nature Astronomy) "How to publish (and write) an i mpactful paper in Nature Astronomy and beyond" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221123T000000Z DTEND:20221123T003000Z DTSTAMP:20261011T152429Z UID:d7hd4q46qg9ivm7g3jbn1vj6h0@google.com CREATED:20221020T054617Z DESCRIPTION:Studying planets over a wide range of ages is the next best thi ng to observing planet formation and evolution in real time. Planets and p lanetary systems evolve rapidly within the first few hundred million years post formation. During this time\, our own Earth lost its primordial hydr ogen-helium atmosphere\, and Jupiter and Saturn migrated to their present- day orbits. I will present our efforts to discover new planets around youn g stars with NASA's TESS mission\, and the follow-up programs we are condu cting to study the dynamical and atmospheric properties of these planets. Together\, these observations are offering a rare glimpse into universal m echanisms\, such as atmospheric mass-loss\, and planetary migration\, that shape all planetary systems. LAST-MODIFIED:20221120T033908Z LOCATION:DLT & ZOOM (host: Neco Kriel) \nZoom: https://anu.zoom.us/j/997853 41005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:George Zhou (University of Southern Queensland) "Evolving planets i n real time with TESS" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231003T000000Z DTEND:20231003T013000Z DTSTAMP:20261011T152429Z UID:b1m81ctd0vm4u2u8t282d5s1e0@google.com CREATED:20230807T023124Z DESCRIPTION:In recent years\, AI\, notably through advancements in Large La nguage Models (LLMs) such as ChatGPT\, has garnered significant attention both within academia and the broader public sphere. However\, these genera l-purpose LLMs have been criticized for their tendency to produce spurious or "hallucinated" information when grappling with specialized or technica l domains. To address this limitation\, we introduce the UniverseTBD Conso rtium - an international collaboration led in part by researchers here at RSAA and AITC\, comprising a diverse team of 30 active contributors from c omputer science and astronomy. Our mission is to democratize the field of astronomy by developing public-facing\, AI-driven large language model too ls specialized for this discipline. Our research presents the first astron omy-centric LLM\, AstroLLaMa\, that can produces text completion and embed ding that outperform GPT models. We also show that LLMs can generate scien tific hypotheses of a complexity comparable to those produced by human exp erts through techniques such as in-context prompting and fine-tuning on do main-specific literature. Moreover\, we posit that these specialized found ational models can revolutionize the methods we employ for literature sear ches and the tracing of intellectual developments within the field. We arg ue that the domain of physical sciences\, particularly astronomy\, serves as an ideal test bed for investigating the potential of modern LLMs. This inquiry stands to fundamentally reshape our understanding of both artifici al and human intelligence and the boundaries of accumulated knowledge. LAST-MODIFIED:20230917T132611Z LOCATION:TBD (host: Mark) \nZoom: https://anu.zoom.us/j/83410388355?pwd=Qm9 CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Yuan-Sen Ting (RSAA) "Can Artificial Intelligence Generate Meaningf ul Scientific Hypotheses?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250624T010000Z DTEND:20250624T020000Z DTSTAMP:20261011T152429Z UID:a3gqbg0h0m0emrei5l5f95io4s@google.com CREATED:20250520T123614Z DESCRIPTION:The Sun's magnetic field is generated somewhere in the interior and emerges onto the surface. Understanding which flows in the Sun are re sponsible for the generation of these magnetically active regions will con strain the location of the solar dynamo in the interior. The Helioseismic and Magnetic Imager onboard NASA's space-based Solar Dynamics Observatory mission has been instrumental in enabling helioseismic investigations of t he observed flows associated with emerging active regions. Recent observat ional results point to convection playing an important role in active regi on formation\, and that all active regions are associated with a convergin g flow in the day preceding emergence. Coupled with sophisticated numerica l simulations\, the interpretation of the observations is challenging the prevailing idea that magnetically active regions on the surface of the Sun have their origins in a deep seated solar dynamo mechanism. LAST-MODIFIED:20250623T235606Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Arunima) \nZoom: https://a nu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Hannah Schunker (U Newcastle) "The role of convection during magnet ic active region emergence on the Sun" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171110T030000Z DTEND:20171110T040000Z DTSTAMP:20261011T152429Z UID:ti2fat9e4vg13skb8m1m7ri31o@google.com CREATED:20171016T121608Z DESCRIPTION:Galaxies grow through the accretion of gas\, minor mergers and major mergers in the hierarchical picture of galaxy evolution. The merging of two gas-rich galaxies cause gas to be driven towards the centres of th e individual galaxies producing intense circum-nuclear star formation and creating a fuel reservoir for the accretion onto the central blackhole. Fe edback due to supernova winds or AGN (Active Galactic Nuclei) accretion bl ows out the surrounding gas through an outflow at later merger stages\, th at may be large enough to deplete the galaxies of their fuel reservoir and hence shut down star formation and starve the central black hole. It is s till uncertain what the impact of outflows is on merging galaxies\, and wh en in the merging process they are most significant. This thesis used Inte gral Field Spectroscopy (IFS) observations of merging galaxies to probe th e impact of outflows on gas-rich major mergers. Using velocity-resolved ab sorption and emission lines arising from the interstellar medium of the ga laxies\, this thesis presentation will show that the occurrence of outflow s increases with merger stage and also that these outflows are not be caus ed by the same physical processes\, such as starformation or an AGN\, in e ach merger system. LAST-MODIFIED:20171101T231111Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Elise Hampton (ANU) "Dissecting Merging Galaxies Using Integral Fie ld Spectroscopy: A Thesis Presentation" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231031T000000Z DTEND:20231031T013000Z DTSTAMP:20261011T152429Z UID:dutn89cvaud161mma7t9f2grro@google.com CREATED:20230917T235115Z DESCRIPTION:The IceCube Neutrino Observatory at the South Pole has been ful ly operational for over a decade. With a cubic kilometre of deep ice as th e detection volume\, the detector has seen thousands of astrophysical neut rinos from across the sky. Initially\, these were observed as an unresolve d diffuse flux\, but with recent improvements in event selection and recon struction the first distinct sources are starting to emerge - the nearby A GN NGC1068 has been revealed as the first steady emitter of high-energy ne utrinos. More recently\, IceCube has revealed that our own galaxy is a sou rce of high energy neutrinos\, likely from populations of as-yet unresolve d particle acceleration environments in the galactic plane. We will also d iscuss results in various areas of particle physics that are accessible wi th the astrophysical neutrinos and the even greater flux of background atm ospheric neutrinos\, and outline plans for the future expansion of the det ector into IceCube-Gen2 -- which would more than double the number of stri ngs in the ice\, and vastly expand the detection volume. LAST-MODIFIED:20231019T131109Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Sven Buder) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Gary Hill (U. Adelaide) "Neutrino astronomy with IceCube at the Sou th Pole" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190322T033000Z DTEND:20190322T040000Z DTSTAMP:20261011T152429Z UID:nma2kqabr3ai0vl3bgjfm8qg9o@google.com CREATED:20190218T011719Z DESCRIPTION:Galactic Archaeology in the light of 3D NLTE spectrum formation LAST-MODIFIED:20190322T000106Z LOCATION:CSO Common Room (host: Pingel) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:abdu Abohalima (RSAA) "Galactic Archaeology in the light of 3D NLTE spectrum formation (Thesis proposal talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200303T000000Z DTEND:20200303T010000Z DTSTAMP:20261011T152429Z UID:t84feivk9su7il6c6pcf4pdsrg@google.com CREATED:20200217T054605Z DESCRIPTION:The 2020's is set to be the decade of mega-constellations and c heap access to space. But humanity is largely unprepared for the increased risk of in-orbit collisions associated with each new object that we launc h. New technology is required to prevent a run-away cascade of collisions which could render entire orbital regions unusable. At the DLR Institute of Technical Physics\, we believe that space debris is a problem with an o ptical solution. This talk covers our research into optical technologies f or the tracking and removal of space debris\, including satellite laser ra nging\, debris laser ranging\, and light curve analysis. LAST-MODIFIED:20200224T110607Z LOCATION:Duffield Lecture Theatre (host: Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ewan Schafer (DLR (German Aerospace Centre)) "Optical Technologies for Preventing Collisions in Orbit: Shining a Light on the Growing Problem of Space Debris" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170803T010000Z DTEND:20170803T020000Z DTSTAMP:20261011T152429Z UID:rdah700huiejrrbk9i6goa11og@google.com CREATED:20170719T020110Z DESCRIPTION:Our view of exoplanets is one derived primarily from Solar-like stars with a strong focus on understanding our Solar System. Our knowledg e about the properties of exoplanets around so called low-mass stars or M dwarfs is much more cursory. The discovery of Proxima b was an exciting de velopment though it should not have been a big surprise because (1) red dw arfs are the most numerous stars\, (2) previous surveys already indicated an abundance of small planets in compact orbits around red dwarfs\, and (3 ) warm terrestrial planets around red dwarfs are 50 to 100 times easier to detect than around Sun-like stars. Based on combining radial velocities o f nearby M dwarfs obtained with HARPS\, UVES and HIRES data we find many n ew M dwarf planets. By computing the estimated detection probability funct ion the occurrence rate of planets less than 10 Earth masses around nearby M dwarfs is found to be around two planet per star. Techniques to overcom e the practical issue of obtaining good quality radial velocity data for M dwarfs are considered: (1) the wavelength sensitivity of radial velocity signals\, (2) the combination of radial velocity data from different exper iments for robust detection of small amplitude signals and (3) optimum sel ection of targets. LAST-MODIFIED:20170719T020110Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Hugh Jones (University of Hertfordshire) "Planets around nearby M d warfs" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250422T010000Z DTEND:20250422T020000Z DTSTAMP:20261011T152429Z UID:cng38sh98l2bthkdogd5mo9r14@google.com CREATED:20250106T230126Z DESCRIPTION:Mergers of galaxy clusters represent the most energetic events since the Big Bang\, releasing energies up to 10^64 ergs over Gyr timescal es. This energy is dissipated through shocks and turbulence in the intracl uster medium\, transforming clusters into the Universe’s largest laborat ories for studying cosmic ray acceleration and magnetic field amplificatio n. However\, our understanding has largely been limited to massive and nea rby clusters due to observational constraints. In this talk\, I will show how observations at the longest wavelengths observable from the ground are revealing new insights into both turbulence and magnetic field amplificat ion. Additionally\, I will discuss how advances in radio polarimetry and n ew surveys such as POSSUM are revealing the first detailed magnetic field structures within individual clusters. LAST-MODIFIED:20250406T234109Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Cameron van Eck) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Erik Osinga (U. Toronto) "Galaxy clusters as the Universe’s large st particle accelerators" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220915T010000Z DTEND:20220915T013000Z DTSTAMP:20261011T152429Z UID:j4p0738fkra72ikcana9kfmq64@google.com CREATED:20220913T004607Z DESCRIPTION:The inherent differentiable nature of optics provides opportuni ties to harness the powerful tools of machine learning. Automatic differen tiation underpins the rise of machine learning in the modern world\, enabl ing the optimisation of million and billion parameter models\, shedding th e curse of dimensionality. By constructing optical models within automatic differentiation frameworks\, simple approaches to challenging problems ar ise\, and access to even more powerful optimisation and inference algorith ms is granted. dLux is a recently developed fully differentiable open-sour ce optical modelling framework that enables users to take full advantage o f these benefits. LAST-MODIFIED:20220913T004607Z LOCATION:DLT & ZOOM (host: TBD) \nZoom: https://anu.zoom.us/j/99785341005?p wd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Louis Desdoigts (University of Sydney) "Differentiable Optics & dLu x" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240208T000000Z DTEND:20240208T010000Z DTSTAMP:20261011T152429Z UID:5n2mnto8784hfgcnc5j7p1t5co@google.com CREATED:20231120T225122Z DESCRIPTION:Over the past century\, black holes transitioned from theoretic al constructs to ubiquitous entities in the Universe. Extensive evidence s upports the notion that supermassive black holes\, which reside in the nuc lear region of most mature galaxies\, play an integral role in the assembl y and dynamics of galactic material on cosmological timescales. However\, the rapid evolution of supermassive black holes and their immediate enviro nments in the early Universe (<= 1 Gyr) is still poorly understood due to the paucity of robust constraints on physical accretion mechanisms\, the l imited statistical significance of available samples\, and the scarcity of independent methodologies of black hole characterisation. My work traces the evolution of super-massive black holes at high redshifts (z ~ 5) using highly complete quasar samples with robustly-measured spectrophotometric properties. I build a spectroscopic analysis tool specifically designed fo r quasar spectra and apply it to a high-redshift quasar samples\, measurin g emission-lines (e.g. Si IV 1398\, O IV 1402\, C IV 1549\, Mg II 2799\, H beta 4863) and inferring black hole properties from mass\, luminosity\, an d metallicity-sensitive features. I also present an analysis of quasar dem ographics in a z ~ 5 sample\, measuring supermassive black hole growth. Fu rthermore\, I showcase how thermal accretion disc models can be used to de scribe quasar spectral energy distributions. This approach has potential a s a physically-motivated independent method that can aid in constraining p roperties of black holes. In summary\, this research yields insights into the understanding of high-redshift supermassive black holes and their grow th\, equipping us with the necessary tools for detailed studies of quasar spectra. LAST-MODIFIED:20240122T233109Z LOCATION:Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.zoom.us/j /83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Samuel Lai (RSAA) "High-Redshift Ultraluminous Quasi-Stellar Object s (End-of-Thesis Talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230523T010000Z DTEND:20230523T020000Z DTSTAMP:20261011T152429Z UID:hevlfku6nt3jnmgq6u7pfd0l9g@google.com CREATED:20230521T073206Z DESCRIPTION:The processes regulating star formation in galaxies act across many orders of magnitude in spatial scale. Thus\, a key challenge in under standing star formation is bridging the small-scale physics within molecul ar clouds and the large-scale structure of spiral galaxies. Fully constrai ning the physics of star formation across these scales requires constraint s on both the 3D spatial structure and dynamical state of the interstellar medium (ISM)\, the combination of which has been an essentially unknown q uantity in the field of star formation research. In this talk\, I will dis cuss ongoing efforts to construct high-dimensional models of the ISM in th e solar neighborhood by combining data science and visualization technique s with wide-field photometric\, astrometric\, and spectroscopic surveys. O n kiloparsec scales\, I will discuss how "3D dust mapping" has enabled con straints on the global distribution of molecular clouds\, revealing new li nks between clouds long thought to be isolated and challenging fundamental assumptions about the shape and position of a nearby spiral arm. On parse c scales\, I will show how combining 3D dust mapping with the 3D space mot ions of young stars can explain the origin of all local star formation as being driven by the expansion of the Local Bubble\, the nearest superbubbl e to the Sun. Finally\, on au-scales\, I will discuss the implications tha t the Sun's trajectory through the ISM has for the properties of the helio sphere and the geological record here on Earth. I will conclude by preview ing the opportunities enabled by future infrared surveys\, including SDSS- V and Roman\, which together will pave the way for a unified understanding of the multi-scale physical processes shaping star formation in diverse e nvironments across the Milky Way's disk. LAST-MODIFIED:20230521T073206Z LOCATION:ZOOM (host: Takafumi) \nZoom: https://anu.zoom.us/j/84138346977?pw d=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Catherine Zucker (Space Telescope Science Institute) "Tracing Star Formation Across Scales: A Case Study in the Solar Neighborhood" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260423T013000Z DTEND:20260423T023000Z DTSTAMP:20261011T152430Z UID:6uvlbe1dh4pa912mti69hepkvo@google.com CREATED:20260503T120159Z DESCRIPTION:The Milky Way's nuclear wind ejects multiphase gas from the Gal actic Centre\, yet the origin\, survival\, and mass of cold molecular clou ds within this outflow remain poorly understood. Cold gas should be rapidl y destroyed by hydrodynamic instabilities when embedded in a hot wind\, an d yet\, high-resolution observations reveal these clouds at kiloparsec dis tances from the disc\, travelling at hundreds of kilometres per second. Th is represents a fundamental gap in our understanding of galactic feedback. \nThis thesis addresses three questions: what is the chemical composition of these clouds\, where do they originate\, and how much cold gas does th e wind carry? I show that the clouds have anomalous HI-to-CO ratios incons istent with standard ISM physics\, and that these ratios cannot be reprodu ced by gas in chemical equilibrium. Instead\, they are consistent with dis c molecular clouds that have had their atomic envelopes stripped by the wi nd and have not yet re-equilibrated. These results demonstrate a disc orig in is possible and implies that their masses have been systematically unde restimated. These results establish non-equilibrium chemistry as a core me chanism in cold galactic outflows. LAST-MODIFIED:20260503T120159Z LOCATION:Zoom or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Karlie Noon (RSAA) "Deciphering the Cold chemistry of the Milky Way ’s nuclear wind (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241219T000000Z DTEND:20241219T010000Z DTSTAMP:20261011T152429Z UID:bmqbluphrc3ldcp5hj079qqo20@google.com CREATED:20241107T114115Z DESCRIPTION:I will provide an overview of the ESO instrumentation programme for VLT and ELT. I will first focus on the future instruments for the VLT and VLTI. Among all the planned instruments\, I will describe MAVIS for t he VLT (led by Australia) and then focus on the upcoming MOONS (for the VL T) and 4MOST (for VISTA) multi-objects spectrographs\, discussing their st atus and the science goals of their large-scale spectroscopic surveys. I w ill then highlight the key science drivers of the new ESO's flagship facil ity: the Extremely Large Telescope. The ELT is now under construction and with its 39-metre primary mirror it will be the largest optical/near-IR te lescope in the world. I will present an overview of the ELT Programme\, fo cusing on the latest status of the telescope\, its instrumentation and sci ence capabilities. LAST-MODIFIED:20241125T223611Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Francois Rigaut) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Michele Cirasuolo (ESO) "From VLT to ELT" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151106T032000Z DTEND:20151106T034000Z DTSTAMP:20261011T152429Z UID:s17icvmft26hnn8fjfof924gko@google.com CREATED:20151029T013606Z DESCRIPTION:I will present theresults from a deep\, extended\, planetary ne bulae survey in a 0.5 sqdeg region centered on the brightest cluster galax y NGC 4486 (M87) in the Virgo cluster core\, carried out with SuprimeCam@S ubaru and FLAMES-GIRAFFE@VLT. Two PN populations are identified out to 150 kpc distance from the center of M87. One population is associated with th e M87 halo and the second one with the intracluster light in the Virgo clu ster core. They have different line-of-sight velocity and spatial distribu tions\, as well as different planetary nebulae specific frequencies and lu minosity functions. The intracluster planetary nebulae in the surveyed reg ion correspond to a luminosity of four times the luminosity of the Large M agellanic Cloud. The M87 halo planetary nebulae trace an older\, more meta l-rich\, parent stellar population. A substructure detected in the project ed phase-space of the line-of-sight velocity vs. major axis distance for t he M87 halo planetary nebulae provides evidence for the recent accretion e vent of a satellite galaxy with luminosity twice that of M33. The satellit e stars were tidally stripped about 1 Gyr ago\, and reached apocenter at a major axis distance of 60-90 kpc from the center of M87. The M87 halo is still growing significantly at the distances where the substructure is det ected. LAST-MODIFIED:20151102T114606Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Magda Arnaboldi (ESO) "The intracluster light in the Virgo cluster core and the mass assembly of the outer halo of NGC 4486 (M87)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150129T000000Z DTEND:20150129T010000Z DTSTAMP:20261011T152430Z UID:d9an02mrt8idvmjogsntf5n784@google.com CREATED:20141205T041610Z DESCRIPTION:Quasar microlensing is a unique probe of quasar structure\, fro m the broad emission line region down to the accretion disc and the superm assive black hole. Moreover\, it can be used to study the mass distributio n of the galaxy-lens and perform measurements of Hubble's constant. So far \, only single\, or small collections\, of lensed quasars have been studie d using microlensing techniques due to the observational and computational challenges involved. However\, this is about to change by the imminent di scoveries of the upcoming all-sky survey facilities (e.g. SkyMapper\, LSST ). I will present results\, data\, and tools from the GPU-Enabled High-Res olution MicroLensing parameter survey (GERLUMPH). In particular\, I will s ystematically investigate modeling properties across the parameter space\, to answer how well we will be able to constrain quasar structure in the f uture. Moreover\, I will demonstrate how our eResearch infrastructure\, vi z. database and web interface to TB-sized microlensing simulations\, compl emented by advanced eTools for an end-to-end online analysis of lensed sys tems\, can accelerate the rate of scientific discovery. Such an online res ource would dramatically speed-up the consistent and systematic study of l arge collections of these systems\, using just a web browser at the user e nd. LAST-MODIFIED:20250925T231031Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Giorgios Vernardos (Swinburne University) "Data Intensive Quasar Mi crolensing" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260730T010000Z DTEND:20260730T020000Z DTSTAMP:20261011T152430Z UID:3pemkop1mpt2tsipoascg4j8kg@google.com CREATED:20260605T021616Z DESCRIPTION:Galaxy mergers and interactions drive substantial changes in ga laxies\, and have been shown to enhance SFRs and disrupt kinematics. The i mpacts of interactions have been extensively investigated in the local uni verse (z~0)\, however\, observational studies at z > 1 are limited. As a r esult\, the evolution of interaction-driven changes across cosmic time is still unclear. By leveraging new analysis techniques and measurements from JWST\, in this EoT talk I will explore the impact of interactions on SFRs \, ionised gas turbulence and stellar disc thicknesses of star-forming gal axies at cosmic noon (z~1-2) and compare the results to those at z~0 to he lp to better constrain interaction-driven changes across cosmic time. LAST-MODIFIED:20260722T060006Z LOCATION:Zoom or Duffield Lecture Theatre (host: TBC) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Isaac Kanowski (RSAA) "Characterising the impact of interactions on galaxies at cosmic noon (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150702T010000Z DTEND:20150702T020000Z DTSTAMP:20261011T152429Z UID:9hjj96hv3l463k9srtjho4esr0@google.com CREATED:20150616T114609Z DESCRIPTION:With experiments returning a vast amount of data\, the ability of humans to explore that data unaided is diminishing. Computers provide a way to query large volumes of data in an efficient manner through the use of databases and Structured Query Language (SQL). However\, in order to u se these technologies\, the data must be digital and machine understandabl e. This presentation will give a brief overview of standardised data forma ts\, how to get your data ready\, applications of databases\, and the type s of questions that databases can answer. LAST-MODIFIED:20150625T044107Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rowan Edwards (ANU) "Databases For Astronomy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160304T030000Z DTEND:20160304T032000Z DTSTAMP:20261011T152429Z UID:ebe40g3v93hremojcarbh2fcss@google.com CREATED:20160209T000612Z DESCRIPTION:The radial distribution of metallicity of star-forming galaxies in a galaxy cluster can inform us about the mass assembly and enrichment history of the galaxy cluster. This paper presents observation of radial d istribution of global metallicity of star-forming galaxies in two CLASH cl usters. We present the first observation of ra- dial distribution of clust er member metallicity in galaxy clusters. The two CLASH clusters\, MACS111 5+01 and RXJ1532+30\, were observed with DEIMOS spectro- graph at Keck-II telescope. Both galaxy clusters are cool-core clusters at redshift z ≃ 0 .35. We identified 22 (14 - emission line galaxies) and 36 (21 - emission line galaxies) cluster members for MACS1115+01 and RXJ1532+30 respectively . ISM properties such as metallicity and ionization parameter\, were estim ated using emission line ratios [NII]/Hα\, [NII]/[SII] and [OIII]/Hβ. Th e gas-phase metallicity of star- forming galaxies in MACS1115+01 exhibit a nti-correlation with projected distance −0.15 ± 0.08 dex/Mpc\, whereas the radial metallicity distribution of RXJ1532+30 is statistically flat ( −0.09 ± 0.12 dex/Mpc). In addition\, the mass-metallicity relation of M ACS1115+01 has 0.2 dex offset metallicity than the local comparison sample \, but the RXJ1532+30 mass-metallicity relation is statistically similar t o the local comparison sample. The negative radial abundance gradient of M ACS1115+01 suggests the impact of cluster environment via ram pressure str ipping\, strangulation on galaxy evolution. Our observations suggests towa rds the un-relaxed dynamical state of RXJ1532+30\, which in turn explains the observed flat metallicity gradient of RXJ1532+30. We compare our metal licity gradient observations with the metallicity gradient in galaxy clust er simulations (Rhapsody-G) after matching with the concentration paramete r. The star-forming galaxies in simulated cluster also exhibit a slight ne gative abundance gradient of −0.04 ± 0.03 dex/Mpc\, however the slope i s significantly smaller than the observations. LAST-MODIFIED:20160229T052105Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anshu Gupta (RSAA) "Radial Distribution of gas-phase metallicities of galaxies in two CLASH clusters at z ~ 0.35" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190312T000000Z DTEND:20190312T010000Z DTSTAMP:20261011T152429Z UID:06gle1et7n2idlj7bl7244d1pc@google.com CREATED:20181206T232616Z DESCRIPTION:One key problem in astrophysics is understanding how and why ga laxies stop forming stars. The exact mechanisms that lead to the disruptio n of the gas supply\, the relative importance of different quenching mecha nisms\, and the timescales involved are still poorly understood. Post-star burst galaxies are an ideal laboratory to study the galaxy transition proc ess as they have undergone a recent\, rapid shutdown in star formation. My recent work showed that post-starburst galaxies are not completely devoid of gas\, which challenges the rapid quenching mode thought to form the qu iescent population. Using wide-area photometric and spectroscopic surveys\ , I will describe what the stellar\, gas\, dust properties of post-starbur st galaxies reveal about the processes causing galaxies to transition from star forming to quiescent. LAST-MODIFIED:20190304T010109Z LOCATION:CSO Common Room (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kate Rowlands (Johns Hopkins University) "Caught in the act: Using post-starburst galaxies to chart galaxy transformation over cosmic time" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180614T010000Z DTEND:20180614T020000Z DTSTAMP:20261011T152429Z UID:3jmjti064ph43b4m7goc8rb9sk@google.com CREATED:20180403T035617Z DESCRIPTION:Type Ia supernovae (SNe Ia) have been instrumental in arriving at our current understanding of the Universe\, from first indicating its a ccelerated expansion in the late 1990s\, to now continuing to improve cosm ological constraints. In particular\, SNe Ia are a powerful probe for the quantities that parametrise LambdaCDM\, and the equation-of-state paramete r w for dark energy. The paradigm for cosmology is now to diminish systema tic errors to obtain precise measurements\, while making observations furt her into the past to measure dark energy. More locally\, the Hubble consta nt H_0 determines the expansion rate of the Universe at present\, normalis ing its distance scale. In the past several years\, the precise value of H _0 has come into contention\, with a significant discrepancy between resul ts determined from a local distance ladder\, and those inferred from obser vations of the early Universe. Taken at face value\, this discrepancy coul d signal systematic errors in either measurement\, or inaccurate assumptio ns about the model. I will discuss these questions at both ends of the Uni verse's expansion history. In the works in my thesis\, I have developed a framework for performing precise cosmological analyses of SN Ia samples\, utilising current best methods to account for the statistical and systemat ic uncertainties by using full covariance matrices\, combined with probabi listic Bayesian methods to estimate cosmological parameters and uncertaint ies. I have applied these methods to supernova data in SH0ES (Riess et al. 2011) and the Dark Energy Survey to address the tension in the Hubble con stant locally\, and the nature of dark energy at higher redshifts. LAST-MODIFIED:20180614T024606Z LOCATION:Duffield Lecture Theatre (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Bonnie Zhang (RSAA) "Precision cosmology with type Ia supernovae: t he Hubble constant and dark energy (End-of-thesis colloquium)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181220T000000Z DTEND:20181220T010000Z DTSTAMP:20261011T152429Z UID:gj964hj96clc72n64bcnnc0qgk@google.com CREATED:20181217T132105Z DESCRIPTION:In this talk\, I'll begin by giving a broad overview of the rec ent work by our group on star and galaxy formation. The most fundamental u nsolved problems in these fields all revolve around "feedback" from massiv e stars (and black holes)\, which new generations of theoretical models an d simulations are now able to incorporate with increasing predictive power . I'll describe how we (and the community in general) has been able to "bu ild up" models of feedback from protostars through the inter-galactic medi um\, and how the competition between gravity and these processes naturally gives rise to a variety of "universal" scalings and properties of stars a nd galaxies. In the second half of the talk\, I'll describe the properties of a remarkable newly-discovered class of instabilities which exist in an y system containing dust and gas. These instabilities come in an infinite variety of "flavors" and can have remarkably diverse outcomes. I'll discus s how this can qualitatively change our predictions for dust growth and ev olution\; ISM chemistry\; stellar abundance patterns\; wind-launching in c ool stars and AGN torii\; dust obscuration\; and planet formation. LAST-MODIFIED:20181219T011105Z LOCATION:CSO Common Room (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Philip Hopkins (Caltech) "Cosmic "Dust" (Galaxies\, Stars\, & Actua l Dust!)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141216T000000Z DTEND:20141216T010000Z DTSTAMP:20261011T152430Z UID:8ulatfj9tub1trar5lm41rq1rg@google.com CREATED:20141117T060342Z DESCRIPTION:The exploration of the outer Solar System has reached an exciti ng point: we are now beginning to understand its dynamical structure\, scu lpted into existence by giant planet migration in the early history of the Solar System. We have designed a survey using 560 hours of Canada-France- Hawaii Telescope (CFHT) time over four years to provide hundreds of new tr ans-Neptunian objects with exquisitely characterised\, high-precision orbi ts. This new wide-field optical survey began observations with CFHT MegaPr ime in February 2013\, and by its conclusion in 2016 aims to have doubled the number of trans-Neptunian objects suitable for testing models of Solar System history. In April\, we were granted a four-year Large Program of 3 86 hours on Gemini North to measure the broad-band colours of the brightes t OSSOS discoveries. These optical and near-IR observations are designed t o allow us to disentangle the complex interplay between the compositions o f planetesimals as they form in the disk\, and the later evolutionary proc esses that act on their icy surfaces. LAST-MODIFIED:20250925T231027Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Michele Bannister (University of Victoria) "Mapping the Deep: First Discoveries from the Outer Solar System Origins Survey" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220531T010000Z DTEND:20220531T020000Z DTSTAMP:20261011T152429Z UID:ibsrtr2p7uclrid8a2rkc5qvqs@google.com CREATED:20220419T012617Z DESCRIPTION:Astronomers now know that supermassive black holes are in nearl y every galaxy. Though these black holes are an observational certainty\, nearly every aspect of their evolution -- from their birth\, to their fuel source\, to their basic dynamics -- is a matter of lively debate. Fortun ately\, LISA\, a space-based gravitational wave observatory set to launch in 2034\, will revolutionize this field by providing data that is compleme ntary to electromagnetic observations as well as data in regimes that are electromagnetically dark. This talk will touch on our current understandin g of how SMBHs form\, evolve\, and alter their galaxy host\, and will outl ine the theoretical\, computational and observational work needed to make the most of LISA observations. LAST-MODIFIED:20220525T024207Z LOCATION:DLT & ZOOM (host: Shyam Menon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kelly Holley-Bockelmann (Vanderbilt University) "Invited Colloquium : Supermassive Black Holes as Revealed by LISA: How Gravitational Wave Ast ronomy Will be a Game Changer" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231207T000000Z DTEND:20231207T010000Z DTSTAMP:20261011T152429Z UID:se5gglbh7tpj6keh658tbpo4gc@google.com CREATED:20231112T225113Z DESCRIPTION:Since launching on Christmas Day\, 2021\, JWST has produced spe ctacular views of the Universe\, both near and far. I will describe observ ations of some of the most distant galaxies yet through near-infrared spec troscopy with NIRSpec. With my colleagues on the NIRSpec and NIRCam instru ment science teams of JWST\, we are undertaking large JADES survey to expl ore galaxy evolution into the epoch of reionization (the first billion yea rs of history). We have recently spectroscopically confirmed galaxies at r edshifts beyond 10 for the first time\, including spectacular spectrum of a galaxy which unexpectedly has Lyman-alpha in emission\, as well as a sug gestion of non-standard elemental abundance ratios. I will discuss the imp lications of these recent discoveries for our understanding of galaxy evol ution\, and the potential role of star-forming galaxies at redshifts beyon d 6 in reionizing the inter-galactic medium. LAST-MODIFIED:20231112T225113Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Emily Wisnioski) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Andy Bunker (Oxford U.) "JWST at the edge of the Universe -- findin g galaxies in the epoch of reionization with NIRSpec" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210909T000000Z DTEND:20210909T004500Z DTSTAMP:20261011T152429Z UID:48a7ij5mbcfkiqg4b02mugqvus@google.com CREATED:20210816T035104Z DESCRIPTION:High contrast interferometry for studying the LSP Phenomenon LAST-MODIFIED:20210908T231606Z LOCATION:ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Benjamin Courtney-Barrer (RSAA) "Thesis Proposal Talk" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231127T020000Z DTEND:20231127T030000Z DTSTAMP:20261011T152429Z UID:ldt0lnt26s2r17i4pjq752nni8@google.com CREATED:20231125T012106Z DESCRIPTION:A mid-infrared nulling interferometer offers a highly promising approach to detect and characterize thermal light from terrestrial planet s within the habitable zones around nearby stars. The main challenge intri nsic to this ambitious goal lies in the deployment of formation flying int erferometry to spatially resolve the faint planet from its host star at mi d-infrared wavelengths. The European Space Agency (ESA) has recognized the Large Interferometer for Exoplanets (LIFE) employing mid-infrared nulling interferometry as a potential candidate for L-class missions in the 2040s . However\, there are no concrete steps towards the realization of LIFE in the domain of formation flight technology. The Pyxis team and Japan plan to launch stellar interferometers using small satellites and CubeSats as t he first step. In this seminar\, we briefly introduce an overview of the o ngoing initiatives in formation flying interferometry within Japan and dis cuss why the collaboration between Pyxis and Japan is essential. LAST-MODIFIED:20231125T012106Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mike Ireland) \nZoom: http s://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Taro Matsuo and Hirotaka Kondo (Nagoya University) "Future collabor ation between Pyxis and Japan towards the realization of space interferome try" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201113T030000Z DTEND:20201113T033000Z DTSTAMP:20261011T152429Z UID:9b2012s53b9o12p30seelm7nqg@google.com CREATED:20201022T005111Z DESCRIPTION:The evolution of molecular clouds and star formation is fundame ntally controlled by turbulence. However\, methods for accurately measurin g the turbulent velocity dispersion of clouds\, particularly in clouds tha t include systematic motion\, such as rotation\, are not well defined. Mot ivated by this\, we have developed a new method to recover the three-dimen sional turbulence of clouds from observable data. We simulated a rotating turbulent\, collapsing molecular cloud and compared its intrinsic 3D turbu lent velocity dispersion with measures of the turbulent velocity dispersio n accessible from observational data. We found that after applying suitabl e filters to the moment maps\, the intrinsic turbulent velocity dispersio n of the cloud could be recovered from the spatial mean of the second-mome nt map or from the standard deviation of the rotation-corrected first-mome nt map by multiplying by an empirically determined factor\, which is reaso nably universal\, i.e.\, it does not significantly depend on the evolution ary stage of the cloud\, the column density threshold\, or the telescope r esolution (as long as the resolution is better than 0.1 pc). LAST-MODIFIED:20201110T064609Z LOCATION:ZOOM 997 8534 1005 (host: Wibking) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Madeleine Stewart (RSAA) "ASC project: A new method for measuring t he 3D turbulent velocity dispersion from position-position-velocity observ ations of molecular clouds" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160212T030000Z DTEND:20160212T032000Z DTSTAMP:20261011T152430Z UID:51t03dubf9a3c090fc4rmtcdp0@google.com CREATED:20151214T010109Z DESCRIPTION:Over the last two years\, we've developed and run a set of four astrophysics MOOCs (Massive Open Online Courses)\, offered for free to an yone in the world who wants to take them. Around a quarter of a million st udents from 180 countries have enrolled in the courses - considerably more than have graduated from the ANU science it was founded. I'll present the lessons learned from this experience. LAST-MODIFIED:20160211T233104Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Paul Francis (RSAA) "MOOCS (Massive Open Online Courses) - lessons learned" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230907T010000Z DTEND:20230907T023000Z DTSTAMP:20261011T152429Z UID:268ghueo5l2m19doq6togflno0@google.com CREATED:20230828T014611Z DESCRIPTION:Kernel-nulling is a beam combination architecture and data redu ction technique for a nulling interferometer optimized for the high-contra st detection of giant exoplanets at high angular resolutions. We present a 4-input beam nuller that creates one bright\, and three nulled outputs. A pair of nulled outputs possess the same response to instrumental/environm ental perturbations while still producing distinct responses to off-axis l ight. The linear combination of these outputs will result in a kernel-null observable which is robust to phase perturbations\, removing the dominant source of noise in conventional nulling. While the traditional approach i s to use bulk-optics based interferometers\, here we present a photonic ap proach where all the necessary routing\, beam splitting\, and recombinatio n is performed within a 16 x 16 mm chip. LAST-MODIFIED:20230831T001610Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Peter Chingaipe (Observatoire de la Cote d'Azur) "Kernel-nulling at the VLTI" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240308T030000Z DTEND:20240308T040000Z DTSTAMP:20261011T152429Z UID:q60metp7ibk0c31do0ac4ck7d0@google.com CREATED:20240204T231618Z DESCRIPTION:TBC LAST-MODIFIED:20240204T231618Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Emily Wisnioski) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Thesis oversight committee (RSAA) "Student thesis proposal talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240430T010000Z DTEND:20240430T023000Z DTSTAMP:20261011T152429Z UID:d8uq6k38kcli86j3atj3rdkqjc@google.com CREATED:20231212T120228Z DESCRIPTION:I will present our recent work using quasars and radio galaxies to confront the cosmological principle\, the idea that sits at the heart of modern cosmological theories. Whilst the cosmological principle states that the universe is isotropic and homogeneous\, our observations of the C osmic Microwave Background (CMB) reveal a pronounced dipole\, interpreted as our kinematic departure from the local Hubble flow. This motion should be imprinted on other cosmological observations\, but recent studies are i n significant tension with the kinematic expectation\, bringing the cosmol ogical principle into doubt. Exploring large-scale surveys of cosmological sources with Bayesian-based approaches\, I show that a dipole aligned wit h the CMB is present. However\, the amplitude of the dipole is still in te nsion with our expectations\, bringing the validity of the cosmological pr inciple into question. I will conclude with some ideas about the source of these tensions and whether a cosmological rethink is on the horizon. LAST-MODIFIED:20240327T050117Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Vanhiep Nguyen) \nZoom: ht tps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Geraint Lewis (U. Sydney) "Confronting the Cosmological Principle: How secure are the foundations of the cosmos?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181025T000000Z DTEND:20181025T010000Z DTSTAMP:20261011T152429Z UID:2us98dk7044f38u7vmpff8htf8@google.com CREATED:20181018T000104Z DESCRIPTION:Modern day galaxies populate a bimodal distribution\, in both m orphology and color space. Their morphological and color properties are al so inter-related\, with lenticular and elliptical galaxies usually exhibit ing red colors and spiral galaxies usually exhibiting blue colors. In col or space\, there is a genuine dearth of intermediate colored galaxies\, su ggesting that the transition a galaxy undergoes to transform must be rapid \, and quenching galaxies\, rare. Gas - its presence\, absence\, and mecha nics - serves as the anchor of a galaxy's transformation from blue to red. I will discuss the nature of gas in transitioning and transitioned galaxi es through two lenses: (1) How a galaxy transition is able to impact the b ehavior of molecular gas\, and (2) how new observations of molecular gas i n quenching and quenched galaxies has recast our understanding of how they ultimately metamorphose from blue\, star-forming spirals into red\, quies cent ellipticals and lenticulars. LAST-MODIFIED:20181022T011604Z LOCATION:Duffield Lecture Theatre (host: Moller) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Katey Alatalo (STSCI) "The life-cycle of gas in dying galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160902T040000Z DTEND:20160902T042000Z DTSTAMP:20261011T152429Z UID:skdnaaeb7ddv6vrgpn3ocnqc64@google.com CREATED:20160823T103110Z DESCRIPTION:In this Feast of Facts talk I will discuss my work investigatin g the properties of the galactic halo and thick disk using blue horizontal branch stars from SkyMapper and the AEGIS survey. LAST-MODIFIED:20160902T014107Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Christopher Owen (RSAA) "Properties of the inner galactic halo (and thick disk) with SkyMapper BHBs" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170518T010000Z DTEND:20170518T020000Z DTSTAMP:20261011T152429Z UID:jupau3s940tsbkb8hff4ie7pho@google.com CREATED:20170428T035108Z DESCRIPTION:ITSO symposium LAST-MODIFIED:20170428T035108Z LOCATION:Duffield Lecture Theatre (host: Joao) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:ITSO symposium (ITSO) "ITSO symposium" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190304T000000Z DTEND:20190304T010000Z DTSTAMP:20261011T152429Z UID:16bl1ijan1hn94dd24vn12pk6k@google.com CREATED:20190201T002116Z DESCRIPTION:Star formation history (SFH) is key to understand galaxy format ion and evolution. For early-type galaxies (ETGs)\, in particular\, their SFHs also record their quenching scenarios. Using stellar alpha-to-iron abundance ratio ([alpha/Fe]) as an indicator of star formation timescale ( t_SF)\, I will present our work on the [alpha/Fe]-velocity dispersion rela tion of ETGs that extends to low masses with a range of dataset\, and show a mass-dependent t_SF for most ETGs across a wide mass range on average\, where more massive ETGs have shorter t_SF. However\, the [alpha/Fe] of l ow-mass galaxies from the highest- and lowest-density environments in the sample are more dependent on environments than galactic masses. The data are from Gemini/GMOS-IFU observations\, the literature\, and the MaNGA sur vey. These results are further supported by a study of globular cluster s pecific frequency of ETGs using the HST/ACS Virgo and Fornax Cluster Surve ys. LAST-MODIFIED:20190227T000105Z LOCATION:CSO Common Room (host: Zhang) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Yiqing Liu (University of Oxford) "The Star Formation History of Ea rly-type Galaxies and Their Dependence on Mass and Environment" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200924T010000Z DTEND:20200924T013000Z DTSTAMP:20261011T152429Z UID:2k2gngi6eafqul8f2ttav42dbg@google.com CREATED:20200907T232610Z DESCRIPTION:TBD LAST-MODIFIED:20200907T232610Z LOCATION:ZOOM 997 8534 1005 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dávid Guszejnov (UT Austin (USA)) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250905T040000Z DTEND:20250905T043000Z DTSTAMP:20261011T152429Z UID:hbd1iulsc4i6t9k7rskn063m7o@google.com CREATED:20250814T070608Z DESCRIPTION:Observations of the cosmic microwave background radiation (CMB) have greatly advanced our understanding of the early universe. Among the four Stokes parameters in conventional CMB measurements\, the T-mode (temp erature) and the E- and B-modes (linear polarization) have already been de tected\, whereas the V-mode\, corresponding to circular polarization\, rem ains unobserved. Upcoming experiments such as the Simons Observatory and L iteBIRD satellite are expected to improve sensitivity to V-mode signals by two orders of magnitude compared to current capabilities. In standard cos mology\, the V-mode amplitude is expected to be negligibly small\, implyin g that its detection would point to new physics beyond the standard model of cosmology. In this talk\, I present a novel and concrete mechanism in w hich hypothetical dark photons generate a measurable V-mode polarization s ignal. LAST-MODIFIED:20250814T070608Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Lilli Sun) \nZoom: https:/ /anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Saki Matsuda (Ochanomizu University) "Generation of CMB V-mode pola rization by dark photons" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241024T000000Z DTEND:20241024T010000Z DTSTAMP:20261011T152429Z UID:8hpg07bi2b9t6vl97q3r90h85k@google.com CREATED:20240805T001138Z DESCRIPTION:The gas-phase metallicity reflects the complex interactions bet ween gas inflows\, gas outflows\, and star formation processes\, making it a crucial factor in understanding galaxy formation and evolution. Most me tallicity diagnostics are designed based on H II regions and are not suita ble for calibrating metallicity when there is contamination from Active Ga lactic Nuclei (AGN). In this talk\, I will introduce a Bayesian method tha t separates the emission line fluxes from H II regions and AGN-ionized nar row-line regions (NLR) in a consistent manner\, allowing us to measure the metallicity in galaxies where AGN and star formation (SF) activities are significantly mixed. Our findings show that in the local universe\, AGN in directly affect both total metallicity and fluctuations in the metallicity field by reducing or correlating with suppressed SF activity. We are also preparing for the next generation of integral field spectroscopy (IFS) in struments with adaptive optics (AO)\, which hold promise for studying meta llicity fields in early-universe galaxies. LAST-MODIFIED:20241020T224209Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Songlin Li (RSAA) "Measuring the gas-phase metallicity in AGN-host galaxies with Bayesian methods (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210928T030000Z DTEND:20210928T040000Z DTSTAMP:20261011T152430Z UID:b3ubadrv0kiam8a0p3gk7luolg@google.com CREATED:20210922T025106Z DESCRIPTION:Our next IDEA seminar (organised by the CoS+CHM Equity and Dive rsity committee) will take place next week (over Zoom obviously). We hope that many of you may be able to make it\, although we understand too well the need to ruthlessly prioritise activities through lockdown. The speaker will be Giverney Ainscough\, a PhD student working on thesis entitled "In tegrating University: Perspectives on Chronic Illness and Disability at an Australian University". NOTE: The seminar will use a different ZOOM link. We will send the link before the talk. LAST-MODIFIED:20210922T025106Z LOCATION:ZOOM 839 1543 3538 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Giverney Ainscough (ANU) "CoS+CHM Seminar: Inclusive education in a n exclusive institution: what are we aiming for here?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161130T220000Z DTEND:20161201T060000Z DTSTAMP:20261011T152429Z UID:btqn76mi34ug5vpi9v1nsto3cc@google.com CREATED:20161130T031604Z DESCRIPTION:This is the annual christmas seminars at Mount Stromlo. Student s from RSAA and elsewhere flok to the mountain to share their research wit h others. Invited talks from members of RSAA will also feature. LAST-MODIFIED:20161130T031604Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Student Christmas seminars (RSAA) "student Christmas seminars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181128T000000Z DTEND:20181128T002000Z DTSTAMP:20261011T152429Z UID:q0lm6m3n539srl99p5qe340sbg@google.com CREATED:20181023T070115Z DESCRIPTION:Evidence from the solar system suggests that\, unlike Venus and Mars\, the presence of a strong magnetic dipole moment on Earth has helpe d maintain liquid water on its surface. Therefore\, planetary magnetism co uld have a signi ficant effect on the long-term maintenance of atmosphere and liquid water on rocky exoplanets. We use Olson & Christensen's (2006) model to estimate magnetic dipole moments of rocky exoplanets with radii R p < 1.23 R+. Even when modelling maximum magnetic dipole moments\, only Ke pler-186 f has a magnetic dipole moment larger than the Earth's\, while ap proximately half of rocky exoplanets detected in the circumstellar habitab le zone have a negligible magnetic dipole moment. This suggests that plane tary magnetism is an important factor when prioritizing observations of po tentially habitable planets. LAST-MODIFIED:20181117T102608Z LOCATION:CSO Common Room (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sarah McIntyre (RSAA) "Planetary Magnetism as a Parameter in Exopla net Habitability" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251215T000000Z DTEND:20251215T010000Z DTSTAMP:20261011T152430Z UID:latalub6vojh41s76eeubic0cg@google.com CREATED:20251202T043608Z DESCRIPTION:Abstract written by Sven: Tom's Tips on Talks has been a fixtur e at MPIA for years because it is consistently requested and consistently useful. Tom delivers clear\, practical advice that helps everyone improve their presentations\, from students to senior researchers. Rated 5/5 stars . Beyond giving great advice\, Tom works on star formation\, high angular resolution astronomy\, and instrumentation. He is involved in the SDSS-V L ocal Volume Mapper\, the Large Binocular Telescope\, and the European Extr emely Large Telescope\, and is happy to talk about ideas that go beyond th e ELT. LAST-MODIFIED:20251202T043608Z LOCATION:DLT and ZOOM (host: Melanie Kaasinen) \nZoom: https://anu.zoom.us/ j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tom Herbst (MPIA Heidelberg) "Tips on Talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250918T010000Z DTEND:20250918T020000Z DTSTAMP:20261011T152429Z UID:qgcm81nppdksl4tdskabmrb6lo@google.com CREATED:20250703T020612Z DESCRIPTION:The James Webb Space Telescope (JWST) has opened an unprecedent ed window into the early Universe\, revealing a surprisingly abundant popu lation of UV-bright galaxies at high redshifts that challenge canonical mo dels of early galaxy formation and\, potentially\, the ΛCDM cosmological framework itself. These early galaxies are also believed to be the primary drivers of cosmic reionization\, and understanding their properties is cr ucial for unraveling the interplay between galaxy formation and the ioniza tion history of the intergalactic medium (IGM). Leveraging these observati ons\, we have developed a physically motivated analytical model that simul taneously tracks galaxy evolution and reionization across redshifts 5 <= z <= 15. The model self-consistently predicts the evolution of the UV lumin osity function\, large-scale galaxy bias\, stellar mass function\, and the global neutral hydrogen fraction in the IGM\, while incorporating the eff ects of radiative feedback on low-mass galaxies. In this talk\, I will pre sent key insights from our studies into the star formation activity\, larg e-scale clustering\, and ionizing efficiency of reionization-era galaxies\ , offering a coherent picture that connects JWST observations to the broad er narrative of cosmic evolution. Time permitting\, I will also briefly di scuss whether these surprising JWST results can be explained solely throug h modifications to the standard cosmological model\, including scenarios t hat alter the background expansion history or enhance matter density pertu rbations. LAST-MODIFIED:20250909T032607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Stu Wyithe) \nZoom: https: //anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anirban Chakraborty (National Centre for Radio Astrophysics (NCRA-T IFR)) "Probing Galaxies in the First Billion Years with JWST" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171107T000000Z DTEND:20171107T010000Z DTSTAMP:20261011T152429Z UID:1funq6gm13q43ahf0kqs92212k@google.com CREATED:20171104T043106Z DESCRIPTION:The theme of the talk is how different modes of stellar feedbac k affect the evolution of galaxies and how\, with appropriate care\, we ca n constrain the role of the historically popular supernova feedback on the evolution of galaxies and their stellar content. We argue that prior wor k has modeled supernovae poorly by ignoring stellar clusters and also the key physics of conduction that governs hot gas evolution. Clustered super novae create superbubbles\, kpc scale feedback events that can drive stron g galactic winds. We show that superbubbles can be modeled via first prin ciples simulations without resorting to common numerical tricks. Galaxie s with superbubble feedback strongly regulate their star formation and glo bal baryon budget. These simulated galaxies match disk galaxy observatio ns very well. However\, there are limits -- supernovae cannot explain the regulation of star formation in all galaxies. LAST-MODIFIED:20171104T043106Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:James Wadsley (McMaster Uni) "Superbubbles and the limits of Supern ovae on Galactic Scales" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170818T043000Z DTEND:20170818T045000Z DTSTAMP:20261011T152429Z UID:jkinkgtpr84l17uk4ti9t3t6bk@google.com CREATED:20170815T011606Z DESCRIPTION:I will show two important ways in which cosmological simulation s of galaxy formation can be used to inform astronomy and cosmology. First ly\, as part of the SAMI project\, I have used a synthetic pipeline to pro duce mock SAMI datacubes of galaxies in simulations. In particular\, I wil l show how synthetic galaxies have been "observed" with proposed designs f or the Hector instrument. Secondly\, cosmological simulations can be used to investigate early-universe cosmological theories. Theories of cosmologi cal inflation often predict that cosmic conditions will vary from place to place in the universe as a whole. In particular\, the value of the cosmol ogical constant can plausibly explained by a combination of environmental variation and its effect on galaxy formation. In such models\, it is cruci al that we understand how quickly and efficiently the onset of acceleratin g expansion shuts down accretion of matter into dark matter haloes and gal axies. I will show simulations\, based on the cosmological galaxy formatio n code of the Eagle collaboration that investigates this effect. LAST-MODIFIED:20170815T011606Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Luke Barnes (University of Sydney) "How cosmological simulations in form observational surveys and fundamental cosmology" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150917T060000Z DTEND:20150917T070000Z DTSTAMP:20261011T152429Z UID:9rfhk3u6svb2n50je483ma71cs@google.com CREATED:20150908T064106Z DESCRIPTION:In the space of a generation\, cosmology has been transformed f rom an almost entirely theoretical activity into a rigorous\, empirical sc ience\; I will describe the resulting 'concordance cosmology' which accoun ts for the overall properties of our universe and identify (some of!) its weaknesses. One of the most exciting aspects of this new age of precision cosmology is that the evolving universe yields evidence for 'new physics'\ , including dark energy and dark matter. Interestingly\, some theories of dark matter and dark energy can be tested with precision laboratory and sp ace-based experiments\, and I will survey current and future opportunities for experimental physicists to put constraints on cosmological physics. LAST-MODIFIED:20150908T064106Z LOCATION:Seminar: Department of Quantum Science\, held in Psychology G6 (ho st: Craig Savage) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Richard Easther (University of Auckland) "Cosmology: Where We Are a nd What Happens Next?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180130T000000Z DTEND:20180130T010000Z DTSTAMP:20261011T152429Z UID:iiui3pejs1apcpiltn9jd7s0dg@google.com CREATED:20180129T005105Z DESCRIPTION:In order to address the mechanism of rich cluster formation I p resent recent analyses on formation of the young rich clusters in the LMC and the Antennae galaxies. In the LMC R136 is the most outstanding cluster which harbors 400 O/B stars in itssurroundings. A new analysis of the HI data taken with the ATCA shows that two velocity components whose velocity separation is ~50 km/s collided with each other 2 Myrs ago and the collis ion triggered the formation of the cluster and the O/B stars.The scenario is supported by the simulations by Bekki and Chiba 2007\, which show that the LMC and SMC encountered closely 0.2 Gyrs ago and that the tidal force removed the HI gas from both the LMC and the SMC. The HI gas is now fallin g back onto the LMC disk to trigger the star formation. The Antennae galax ies at a larger distance allow us to make a similar analysis on CO data ta ken with ALMA. We found similar possible collision signatures toward a few of the young cluster candidates in the overlapping area\, where two CO cl ouds of ~100 km/s velocity separation are interacting dynamically. Trigger s of cluster formation are a probable outcome of the collisions. I will pr esent a few more cases in the Local Group which lend support for the galac tic collisional events as triggers of rich cluster formation. LAST-MODIFIED:20180129T231105Z LOCATION:Duffield Lecture Theatre (host: Battisti) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Yasuo Fukui (Nagoya University) "Galactic interactions triggering f ormation of the young rich clusters" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170529T230000Z DTEND:20170530T070000Z DTSTAMP:20261011T152429Z UID:in6f7dcs8hpulj172hae4sngpk@google.com CREATED:20170202T044212Z DESCRIPTION:SERC annual colloquia LAST-MODIFIED:20170529T032105Z LOCATION:Duffield Lecture Theatre (host: SERC) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:SERC Colloquium (SERC) "SERC annual colloquia" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241105T223000Z DTEND:20241106T053000Z DTSTAMP:20261011T152429Z UID:4at4a6suokaie8ubl7fmrufnm4@google.com CREATED:20240927T033125Z DESCRIPTION:Confirmation of Candidature talks from first-year PhD students LAST-MODIFIED:20240927T033125Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Christoph Federrath) \nZoo m: https://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA first-year PhD students (RSAA) "Confirmation of Candidature pr esentations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250923T010000Z DTEND:20250923T020000Z DTSTAMP:20261011T152429Z UID:31rkg1gg7j0ag1c7m3a82g8em4@google.com CREATED:20250520T123620Z DESCRIPTION:Despite a history stretching back more than two millennia\, the science of geodesy is relatively unknown. Geodesy measures Earth's shape\ , its orientation in space\, and its gravity field\, and it is essential t o a modern\, spatially enabled society. Geometrical geodesy is used to def ine our terrestrial reference frames and consists of four techniques: Glob al Navigation Satellite Systems (GNSS)\, Very Long Baseline Interferometry (VLBI)\, Satellite Laser Ranging (SLR)\, and Doppler Orbitography and Rad iopositioning Integrated by Satellite (DORIS). Three of these are located on Mt Stromlo. In this talk\, I will introduce Geoscience Australia's Posi tioning Australia Program\, which aims to provide 5cm accurate positioning with a mobile phone\, and show how geodesy is fundamental to achieving th is goal. LAST-MODIFIED:20250922T023106Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Tomasz Rozanski) \nZoom: h ttps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Craig Harrison (Geoscience Australia) "Geodesy\, the foundations fo r a spatially enabled world" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201022T000000Z DTEND:20201022T003000Z DTSTAMP:20261011T152429Z UID:hb2m90vg4dqrg7lgdq2n7ir0u0@google.com CREATED:20201008T052610Z DESCRIPTION:The SAGA Survey will spectroscopically identify satellite galax ies brighter than Mr = -12.3 around one hundred Milky Way analogs at z 0.0 1. We recently published our Stage II data release\, which included 127 s atellites around 36 hosts. The data quadruple the sample size presented i n 2017 and significantly increases spectroscopic coverage for very low-red shift galaxies with magnitudes 17 < r < 21 around SAGA hosts\, creating a unique data set that places the Local Group in a wider context. I will di scuss results from SAGA Stage II on the quenched fraction of satellites\, luminosity functions\, radial distributions and more\, comparing these bot h to the Milky Way itself and predictions from simulation. LAST-MODIFIED:20201013T232109Z LOCATION:ZOOM 997 8534 1005 (host: Jung) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Marla Geha (Yale\, USA) "The SAGA Survey: Exploring Satellite Galax ies Around Milky Way Analogs" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170303T030000Z DTEND:20170303T032000Z DTSTAMP:20261011T152430Z UID:pubu2hh72poo1vcboorttq1pa4@google.com CREATED:20170123T210110Z DESCRIPTION:Boyajian's star\, an otherwise unremarkable F-type dwarf\, unde rwent several unusual dimming events over the four years it was observed b y Kepler. Subsequent work has also found a long-term trend\, though the de tails of this "secular dimming" remain controversial. Proposed explanation s include post-collisional debris\, cometary dust\, interstellar material\ , and alien megastructures. I will discuss some of the typical circumstell ar causes of large-scale stellar variability\, why these are a poor expla nation for Boyajian’s star\, and current work that explores the cometary dust interpretation. LAST-MODIFIED:20170303T032104Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Grant Kennedy (Cambridge University) "Things that go bump in the ni ght: the comet interpretation of Boyajian's star" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201130T230000Z DTEND:20201201T000000Z DTSTAMP:20261011T152429Z UID:hrbgvgjua4c3drq870k8nj7134@google.com CREATED:20200826T081717Z DESCRIPTION:Imaging and spectrally analyzing extrasolar planets is a very e xciting approach to derive the chemical composition of their atmosphere\, perform comparative exoplanetelogy\, and understand the formation and evol ution of the planets. However\, this observing method is also very challen ging as it requires observations of planetary companions that are 10^6 to 10^10 fainter than their host stars at separations shorter than 1 arcsec. In this presentation\, I will briefly review the recipes to achieve exopla net images and lift the veil on the nature of these planets. One of the ma in limitations is the residual speckles\, the seeds of light that are left in these images of exoplanets and prevent us from observing the faintest planets. I will tell you the stories about ZELDA\, our wavefront sensing a pproach to calibrate these errors and show some promising results on the e xoplanet imager SPHERE on the VLT to push limits further for exoplanet obs ervations. The second part of my talk will be dedicated to Astronomy and A strophysics across Africa (5A)\, a project that I am co-leading with my co lleague Eric Lagadec in Nice to expand and strengthen Africa-Europe collab orations towards the Sustainable Development Goals. LAST-MODIFIED:20201124T011108Z LOCATION:ZOOM 997 8534 1005 (host: Martinez) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mamadou N'Diaye (OCA Nice\, France) "Invited Colloquium: ZELDA: a L ink to exoplanet imaging with current and future observatories / 5A: Astro nomy and Astrophysics Arising Across Africa" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261001T010000Z DTEND:20261001T020000Z DTSTAMP:20261011T152430Z UID:q932jtiosiprecmca302si5mrg@google.com CREATED:20260615T020023Z DESCRIPTION:The Galactic magnetic field plays an important role in the evol ution of the interstellar medium\, influencing star formation\, cosmic-ray propagation\, and gas dynamics. However\, the vertical structure of its s mall-scale turbulent component remains poorly constrained. In this talk\, I present results from my PhD using ASKAP POSSUM to probe Galactic magneti sm through the Faraday rotation of polarised background radio galaxies. I develop and validate methods for removing diffuse Galactic emission and as sess the reliability of QU-fitting across the POSSUM frequency bands. I th en apply these methods to over 37\,000 polarised sources to measure the la titude dependence of Faraday complexity and constrain the vertical extent of the turbulent magnetic field. I find evidence for a turbulent field con centrated close to the Galactic plane\, with an inferred scale height of a pproximately 10–240 pc under the adopted physical assumptions. I discuss what this reveals about the vertical distribution and dissipation of turb ulent energy in the Galactic interstellar medium. LAST-MODIFIED:20260929T060004Z LOCATION:Zoom or Duffield Lecture Theatre (host: Naomi McClure-Griffiths) \ nZoom: https://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOnt d.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Lindsey Oberhelman (RSAA) "Probing the Magnetised ISM - The turbul ent Milky Way (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190308T030000Z DTEND:20190308T033000Z DTSTAMP:20261011T152429Z UID:n9s3kl2vcaumndjfv7hd7i99i4@google.com CREATED:20190110T003818Z DESCRIPTION:Adaptive optics (AO) has revolutionized astronomical instrument ation\, beginning in 1953 with a technologically impossible concept and cu lminating in the implementation of AO systems on almost all 8m-class teles copes. Multi-Conjugate Adaptive Optics (MCAO) pushes the classical AO conc ept to the mechanical and computational limit\, providing near-diffraction limited angular resolution across a wide field of view. Unfortunately bot h current and future MCAO systems\, including those planned for the next g eneration of extremely large telescopes\, are limited in their wavelength coverage\, only correcting light in the near-infrared regime (1-2.5 micron s). The MCAO Assisted Visible Imager and Spectrograph (MAVIS) is set to ch ange that. MAVIS is a proposed third generation instrument for the ESO VLT UT4 that will perform AO corrections from 450-980 nm\, making it the firs t MCAO system to operate in the visible. In this thesis proposal talk I wi ll discuss my planned PhD work both on a key MAVIS AO subsystem\, and buil ding three of the major science cases for MAVIS using existing data: resol ved stellar populations beyond the local group\, crowded field photometry and spectroscopy and precision astrometry and proper motions. LAST-MODIFIED:20190304T025608Z LOCATION:CSO Common Room (host: Oh) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Stephanie Monty (RSAA) "Adaptive Optics Work & Resolved Stellar Pop ulation Studies: Towards the Next Generation VLT Instrument MAVIS (Thesis Proposal talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241127T020000Z DTEND:20241127T030000Z DTSTAMP:20261011T152429Z UID:ironovhoshanm9l4c1aj9oj7n8@google.com CREATED:20241108T052614Z DESCRIPTION:We present a method for identifying\, classifying\, and disting uishing unresolved reflective objects. A forward model is developed to pre dict how the radiance field from a specular surface will be angularly dist ributed and how samples detected from that field can be used to infer surf ace profile characteristics. We present lab studies to validate the forwar d model and demonstrate unresolved object identification and classificatio n. We demonstrate unresolved specular object identification for a 35 mm ta rget at a 4.6 km and 50 mm targets at a 27.6 km range with a 28 cm apertur e telescope. Preliminary observations for specular signatures of drones an d helicopters are also presented. LAST-MODIFIED:20241108T052614Z LOCATION:ZOOM only (host: N/A) \nZoom: https://anu.zoom.us/j/83410388355?pw d=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Greg Nero (University of Arizona College of Optical Sciences) "Refl ective signatures of unresolved objects" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230224T030000Z DTEND:20230224T040000Z DTSTAMP:20261011T152429Z UID:16jds4vjua4j3jkojintl5ot18@google.com CREATED:20230219T220606Z DESCRIPTION:Andor OI is a global leader in the development and manufacture of high-performance scientific digital cameras\, microscopy systems\, and spectrographs for academic\, industrial\, and governmental applications. T hrough continuous dialogue with customers and strong teamwork\, we continu e to innovate our product collection\, with the auspice of improving the q uality of scientific research and\, ultimately\, the world we live in. The main aim of Andor is to accelerate the scientific advancements of our age \, tackling the necessities of our customers in their own research field. In this regard\, Andor's extensive portfolio of high-performance imaging c ameras\, spectroscopy\, and microscopy solutions is suited to a wide range of applications across physical science and life science\, offering a sup erb combination of sensitivity\, speed\, and dynamic range. This presentat ion will show Andor commercial instruments such as Charge Coupled Devices (CCDs)\, Electron Multiplying CCDs (EMCCDs)\, and Complementary Metal Oxid e Semiconductor (sCMOS) cameras\, with the aim of offering an overview of their functionalities. At the same time\, a few implementations for each c amera will be provided\, to elucidate their possible applications both in Astronomy and Quantum research fields. LAST-MODIFIED:20230219T220606Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Maddie McKenzie) \nZoom: h ttps://anu.zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Emilia Capozzi (Andor) "Andor cameras portfolio for assisting in th e Astronomical and quantum research." TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180125T030000Z DTEND:20180125T040000Z DTSTAMP:20261011T152429Z UID:j7th3pfvggreppfhrvf7nlasic@google.com CREATED:20180123T032606Z DESCRIPTION:In standard cosmological perturbation theory\, peculiar velocit ies - or cosmic flows - arise from large-scale structure in the nearby Uni verse. Since the late 1970s there has been a long-standing effort to map q uantitatively the structures in the nearby Universe and to reconcile these with the peculiar velocities of the Local Group and other nearby galaxies . We have now reached the stage where most - but not all - of this motion is understood. I will review recent progress in this area\, focusing on ou r recent work on the 2M++ redshift compilation\, which relies heavily on t he 6dF and other surveys. I will also discuss how one can obtain constrain ts on the cosmological parameters from this approach. Finally\, I will dis cuss the prospects from ongoing and future surveys. LAST-MODIFIED:20180123T032606Z LOCATION:Duffield Lecture Theatre (host: Panther) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Michael Hudson (University of Waterloo) "The Origin of the Local Gr oup's 600 km/s Motion with respect to the Cosmic Microwave Background" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151113T030000Z DTEND:20151113T034000Z DTSTAMP:20261011T152429Z UID:ee7ll6hklh3q3vc6gd1nemcvgs@google.com CREATED:20151028T035107Z DESCRIPTION:TBD LAST-MODIFIED:20151109T020106Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Hugues Poincelin (RSAA) "Beam Transfer Optics and Laser Launch Tele scope Design for Space Debris Tracking Adaptive Optics (Masters Research P roject Final Presentation)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141222T000000Z DTEND:20141222T010000Z DTSTAMP:20261011T152430Z UID:h170pske8rk1m2rcspiro5s4ns@google.com CREATED:20141117T060343Z DESCRIPTION:In this presentation I will recap what we know about the dwarf planet Pluto & its companion moons\, including some recent results from th e Division of Planetary Sciences October 2014 meeting (Tucson\, AZ). Next I will describe NASA's New Horizons mission\, launched in January 2006\, w ho has been traveling across the solar system and will reach the Pluto sys tem in July 2015. It's been 25 years since we last visited a new world wit h a spacecraft for the first time (Voyager-2's August 1989 flyby of Neptun e/Triton)\, so we can expect the unexpected. Images from New Horizons hi-r es camera become "better than Hubble" in early May 2015. I will end the pr esentation with the latest news from the New Horizons mission and its plan s after the July 2015 Plutoflyby. LAST-MODIFIED:20250925T231029Z LOCATION:Duffield Lecture Theatre (host: Ian Price) \nZoom: https://anu.zoo m.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kimberly Ennico-Smith (NASA) "Distant worlds revealed - NASA's New Horizons spacecraft reaches the Pluto System in 2015" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231010T000000Z DTEND:20231010T013000Z DTSTAMP:20261011T152429Z UID:f50t05ta6m81vpgfneei0n6ebs@google.com CREATED:20230917T235112Z DESCRIPTION:The chemical evolution of the Universe is largely guided by the lives of massive stars. These stars are born with a convective core on th e main-sequence and are heavily influenced by additional mixing occurring at both the convective core boundary and in the radiative envelope. Such m ixing transports additional hydrogen fuel from the envelope to the convect ive core\, allowing the stars to live longer and to enhance their final he lium core mass at the end of the main-sequence evolution. Consequently\, c hemical mixing has a high impact on the stellar evolution of both intermed iate- and high-mass stars and is one of the dominant uncertainties in thei r stellar structure and evolution theory\, along with their interior angul ar momentum transport. Asteroseismology is a powerful tool for probing ste llar interiors through the detection and interpretation of stellar oscilla tions. With the advent of space telescopes\, our ability to precisely dete ct and measure these oscillations has greatly improved and lead to signifi cant advances in our understand of the interiors of pulsating stars. Espec ially since the launch of the TESS space telescope in 2018\, asteroseismol ogy of massive stars has become readily accessible. With this talk I will demonstrate how we can use stellar oscillations to probe the internal mixi ng and rotation\, as well as discuss recent results from the Kepler space telescope for single B-type stars and the promises of TESS for studying ma ssive stars in OB associations. LAST-MODIFIED:20230927T233208Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Trey) \nZoom: https://anu. zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:May Gade Pedersen (U. Sydney) "Asteroseismology of massive stars in the era of space telescopes" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250318T000000Z DTEND:20250318T010000Z DTSTAMP:20261011T152429Z UID:d78gbo4idneq7gfs7m7h5qpe18@google.com CREATED:20250106T230121Z DESCRIPTION:Orbiting telescopes have traditionally required at least a medi um sized satellite platform to provide the necessary on-board power and vo lume to host remote sensing instrumentation\, as well as associated suppor t systems and general avionics. The Australian-Italian SpIRIT CubeSat miss ion - launched in a low Earth orbit in December 2023 - is demonstrating th e potential for breakthrough science and technology through a 12kg satelli te equipped with innovative payloads. SpIRIT's main instrument is the HERM ES telescope - covering the 3keV-2MeV energy range for identification of h igh-energy astrophysics transients and for studies of their variability at millisecond scales. The satellite also includes a novel thermal managemen t system for its class\, based on a Stirling-cycle cooler and deployable t hermal radiators\, designed to reduce instrumental background noise on HER MES\, and aimed at demonstrating feasibility of cooling IR focal plane arr ays on future CubeSats. I will present a brief mission overview and the in -orbit results from HERMES observations. Finally\, I will conclude with le ssons learned throughout the mission development and operations\, highligh ting opportunities for distributed aperture constellations of nanosatellit es to play a pivotal role in multi-messenger astrophysics during the next decade. LAST-MODIFIED:20250220T232614Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hayden Park) \nZoom: https ://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Michele Trenti (U. Melbourne) "The SpIRIT mission: An Australian Sp ace Telescope contributing to multi-messenger astrophysics" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161104T030000Z DTEND:20161104T032000Z DTSTAMP:20261011T152429Z UID:gfl6scle22j5a7hs9qn7h8l2fs@google.com CREATED:20161018T023106Z DESCRIPTION:Supernova-driven turbulence can have massive effects on the evo lution of the surrounding interstellar medium (ISM)\, affecting nearby sta r formation and the initial mass function. This makes supernovae an integr al element to simulating the evolution of the ISM. Many previous supernova implementations make assumptions about the internal structure\, size\, or energy distribution of the supernovae that may not agree with accepted li terature. In this talk\, I present my implementation of supernovae based o n the analytical Sedov solution\, a self-similar blast wave solution linke d to the main stage of supernova evolution. I apply this solution to explo ring supernova-driven turbulence\, finding the generated density and veloc ity power spectra to have scaling laws that are in line with current liter ature. LAST-MODIFIED:20161031T233107Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jacob Buete (RSAA) "Exploring Supernova Driven Turbulence Through I mplementing Realistic Supernovae" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251002T010000Z DTEND:20251002T020000Z DTSTAMP:20261011T152430Z UID:rqfg3p1r08ouuh3i80d2eh35p8@google.com CREATED:20250925T231107Z DESCRIPTION:The initial mass function (IMF) is essential for understanding the formation and evolution of stars and galaxies. However\, our understan ding of the IMF in the early universe is not comprehensive. Recent advance ments in numerical simulations indicate that stellar masses in the early u niverse were significantly larger\, often reaching several hundred times t he mass of our sun\, a stark contrast to what we observe in the modern uni verse. This suggests a potential shift in the IMF over the course of cosmi c evolution. To explore this\, we conducted three-dimensional hydrodynamic s simulations to track the formation of star clusters across various metal licities and redshifts. These simulations are detailed enough to capture t he formation of protostars down to ~au scales\, providing insights into th e IMF. We discovered that both metallicity and redshift are pivotal in sha ping the IMF. Metallicity influences cooling efficiency\, and redshift alt ers the baseline temperature by modifying the cosmic microwave background temperature. Our findings reveal that the IMF becomes more top-heavy in en vironments with metallicity Z/Zsun < 0.01 or with a redshift greater than 10. These insights may elucidate the recent observations by the James Webb Space Telescope (JWST) of an unexpectedly high number of bright\, high-re dshift galaxies. Our results suggest that a top-heavy IMF in these galaxie s could lead to increased UV luminosity at a consistent stellar mass\, the reby elevating the number density of UV-bright galaxies. LAST-MODIFIED:20250925T231107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sunmyon Chon (Max Planck Institute for Astrophysics) "Transition of the IMF from the high-z universe to present-day universe" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170825T040000Z DTEND:20170825T042000Z DTSTAMP:20261011T152429Z UID:u3qko4rm3j4l9m5g7hu1js3gsk@google.com CREATED:20170720T054617Z DESCRIPTION:A Churchill Fellowship offers Australian citizens the remarkabl e opportunity to travel overseas to investigate a topic or an issue that t hey are passionate about. It is for anyone who feels they have exhausted alternatives within Australia and would like to see what other countries a re doing successfully in a similar space to inspire new ideas\, innovation \, and excellence. The high international regard for Churchill Fellowship s provides a pathway for Fellows to access expertise from around the world \, expanding their knowledge and experience for the benefit of Australian society. There is a high level of visibility and credibility associated w ith being a Churchill Fellow. The subject of your proposed project is lim itless provided a benefit to Australia is evident and a willingness to sha re the knowledge gained with Australia is displayed. Applications open 1 February 2018 LAST-MODIFIED:20170815T005608Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Churchill Trust (Churchill Trust) "We make a living by what we get\ , but we make a life by what we give. Hear why a Churchill Fellowship is m uch more than an academic scholarship" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141205T030000Z DTEND:20141205T031500Z DTSTAMP:20261011T152430Z UID:am6b5vjeh97sfljtffllftoc2k@google.com CREATED:20250925T231025Z DESCRIPTION:I will summarise the work I have done here at RSAA on transitin g exoplanets\, particularly with regard to the HATSouth discoveries. I wi ll then discuss some of the exoplanet projects I will be involved with in my new position at Geneva Observatory - primarily NGTS\, CHEOPS\, ESPRESSO \, TESS and PLATO. LAST-MODIFIED:20250925T231025Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) \nZoom: https://anu.zoo m.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Daniel Bayliss (RSAA) "Final Talk: Transiting Exoplanets" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160902T003000Z DTEND:20160902T005000Z DTSTAMP:20261011T152429Z UID:dsjjkc04ir84gceru3fv0sgs2o@google.com CREATED:20160823T103109Z DESCRIPTION:I shall provide an overview of the extensive suite of internati onal telescopes and their instrumentation available to Australian astronom ers in Semester 2017A. This includes Keck\, Magellan\, the CTIO Blanco tel escope\, and additional classical nights on Gemini. I shall also summarise the range of activities undertaken by the AAO's International Telescopes Support Office. LAST-MODIFIED:20160902T014106Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Stuart Ryder (AAO) "International Telescope Access in 2017" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250930T010000Z DTEND:20250930T020000Z DTSTAMP:20261011T152429Z UID:54lejfiq4oc3m722jaj2k2kbls@google.com CREATED:20250605T033117Z DESCRIPTION:One of the key choices we have as scientists is to design infor mative experiments. Using examples from astronomy\, we discuss a machine l earning perspective of the scientific method. With AI promising accurate p redictions\, we revisit the question of adaptively designing new measureme nts that take previous data into account. Following this scientific method framing\, we illustrate some recent ideas on using machine learning to re commend experiments in genomics. The goal of this talk is to start a conve rsation about what it means to recommend experiments in astronomy. LAST-MODIFIED:20250909T030111Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hiep Nguyen) \nZoom: https ://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Cheng Soon Ong (CSIRO/Data61) "On Finding Good Experiments" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190529T010000Z DTEND:20190529T013000Z DTSTAMP:20261011T152429Z UID:8v1ucn9v1v9eksj2kk1lu023v0@google.com CREATED:20190430T055611Z DESCRIPTION:Over the last two decades\, type Ia supernovae (SN Ia) have act ed as one of the best probes of the expansion history of the Universe. La rge-scale survey telescopes are now able to detect and observe thousands o f SN Ias\, to measure the dark energy equation of state with ever-increasi ng accuracy. For example\, the Dark Energy Survey (DES) has recently fini shed five years of high-quality SN Ia light-curve observations\, which I w ill fit during my PhD at RSAA. These results will form the foundation of the DES five-year photometric supernova analysis\, which will produce the tightest measure of the dark energy equation of state every seen. During this talk\, I will discuss the general methods used to fit a light-curve a nd propagate the results through to a measure of dark energy. I will then introduce the Dark Energy Survey and outline the work I will be doing for DES as part of my PhD. LAST-MODIFIED:20190528T140104Z LOCATION:Duffield Lecture Theatre (host: Cultinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Georgina Taylor (RSAA) "Tightening Constraints on Dark Energy Throu gh Better Distances to Type Ia Supernovae (Thesis proposal talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230623T040000Z DTEND:20230623T043000Z DTSTAMP:20261011T152429Z UID:lklnfv11v330ltcb9gg7rd9euk@google.com CREATED:20230613T024110Z DESCRIPTION:The Hosking integral (Hosking & Schekochihin 2021\, PRX 11\, 04 1005) has recently been recognised as a key invariant constraining the dec ay of magnetic fields that are statistically homogeneous\, isotropic and n on-helical. In this talk\, I provide a theoretical background on the decay of primordial MHD turbulence\, and I construct von-Karman-Howarth-Monin r elations for the Hosking correlator (i.e.\, the two-point correlation func tion of the magnetic-helicity density) for the first time\, and provide ex act scaling relations for its behaviour in both incompressible and compres sible magnetohydrodynamic (MHD) turbulence. I will show that the condition of rapid decorrelation of velocity and magnetic fields are indeed satisfi ed\, so that the Hosking integral becomes a conserved quantity of ideal\, non-helical incompressible magnetohydrodynamic (MHD) turbulence. Furthermo re\, I provide explicit forms of the relevant fourth and fifth-order two-p oint correlation functions. Moreover\, I outline conditions for its conser vation in compressible MHD turbulence. LAST-MODIFIED:20230613T024110Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Christoph) \nZoom: https:/ /anu.zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Justin Kin Jun Hew (RSAA) "Exact von-Karman-Howarth scaling relatio ns for the Hosking integral in non-helical magnetohydrodynamic turbulence" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240910T010000Z DTEND:20240910T020000Z DTSTAMP:20261011T152429Z UID:ca5n9imoh97s87gac5qts5mc6k@google.com CREATED:20240415T235644Z DESCRIPTION:Fast Radio Bursts (FRBs) are short timescale (usec to msec) tra nsients occurring thousands of times daily on the radio sky. First discove red at Parkes in archival data\, they have led to wide ranging research an d intense search programs at multiple telescopes around the globe. In this talk I'll concentrate on FRB search programs at three facilities in Austr alia -- Parkes\, Molonglo and ASKAP. Parkes made the first detection and w as used to provide initial estimates of the event rates and brightnesses o f FRBs\, and the distribution of their "dispersion measures" (indicating t hey are likely originating well beyond the Milky Way). We used Molonglo to validate the celestial origin of FRBs and make the first live-detections using machine learning -- opening up 100x higher-detail studies of FRB bur st properties. We are currently operating an FRB search program at ASKAP\, which allows localisation of individual FRBs to their host galaxies\, est imates of their intrinsic luminosities\, pointers to FRB progenitors\, and measurement of the baryon density of the Universe\, amongst other applica tions. Finally I'll report on our significantly improved sensitivity upgra de at ASKAP -- the CRACO FRB search experiment. LAST-MODIFIED:20240906T100709Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hilay Shah) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Chris Flynn (Swinburne U.) "Fast Radio Bursts down under -- from Pa rkes to Molonglo to ASKAP" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210413T010000Z DTEND:20210413T020000Z DTSTAMP:20261011T152429Z UID:83joeirkr1tj4f5m6jdoeh1290@google.com CREATED:20210329T220108Z DESCRIPTION:High speed metal 3D printing is a growing industry\, with Austr alian company SPEE3D at the forefront. As technology advances\, SPEE3D is observing a growing trend - more and more real world operations can be opt imised in a simulated 3D space prior to being generated in reality. How sh ould all of this 3D data be managed and manipulated? It turns out that tec hniques found in Astronomy are particularly relevant. About Steve: Steve i s co-founder and CTO of Melbourne\, Australia-based SPEE3D\, a high-speed\ , metal 3D printing company that developed the world's first metal 3D prin ter leveraging supersonic 3D deposition technology to deliver manufacturin g grade printing at production speeds. Steve\, a holder of multiple patent s\, has a Masters degree in Engineering. Prior to founding SPEE3D\, he co -founded In Motion Technologies\, a Charles Darwin University spin-off lau nched to commercialize axial flux electric motors. In Motion Technologies was acquired by Fasco Motors\, part of NYSE listed Regal Beloit. Steve's p roduct successes have included world record holding solar cars\, innovativ e electric motors\, electric bicycles and high efficiency pool pumps. Stev e has a wide range of interests across many fields of manufacturing\, scie nce and engineering and speaks several languages. LAST-MODIFIED:20210411T224605Z LOCATION:ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Steven Camilleri (SPEE3D) "SPEE3D - the surprising connections betw een Astronomy and Industrial 3D Printing" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230608T010000Z DTEND:20230608T020000Z DTSTAMP:20261011T152429Z UID:9uicgdelc6o17dt60vpasjemr0@google.com CREATED:20230528T225107Z DESCRIPTION:Throughout the history of our Galaxy\, various mechanisms have contributed to its chemical enrichment\, from light elements formed during the Big Bang to heavier elements produced in stars and released into the interstellar medium near the end of their lives. To understand the relativ e contributions of these sources to the Galactic chemical budget\, we need to examine nucleosynthesis processes and star properties in detail. In th is context\, observations are fundamental to verify and constrain theoreti cal models to improve our current knowledge and better address the questio n\, "How are the elements produced and recycled through galaxies?" This th esis focuses on the chemical abundances of two sources: (i) 12 stars from the intermediate-age globular cluster GLIMPSE-C01\, and (ii) 8 Carbon Enha nced Metal-Poor (CEMP) stars. By analyzing high-resolution\, high signal-t o-noise ratio infrared observations using the Immersion GRating INfrared S pectrometer (IGRINS)\, we obtained valuable chemical abundance information . (i) Our findings reveal super-solar Fe abundances and star-to-star Na ab undance variations in GLIMPSE-C01\, indicating that it is the most metal-r ich and youngest globular cluster hosting multiple populations in our Gala xy. (ii) The distinct chemical patterns observed in CEMP stars provide ins ights into stellar nucleosynthesis in the early Galaxy. We present results for fluorine abundances from carefully selected observations of 8 CEMP st ars\, including the detection of F at the lowest metallicity so far. Compa ring these results to theoretical models\, we identify inconsistencies and emphasize the significance of F measurements in constraining the properti es of the chemical enrichment mechanisms in the first stars. LAST-MODIFIED:20230531T104108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Christoph) \nZoom: https:/ /anu.zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Aldo Mura (RSAA) "Probing Nucleosynthesis and Chemical Properties: IR Spectroscopy in CEMP Stars and Obscured Star Clusters (End of Thesis Ta lk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241004T040000Z DTEND:20241004T043000Z DTSTAMP:20261011T152429Z UID:qjedpkm6rpld2k59giv9ivjcqs@google.com CREATED:20240913T033116Z DESCRIPTION:Astronomy Data and Computing Services (ADACS) was established i n 2017 by the Australian Astronomy community - with the leadership of Astr onomy Australia Ltd. (AAL) - to provide astronomy-focused training\, suppo rt and expertise to maximise scientific return on Australia's investments in astronomical data & computing infrastructure. One of our flagship servi ces is the ADACS Merit Allocation Program (MAP). This program provides an opportunity for any Australian astronomer to compete (in the same way the y compete for computing or telescope resources) for the time of dedicated software professionals to deliver: (1) Bespoke training in skills related to software development\, &/or (2) Dedicated software development or desig n effort for new or established codebases. To date we have successfully de livered over 120 projects involving over 100 unique applicants across all areas of Australian astronomy through this program. The ADACS MAP is solv ing problems for researchers that otherwise could not have been solved\; a ccelerating old science and enabling new science. More broadly however\, we are working to shift the culture of computing in our community\; moving to a more collaborative model\, where wider skill-sets of multifunctional teams can be exploited. By the date of this talk\, the deadline for Expre ssions of Interest (EoIs) for the 2025A semester of the ADACS MAP will be approaching. This will be a good opportunity to get answers to any questi ons you may have about the program and how it could help you with your res earch program. LAST-MODIFIED:20240923T012213Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Greg Poole (ADACS) "ADACS Merit Allocation Program: A brief introdu ction and Q & A" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160922T010000Z DTEND:20160922T020000Z DTSTAMP:20261011T152429Z UID:s5mi7i5goefgt4ftseo16utvac@google.com CREATED:20160830T002110Z DESCRIPTION:Gas accreting onto halos and filaments is expected to heat to t he "virial temperature" of the perspective structure and produce a hydrost atic\, stable atmosphere. I will show that\, in fact\, accreting gas does not always heat\, leading to unstable free falling gas\, a.k.a cold flows. The instability of the gas\, and subsequent existence of cold flows\, dep end on the cooling rate and infall velocity of the gas. Once these flows p enetrate through a hot halo\, supersonic Kelvin Helmholtz instability occu rs. I will discuss this non-standard situation. Finally\, as cold flows sm ash into the galaxy\, magnetic fields can play a non-trivial role in how t his gas actually mixes with the ISM. LAST-MODIFIED:20160920T062604Z LOCATION:Duffield Lecture Theatre (host: Helga Denes) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Yuval Birnboim (Racah Institute of Physics) "Cold flows\; when they occur\, and how they interact with halos and galaxies." TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190322T030000Z DTEND:20190322T033000Z DTSTAMP:20261011T152429Z UID:0b6h93gq936dveal6f9rqbv6gg@google.com CREATED:20190204T232138Z DESCRIPTION:Turbulence is ubiquitous in astrophysics\, occurring at scales from planetary atmospheres to clusters of galaxies. It plays a key role in the dynamics and thermodynamic evolution of gas in the intracluster mediu m (ICM) - it can both enhance and arrest radiative cooling of the ICM gas under different conditions. Estimating turbulent gas velocities and correl ation length scales is a key step in determining the fate of the ICM gas. In this talk\, I shall give a brief overview of the current state of ICM s imulations and observations. Following this\, I shall present my planned P hD work on simulations of ICM gas and how it will add to our current under standing of turbulence in the ICM. I shall also discuss my planned side pr oject on the circumgalactic medium (CGM) - modifying the ICM setup to stud y turbulence in the CGM\, and how it can be used to explain the ubiquitous presence of high velocity clouds (HVCs) in the halo of galaxies. LAST-MODIFIED:20190322T000105Z LOCATION:CSO Common Room (host: Pingel) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rajsekhar Mohapatra (RSAA) "Turbulence around galaxies: application s in the ICM and CGM (Thesis proposal talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230727T010000Z DTEND:20230727T023000Z DTSTAMP:20261011T152429Z UID:pn5hpruv4uur6vgah4rdsfuido@google.com CREATED:20230720T231607Z DESCRIPTION:The recent commissioning JWST has opened a new window to the hi gh-redshift Universe. In particular\, NIRCam and NIRSpec provide imaging a nd spectroscopy of the rest-frame optical of early galaxies with unprecede nted depth and resolution\, affording new insights into the properties of stellar populations and interstellar medium (ISM) at early cosmic times. T he JWST Advanced Deep Extragalactic Survey (JADES) is a large GTO program executed across JWST Cycles 1 and 2\, comprising over 600 hours of deep NI RCam imaging and NIRSpec multi-object spectroscopy. This survey will assem ble a large near-infrared dataset with enormous legacy value for studying galaxies from cosmic noon out to the highest redshifts. In this talk\, I w ill present early results from JADES focusing on galaxies in the epoch of reionisation (z>6). With this dataset we can probe the ISM conditions of t hese galaxies\, including metallicity\, temperature and ionisation state\, finding a large variety of conditions in these galaxies. Combined with an alysis of the stellar populations and star-formation histories\, these fin dings suggest that these galaxies are experiencing rapid evolution dominat ed by bursty star formation. n addition to results from samples of typical galaxies at these redshifts\, I will also discuss results from some of th e most extreme outliers\, and some of the insights gained from these into the conditions of early star formation. LAST-MODIFIED:20230720T231607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Trey) \nZoom: https://anu. zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alex Cameron (Oxford University) "Early results from JWST/NIRSpec w ith JADES: properties of early galaxies and their impact on the Universe a round them" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210330T000000Z DTEND:20210330T010000Z DTSTAMP:20261011T152429Z UID:nlsd98368i2otk5povcmseu0m0@google.com CREATED:20210122T024114Z DESCRIPTION:Massive stars have a profound astrophysical influence on the in terstellar medium (ISM) throughout their tumultuous lives and deaths. Stel lar feedback occurs through a variety of mechanisms: radiation\, photoioni zation heating\, winds\, protostellar jets\, supernovae\, and cosmic rays. Despite its importance\, stellar feedback is cited as one of the biggest uncertainties in astrophysics today\, stemming from a need for observation al constraints and the challenges of considering many feedback modes simul taneously. In this talk\, I will discuss recent studies of feedback from s mall scales of star clusters to large scales of galactic disks and outflow s. By comparing multiwavelength observations with theoretical models\, I w ill present constraints on the comparative role of different feedback mode s and how they vary over time and conditions. Moreover\, I will discuss th e latest developments in understand the importance of cosmic-ray feedback based on simulations and high-energy observations. LAST-MODIFIED:20210325T231108Z LOCATION:ZOOM (host: Amit Seta) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Laura Lopez (Ohio State) "Invited Colloquium: The Importance and Ch allenges of Assessing Stellar Feedback" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260901T010000Z DTEND:20260901T020000Z DTSTAMP:20261011T152430Z UID:b4c8ldpvq0kn227k7893dgpfb0@google.com CREATED:20260605T021619Z DESCRIPTION:Direct detection experiments seek to observe rare interactions between dark matter particles and ordinary matter\, requiring extreme sens itivity and deep underground locations to shield against cosmic-ray backgr ounds. The two dark matter searches I will introduce in this talk happen t o share an unusual home: gold mines.\n\nLUX-ZEPLIN (LZ) is located 1.5 km underground at the Sanford Underground Research Facility\, in a decommissi oned gold mine in Lead\, South Dakota. The experiment uses a dual-phase ti me projection chamber containing 7 tonnes of active liquid xenon and\, dur ing its 1000-day science run\, aims to probe WIMP-nucleon spin-independent cross sections down to about 1.4 × 10⁻⁴⁸ cm² for a 40 GeV/c² WIM P. I will give an overview of the experiment\, its current status\, and re cent results\, including world-leading dark matter search limits and the d etection of Boron-8 solar neutrinos.\n\nI will also discuss SABRE South\, Australia’s first underground dark matter experiment. It is part of an i nternational collaboration with twin detectors in the Northern and Souther n Hemispheres (SABRE North and South). SABRE aims to exploit its dual-hemi sphere design to help distinguish possible dark matter signals from season al backgrounds\, a strategy that is only possible with a southern-hemisphe re experiment. SABRE South is housed at the new Stawell Underground Physic s Laboratory (SUPL)\, located 1024 m underground within the still-active S tawell Gold Mine in regional Victoria\, Australia. I will provide an overv iew of the experiment’s current status and expected reach. LAST-MODIFIED:20260721T000016Z LOCATION:Zoom or Duffield Lecture Theatre (host: TBC) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Theresa Fruth (U. Sydney) "Searching for Dark Matter Deep Undergrou nd: Tales from Two Gold Mines" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171208T003000Z DTEND:20171208T005000Z DTSTAMP:20261011T152429Z UID:p3cjjci15kpvv4m09ulv540ldo@google.com CREATED:20171207T053606Z DESCRIPTION:Mandatory lecture on specific fire preparedness at MSO LAST-MODIFIED:20171207T053606Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Adam Agius (Engineering and Technical Services\, Facilities and Ser vices) "Specific Fire Preparedness at MSO" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210511T010000Z DTEND:20210511T020000Z DTSTAMP:20261011T152429Z UID:5feeq799pprolhr0etsok8fctk@google.com CREATED:20210508T025106Z DESCRIPTION:In this talk\, a new class of high-order numerical algorithms f or computational fluid dynamics is described. The new method is based on t he Gaussian Processes (GP) modeling that generalizes the Gaussian probabil ity distribution. The new approach is to adopt the idea of the GP predicti on technique\, which utilizes the covariance kernel functions and use it t o reconstruct high-order approximations for computational simulations. The new GP high-order method is proposed as a new numerical high-order formul ation\, alternative to the conventional polynomial-based approaches. LAST-MODIFIED:20210508T025106Z LOCATION:DLT and ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dongwook Lee (UC Santa Cruz\, USA) "Polynomial-free\, Variable High -order Methods using Gaussian Process Modeling for Computational Astrophys ics" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190208T030000Z DTEND:20190208T033000Z DTSTAMP:20261011T152429Z UID:fngfclvrqelv3491o6dqd7heb8@google.com CREATED:20190108T053110Z DESCRIPTION:The Magellanic Stream (MS) is a low density\, metal poor tidal stream of neutral Hydrogen (HI) trailing out behind the Magellanic Clouds. In such an environment we would not expect cold HI to be found\, yet cold HI has been observed in the MS. The formation of cold HI is an important step in star formation and the MS replicates conditions in the high red-sh ift universe\, but right on our doorstep. Using the GASKAP HI observations \, I will explore how the fraction of cold HI varies in the Magellanic Str eam as it reduces in density as it stretches away from the Magellanic Clou ds. LAST-MODIFIED:20190204T230109Z LOCATION:CSO Common Room (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:James Dempsey (RSAA) "GASKAP Observations of Cold HI in the Magella nic Stream (Thesis proposal talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241023T023000Z DTEND:20241023T043000Z DTSTAMP:20261011T152429Z UID:o895ggsapm1r6ufc7rlv31fc5k@google.com CREATED:20241020T224207Z DESCRIPTION:End-of-semester presentaions from the ASTR 3005 students. LAST-MODIFIED:20241020T224207Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Helmut Jerjen) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:ASTR3005 students (RSAA) "End-of-semester presentations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250206T000000Z DTEND:20250206T010000Z DTSTAMP:20261011T152429Z UID:lqobmc07f5jjmqkmbess5m7oh0@google.com CREATED:20241108T052618Z DESCRIPTION:Weakly collisional plasmas\, such as the solar wind\, hot accre tion flows and the intracluster medium of galaxy clusters\, have dynamical ly strong magnetic fields. In collisional plasmas\, which can be approxima ted in the magnetohydrodynamical (MHD) limit\, the turbulent dynamo mechan ism can amplify seed magnetic fields of much weaker strength of astrophysi cal or primordial origin to strong dynamical levels efficiently by convert ing turbulent kinetic energy into magnetic energy. However\, the viability of this mechanism in weakly collisional or completely collisionless plasm a is much less understood. In this talk\, I will discuss the properties of the collisionless turbulent dynamo using three-dimensional hybrid-kinetic particle-in-cell simulations with the "AHKASH" code. I will describe "AHK ASH" - a new Hybrid particle-in-cell (PIC) code developed within the frame work of the multi-physics code FLASH. Our new second-order accurate hybrid PIC method uses the Boris particle integrator and a predictor-predictor-c orrector algorithm for advancing the Hybrid-kinetic equations. We introduc e turbulence driving\, modelled using the Ornstein-Uhlenbeck process\, in the new Hybrid PIC code. To investigate steady-state turbulence with a fix ed Mach number\, it is important to maintain isothermal conditions\, and w e introduce a novel cooling method for PIC codes to achieve this. I will d escribe the properties of the collisionless turbulent dynamo in the kinema tic regime for different values of the magnetic Reynolds number\, initial magnetic-to-kinetic energy ratio\, and initial Larmor ratio\, i.e. the rat io of the Larmor radius to the size of the turbulent system. I will also d iscuss the distribution and evolution of the pressure anisotropy in the co llisionless plasma and compare our results with the MHD turbulent dynamo. The nature of the collisional turbulent dynamo in the subsonic and superso nic regimes can differ significantly\, as demonstrated by numerical MHD st udies. I will discuss the features of turbulence and magnetic field amplif ication from the collisionless turbulent dynamo in both the subsonic and s upersonic regime. LAST-MODIFIED:20250203T030608Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Amit Seta) \nZoom: https:/ /anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Radhika Achikanath Chirakkara (RSAA) "Magnetic field amplification in collisionless plasma (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190201T030000Z DTEND:20190201T033000Z DTSTAMP:20261011T152429Z UID:ghv2l9bhv3e70nlhpfs403kotc@google.com CREATED:20190108T053108Z DESCRIPTION:The Transiting Exoplanet Survey Satellite (TESS) is a new space telescope aimed at providing high cadence photometry of the local Univers e. While it is primarily designed for the study of exoplanets\, TESS will also provide the scientific community with a wealth of high-quality data t hrough which stellar transients can be analysed. In this talk\, I will pre sent my proposed thesis work on the methods through which TESS can be used to study early phases of a supernova (SN)\, with an emphasis on type Ia S N and 'peculiar' SN. I will then use this data to constrain SN progenitor systems\, which has important implications for both stellar evolution and measurements of dark energy. LAST-MODIFIED:20190201T002605Z LOCATION:CSO Common Room (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Harrison Abbot (RSAA) "Real time detection of shock physics in TESS (Thesis Proposal Talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141127T000000Z DTEND:20141127T010000Z DTSTAMP:20261011T152430Z UID:v1aqgn95m6lhuels2krdkjlmb8@google.com CREATED:20141118T034100Z DESCRIPTION:I will discuss how Hubble Space Telescope images of deep fields \, coupled with wider-field surveys\, have discovered star-forming galaxie s out to very high redshifts\, close to the epoch that the intergalactic m edium reionizes (at z>6). From their rest-frame UV emission we can estimat e individual star formation rates\, and study evolution of the star format ion rate density with cosmic time. At lower redshifts\, near-infrared spec troscopy (including slitless spectroscopy with WFC3 on HST) has enabled us to measure star formation rates at redshifts beyond one through the redsh ifted rest-frame optical lines. I will review current work on this\, and l ook to future developments (in particular JWST). LAST-MODIFIED:20250925T231021Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) \nZoom: https://anu.zoo m.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Andrew Bunker (Oxford University) "Finding Distant Galaxies and Det ermining the Star Formation History of the Universe" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191122T030000Z DTEND:20191122T033000Z DTSTAMP:20261011T152429Z UID:1neaq81aen9gfae8j6c2sc3kcc@google.com CREATED:20191022T041211Z DESCRIPTION:We're all familiar with geostationary satellite antennas – th e Foxtel dishes atop many rooftops that point to a fixed location in space . The AITC has a number of programs\, however\, that rely on our ability to interact with satellites that freely zip across the sky under the influ ence of a plethora of perturbing forces. Understanding these forces is th e first step to being able to predict where any of the 20\,000+ catalogued orbital objects are at any particular instant so we know where – and wh en – to point our telescopes at them. In this talk I’ll outline how s atellites move\, how we find them and the challenges and opportunities the y afford to our communications and space environment research programs. LAST-MODIFIED:20191022T041211Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:James Webb (RSAA/AITC) "AITC Series – Space is big\, satellites a re (comparatively) small… the joys of finding\, tracking\, and using th em!" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181129T220000Z DTEND:20181130T060000Z DTSTAMP:20261011T152429Z UID:qu55hha1oi58kn1tit6bi7ion0@google.com CREATED:20180822T015209Z DESCRIPTION:This is the annual christmas seminars at Mount Stromlo. Student s from RSAA and elsewhere flock to the mountain to share their research wi th others. Invited talks from members of RSAA will also feature. LAST-MODIFIED:20181117T102112Z LOCATION:CSO Common Room (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Student Christmas Seminars (RSAA) "Student Christmas Seminars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240116T220000Z DTEND:20240117T010000Z DTSTAMP:20261011T152429Z UID:hbnvh9meni2lg63manb6afbbnc@google.com CREATED:20240102T025105Z DESCRIPTION:TBC LAST-MODIFIED:20240102T025105Z LOCATION:Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.zoom.us/j /83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA Summer Students (RSAA) "Summer Student Talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210126T230000Z DTEND:20210127T012000Z DTSTAMP:20261011T152429Z UID:ld1c4nfp73ls9gvl091f068mv0@google.com CREATED:20210105T043106Z DESCRIPTION:Schedule: 10:00 David Ashworth (AITC) 10:20 Mallika Sinha (RSAA ) 10:40 Kieran Hamley (AITC) 11:00 Jianling Tang (RSAA) 11:20 Weihao Luo ( AITC) 11:40 Hancheng Shao (RSAA) 12:00 James Li and Andrew Waddell (AITC) LAST-MODIFIED:20210105T043106Z LOCATION:DLT and ZOOM 997 8534 1005 (host: Travouillon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Summer Students (RSAA and AITC) "Summer student presentations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160609T010000Z DTEND:20160609T020000Z DTSTAMP:20261011T152429Z UID:d8v52rq6c7fhdvvf5ada3bm38o@google.com CREATED:20160307T024123Z DESCRIPTION:In this talk I will present in details the major features that govern the geometry and dynamics of cosmic flows on Mpc scales\, and furth er develop the consequences for mergers and gas inflows on galactic scales . In particular\, I will explain how the dynamical and anisotropic nature of the cosmic web imprints the cold gas steams and their later accretion o nto galaxies\, and how it affects the satellite distribution\, spin\, morp hology and scaling relations of galaxies over a wide range of redshifts. T o perform this analysis\, I will rely on both insights from lagrangian the ory and recent results drawn from zoom simulations of clusters and the ana lysis of the 100Mpc.h-1 box « full-physics» hydrodynamical cosmological simulation Horizon-AGN. LAST-MODIFIED:20160607T062105Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Charlotte Welker (University of Western Australia) "Mergers and gas accretion onto galaxies: the imprint of the cosmic web" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210607T233000Z DTEND:20210608T020000Z DTSTAMP:20261011T152429Z UID:qti6611krj6eb9f1lcq1j2blao@google.com CREATED:20210525T005709Z DESCRIPTION:09:00-10:00: Ethan Crosby Near-Field Cosmology and the satellit e galaxies of the local spiral NGC2583 10:00-10:30: Yuxuan Yuan The obser vable properties of cool winds from galaxies\, AGN\, and star clusters - I I. Multiphase wind in M82 10:30-11:00: Astrocoffee 11:00-11:40: Shumeng Zhang A panoramic survey of the LocalGroup dwarf galaxy NGC 6822. LAST-MODIFIED:20210602T010107Z LOCATION:ZOOM and DLT (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA Students (RSAA) "Honours and Masters Talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251007T000000Z DTEND:20251007T010000Z DTSTAMP:20261011T152430Z UID:o9b5cee5vlv355ogo0hqvq9a8s@google.com CREATED:20250907T234110Z DESCRIPTION:What are the chances of us gaining an understanding of the fund amental makeup of the cosmological dark matter? I will cover some pessimis tic viewpoints where the answer to this question might be forever out of r each\, as well as some more optimistic prospects for real advances in our understanding that will come over the next decade. LAST-MODIFIED:20250924T013609Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ciaran O'Hare (U Sydney) "Will we ever know what dark matter is mad e of?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230815T010000Z DTEND:20230815T023000Z DTSTAMP:20261011T152429Z UID:8d06hqofqbvjar7d7km9m6mlm4@google.com CREATED:20230804T094111Z DESCRIPTION:Correct interpretation of observations relies on proper modelli ng of the astrophysical systems and proper treatment of the radiation from the systems it is generated and of how the radiation is modified when it propagates to the observer. With the coming of high quality spectroscopic and timing data\, proper treatment of the transport of the radiation is th erefore required. In this talk I will present a covariant formulation of t he transport of photonic and non-photonic particles and discuss the ration ales behind it. The objective of constructing this covariant formulation i s for practical applications in real astrophysical situations\, in particu lar\, in extremely strong gravity environments and cosmology. I will show results of our calculations in three cases: (1) eruptive magnetic flares f rom near black-hole event horizon\, (2) all-sky radio polarisation and (3) 21-cm signals from the cosmological reionisation epoch. I will also brief ly discuss applications in timing of millisecond pulsars in extreme-mass-r atio inspirals/binaries\, Lyman-alpha emission from distant galaxies\, len sing of non-photonic relativistic particles in black-hole environments\, a nd propagation of radiation from neutron star - neutron star mergers. LAST-MODIFIED:20230807T024109Z LOCATION:TBD (host: Samuel) \nZoom: https://anu.zoom.us/j/83410388355?pwd=Q m9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kinwah Wu (University College London) "Covariant transport of radia tion and particles and applications in strong gravity environments and cos mology" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190724T230000Z DTEND:20190725T000000Z DTSTAMP:20261011T152430Z UID:bvhs69vgk56oa2h3o3fel18h5k@google.com CREATED:20190712T010607Z DESCRIPTION:[A colloquium by the shortlisted candidate for the new Centre f or Gravitational Astrophysics] The observation of gravitational waves from the compact binary coalescences (CBC) opens a new era of gravitational-wa ve physics and multi-messenger astronomy. What happens after the coalescen ce? What else can we learn from the remnants? In this talk\, I will introd uce two studies about the CBC remnants. One is to search for gravitational waves from the remnant of the binary neutron star merger\, GW170817. Alth ough no significant signal candidate is found for this particular event\, development and verification of new methods is of importance for future ap plications. Prospects will become good with future detectors and the combi nation of multiple channels. The other is to search for yet-undiscovered\, weakly interacting\, ultralight bosons by following up the newly born bla ck holes after the coalescences. The number of such particles around a rap idly rotating black hole can grow exponentially due to the phenomenon of s uperradiance\, forming a macroscopic cloud and generating continuous gravi tational waves. The theory of boson clouds around black holes and the grav itational-wave emission mechanism will be explained. The search challenges and the empirical estimates of the search sensitivity will be discussed. These gravitational-wave searches are closely connected to theoretical pre dictions and electromagnetic observations. One of the most exciting aspect s of gravitational-wave discovery is that pieces from different channels a re being brought together to study fundamental physics. LAST-MODIFIED:20190712T010607Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ling (Lilli) Sun (Caltech) "After the coalescences — searches for the binary neutron star post-merger remnants and ultralight bosons" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160825T010000Z DTEND:20160825T020000Z DTSTAMP:20261011T152429Z UID:k2rpp3j6af0hm3t9sk1ldc8vrg@google.com CREATED:20160601T004617Z DESCRIPTION:TBD LAST-MODIFIED:20160712T030713Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Skymapper workshop (DLT taken up) (RSAA) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160428T010000Z DTEND:20160428T020000Z DTSTAMP:20261011T152429Z UID:pq5dgit6m80m1ha5tqa53dttbs@google.com CREATED:20151203T024614Z DESCRIPTION:The first billion years after the Big Bang poses many open ques tions: How and when the first stars and galaxies were formed? How does the interplay between baryonic and dark matter physics determine the properti es of these objects and evolve them with time into the galaxies\, stars an d black holes observed today? In this talk\, I will present the latest Hub ble Space Telescope observations of galaxies in the first billion years an d discuss how the evolution of their luminosity function can be linked to the dynamical assembly of dark matter halos. Modeling the connection betwe en dark and light not only complements observations by unveiling widesprea d star formation below the current detection limits\, but it also inspires the design of future investigations aimed at characterizing the earliest forming galaxies in the young Universe. LAST-MODIFIED:20160414T101607Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Michele Trenti (University of Melbourne) "Dark and Light at Cosmic Dawn" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150326T000000Z DTEND:20150326T010000Z DTSTAMP:20261011T152429Z UID:hrjh61k0bq5h2v0e4nuvqjr39s@google.com CREATED:20141209T010113Z DESCRIPTION:Local galaxies are in a state of 'energy equipartition' which m eans that the kinetic energy density equals roughly the thermal one and th e magnetic one. Thus\, we can deduce that magnetic fields play a crucial r ole in galactic processes like for example star formation. In models of yo ung galaxies magnetic fields are usually not considered as they are assume d not to be dynamical important at high redshifts. In the presence of turb ulence\, however\, the 'turbulent dynamo' can amplify weak magnetic seed f ields by randomly stretching\, twisting\, and folding the field lines. The details of this process depend on the nature of turbulence\, i.e. on the hydrodynamic and magnetic Reynolds numbers\, and on the compressibility of the gas. In my talk I will discuss the physics of the turbulent dynamo an d sketch the analytical derivation of its properties. I compare these theo retical results with the ones found in state-of-the-art numerical simulati ons. As an application I discuss the magnetic field amplification in a you ng galaxy\, where turbulence is driven by accretion and supernova explosio ns. In our semi-analytical model we follow the exponential growth of the m agnetic field on the dissipative scale and also the subsequent transport o f the magnetic energy to larger scales in the non-linear dynamo phase. Dep ending on the parameters of our model we find that equipartition of magnet ic and kinetic energy\, i.e. a field strength of roughly 10^(-5) G\, is re ached within 4 to 270 Myr. Thus\, we expect that the turbulent dynamo can generate strong unordered fields already in very young galaxies. LAST-MODIFIED:20150612T083202Z LOCATION:Duffield Lecture Theatre (host: Christoph Federrath) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jennifer Schober (Heidelberg University) "The Origin of Strong Magn etic Fields in Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220712T232000Z DTEND:20220713T034000Z DTSTAMP:20261011T152429Z UID:ud5rjt0oqhk2e1q2s93rv92f90@google.com CREATED:20220705T052108Z DESCRIPTION:Schedule available at : https://anu365-my.sharepoint.com/:x:/g/ personal/u1057001_anu_edu_au/EX00_zlqLHdKpjR-rZiRGBABRC1a20hn3dM4wEmmIMyoT Q?e=DpJnwu LAST-MODIFIED:20220705T052108Z LOCATION:DLT & ZOOM (host: Tony Travouillon) \nZoom: https://anu.zoom.us/j/ 99785341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA HDR Students (RSAA) "RSAA HDR Students Thesis Proposals and An nual Reviews" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220816T010000Z DTEND:20220816T020000Z DTSTAMP:20261011T152429Z UID:nc05996gao148e7qmj0sdt1v20@google.com CREATED:20220615T083608Z DESCRIPTION:Recent developments have enabled the usage of asteroseismology for measurement of stellar masses\, hence ages\, at a high level of precis ion and accuracy for red giants\, thanks to the exquisite photometry from space-based observatories. Combining precise chronological information wit h other observables such as chemical abundances is refining our understand ing of the Milky Way. In this work\, we dissect in depth a sample of 23 st ars\, making a detailed chemical analysis from high-quality HIRES@Keck spe ctra. We combine the chemical information with a careful asteroseismic gri d-based modelling that determines the fundamental parameters of these 23 s tars\, ages included\, and we study their kinematics to complete their big picture. These stars were selected due to being identified as outliers in past surveys\, with their previously estimated ages in disagreement with their overall chemistry: old and metal-rich\, young and metal-poor\, young and alpha-rich. The chemical abundances are derived with a classical 1D L TE spectroscopic method. The asteroseismic grid-based modelling uses inter polation of several observables\, including asteroseismic information. The kinematic analysis relies on modelling with GalPy. Our results confirm th e need for a model-based correction in the determination of stellar masses in red giants. However\, such correction was not enough to make the 'youn g and metal-poor' objects be old enough to have ages compatible with the e xpectations for the formation of the Milky Way halo. Two of these stars we re identified as being likely accreted by the Milky Way\, while two other stars are potential evolved blue stragglers. Our findings also suggest tha t the uncertainties of Gaia (E)DR3 parallaxes might be underestimated. Als o\, the understanding of the stars in the core He-burning phase is still h ampered by uncertainties regarding mass loss in the previous evolutionary stage. Finally\, we show that our method yields better precision in the de termination of stellar masses of red giants when compared to recent large- scale surveys. LAST-MODIFIED:20220808T034106Z LOCATION:DLT & ZOOM (host: Shyam) \nZoom: https://anu.zoom.us/j/99785341005 ?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Arthur Alencastro Puls (RSAA) "Investigating the Relationship Betwe en Chemical Abundance Ratios and Ages in Red Giant Stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240808T010000Z DTEND:20240808T020000Z DTSTAMP:20261011T152429Z UID:hpqsui12gk6dut471oetcn8m9s@google.com CREATED:20240417T012641Z DESCRIPTION:Laser Guide Star Adaptive Optics (LGS AO) systems play a fundam ental role in correcting atmospheric distortions for astronomical observat ions. Adaptive Optics requires at least one bright star near the scientifi c object of interest as a reference for measuring the distorted wavefront. Requirements on brightness and proximity restrict Natural Guide Star (NGS ) AO systems to a small fraction (< 10%) of the sky. Since the inclusion o f Laser Guide Stars (LGS)\, the sky coverage has risen dramatically to ~85 %. However\, the tip-tilt indetermination problem remains unsolved: the ti p-tilt uplink component is dominant over the tip-tilt downlink component o f the LGS and cannot be distinguished from one another using only the ligh t from the artificial star. This means that the LGS cannot measure tip-til t modes\, preventing 100% sky coverage. NGSs are required to be sufficient ly bright\, being currently the main limitation for AO systems. This is an issue for targets at the galactic poles where the density of stars is low er\, high redshift targets\, and for targets of opportunity operations\, r esponding to transient events such as gravitational waves\, gamma-ray burs ts\, and supernova explosions. This presentation explores the intricacies of tip-tilt determination in LGS AO\, examining current methodologies\, te chnological advancements\, and unresolved issues. We have identified key r esearch directions and potential solutions to enhance tip-tilt estimation in LGS AO systems\, ultimately advancing the adaptive optics technology fo r groundbreaking astronomical observations with 100% sky coverage. LAST-MODIFIED:20240715T070614Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Noelia Martinez Rey (RSAA) "Towards 100% sky coverage\, challenges and potential solutions for tip-tilt sensing in Laser Guide Star Adaptive Optics" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261013T040000Z DTEND:20261013T051500Z DTSTAMP:20261011T152430Z UID:kglvk847r6drhtlb744h7r7rj4@google.com CREATED:20260503T114417Z DESCRIPTION:Our monthly Skillshare sessions provide an informal\, supportiv e\, and practical space for students and postdoctoral researchers to devel op and exchange research skills\, professional-development tools\, and eff ective workflows. The format is primarily focused on students\, in particu lar those enrolled in the ASTR8030 course Astronomy and Astrophysics Resea rch Skills. However\, everyone is very warmly invited to join and contribu te.\n\nSessions are held on selected Tuesdays from approximately 3:00-4:15 ish pm in the CSO Common Room. Depending on the topic\, they may include s hort introductions\, demonstrations\, panel discussions\, interactive exer cises\, or open-ended hands-on activities. LAST-MODIFIED:20261007T220006Z LOCATION:Zoom or CSO Common Room (host: Sven Buder and Melanie Kaasinen) \n Zoom: https://anu.zoom.us/j/89544552112?pwd=Bdoo5fgMVS2Ls6e3Fs0NSNk9OMpaXn .1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:RSAA Skillshare (RSAA) "The subtle art of reviewing" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191127T000000Z DTEND:20191127T010000Z DTSTAMP:20261011T152429Z UID:9pqr015gk43rdo7973gm0igr9c@google.com CREATED:20191116T215608Z DESCRIPTION:Science missions to comets and moons in our solar system have r eturned surprising results about the presence and abundance of small molec ules\, such as H2\, O2\, CH3OH\, and even Glycine\, whose formation in the extreme conditions of outer space is puzzling. Such molecules are conside red biomarkers and may relate to the origin of life and water on Earth. Th is talk will explore new and unusual reaction dynamics of energetic H2O mo lecules colliding with surfaces of astrophysical relevance\, where reactio n barriers are overcome by kinetic energy. Three such reactions will be di scussed: (i) the splitting of water directly into molecular H2 and atomic oxygen in single collisions of water ions with generic surfaces\, (ii) the abstraction of oxygen from oxidized surfaces by water ions\, which leads to facile production of molecular O2 and (iii) the dynamic deuterium excha nge in normal water ion collisions with deuterated surfaces. The former tw o reactions offer abiotic explanations for the origin of the H2 discovered recently on Enceladus\, and the O2 found in abundance on comet 67P. The l ast reaction suggests a possible way to alter the D/H ratio in water when detected in situ in cometary comae. The findings have broad implications f or measurements of gas-phase composition in astrophysical environments. LAST-MODIFIED:20191119T105607Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Konstantinos P. Giapis (Caltech) "Chemical Reactions Out Of This Wo rld" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260206T030000Z DTEND:20260206T033000Z DTSTAMP:20261011T152430Z UID:rhcddfn309slgrll3jbu4ghqhg@google.com CREATED:20260122T000605Z DESCRIPTION:Galaxy formation depends not only on large-scale cosmological f lows but also on small-scale processes that shape the thermodynamic and mu ltiphase structure of galactic gas. I will present insights from simulatio ns that explicitly resolve these small-scale processes. In massive ellipti cal galaxies\, I demonstrate that resolving individual Type Ia supernovae\ , rather than treating them as smooth heating\, is crucial for determining whether gas cools to feed black holes or escapes in outflows. In the circ umgalactic medium\, I show that resolving cold gas embedded in multiphase turbulence is key to understanding whether cold clouds survive or are dest royed. These processes occur far below the resolution of cosmological simu lations\, making idealized simulations indispensable for connecting microp hysics to galaxy evolution. LAST-MODIFIED:20260202T223107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Christoph Federrath) \nZoo m: https://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rajsekhar Mohapatra (Princeton U.) "Modelling The Hidden Architects of Galaxy formation: Turbulence\, Cooling\, and Supernovae" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181128T002000Z DTEND:20181128T004000Z DTSTAMP:20261011T152429Z UID:s7jnje88hgtna310neqdhhtoh4@google.com CREATED:20181105T050114Z DESCRIPTION:Origins of life research is a complex interdisciplinary field i nformed by many areas\, at the centre of which is prebiotic chemistry. A b ranch of synthetic chemistry\, prebiotic chemistry additionally draws heav ily on biology\, physics and planetary sciences in order to shape plausibl e scenarios by which building blocks could arise and unite to form the fir st primitive biological systems. This talk will briefly highlight some key problems and recent advances in prebiotic synthesis with perspective on h ow they have been informed by geo- and astro- sciences. Such an approach h as led to the construction of a chemical network\, limited by reasonable g eological and extraterrestrial constraints\, that provides key ingredients of life such as RNA\, sugars\, amino acids\, lipids\, polymers\, and\, mo st recently\, DNA. LAST-MODIFIED:20181121T004608Z LOCATION:CSO Common Room (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Nick Green (University of Cambridge) "Chemistry and the Origins of Life" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191018T030000Z DTEND:20191018T033000Z DTSTAMP:20261011T152429Z UID:iq7kknjv25qmris2hlpi39hbp4@google.com CREATED:20191004T042608Z DESCRIPTION:With DREAMS in production and Palomar-Gattini collecting data\, it is time to prepare for the next generation of IR transient telescopes. A wide-field\, meter class telescope located in Antarctica would bring th e deepest all-sky survey ever taken in K-band with unprecedented cadence. AITC and Caltech are already leading the charge and plan to complete suc h this telescope in 5 years in order to match the LIGO upgrade that would allow us to find IR counterparts to gravitational waves. Now is time to bu ild the Australian side of the Antarctic-DREAMS consortium (BYO white pape rs...). LAST-MODIFIED:20191017T013105Z LOCATION:Duffield Lecture Theatre (host: Monty) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tony Travouillon (RSAA/AITC) "AITC Series - Antarctic-DREAMS" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150424T042000Z DTEND:20150424T044000Z DTSTAMP:20261011T152429Z UID:bv104p4j7h6gs2pmlh4lp7ioj8@google.com CREATED:20150410T063112Z DESCRIPTION:Astronomy and astrophysics provide an excellent set of skills t hat can be used in other fields. I will present a summary of my previous a stronomy work and my current career in river management. This will include an introduction to the Murray-Darling Basin\, and a discussion about the ability of science to influence government policy. LAST-MODIFIED:20150420T035106Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Matthew Coleman (Murray-Darling Basin Authority) "From Stellar Stre ams to Rivers and Streams: Astrophysics in the Murray-Darling Basin" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160512T010000Z DTEND:20160512T020000Z DTSTAMP:20261011T152430Z UID:kgfllg0kjnavif2agtmke910uo@google.com CREATED:20151202T024113Z DESCRIPTION:The Laser Interferometric Gravitational-wave Observatory (LIGO) has detected gravitational waves from the merger of two 30Msun black hole s (Abbott et al. 2016). An earlier prediction (Belczynski et al. 2010a) th at binary black holes would constitute the first detection was therefore b orne out\, but predictions of merger rates have varied over several orders of magnitude (Abadie et al. 2010). We have generated and analyze a suite of models\, each with 640 million simulations of black hole formation and mergers under a range of environmental conditions and physical processes. We find that\, given the sensitivity of current gravitational wave detecto rs\, the most common detections will originate from two comparable-mass co alescing black holes\, with total masses in the range 20-80 Msun. Within t he framework of our simulations\, we conclude that the stellar progenitors of the LIGO event GW150914 were formed in an environment where the metall icity was less than 10 per cent of solar\, and had initial masses of 40-10 0 Msun. They interacted through mass transfer and a common envelope phase\ , and both black holes formed without supernova explosions. The black hole s' spins and orbital angular momenta are nearly parallel and nearly unchan ged since birth. The progenitors likely formed either at 2 Gyr\, or somewh at less likely at 11 Gyr after Big Bang. The field formation of binary bla ck holes\, with low BH natal kicks and restricted common envelope evolutio n\, produces 40 times more binary black holes than dynamical formation cha nnels involving globular clusters. LAST-MODIFIED:20160415T073611Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Krzysztof Belczynski (Warsaw University) "The origin and evolution of LIGO's first gravitational-wave source" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20211209T000000Z DTEND:20211209T003000Z DTSTAMP:20261011T152429Z UID:p638q4o8re7oc018oel72t11ds@google.com CREATED:20211130T040611Z DESCRIPTION:Giant molecular clouds (GMCs) are the sites of star formation i n galaxies. Their lifecycle determines the galactic-scale star formation r ate and efficiency\, and so they form the communication channel between th e galactic environment and the parsec-scale physics of star formation and stellar feedback. Here\, I use high-resolution isolated galaxy simulations in the moving-mesh code Arepo\, including a full suite of chemistry\, sta r formation and stellar feedback physics\, to investigate (1) the impact o f the galactic environment on GMC properties\, and (2) the impact of sub-c loud stellar feedback (supernovae and HII region pressure from young massi ve stars) on the GMC lifecycle. I find evidence that the rate of GMC forma tion increases with the galactic mid-plane pressure\, while the sub-cloud star formation efficiency and rate of cloud destruction are determined pri marily by stellar feedback. I also present results demonstrating that GMC kinematics can be used to accurately predict the molecular gas disc scale- height in galaxies. LAST-MODIFIED:20211206T050107Z LOCATION:ZOOM and DLT (host: Mark Krumholz) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sarah Jefferson (Havard CfA) "Galactic-scale star formation via Gia nt Molecular Clouds" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150624T230000Z DTEND:20150625T065000Z DTSTAMP:20261011T152429Z UID:1nocoqu4cpv2sh31g8rtji7vlo@google.com CREATED:20150511T053110Z DESCRIPTION:Various student talks will be presented. LAST-MODIFIED:20150625T044105Z LOCATION:Duffield Lecture Theatre (host: David Yong) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Students (RSAA) "Annual student thesis talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251202T000000Z DTEND:20251202T010000Z DTSTAMP:20261011T152430Z UID:thovp2o4rlc0or8evvm62e29m0@google.com CREATED:20250725T120618Z DESCRIPTION:Once thought to be clumpy\, turbulent systems\, high-redshift g alaxies are now revealed by the James Webb Space Telescope to host spiral arms\, bars\, and even thick and thin disks. These discoveries raise funda mental questions about how disk galaxies assemble\, how quickly they settl e into ordered rotation\, and what physical processes shape their long-ter m evolution. Closer to home\, Gaia together with Galactic archaeology surv eys such as GALAH and APOGEE\, reveal a complex picture in which the Milky Way is shaped through minor collisions with satellite galaxies and the de licate interplay of chemical and dynamical processes. Yet there is still n o consensus on how its distinct thin and thick disks formed and evolved\, and the answer is unlikely to come from studying the Milky Way alone. In t his talk\, I will present new results from the GECKOS survey\, a VLT/MUSE program targeting 36 edge-on Milky-Way-mass galaxies that provides detaile d\, spatially resolved chemistry and kinematics across a representative sa mple of local analogues. Our data are revealing a variety of kinematic sub -structures that require a contemporary view of galaxy morphology\, expand ing the traditional picture and linking the Milky Way's kinematic complexi ty with that seen in other galaxies. I will show how linking GECKOS with h ighly resolved face-on surveys such as PHANGS and MAUVE\, together with la rge multi-object IFS surveys like SAMI and Hector\, allows us to connect b ars and spiral features to the vertical structures seen in GECKOS. Alongsi de these latest results\, I will also discuss our work on placing the Milk y Way in a cosmological context and explore the likely outcome of the futu re collision between our Galaxy and Andromeda. LAST-MODIFIED:20251124T233607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Tim Gao) \nZoom: https://a nu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jesse van de Sande (UNSW) "The Milky Way's Past\, Present\, and Fut ure through an Extragalactic Lens" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260327T030000Z DTEND:20260327T033000Z DTSTAMP:20261011T152430Z UID:tbvmd438hb4cm6t06agidkihs8@google.com CREATED:20260323T092606Z DESCRIPTION:The Quantum Optical Ground Station has been equipped and tested to support a demonstration of high-speed optical communication with the A rtemis II mission. With the SLS rocket back at the launch pad and launch w indows starting next week this presentation will give an overview of what we are doing with the mission\, the techniques and technology involved\, a nd some of the challenges we have faced over the last 5 years of developme nt. LAST-MODIFIED:20260323T234807Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Francis Bennet (RSAA/AITC) "Overview of the Artemis II Optical Comm unication Demonstration at Mt Stromlo" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260820T010000Z DTEND:20260820T020000Z DTSTAMP:20261011T152430Z UID:d47tnbg40dv8m1djcfvodbldg0@google.com CREATED:20260615T020019Z DESCRIPTION:I will present the JWST ORCHIDS (“ORigin of [CII] halos In Di stant Systems”) project\, designed to uncover the origin of extended ion ized gas around massive galaxies at z=4–6 (“[CII] halos”)\, a key ye t poorly understood component of ISM–CGM interactions. ORCHIDS combines ~60 hours of deep JWST/NIRSpec and Keck/KCWI IFU spectroscopy of eight z=5 –6 star-forming galaxies\, together with public NIRCam/MIRI imaging\, an cillary NIRSpec data\, and high-resolution ALMA [CII] and dust maps. This multi-wavelength dataset enables a systematic investigation of the physica l drivers of [CII] halos\, including mergers\, outflows\, inflows\, and ex tended PDR and H II emission.\n\nEarly results reveal that [CII] halos are dynamically complex and frequently associated with interacting systems\, pointing to mergers as a primary driver of their formation\, while additio nal mechanisms likely contribute. I will highlight two representative syst ems\, including one showing broad [CII] emission and clear NIRCam evidence for a close merger\, illustrating how these halos trace the assembly and enrichment of the CGM in the early Universe. LAST-MODIFIED:20260816T220005Z LOCATION:Zoom or Duffield Lecture Theatre (host: Melanie Kaasinen) \nZoom: https://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Manuel Aravena (Universidad Diego Portales) "ORCHIDS: The Origin of [C ii] Halos in Distant Systems" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250325T000000Z DTEND:20250325T010000Z DTSTAMP:20261011T152429Z UID:ncnq5ri48qhhsfprdetcfekc3g@google.com CREATED:20250106T230122Z DESCRIPTION:Low- and intermediate-mass stars disgorge their outer layers du ring the asymptotic giant branch (AGB) phase\, one of the last stages of t heir lives. Material containing newly-formed elements and a variety of dus t and molecules streams out of them in what we call a stellar wind. Studie s resolving the extended circumstellar environments of AGB stars have reve aled spirals\, discs and bipolar outflows\, with the shaping of the gas at tributed to interactions with a companion. However\, most of these compani ons are not directly observed\, because their light is so strongly attenua ted by the dust created around the AGB star. Astrochemistry is the study o f molecules\, dust and the chemical reactions that link them in astrophysi cal environments. I will discuss new methods that combine theoretical astr ochemistry with observations to allow us to deduce the nature of the compa nion stars in binary systems with AGB stars. From this we can begin to und erstand how companion stars affect the length of the AGB phase. LAST-MODIFIED:20250218T105114Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Maya Jablonska) \nZoom: ht tps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Taissa Danilovich (Monash U.) "Astrochemistry as a diagnostic of ev olved stars in binary systems" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240528T010000Z DTEND:20240528T020000Z DTSTAMP:20261011T152429Z UID:6lok6obhlvcgfs0p6d1c27qdgc@google.com CREATED:20240430T055117Z DESCRIPTION:Supermassive black holes are thought to exist in the centres of most massive galaxies and their masses have been found to correlate stron gly with the properties of their host galaxies like overall luminosity or central velocity dispersion. Yet it is unknown what processes have establi shed these correlations and if and how they continue towards lower mass sy stems. In my talk I will present results from our search for massive black holes in ultra-compact dwarf galaxies and in massive globular clusters of the Milky Way. LAST-MODIFIED:20240521T214109Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Melissa Ness) \nZoom: http s://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Holger Baumgardt (U. Queensland) "Massive Black Holes in Stellar Sy stems" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250130T000000Z DTEND:20250130T010000Z DTSTAMP:20261011T152429Z UID:tg4tjb54mht0s6lnhordk9hjpk@google.com CREATED:20250107T045708Z DESCRIPTION:In the past two years\, the James Webb Space Telescope (JWST) h as revolutionized our understanding of the early universe\, uncovering gal axies as early as z~14 and revealing that nearly 80–90% of galaxies at z > 6 exhibit extreme emission lines. However\, the lack of direct Lyman-co ntinuum detections beyond z > 4.5\, combined with limited photometric cove rage\, challenges our ability to quantify the ionising photon budget of ga laxies during the reionisation era. In this talk\, I will demonstrate how carefully curated samples of galaxies at cosmic noon (z ~ 2–3) can infor m our understanding of early galaxy evolution. My work focuses on extreme emission line galaxies (EELGs) and Lyman-alpha emitters at z ~ 3 to explor e the production and escape of ionising radiation\, as well as the role of galaxy-galaxy interactions in shaping early galaxies. I will present evid ence that mergers trigger recent starbursts in EELGs and promote the escap e of Lyman-continuum radiation by inducing asymmetries in the neutral hydr ogen gas. I will also show the discovery of a giant (75 kpc) Lyman-alpha n ebula at z~3.25 created by interaction of two ~10^10 Msun galaxies that is triggering a new star cluster formation in a dwarf satellite galaxy. Thes e findings shed light on key processes such as gas accretion and Lyman-con tinuum escape\, offering deeper understanding of early galaxy evolution an d reionisation. LAST-MODIFIED:20250115T081607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anshu Gupta (Curtin U.) "MOSEL Survey: Understanding Epoch of Reion isation using galaxies cosmic noon" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190503T040000Z DTEND:20190503T042000Z DTSTAMP:20261011T152429Z UID:ds8vhgp9mfpma1intno7dsbiho@google.com CREATED:20190430T004606Z DESCRIPTION:In physics we often encounter high-dimensional data\, in the fo rm of multivariate measurements or of models with multiple free parameters . The information encoded is increasingly explored using machine learning\ , but is not typically explored visually. The barrier tends to be visualis ing beyond 3D\, but systematic approaches for this exist in the statistics literature. I will review some of these methods and discuss in detail the grand tour\, which visualises high-dimensional distributions as animation s of smoothly interpolated projections\, allowing the viewer to extrapolat e the shape of the parameter space in high dimensions. We can for example use the tour for the visualisation of multidimensional posterior distribut ions or to explore grouping in high dimension. I will then show how to use the idea of projection pursuit\, i.e. searching the high-dimensional spac e for 'interesting' low dimensional projections\, to detect complex associ ations between multiple parameters. LAST-MODIFIED:20190430T004606Z LOCATION:Duffield Lecture Theatre (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ursula Laa (Monash University) "High-dimensional data visualisation for physics applications" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240308T003000Z DTEND:20240308T013000Z DTSTAMP:20261011T152429Z UID:fhgmbavgmdad78pbn1isna2n10@google.com CREATED:20240307T050608Z DESCRIPTION:The ESO Science Archive is a powerful scientific resource for t he entire astronomical community\, contributing to about 40% of the overal l ESO science output as quantified by refereed papers. It stores both the raw data generated by all ESO instruments\, as well as selected processed data. These come from ESO public surveys\, large programmes and from bulk processing of selected instruments. They are processed to a level where ca n be used directly for scientific measurements. An added service is also b rowsing and retrieval of ALMA data\, conjointly with those of La Silla-Par anal Observatory. User access services and capabilities are provided to ma ke this rich content discoverable to the science community in the face of the ever increasing volume and complexity of the archive holdings. In this presentation\, the capabilities\, archive user services\, the diversified data holding and user community statistics\, including scientific publica tions\, of the ESO Science Archive are briefly illustrated. It highlights the legacy of the ESO archive as a resource in support of future multi-wav elength multi-messenger time-domain investigations of the Southern Sky. LAST-MODIFIED:20240307T050608Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBC) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Magda Arnaboldi (ESO) "The ESO Science Archive: a powerful scientif ic resource for the international astronomical community" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160429T040000Z DTEND:20160429T042000Z DTSTAMP:20261011T152429Z UID:4osck1moa5m3rjl3ld8uqu9njg@google.com CREATED:20160311T050112Z DESCRIPTION:In this talk\, I will introduce the simulated galaxy cluster ca talogue for the MACRO project\, the main aim of it\, and what we find. The hydro-dynamical simulations have a rapid development recently. With compl ex baryonic models\, they now can produce galaxies much closer to observed ones. So we should think about the next move in this research field. Wit h this MACRO project\, we want to deliver an message that simulations are not only for theoretical studies\, and can not only provide theoretical un derstandings by matching the observational relations\, they can also give suggestions to observations if we can properly bridge the gap between simu lations and observations. LAST-MODIFIED:20160429T012605Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Weiguang Cui (ICRAR) "MACRO: what does simulation suggest?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181212T030000Z DTEND:20181212T032000Z DTSTAMP:20261011T152429Z UID:o47s09c6kci3frruhhmseo0o2g@google.com CREATED:20181122T233614Z DESCRIPTION:The stellar population of a galaxy contains a record of its sta r formation and assembly history\, making it an important area of research to develop our understanding of galaxy formation and evolution. So far in my PhD I’ve worked on two projects\, the first focussing on early-type galaxies (ETGs)\, the second on late-types (LTGs). These works aim to unde rstand the link between the overall structure and dynamics of a galaxy\, a nd the evolution of the stars within it. Currently\, the well-established correlations between the mass of a galaxy and the properties of its stars are considered evidence for mass driving the evolution of the stellar popu lation. However\, in our ETGs project using the SAMI Galaxy survey\, we fo und that stellar population parameters correlate more tightly with gravita tional potential and surface mass density\, rather than mass. More recentl y\, we've extended this research to investigate the stellar populations of late-type galaxies (LTGs) using the Sloan Digital Sky Survey. In this fir st annual research update\, I will provide a recap of my first project usi ng ETGs\, before detailing the progress made on the LTGs project. LAST-MODIFIED:20181204T021608Z LOCATION:CSO Common Room (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tania Barone (RSAA) "Annual PhD research update: Dynamical Drivers of Stellar Populations in Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201023T030000Z DTEND:20201023T033000Z DTSTAMP:20261011T152429Z UID:ffcd1mqiih6b8ro2uftgmrudvg@google.com CREATED:20201012T002116Z DESCRIPTION:The new FoF format is like an Open Mic: Our speakers have 15 mi nutes each to talk about topics of their choice. The idea of the new FoF i s to get to know the many individuals that work under the same roof\, allo w newcomers to find friends easily\, and find new friends or colleagues wi th similar interests and hobbies. So feel free to talk about some of your most favourite adventures\, memorable Stromlo anecdotes\, your hobbies\, y our last COVID-DIY project\, your voluntary activities outside of Stromlo or whatever you are passionate about. Science talks (about a scientific to pic/question that you are interested in) are also welcome\, but be mindful of your audience (astronomers\, students\, engineers\, professional staff ). LAST-MODIFIED:20201012T050510Z LOCATION:ZOOM 997 8534 1005 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ayan Acharyya and Harry-Dean Kenchington Goldsmith (RSAA) "Illumina tion and Rangoli at IITKgp and (Astro-)Physics on the Acton Campus" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200129T000000Z DTEND:20200129T010000Z DTSTAMP:20261011T152429Z UID:nlkng8gvg0r4c0i49l4tmfva4c@google.com CREATED:20200113T004107Z DESCRIPTION:Adaptive Optics with Laser guide star is the most modern tool f or the astronomical observations\, in which high spatial resolution is req uired. After more than 20 years of developments\, it has reached full matu rity and routine operation\, allowing galactic and extragalactic observati ons with optimum and unique scientific returns. In this talk I will speak about the ESO VLT Adaptive Optics Facility\, the most recent LGS-AO projec t of ESO\, now in full operation at Cerro Paranal\, Chile. Of course\, the astrophysicists appetite for more discoveries with future ELTs\, requires to win more LGS-AO challenges\, via further technology developments. I wi ll therefore speak about some ongoing ESO Technology Developments\, relate d to future LGS-AO systems. LAST-MODIFIED:20200119T074108Z LOCATION:Duffield Lecture Theatre (host: Rey) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Domenico Bonaccini (ESO) "Laser Guide Star Systems: the ESO Adaptiv e Optics Facility and ongoing LGS Technologies R&D" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240314T000000Z DTEND:20240314T013000Z DTSTAMP:20261011T152429Z UID:lhcu6tq8qme882cd9ggktdgigg@google.com CREATED:20240220T233618Z DESCRIPTION:NASA’s Transiting Exoplanet Survey Satellite (TESS) is the fi rst all-sky space-based transiting planet survey mission. Using its full-s ky observations\, we have been able to discover and characterise some rare planet populations. These include the "scaled down" Solar Systems – mul tiplanetary systems with Jovian planets and Super Earths orbiting closely to their host stars. Understanding the formation of these planetary system s will be the first step towards placing the Solar System amongst the exop lanets. I have been using a new generation of ground and space based teles copes to examine their atmospheres\, interiors\, and population statistics . I will describe our JWST program aimed at examining the formation routes of one such exemplary system in exquisite detail. In the next five years\ , we look towards the full data release from the Gaia mission that will en able us to extend our knowledge to planets with orbital periods more compa rable to the Solar System planets. LAST-MODIFIED:20240308T100614Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Stu Wyithe) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Chelsea Huang (USQ) "How to form scaled down Solar Systems?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150514T010000Z DTEND:20150514T020000Z DTSTAMP:20261011T152429Z UID:1a02jh5pqgv31iih05tij04468@google.com CREATED:20150417T002112Z DESCRIPTION:The Southern African Large Telescope (SALT) was a relatively ch eap (~$20M) 10m class telescope\, for which the construction phase was com pleted\, relatively quickly\, by late 2005. However it took a number years before the commissioning was fully completed and the telescope only enter ed into full-time science operations in 2011. In this talk I will discuss some of the technical challenges that had to be overcome. The suit of firs t generation instruments will be described\, with particular emphasis on t he recently commissioned high resolution spectrograph\, and some of the sc ience highlights will be presented. These cover a range of topics\, and so me will focus on studies using the unique or rarer instrument capabilities for large telescopes. Finally\, I look to the future of SALT and the pros pects of new instruments and capabilities and I will also discuss some of other new SAAO facilities and future plans. LAST-MODIFIED:20150513T084605Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:David Buckley (SALT) "The Long Road to Science with the SALT" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151023T030000Z DTEND:20151023T032000Z DTSTAMP:20261011T152430Z UID:68n4ehbbkapjtb7jk5lptpqn1k@google.com CREATED:20150915T003610Z DESCRIPTION:In October last year I made the tough decision to leave astrono my\, after 11 years and 4 postdocs in three different countries. I made th e move into the relatively new field of data science\, originally working for the Department of Defence before moving to my current position at Tera data. In this talk I will describe my journey from academia to industry\, outline what a day in my life as a data scientist is like\, and discuss th e outlook for data science over the next few years. I will also suggest ho w someone from an astronomy background can best prepare themselves for a s imilar transition into data science. LAST-MODIFIED:20151018T222606Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sean Farrell (Teradata) "Life After Astronomy: Data Science as an A lternative Career" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240730T010000Z DTEND:20240730T020000Z DTSTAMP:20261011T152429Z UID:07eo4vcechv5grgs125o4red60@google.com CREATED:20240415T054236Z DESCRIPTION:Understanding the Near Earth Object population is a key compone nt of planetary defence. Telescopic surveys are near complete for >200m si zed bodies\, but even metre sized objects are capable of posing a threat t o people and property. The increasing number of manmade objects in orbit a round the Earth is also becoming a concern and not all re-enter in a contr olled manner. When objects hit the Earth's atmosphere\, they produce light \, heat and shock waves. Observing these phenomena\, gives us a huge amoun t of information about the impacting object\, be they natural or manmade. We can calculate the orbit they came from\, what they're made of\, their s ize\, and even where any debris or meteorites might land. The Global Fireb all Observatory is a planetary-scale observational facility for rare\, fir eball events occurring when objects hit our atmosphere. Multi-sensor obser vations allow us to characterise these objects\, underlying planetary defe nce efforts. LAST-MODIFIED:20240705T035108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hilay Shah) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ellie Sansom (Curtin U.) "A Global Fireball Observatory for planeta ry defence: a multidisciplinary approach" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240612T000000Z DTEND:20240612T024500Z DTSTAMP:20261011T152429Z UID:05o9l3d6c51t5rrpu50cn4huk0@google.com CREATED:20240305T110640Z DESCRIPTION:TBC LAST-MODIFIED:20240305T110640Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Chris Wolf) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Hons/MSc End-of-thesis talks (RSAA) "Hons/MSc End-of-thesis talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170217T030000Z DTEND:20170217T032000Z DTSTAMP:20261011T152429Z UID:3h6369h8l2v1pig52bibgqq9vo@google.com CREATED:20170210T023607Z DESCRIPTION:Typical star-forming galaxies show a strong correlation between their global star formation rates and stellar masses\, with starbursts id entified as outliers above and quenched galaxies as outliers below. Using data from the SAMI Galaxy Survey\, I will explore the spatial signatures of quenching star formation as a function of mass\, morphology\, and envir onment. We show signatures of inside-out quenching for typical galaxies a nd an outside-in reduction of star formation for galaxies in denser enviro nments. This program represents one of many science topics that you shoul d think about investigating with the upcoming public data release -- emiss ion line fits\, SFR maps\, and other data products included! LAST-MODIFIED:20170214T005606Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anne Medling (Caltech) "Resolving the Star-Forming Main Sequence wi th SAMI" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180302T030000Z DTEND:20180302T032000Z DTSTAMP:20261011T152429Z UID:sdgg8i6cm1uu271gdgmqodte2k@google.com CREATED:20180226T230607Z DESCRIPTION:Understanding the formation of stars and their mass distributio n remains an important unsolved problem in astrophysics. It has been sugge sted that turbulence plays a key role in the process. This ASC project aim ed to test the dependence of the stellar Initial Mass Function (IMF) on th e power spectrum of the turbulence\, as predicted by Hennebelle and Chabri er's analytical derivation. Numerical hydrodynamical simulations were used to produce mass distributions at several star formation efficiencies. Ini tial data is incomplete\, but the simulated slope of the IMF differed in p otentially significant ways to the theoretical prediction. This talk outli nes the project and its results\, and possible explanations for these diff erences. LAST-MODIFIED:20180228T062108Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Elizabeth Parkinson (RSAA) "The Role of Turbulence for the Origin o f Stellar Masses" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141121T032000Z DTEND:20141121T034000Z DTSTAMP:20261011T152429Z UID:vlsve005cknmthnt63sc99hg2g@google.com CREATED:20141117T060337Z DESCRIPTION:We use Integral Field Spectroscopic data from the Gemini Multi- Object Spectrograph to analyse the 3D kinematics\, ionization state\, temp erature and density of ionized gas in the "Green Bean" (GB) galaxy quasar ionization echo candidate J2240-0927. We model the emission line spectrum of each spaxel as a superposition of up to three Gaussian components and a nalyse the physical properties of each component individually. Two narrow components\, tracing the velocity fields of the disc and the ionized gas c loud\, are superimposed over the majority of the galaxy. A broader kinemat ic component is also ubiquitous across the galaxy disc. Fast shocks produc e hot\, dense\, turbulent\, [O III]-bright regions with large [N II]/Halph a and [S II]/Halpha ratios. The most prominent such spot is consistent wit h a radio jet shock-heating the interstellar medium. However\, the active galactic nucleus (AGN) is still responsible for > 82% of the galaxy's tota l [O III] luminosity\, confirming that J2240 is a quasar ionization echo. The ionized gas cloud has a strong kinematic link to the central AGN and i s co-rotating with the main body of the galaxy\, suggesting that it may be the remnant of a quasar-driven outflow. The extremely low space density o f GB galaxies suggests that they may be manifestations of normal but short -lived stages in the lives of quasar host galaxies. Detailed 3D spectrosco pic analysis of other GB galaxies will provide further insight into the ev olutionary history of this unique class of objects. LAST-MODIFIED:20141119T225620Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rebecca Davis (RSAA) "The Extended Emission Line Region of the "Gre en Bean" Galaxy SDSS J2240-0927: a quasar ionization echo illuminating the remnant of a quasar-driven outflow?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260304T000000Z DTEND:20260304T010000Z DTSTAMP:20261011T152430Z UID:m2humk7rrqlor7ivikkj8p0644@google.com CREATED:20260210T105611Z DESCRIPTION:Stars are the engines of the Universe\, recycling and distribut ing the elements that make up all matter. Stars also critically influence the planets that orbit them\; impacting their formation\, atmospheric comp osition\, and temperature. Yet\, despite the diagnostic power of radio emi ssion - which directly traces particle acceleration\, magnetospheric curr ents and probes stellar space weather environments - fewer than 1\,500 sta rs have been detected in the radio. Recent advances in the sensitivity\, b andwidth and survey speed of radio telescopes are transforming stellar rad io astronomy. My work on the Sydney Radio Star Catalogue has more than dou bled the number of known radio stars since the first version of the catalo gue released in late 2024. I will talk about the reinvigoration of the fie ld of stellar radio astronomy and discuss some of the key science question s I am addressing using the powerful ASKAP telescope. This includes stella r flares\, space weather\, and exoplanet habitability and magnetic fields. I will share my latest work on the Sydney Radio Star Catalogue and also l ook forward to the future of stellar radio astronomy with upcoming radio i nstruments. LAST-MODIFIED:20260225T090109Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Stu Wyithe) \nZoom: https: //anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Laura Driessen (U. Sydney) "Radio Stars: now and in the future (Str omlo Radio Fellow candidate talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260811T010000Z DTEND:20260811T020000Z DTSTAMP:20261011T152430Z UID:rgolrt0uchkk4e2bbufniuim30@google.com CREATED:20260722T060008Z DESCRIPTION:TBC LAST-MODIFIED:20260722T060009Z LOCATION:Zoom or Duffield Lecture Theatre (host: Katie Grasha) \nZoom: http s://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Janet Tang (RSAA) "TBC (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170428T040000Z DTEND:20170428T042000Z DTSTAMP:20261011T152429Z UID:k9ep55ou3h4h7f7lfp8o9ir6q4@google.com CREATED:20170426T052104Z DESCRIPTION:The Centre for Translational Data Science is a new entity at th e University of Sydney devoted to doing quantitative modeling of challengi ng problems in "narrative science" that don't have reductionistic theories \, thereby driving simultaneous progress in the respective domain areas an d in statistics or machine learning. I'll discuss my experiences at the C entre through the lens of two example problems I encountered: network lear ning in molecular biology\, and poll prediction in quantitative social sci ence. LAST-MODIFIED:20170427T235104Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Richard Scalzo (University of Sydney) "Lost in Translation: Model- Building For Fun And (Eventually\, With Luck) Profit" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161007T033000Z DTEND:20161007T035000Z DTSTAMP:20261011T152429Z UID:oir9kbvjv3jmhem1fku0oo3tmg@google.com CREATED:20160928T050106Z DESCRIPTION:TBD LAST-MODIFIED:20161005T050505Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Daniel Muthukrishna (University of Queensland) "Automated Spectral Classification of Transient Objects with Deep Learning" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220503T010000Z DTEND:20220503T020000Z DTSTAMP:20261011T152429Z UID:4llf3bpifo5js1pekivrs3ihko@google.com CREATED:20220201T005114Z DESCRIPTION:The existence of luminous quasars hosting supermassive black ho les within the first billion years of cosmic history challenges our unders tanding of black hole growth. An important piece of the puzzle is the life time of quasars - the time that galaxies shine as active quasars and durin g which the bulk of the black hole growth occurs - but to date its value r emains uncertain by several orders of magnitude. I will present a new meth od to obtain constraints on the lifetime of quasars based on the sizes of ionized regions around quasars known as proximity zones. These proximity z ones act as a quasar clock and enable us to study the co-evolution of supe rmassive black holes and their host galaxies from a new perspective. Surpr isingly\, our results indicate that black holes might be able to grow seve ral orders of magnitude faster than previously thought. I will show how fu ture observations with the upcoming James Webb Space Telescope will enable new insights into the early assembly of supermassive black holes and gala xy-quasar co-evolution across cosmic time. LAST-MODIFIED:20220427T002610Z LOCATION:DLT & ZOOM (host: Stefania) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anna-Christina Eilers (MIT\, USA) "Invited Colloquium: The Growth o f Supermassive Black Holes" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170721T043000Z DTEND:20170721T045000Z DTSTAMP:20261011T152429Z UID:fbti0c589soh7dtbcsuvp36h2k@google.com CREATED:20170710T014107Z DESCRIPTION:Annual thesis review. LAST-MODIFIED:20170720T042105Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dilyar Barat (RSAA) "Annual review: SAMI galaxy scaling relations a nd update on Taipan\, TLDR." TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241113T000000Z DTEND:20241113T010000Z DTSTAMP:20261011T152429Z UID:6ijjq0bgt6qkd4ed1blnrdnt14@google.com CREATED:20241108T052608Z DESCRIPTION:The future of extreme adaptive optics (exAO) lies in higher fid elity corrections at shorter wavelengths. While most AO systems operate at ~ kHz timescales\, earth atmosphere – especially as seen through visibl e light – moves faster\, driven by wind layers that blow an AO correctio n into history before it can be applied. However\, with predictive wavefro nt control\, linear algorithms can learn and predict where the atmosphere will be\, not only reducing atmospheric speckles in current observations\, but also opening up the sky to targets that would otherwise be too faint to be natural guidestars. Keck Observatory\, with two 10 meter segmented t elescopes\, is the largest facilitized AO-fed observatory\; Keck-AO not on ly improves current science but acts as a pathfinder for future ELTs. I wi ll discuss two projects in support of pushing Keck in the direction of exA O: work to implement predictive wavefront control at Keck-II and efforts t o unpack the current performance of Keck-II AO in the visible with the ORK ID instrument. LAST-MODIFIED:20241108T052608Z LOCATION:ZOOM only (host: N/A) \nZoom: https://anu.zoom.us/j/83410388355?pw d=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jules Fowler (University of California\, Santa Cruz) "A Keck-cophon y of speckles: supporting the next generation of Keck adaptive optics with predictive wavefront control and visible light AO" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170512T040000Z DTEND:20170512T042000Z DTSTAMP:20261011T152429Z UID:998du6ddjvi2r3qm3bus616fr4@google.com CREATED:20170501T063607Z DESCRIPTION:Have you heard of the Eurovision Song Contest? If not\, come to this talk and I'll give you a quick intro! I'll talk about some of the co ntroversies this year such as Ukraine vs. Russia\, Norway vs. the EBU and the UK's entry "I will never give up on you (EU)". If I've managed to conv ince you that Eurovision is awesome\, stick around that evening and watch the first semifinal (the one Australia is in) with myself and other enthus iasts and multicultural food! LAST-MODIFIED:20170508T092607Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rajika Kuruwita (ANU) "Eurovision 2017: Celebrate Diversity" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260821T040000Z DTEND:20260821T043000Z DTSTAMP:20261011T152430Z UID:g1b7f7p8irl2q0lm659rvvaqkg@google.com CREATED:20260816T220005Z DESCRIPTION:Circinus X-1 is an enigmatic accreting neutron star which defie s conventional classification despite decades of study. Surrounded by its natal supernova remnant\, aged at ~2900 years\, it is the youngest known X -ray binary (XRB). I will show that new radio observations of this system with MeerKAT\, combined with archival data from ATCA going back over 20 ye ars\, have allowed for unprecedented insight into the outflows in this sys tem. In particular the first observation of precessing jets from an accret ing neutron star\, the discovery of parsec scale jets from a neutron star XRB\, and the first observation of dynamic large scale structures in any X RB. These data allow for insights into a variety of different physics from accretion and jet launching\, to PeV particle acceleration and ultra-fast outflows. Finally\, I will highlight some more general recent results fro m the X-KAT program\, particularly focussing on systematically probing rad io polarisation in XRB jets for the first time. LAST-MODIFIED:20260817T000006Z LOCATION:Zoom or Duffield Lecture Theatre (host: Brian Schmidt) \nZoom: htt ps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Fraser Cowie (Oxford U.) "Dynamic shocks and precessing jets from a n enigmatic accreting neutron star" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190402T000000Z DTEND:20190402T010000Z DTSTAMP:20261011T152429Z UID:j6lv52nm9f14aqlsn9u8utkq6s@google.com CREATED:20190228T042618Z DESCRIPTION:Our spacecraft have taken us to visit and explore many stark an d ancient landscapes in the solar system. At first glance\, very little ap pears to have changed for billions of years\, but if we look to the atmosp here we see a dynamism that belies active processes in the present era and that hints at changes at and below the surface. In this talk\, we will pr oceed through these open doors to explore the movement of dust and ice in the hauntingly familiar environment of Mars. We will then travel further t o more exotic planetary destinations such as Pluto to see how the atmosphe re has sculpted the landscape into eerily familiar forms. LAST-MODIFIED:20190324T003607Z LOCATION:CSO Common Room (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:John Moores (York University) "Doors held ajar in storms: Insights into Atmospheric Planetary Science" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150410T042000Z DTEND:20150410T044000Z DTSTAMP:20261011T152430Z UID:1593gubecr9vsolo9tj3urko10@google.com CREATED:20150119T064122Z DESCRIPTION:The progenitor problem of Type Ia supernovae (SNe Ia) is still unsolved. Most of these events are thought to be explosions of Carbon-Oxyg en White Dwarfs\, but recent developments suggest that WDs with alternativ e compositions may contribute. But there is also the possibility of oxygen -neon white dwarf (ONe WD) or Carbon-Oxygen-Neon-hybrid white dwarf (CONe WD) progenitors in some of the explosion scenarios. I will present results from recent hydrodynamical simulations of explosions in Oxygen-Neon and ' hybrid' Carbon-Oxygen-Neon WDs. I will present synthetic light curves and spectra of the explosions and show that detonations in ONe WDs would produ ce relatively normal SN Ia and deflagrations in the 'hybrid' models likely explain the faint subclass of Type Iax supernovae. LAST-MODIFIED:20150331T232607Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kai Marquardt (Uni Wuerzburg) "Type Ia Supernovae from exploding (C arbon-)Oxygen-Neon White Dwarfs" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240530T010000Z DTEND:20240530T020000Z DTSTAMP:20261011T152429Z UID:0o7qk0lp0bi3cpbvdsbt7hp9u4@google.com CREATED:20240415T051622Z DESCRIPTION:Annual review talks by students LAST-MODIFIED:20240415T051622Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Emily Wisnioski) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA student annual review talks (RSAA) "Student review talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151127T030000Z DTEND:20151127T032000Z DTSTAMP:20261011T152429Z UID:c7sbie76psbii51g71moi72km4@google.com CREATED:20151007T033617Z DESCRIPTION:The Zooniverse has created an online interface\, Panoplies\, wh ere you can develop your own visualisation portal that can be made public or private. In this talk I will discuss some of the ways you can utilise this online system for your own research even if you know nothing about we b design. LAST-MODIFIED:20151123T041106Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Julie Banfield (RSAA) "Panoptes: an online interface for visualisat ion of data" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260224T000000Z DTEND:20260224T010000Z DTSTAMP:20261011T152430Z UID:svf02ubq1a1fcipr0gdqd02r24@google.com CREATED:20251203T021612Z DESCRIPTION:An omnipresent feature of the "cosmic web" -- the large-scale f ilamentary backbone of the Universe -- is represented by a warm/hot gas c omponent. This is a dominant component in the overall matter budget on a m ulti-scale realm spanning from Mpc-scale intergalactic filaments\, to the intracluster medium (ICM) and the circumgalactic medium (CGM) surrounding individual galaxies. Therefore\, the study of the warm/hot gas represents a powerful means for tracing the matter assembly in the Universe\, its the rmal history\, and the intertwined evolution of galaxies and their large-s cale environment. In my talk\, I will discuss how state-of-the-art and fut ure radio-to-submillimeter facilities like the Atacama Large Millimeter/Su bmillimeter Array\, the Square Kilometer Array\, and\, ultimately\, the At acama Large Aperture Submillimeter Telescope can revolutionize our perspec tive on the hot and ionized Universe via the possibility of tracing the mu lti-faceted Sunyaev-Zeldovich (SZ) effect -- a distinct spectral signature imprinted in the ubiquitous cosmic microwave background by the warm/hot g as within cosmic structures. LAST-MODIFIED:20260215T224107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Melanie Kaasinen) \nZoom: https://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Luca di Mascolo (U. Groningen) "A resolved SZ view of the hot Unive rse" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221031T221500Z DTEND:20221101T033000Z DTSTAMP:20261011T152429Z UID:js030471hm0qg60gd955u47sr0@google.com CREATED:20220926T013812Z DESCRIPTION:Welcome (9:15)\, 4 Honours talks (9:20 - 11:00)\, tea break (11 :00 - 11:15)\, 3 Honours talks (11:15-12:30)\, lunch break (12:30 - 13:00) \, 2 Honours talks (13:00 - 13:50)\, 1 longer Master talk (13:50-14:30) LAST-MODIFIED:20220926T013812Z LOCATION:DLT & ZOOM (host: Christian Wolf) \nZoom: https://anu.zoom.us/j/99 785341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA Honours/Masters Students (RSAA) "RSAA Hons and Masters thesis talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160602T010000Z DTEND:20160602T020000Z DTSTAMP:20261011T152429Z UID:itca07nlgipjikqqhqtp8lj194@google.com CREATED:20151214T010115Z DESCRIPTION:Protoplanetary disks are the birth cradles of planets\, but the planet formation process is still not well understood. Of particular inte rest are the so-called transitional disks: disks with large inner cavities . In recent years\, ALMA has revealed that gas and dust show different str uctures in these disks. Most remarkable is the discovery of strong asymmet ries in the dust continuum emission in some of these disks\, whereas the g as shows a full Keplerian disk. These asymmetries can be interpreted as du st traps\, places where dust particles concentrate and grow. Multi wavelen gth observations confirm an increase in dust growth in the center of these dust traps. On the other hand\, the gas distribution as mapped by high sp atial resolution CO observations reveals gas cavities at smaller radii tha n their dust counterparts\, hinting at the presence of already formed Jupi ter-like planets. This phenomenon turns out to be common in transition dis ks with large cavities in various studies. In this talk I will discuss the new structures found with ALMA and their implications for our understandi ng of planet formation. LAST-MODIFIED:20160525T032106Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Nienke van der Marel (Institute for Astrophysics\, Hawaii Universit y) "Planet formation in the ALMA era: gas and dust in protoplanetary disks " TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160701T043000Z DTEND:20160701T045000Z DTSTAMP:20261011T152429Z UID:l8i3ifqqhaer06hjvh5q4n7c60@google.com CREATED:20160610T060109Z DESCRIPTION:In Earth orbit\, over 250 objects to date have exploded\, colli ded with other objects or have broken up due to malfunctions or for unknow n reasons. Such 'breakups' are especially critical whenever they occur in highly utilized regions such as near 800 km altitude\, where most Earth ob servation satellites reside or in the GEO region near 36000 km altitude wh ich is heavily utilized by telecommunications satellites. Collision veloci ties on the order of 10 km/s are typically encountered in low Earth orbits \; at these velocities even small pieces of debris can cause a satellite's mission to end instantly. Because atmospheric drag decreases roughly expo nentially\, debris at 800 km altitude may remain on orbit for decades or e ven centuries and so can collide with other objects many years in the futu re with potentially catastrophic consequences. Long-term simulations show that the collision cascading\, also known as the ”Kessler Syndrome”\, will become a dominant source for debris. Large\, massive objects are the driver within this process as a complete breakup will create many more fra gments which in turn can trigger catastrophic collisions. In February 2016 \, the X-ray Astronomy Satellite “Hitomi”\, also known as ASTRO-H was launched with a multitude of scientific payloads to examine the universe. Not even two months into its mission\, the spacecraft suffered an anomaly in which several large pieces including the solar panels and scientific bo om separated from the main body - the cause: a mixture of machine and huma n error. Although Hitomi’s orbit was below the critical 800 km altitude\ , it was neighbour to some other significant satellites whose demise would be hard felt. The talk explores details of the breakup and investigates t he potential risk which the fragments may pose to active spacecraft in the ir vicinity and to the Kessler Syndrome. LAST-MODIFIED:20160624T125108Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sven Flegel (SERC) "Analysis of the ASTRO-H breakup and its impact on the collision risk of intact objects" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141211T000000Z DTEND:20141211T010000Z DTSTAMP:20261011T152430Z UID:4oao7feabnkd9rnuhqng3pg5qs@google.com CREATED:20141117T060341Z DESCRIPTION:In accreting binary neutron star systems matter is channelled b y the strong magnetic field to the poles of the neutron star. The accreted matter accumulates at the poles to form accretion mounds. Pressure from t he confined matter can significantly distort the local magnetic field stru cture\, affecting the X-ray observations and long term evolution of the ma gnetic field. I will present our recent results on modelling such accretio n mounds and MHD simulations performed to study the presence of MHD instab ilities in such systems. I will discuss how such instabilities may affect the evolution of the local magnetic field and leave its imprint on X-ray o bservations in the form of cyclotron resonance scattering features. LAST-MODIFIED:20250925T231026Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) \nZoom: https://anu.zoo m.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dipanjan Mukherjee (RSAA) "Accretion on neutron stars: effects on m agnetic field evolution and X-ray observations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220317T000000Z DTEND:20220317T010000Z DTSTAMP:20261011T152429Z UID:3mn1udv4h8dglbb4ns2eeag32k@google.com CREATED:20220105T010606Z DESCRIPTION:A broader concept of 'resistance to acceleration' than used in classical dynamics\, called 'inertial resistance'\, is needed in Special R elativity. It will be shown that inertial resistance is more than particl e inertia and originates from Minkowski spacetime structure. Current mains tream explanations of inertia do not take inertial resistance into account and are\, therefore\, incomplete. LAST-MODIFIED:20220308T132109Z LOCATION:ONLY DLT (host: Shyam Menon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Peter Riggs (RS Physics\, ANU) "Inertia and Inertial Resistance in Special Relativity" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241008T000000Z DTEND:20241008T010000Z DTSTAMP:20261011T152429Z UID:kpl146jhnocqu0bkitrp219vms@google.com CREATED:20240501T002158Z DESCRIPTION:We demonstrate the importance of radio selection in probing hea vily obscured galaxy populations. Using Evolutionary Map of the Universe ( EMU) Early Science data in the Galaxy and Mass Assembly (GAMA) G23 field t ogether with GAMA and Wide-field Infrared Survey Explorer (WISE) data\, we demonstrate that the radio detected population has on average higher leve ls of obscuration than the parent optical sample. This arises through miss ing the lowest Balmer decrement (BD) and lowest mass galaxies\, which are also the lower star formation rate (SFR) and metallicity systems. Possible explanations include speculation around steeper stellar initial mass func tions in low mass\, low SFR galaxies. We further investigate the link betw een dust obscuration and SFR estimators using Halpha luminosities and radi o luminosities. We explore this by drawing on dust estimates using both th e BD and the dust mass\, demonstrating systematic underlying dependencies with the radio-to-Halpha ratio. Defining two novel dust geometry metrics b y combining the BD and dust mass\, we confirm their utility as a way to qu antify dust geometry. We use this approach to establish an improved estima tor for the Halpha SFR that accounts for optically thick dust. We also est ablish a strong correlation between specific SFR and the dust opacity and geometry in galaxies. Additionally\, we present a tool designed to model c urrent astronomical fibre positioning systems. Through a systematic analys is of both observational and instrumentation parameter spaces\, we evaluat e fibre allocation efficiency across multiple visits. This analysis provid es valuable insights for designing next-generation multi-object spectrosco py instrumentation for future telescopes. LAST-MODIFIED:20240923T012215Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Maya Jablonska) \nZoom: ht tps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tania Ahmed (Macquarie U.) "Dust obscuration\, and star formation r ate in galaxies: insights and key technologies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160630T010000Z DTEND:20160630T020000Z DTSTAMP:20261011T152430Z UID:mg32mt0b97afh2ho3sqd3ed2ag@google.com CREATED:20160614T060107Z DESCRIPTION:Metal absorption lines along the line of sight to distant quasa rs provide an unbiased census of the metal enrichment and ionisation histo ry of the Universe. We present a search and consistent analysis for MgII a bsorption systems in the foreground of 4 high redshift (z ∼ 6) quasar sp ectra obtained with the ESO Very Large Telescope X-shooter. The medium res olution and high sensitivity allow us to measure\, for the first time\, th e evolution of the comoving mass density\, Omega(MgII)\, from z = 2 to 5.5 \, approaching the end of the Epoch of Reionisation. LAST-MODIFIED:20160614T060107Z LOCATION:Duffield Lecture Theatre (host: Helga Denes) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alex Codoreanu (Swinbourne University) "racking Magnesium across 10 billion years: the comoving mass density of MgII from redshift 2 to 5.5" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180621T010000Z DTEND:20180621T020000Z DTSTAMP:20261011T152429Z UID:k9bmei3t34sin81f3m344pqlrc@google.com CREATED:20180503T001623Z DESCRIPTION:Powerful radio-galaxies feature heavily in our understanding of galaxy evolution. However\, when it comes to studying their properties as a function of redshift and/or environment\, the most-detailed studies ten d to be limited by small-number statistics. In this talk\, I will present a new sample of nearly 2\,000 of the brightest radio-sources in the southe rn hemisphere (Dec. < 30 deg). These were observed at low radio-frequencie s as part of the GaLactic and Extragalactic All-sky MWA (GLEAM) survey\, c onducted using the Murchison Widefield Array (MWA). Being brighter than 4 Jy at 151 MHz\, we refer to these objects as "The GLEAM 4-Jy Sample". Than ks to the location of the MWA in a protected\, radio-quiet zone\, we have excellent spectral coverage for these sources\, with 20 radio flux-densiti es spanning a frequency range of 72-231 MHz. A key component of this proje ct is identifying the appropriate host galaxy of the radio emission\, with these positions feeding into target lists for the Taipan Galaxy Survey. H aving 10 times as many sources as the most-prominent\, low-frequency radio -source sample that is optically complete (the revised Third Cambridge Cat alogue of Radio Sources\; 3CRR)\, the GLEAM 4-Jy Sample will allow models of powerful active galactic nuclei to be tested more robustly. LAST-MODIFIED:20180613T042107Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sarah White (ICRAR) "The most powerful radio-sources in the souther n hemisphere" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230616T040000Z DTEND:20230616T050000Z DTSTAMP:20261011T152429Z UID:heh5uiq64pqlk0c76d25sjabm4@google.com CREATED:20230615T002608Z DESCRIPTION:The Einstein-First project addresses the need to introduce Eins teinian concepts to students at an early age by developing tangible and ta ctile tools\, such as models and analogies. These innovative teaching aids bridge the gap between complex theoretical concepts and students' everyda y experiences\, fostering their interest and understanding of Einsteinian science. In this talk\, I will share my 10-year journey of teaching Einste inian concepts to primary and high school students\, highlighting the impa ct on their understanding and how girls' attitudes have changed towards le arning physics. While the project has been running successfully in Western Australia\, our goal is to extend its reach to all 9\,500 schools across Australia. Additionally\, I will discuss our newly funded project called " Quantum Girls\," which aims to improve female students' attitudes towards Quantum science. To achieve our objective\, two projects were launched nat ionally in Canberra on 13th June. LAST-MODIFIED:20230615T002608Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Bailey) \nZoom: https://an u.zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jyoti Kaur (UWA) "Introducing Einsteinian Concepts to Students: The Einstein-First Project" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150313T030000Z DTEND:20150313T032000Z DTSTAMP:20261011T152429Z UID:ple0hefdmobccfmnrui9l5g8e8@google.com CREATED:20150119T064116Z DESCRIPTION:Accurate flux calibration is required to derive to many intrins ic properties of the galaxy like star formation rate. It is also required to compare the data from different instruments. In this FoF I will summari se some of the issues (and hopefully their solutions) encountered while fl ux calibrating data from DEIMOS spectrograph on KECK. LAST-MODIFIED:20150313T003104Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anshu Gupta (RSAA) "Flux Calibration of DEIMOS-KECK data" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141128T030000Z DTEND:20141128T032000Z DTSTAMP:20261011T152429Z UID:929dde96b8r77n9okpfklvbv1g@google.com CREATED:20141117T060339Z DESCRIPTION:I revisit the Cepheid-distance determination to the nearby spir al galaxy M101 (Pinwheel Galaxy)\, in light of several recent investigatio ns questioning the shape of the interstellar extinction curve. I find that the (steeper) extinction curve of Fitzpatrick & Massa (2007) is slightly favoured relative to the vastly more cited curve of Cardelli et al. (1989) \, and this consequently increases the inferred distance modulus by ~0.06 mag. I also briefly discuss an undiagnosed and possibly significant system atic error I noticed while perusing the literature\, that the assumptions of metallicity-dependence in the literature may be invalid. LAST-MODIFIED:20141124T042338Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:David Nataf (RSAA) "Uncertainties in the Interstellar Extinction an d the Cepheid Distance to M101" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180208T000000Z DTEND:20180208T010000Z DTSTAMP:20261011T152429Z UID:qhfbgj8gh3lvshcu8s64vmgirs@google.com CREATED:20171221T005107Z DESCRIPTION:The Earth is considered to be a devolatilized piece of the sola r nebula. Similarly\, rocky exoplanets are most likely devolatilized piece s of the stellar nebulae out of which they and their host stars formed. If this is correct\, we can estimate the chemical composition of rocky exopl anets by applying a devolatilization algorithm to the elemental abundances of their host stars. My PhD thesis was an investigation of this potential ly universal devolatilization pattern\, and is now being wrapped up with t he following four major outcomes: i) the estimates of the bulk elemental a bundances (with uncertainties) of the Earth by calibrating a variety of Ea rth observations and models\; ii) the estimates of protosolar elemental ab undances based on an improved combination of solar photospheric abundances and CI chondritic abundances\; iii) quantification of the devolatilizatio n pattern from the solar nebula to Earth by using the Earth-to-Sun abundan ces ratios as a function of elemental condensation temperatures\; iv) appl ication of the devolatilization algorithm to other planetary systems to es timate the bulk elemental composition of habitable-zone rocky exoplanets\, and then to explore the interior composition and structure of such exopla nets and analyze their habitability. We mainly conclude that i) the Sun-to -Earth devolatilization pattern can be used as a first-order fiducial mode l of chemical relationships between rocky planets and their host stars\, w hich provides a principal constraint to enhance the current studies of exo planetary chemistry\; ii) the interior composition and structure of terres trial exoplanets orbiting different stars can be distinguished between eac h other\, by using the current high-precision estimates of host stellar ab undances (with a typical uncertainty less than 0.04 dex). LAST-MODIFIED:20180131T001608Z LOCATION:Duffield Lecture Theatre (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Haiyang Wang (RSAA) "Devolatilization during the Formation of Rocky Planets: Bulk Elemental Composition and Habitability (End-of-Thesis Collo quium)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170511T010000Z DTEND:20170511T020000Z DTSTAMP:20261011T152429Z UID:p7bp3mlefu7a40e44ri98ref9g@google.com CREATED:20170320T052108Z DESCRIPTION:We present the E-MOSAICS project (MOdelling Star cluster system Assembly In Cosmological Simulations in the context of EAGLE): a suite of cosmological\, hydrodynamical simulations run with the EAGLE model that i ncludes a semi-analytic model for star cluster formation and disruption. T his is the first work to self-consistently model the formation and evoluti on of star clusters through cosmic history in fully cosmological\, hydrody namical simulations of galaxy formation. The project includes zoom simulat ions of Milky Way-like analogues\, galaxy groups and massive galaxy cluste rs. We will show how globular cluster and young massive cluster population s can form through the same mechanisms and how globular cluster population properties relate to the formation histories of their host galaxy. LAST-MODIFIED:20170504T012109Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Joel Pfeffer (Liverpool John Moores University) "The E-MOSAICS proj ect: simulating the formation and evolution of galaxies and their globular cluster systems across full cosmic history" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220412T233000Z DTEND:20220413T003000Z DTSTAMP:20261011T152429Z UID:d90oiohhlrj2n5tjl2ttqr6ndk@google.com CREATED:20220405T002110Z DESCRIPTION:Observations of large scale 21cm emission from Hydrogen in the early Universe is an emerging technique on the cusp of a major breakthroug h. Once realized\, 21cm cosmology will transform our understanding of how the first stars\, galaxies\, and black holes formed\, reionized the Univer se\, and set the stage for the sources we observe at later times. As an ex quisite probe of large scale structure\, 21cm also promises to shed light on fundamental physics including dark energy. Vastly brighter foreground e mission and spectral variations in the bandpasses of radio telescopes toge ther pose formidable obstacles to the realization of 21cm science. I will overview recent advances I've developed in systematics mitigation that are enabling the best upper limits in the field and even a first detection at lower redshifts\, focusing on my work on SKA precursors including the Mur chison Widefield Array and the Hydrogen Epoch of Reionization Array. I wil l finish by outlining the analysis and instrumentation directions that I t hink will enable the next major sensitivity improvements. LAST-MODIFIED:20220411T012209Z LOCATION:DLT & ZOOM (host: Jackie) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Aaron Ewall-Wice (Berkeley Radio Astronomy Lab and Center for Cosmo logical Physics) "Invited Colloquium: Chasing the Cosmic Dawn with Novel R adio Telescopes" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200130T000000Z DTEND:20200130T010000Z DTSTAMP:20261011T152429Z UID:sn7ivamlkilrb992ojqthi324k@google.com CREATED:20191119T105611Z DESCRIPTION:Stars are fossils that retain the history of their host galaxie s. At the end of their lives\, some explode as supernovae\, producing heav y elements that are distributed into the surrounding interstellar gas. New stars that are created from this gas contain the elements that were produ ced from the previous generations of stars. From the spatial distribution of elements\, it is therefore possible to constrain the star formation and chemical enrichment histories of the galaxies. This approach\, Galactic A rchaeology\, has been popularly used for our Milky Way Galaxy. It can also be applied to external galaxies thanks to the recent and future observati ons with integral field units (extra-galactic archaeology). My team has be en running hydrodynamical simulations from cosmological initial conditions including detailed chemical enrichment. By comparing with observations\, I will discuss the role of metal flows\, i.e.\, gas infall\, outflow\, rad ial flow\, and stellar migration\, in the evolution of Milky Way Galaxy an d galaxies in general. LAST-MODIFIED:20200129T231605Z LOCATION:Duffield Lecture Theatre (host: Monty) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Chiaki Kobayashi (University of Hertfordshire) "Metal flows in simu lated galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251113T000000Z DTEND:20251113T010000Z DTSTAMP:20261011T152430Z UID:v0v1vq4rhd6llgsatasjo51eg8@google.com CREATED:20251109T225606Z DESCRIPTION:Astronomers used to worry that there would not be a supercomput er big enough to process data from the SKA. But high performance computin g has continued to grow exponentially\, and today there are multiple comme rcial providers who operate computers larger than the ngVLA & SKA requirem ents. We are already on the way to having a cheap and plentiful source of HPC for radio astronomy. But can we as radio astronomers take advantage o f this resource? How easy or hard is it to use a 'bare metal' provider lik e DUG or a 'commercial cloud' provider like Amazon? Over the last four yea rs I've been finding out via a set of research projects involving heavy da ta processing at commercial providers. In this talk I'll cover my FRB sear ch using the MWA telescope\, and high spatial & frequency resolution imagi ng of HI gas in the Magellanic Clouds using ASKAP. I also got to experien ce the world of social science by collecting and analysing other researche rs' experiences with commercial supercomputing. In this talk I will summar ise the good and bad of commercial HPC\, and give you some tips on the dif ficult decision about how much effort to put in to optimising your code. LAST-MODIFIED:20251109T235107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hiep Nguyen) \nZoom: https ://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ian Kemp (ICRAR/Curtin U.) "The application of commercial supercomp uting to next-generation radio astronomy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220421T010000Z DTEND:20220421T020000Z DTSTAMP:20261011T152429Z UID:mq57g9oc0e08ponvjt2j48jbo8@google.com CREATED:20220411T012214Z DESCRIPTION:The intracluster medium (ICM) pervades the dark matter halo of galaxy clusters and is intimately linked to the evolution of the member ga laxies through the cosmic baryon cycle. Jets driven by active galactic nuc lei (AGNs)\, sloshing by passage of galaxies during infall and mergers can drive turbulence in the ICM. Turbulence plays an important role in cluste r thermodynamics through turbulent heating and turbulent mixing and can pr event runaway cooling in cool cores. On larger scales\, it affects cluster mass measurements by providing non-thermal pressure support to the gas\, causing gas profiles to deviate from hydrostatic equilibrium. However\, cu rrent X-ray observations lack the spectral resolution to directly measure turbulent velocities in the hot ICM. The different indirect observational methods of measuring turbulence include X-ray brightness fluctuations\, th ermal Sunyaev Zeldovich effect (tSZ) fluctuations and velocity measurement s of cold (10^4 K) Halpha emitting filaments using integral field unit spe ctroscopy (IFU). Using our idealised simulations\, we have studied the eff ects of the gas density stratification\, amount of turbulent heating and t he method of driving (incompressible vs compressible) on different statist ical properties of the ICM gas\, such as its temperature and density distr ibution\, velocities of hot (10^7 K gas) and cold (10^4 K) phases\, etc. W e use our results to constrain the different indirect observational techni ques for measuring turbulent velocities\, such as X-ray brightness fluctua tions\, thermal Sunyaev-Zeldovich effect fluctuations\, which are dependen t on the density and pressure fluctuations\, respectively. We also correla te between the velocities of hot (10^7 K gas) and cold (10^4 K) phases whi ch would let us recover hot phase velocities from IFU observations of the cold phase. LAST-MODIFIED:20220411T013614Z LOCATION:DLT & ZOOM (host: Shyam Menon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rajsekhar Mohapatra (RSAA) "PhD Thesis Talk: The role of stratifica tion\, turbulence and cooling in the intracluster medium" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190118T032000Z DTEND:20190118T034000Z DTSTAMP:20261011T152429Z UID:m2nb21d4fuilcp97lh9rhagqq8@google.com CREATED:20181204T050609Z DESCRIPTION:In this talk I'll give an update on my current research\, say f arewell after three years at RSAA and chat about the challenges of writing an open source code. So if you are wondering what happened with the SkyMa pper Transient Survey\, machine learning applications to astronomy and ope n-sourcing your code\, come by. LAST-MODIFIED:20190115T235105Z LOCATION:CSO Common Room (host: Monty) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anais Moller (RSAA) "Supernovae\, SuperNNova and writing an open so urce code" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20211014T000000Z DTEND:20211014T003000Z DTSTAMP:20261011T152429Z UID:i6uorcv2i876pkemboqualedr0@google.com CREATED:20210917T001612Z DESCRIPTION:The Galactic disk exhibits complex chemical and dynamical subst ructure thought to be induced by the bar\, spiral arms\, and satellites. In this talk\, I will explore the chemical signatures of bar resonances in action and velocity space and characterize the differences between the si gnatures of corotation and higher-order resonances using test particle sim ulations. Thanks to recent surveys\, we now have large homogeneous dataset s containing metallicities and kinematics of stars outside the solar neigh borhood. We compare the simulations to the observational data from Gaia\, LAMOST\, and APOGEE and find weak evidence for a slow bar that associates the ''hat'' moving group with its outer Lindblad resonance and ''Hercules' ' with corotation. While constraints from current data are limited by thei r spatial footprint\, stars closer in azimuth than the Sun to the bar's mi nor axis show much stronger signatures of the bar's outer Lindblad and cor otation resonances in test particle simulations. Future datasets with gre ater azimuthal coverage\, including the final Gaia data release\, will all ow reliable chemodynamical identification of bar resonances. I will also b riefly discuss Korg\, my from-scratch 1D LTE spectral synthesis code. LAST-MODIFIED:20211006T230607Z LOCATION:ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Adam J. Wheeler (Columbia University\, USA) "Chemodynamical signatu res of bar resonances in the Galactic disk: current data and future prosp ects" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260303T000000Z DTEND:20260303T010000Z DTSTAMP:20261011T152430Z UID:upji7vpeqvnib4pgdg7qtenoqs@google.com CREATED:20251203T021613Z DESCRIPTION:Light carries a vast amount of information about the world arou nd us\, but most of it remains invisible to our eyes. This information is contained in the light's polarisation\, phase\, momentum\, and frequency r ange beyond the visible spectrum. Metasurfaces\, arrays of subwavelength r esonant nanostructures\, offer unique opportunities to visualise this hidd en information by enabling smart and precise measurements of these propert ies. Prominent examples include polarisation imaging\, which can remove sp ecular reflections or edge-detection that can improve object recognition f or autonomous vehicles. This presentation will explain the underlying prin ciples for the detection of such hidden properties of light and demonstrat e new applications in astronomical and satellite imaging. These include hy perspectral and polarisation imaging\, as well as in aberration correction for large telescope adaptive optics. We will further show how metasurface s can enhance the conversion of infrared light to visible\, enabling compa ct and low-noise infrared imaging. Finally\, we'll demonstrate how such no nlinear up-conversion can offer unique opportunities for all-optical image processing and advanced image processing for object recognition applicati ons. LAST-MODIFIED:20260226T003608Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dragomir Neshev (ANU Research School of Physics) "Smart imaging ena bled by meta-optics" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190205T000000Z DTEND:20190205T010000Z DTSTAMP:20261011T152429Z UID:e9shh7b7palifgar0nlujhk44c@google.com CREATED:20181013T132614Z DESCRIPTION:Acceleration at relativistic shocks is likely to be important i n various astrophysical jet sources\, including blazars and other radio-lo ud active galaxies. Recent work on combining multi-wavelength (MW) lepton ic emission models with complete simulated distributions from shock accele ration theory has resulted in new insights into plasma conditions in blaza rs. This has demonstrated the ability to infer the cyclotron frequency\, t he plasma density and thus also the Alfven speed\, thereby determining the rapidity of particle energization. An important inference was that turbu lence levels decline with remoteness from jet shocks\, assessed for blazar s such as Mrk 501 and Bl Lac. In this talk\, an overview of the MW modelin g that yielded these insights is presented\, including a recent extension to a two-zone\, time-evolving construction. In this development\, both ext ended\, enhanced emission states from larger radiative regions\, and promp t flare events from compact acceleration zones proximate to shocks are tre ated. An application to the LBL blazar 3C 279 is addressed: as the acceler ation first proceeds and then abates\, the radiative simulations obtain sp ectral hysteresis in the hardness-flux diagram in all wavebands. Distinct ive temporal correlations and lags between radio and optical/gamma-ray ban ds are identified\, yielding potential observational diagnostics. LAST-MODIFIED:20190131T044606Z LOCATION:CSO Common Room (host: Pingel) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Matthew Baring (Rice University) "A Time Evolution Picture of Multi -wavelength Flares in Blazars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230309T000000Z DTEND:20230309T010000Z DTSTAMP:20261011T152429Z UID:ho35898osl47rg5pjfs7u3tpeo@google.com CREATED:20230305T084206Z DESCRIPTION:Given the low ionization fraction of molecular clouds\, ambipol ar diffusion is thought to be an integral process in star formation. Howev er\, chemical and radiative-transfer effects\, observational challenges\, and the fact that the ion-neutral drift velocity is inherently very small render a definite detection of ambipolar diffusion extremely non-trivial. I studied the ion-neutral drift velocity in a suite of chemodynamical\, no n-ideal magnetohydrodynamic (MHD)\, 2-dimensional axisymmetric simulations of prestellar cores where I altered the temperature\, cosmic-ray ionizati on rate\, visual extinction\, mass-to-flux ratio and chemical evolution. S ubsequently\, I performed a number of non-local thermodynamic equilibrium (non-LTE) radiative-transfer calculations considering various idealized an d non-idealized scenarios in order to assess which factor (chemistry\, rad iative transfer and/or observational difficulties) is the most challenging to overcome in our efforts to detect the ion-neutral drift velocity. I fo und that temperature has a significant effect in the amplitude of the drif t velocity with the coldest modeled cores (T = 6 K) exhibiting drift veloc ities comparable to the sound speed. Against all odds\, I found that\, in idealized scenarios (where two species are perfectly chemically co-evolvin g) the drift velocity "survives" radiative-transfer effects and can be obs erved. However\, I found that observational challenges and chemical effect s can significantly hinder our view of the ion-neutral drift velocity. Spe cifically\, I found that the pairs of HCN and HCO+\, and NH3 and N2H+\, pr eviously used in observational studies of ambipolar diffusion\, exhibit si gnificantly different abundance distributions within the modeled clouds an d are thus not suitable for probing the ion-neutral drift velocity. Finall y\, I propose that HCN and HCNH+\, being chemically co-evolving\, could be used in future observational studies aiming to measure the ion-neutral dr ift velocity. LAST-MODIFIED:20230305T084206Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Lindsey Oberhelman) \nZoom : https://anu.zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Aris Tritsis (Western Science) "Can we observe the ion-neutral drif t velocity in molecular clouds?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150619T040000Z DTEND:20150619T042000Z DTSTAMP:20261011T152429Z UID:kp6afg9jobu5fd89d5uscsb15k@google.com CREATED:20150515T064609Z DESCRIPTION:The detection of exoplanets using Radial Velocity (RV) measurem ents is commonly limited by the temperature and pressure stability of spec trographs and efficient fibre scrambling. Additionally\, noise from stella r activity is becoming increasingly important\, particularly in giant star s\, where the amplitude of pulsations is comparable to RV signals from hot -Jupiters. Thus\, long-baseline RV measurements are required to measure th e intrinsic pulsations of the host star and de-correlate them to search fo r the planetary signals. This is impractical using large telescopes\, but possible to do on bright stars with 0.2-0.4m class telescopes\, provided t hey can be fitted with cheap high-resolution spectrographs. In this talk I will report on the current status of development of the RHEA spectrograph \, an inexpensive compact single-mode fibre-fed spectrograph being develop ed at Macquarie University and ANU currently serving as the basis for a se ries of spectrographs to be deployed on other amateur sized telescopes for exoplanet and asteroseismological studies. LAST-MODIFIED:20150622T074542Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Joao Bento (RSAA) "Update on the status of the RHEA spectrograph" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201202T234500Z DTEND:20201203T003000Z DTSTAMP:20261011T152429Z UID:0di2oacn7565lstjmvhvg5qgt0@google.com CREATED:20200916T103123Z DESCRIPTION:Delta Scuti stars are pulsating A- and F-type stars which\, in principle have their internal structure and parameters including age\, asc ertained by their pulsation modes. Despite the vast amount of photometric data from space-based probes\, observations are often still not matched wi th theoretical models. It remains uncertain if there are significant miss ing physics in the models\, or if the observations are insufficient or ina ccurate to explain these stellar objects. Two factors significantly contr ibute to this failure: accurate rotation rates and densities of the delta Sct stars. Both these parameters can be determined if the delta Sct star is a component of a binary system as I illustrate by the binaries\, TT Hor and RZ Mic. Successful mode identification in both delta Sct components required higher than solar metallicity for evolutionary models suggesting some short comings in this procedure. In the future\, the combination of t he mode spectrum\, Gaia distance and projected rotational velocity\, may e nable the application of work in this thesis to single stars. LAST-MODIFIED:20201203T000106Z LOCATION:DLT and ZOOM 997 8534 1005 (host: Seta) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Margaret Streamer (RSAA) "End-of-Thesis Talk: Delta Scuti stars in Binary Systems" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220610T040000Z DTEND:20220610T050000Z DTSTAMP:20261011T152429Z UID:ar15mm3gsulna10dj2h0occ20k@google.com CREATED:20220525T060110Z DESCRIPTION:TBD LAST-MODIFIED:20220602T042608Z LOCATION:DLT & ZOOM (host: Mike Ireland) \nZoom: https://anu.zoom.us/j/9978 5341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Honours students (RSAA) "RSAA Honours student talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150423T010000Z DTEND:20150423T020000Z DTSTAMP:20261011T152429Z UID:itgkkjq57t7g0qd1l0r2iqvteo@google.com CREATED:20150415T055606Z DESCRIPTION:The environment of a galaxy can play a major role in its evolut ion. Late-type gas-rich galaxies can be transformed into gas-poor early-ty pe galaxies in dense environments. Observations show that spiral galaxies in galaxy cluster tend to have on average less neutral hydrogen (HI) than galaxies of the same type and size in the field. Recently there is accumul ating evidence that HI-deficient galaxies are also relatively frequent in galaxy groups and that galaxy transformation can already start in the grou p environment. In this talk I will investigate how the environment influen ces the HI content of galaxies\, and which mechanisms are responsible for the gas deficiency in galaxy groups? LAST-MODIFIED:20150420T035104Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Helga Denes (RSAA) "A wide-field investigation into the HI content of galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250214T030000Z DTEND:20250214T040000Z DTSTAMP:20261011T152429Z UID:2ej6h90e9ngb19pg0e07v6ebt0@google.com CREATED:20250212T113606Z DESCRIPTION:A presentation of the exposure draft of the 2025 Decadal Plan\, with opportunities for feedback. LAST-MODIFIED:20250212T113606Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Stu Wyithe) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Virginia Kilborn (National Committee for Astronomy / Swinburne U.) "Decadal Plan Roadshow" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160513T040000Z DTEND:20160513T042000Z DTSTAMP:20261011T152430Z UID:o9gea5mjsddh35fjcu1j31lrgk@google.com CREATED:20160503T034607Z DESCRIPTION:A recent discovery from Radio Galaxy Zoo are “green double ra dio sources associated with a galactic nuclei (DRAGNs)”.These unique gal axies live between 0.2 < z < 0.3 with large [OIII] emission lines making t hese galaxies appear “green”. Recent observations with WiFeS have sho wn that these galaxies have a complex structure with high velocities (+/- 400 km/s) and high star formation rates (~1 star mass per year). AND they host luminous radio-loud AGN. Observational evidence illustrates the poss ibility of jet induced star formation. In this talk I will produce this e vidence. LAST-MODIFIED:20160503T034607Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Julie Banfield (RSAA) "The hunt for green DRAGNs" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231124T030000Z DTEND:20231124T040000Z DTSTAMP:20261011T152430Z UID:r4efuccfde0hlfv63sqkedteik@google.com CREATED:20230926T234113Z DESCRIPTION:TBC LAST-MODIFIED:20231004T013612Z LOCATION:Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.zoom.us/j /83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Chris Lidman (RSAA) "SSO Town Hall Meeting" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240206T000000Z DTEND:20240206T013000Z DTSTAMP:20261011T152429Z UID:lu3s9ci4k0vr88g482h4qgpdi0@google.com CREATED:20231212T003611Z DESCRIPTION:A neutron star binary merges somewhere in the Universe approxim ately every 10 to 1000 seconds\, creating violent explosions potentially o bservable in gravitational waves and across the electromagnetic spectrum. The observational signatures associated with a binary neutron star merger are intrinsically connected to the fate of the merger remnant. I will disc uss the different observational signatures expected in binary neutron star mergers and what kilonovae and short gamma-ray burst observations tell us about the fate of other binary mergers. I will discuss how these observat ions can shed light onto fundamental questions\, such as the behaviour of nuclear matter at supranuclear densities\, the jet-launching mechanism of gamma-ray bursts and r-process nucleosynthesis. I will also look to the fu ture\, and discuss what we can learn by maximising the value of different messengers in the gravitational-wave multi-messenger era. LAST-MODIFIED:20240201T050607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Lilli Sun) \nZoom: https:/ /anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Nikhil Sarin (NORDITA) "Leveraging observations of electromagnetic and gravitational-wave transients (Joint CGA-RSAA colloquium)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190725T010000Z DTEND:20190725T020000Z DTSTAMP:20261011T152429Z UID:icbelj5m7e37e302innaagm6ig@google.com CREATED:20190228T030119Z DESCRIPTION:Neutral hydrogen is the dominant component of the universe afte r recombination with high density regions harbouring the first luminous ob jects. The radiation from these first luminous objects changes the thermal and ionization state of the intergalactic medium leading to a major trans ition in the history of the universe called the Epoch of Reionization (EoR ). The EoR is marked by the appearance of ionized regions around these col lapsed objects which grow and merge until the entire universe is ionized. The growth and topology of these ionized regions depends upon the properti es of these first luminous sources. One important observational probe of t he EoR is the 21cm spin flip hyperfine transition of the neutral hydrogen. The brightness temperature of this transition encodes the ionization and heating history of the IGM. We introduce real space morphological descrip tors\, called Minkowski Tensors (MTs) and topological quantities Betti num bers\, to probe the morphology of the 21cm brightness temperature field. T he MTs provide shape and anisotropy information of the structures in the e xcursion set of the fields\, while Betti numbers describe the topology in terms of the number of connected regions and holes. We obtain different r egimes of morphological evolution of brightness temperature\, as the unive rse evolves depending upon different astrophysical settings of the EoR. Th erefore\, we show that the ionization history of the IGM can be reconstruc ted using the morphological description of brightness temperature in real space and help us further probe the properties of the first luminous objec ts. LAST-MODIFIED:20190715T005607Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Akanksha Kapahtia (Indian Institute of Astrophysics) "Morphology of cosmological fields during the epoch of Reionization" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221025T000000Z DTEND:20221025T010000Z DTSTAMP:20261011T152429Z UID:2cdite0dqcrdrsj129qm404jmc@google.com CREATED:20221005T054214Z DESCRIPTION:The assembly history of the Milky Way has been revealed in fant astic detail in recent years thanks to dedicated spectroscopic and astrome tric surveys of millions of its stars. At the same time\, IFU observation s of external galaxies at intermediate redshifts are producing statistical snapshots of the diverse kinematic and chemical structures intrinsic to p opulations of galaxies. Our group's ongoing collaborative work at ANU aim s to connect the Milky Way to higher redshift observations\, by developing tools that quantify how different accretion and star formation histories imprint themselves on present day galaxy disk properties. After testing t hese models on the velocity dispersion and scale height data of the Milky Way's disks\, I will show a first application to MUSE observations of a ga laxy in the Fornax cluster\, which have revealed signatures of an ancient (z=2) merger event in that galaxy. This offers an example of how semi-ana lytic models applied to chemo-dynamical observations of external galaxies can provide a 'MilkyWay-like' view of their assembly history. This will n ot only help us quantify the impact of mergers on disk structure and test cosmological predictions for merger rates\, but also understand if the rec overed merger history of the Milky Way is (a)typical for galaxies of its m ass. LAST-MODIFIED:20221024T015106Z LOCATION:DLT & ZOOM (host: TBD) \nZoom: https://anu.zoom.us/j/99785341005?p wd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ryan Leaman (University of Wien) "A (g)Astronomical cookbook for ba king galaxy disks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180508T010000Z DTEND:20180508T020000Z DTSTAMP:20261011T152430Z UID:s54ndven56of188k0eilao1mlg@google.com CREATED:20180302T030113Z DESCRIPTION:Stars form in molecular clouds. These clouds are dense concentr ations of H2 that are traditionally traced in external galaxies using tran sitions of CO or other\, more complex molecules. But dwarf irregular (dIm) galaxies seemingly contradict this fundamental picture. Tracers of recent star formation\, such as Halfa or far-ultraviolet (FUV) emission\, show t hat most dwarfs contain young stars and star clusters\, but CO observation s often yield only upper limits. The Magellanic Clouds are the best local templates for studying the life cycle of the ISM and star formation in low metallicity environments (LMC\;Z=0.5 Zo and SMC\, Z=0.2 Zo). Their proxim ity (LMC: D = 50 kpc\; SMC: D = 60 kpc)\, provide a unique opportunity to resolve individual clouds\, allowing us to conduct detailed studies of the different phases of the ISM in low-metallicity environments using various gas and dust tracers. I will present CO observations with ALMA of star-fo rming regions at the lowest metallicities dwarf galaxies from SMC to WLM. LAST-MODIFIED:20180504T051607Z LOCATION:Duffield Lecture Theatre (host: Jameson) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Monica Rubio (Universidad de Chile) "Low metallicity molecular clou ds with ALMA" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160422T040000Z DTEND:20160422T042000Z DTSTAMP:20261011T152429Z UID:dnt10dr4ua0eep6b8slttf4q90@google.com CREATED:20160415T073605Z DESCRIPTION:With SDSS and WISE data\, we study the mid-IR properties of a l arge sample of local Seyfert 2 galaxies. We find the host-subtracted mid-I R luminosities are linearly correlated with [OIII] luminosities for three orders of magnitude. The partition functions of the total integrated [OIII ] and mid-IR luminosities from AGNs\, as a function of a variety of host g alaxy properties\, are identical\, consistent with the expectation of simp le AGN unified model. However\, the mid-IR emission is correlated with exc essive number of neighbouring galaxies within a projected distance of 100 kpc\, while [OIII] emission is not. It implies a phase of torus formation during galaxy interactions.​ LAST-MODIFIED:20160421T052605Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Li Shao (CSIRO) "AGN obscuration and host galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141218T000000Z DTEND:20141218T010000Z DTSTAMP:20261011T152430Z UID:5n1sanabk7cagle0rlppctlkfc@google.com CREATED:20141117T060342Z DESCRIPTION:Ultracompact dwarf galaxies (UCDs) are among the densest stella r systems in the Universe. With typical masses of 10^7 to 10^8 solar masse s and half-mass radii between 10 to 100 pc they are more than a factor 100 0 denser than dwarf galaxies of the same mass. They also show evidence for elevated mass-to-light ratios\, which could be due to the presence of mas sive black holes or unusual stellar IMFs as a result of their extreme dens ities. While the first UCD was discovered only 15 years ago\, hundreds of of them have meanwhile been found in nearby galaxy clusters\, making it al l the more important to understand where UCDs come from. In my talk I will discuss our current knowledge about UCDs and the various formation channe ls that have been suggested for them\, and explain what we can learn from UCDs about the early evolution of galaxies. LAST-MODIFIED:20250925T231028Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) \nZoom: https://anu.zoo m.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Holger Baumgardt (University of Queensland) "The formation of the s mallest galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200925T040000Z DTEND:20200925T043000Z DTSTAMP:20261011T152429Z UID:9bb1flf4vsu24hqr4o0gahh6h8@google.com CREATED:20200826T024111Z DESCRIPTION:Meridith will talk about: Dance til you drop: the queer and cou ntercultural origins of raving James will talk about: Turbulence in the ni ght sky LAST-MODIFIED:20200916T103109Z LOCATION:ZOOM 997 8534 1005 (host: Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Meridith Joyce and James Beattie (RSAA) "Raving and Turbulence" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210513T040000Z DTEND:20210513T050000Z DTSTAMP:20261011T152430Z UID:3tcp4cp01puunb729enju7qc0s@google.com CREATED:20210506T054108Z DESCRIPTION:Kate Harriden and Renee Hartley will be coming to Mount Stromlo to hold a session on acknowledging Country. Kate is the co-ordinator of t he Fenner Circle\, a space for yarning about the interconnections between land\, water\, biota\, climate and Indigenous cultures with a focus on und erstanding how these synergies can best inform our research and teaching. Kate is also a phd scholar and visiting indigenous fellow co-ordinator at the Center for Aboriginal Economic Policy Research (CAEPR). Renne is a Fen ner Circle member and PhD Scholar with the Fenner School\, studying landsc ape ecology. The session will be run in an informal manner. There will be time to listen and learn and time to engage and ask questions. This will b e a safe space where no questions will be seen as 'silly'. To facilitate t his\, we will take a few minutes break somewhere in the middle of the sess ion\, when people will be able to write down questions anonymously if they feel more comfortable doing so. We are hoping to see a big turn up from a ll staffs and students to the session! LAST-MODIFIED:20210513T025706Z LOCATION:CSO Common Room and ZOOM (host: Tiphaine Lagadec) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kate Harriden\, Renee Hartley (Fenner Circle) "Acknowledging Countr y" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260317T000000Z DTEND:20260317T010000Z DTSTAMP:20261011T152430Z UID:3mottqj65ehpqcmbh879dfsh34@google.com CREATED:20251203T021615Z DESCRIPTION:Massive stars and their spectacular end-of-life explosions have far-reaching implications for a broad range of astrophysics\, including t he enrichment of the interstellar medium\, the evolution of galaxies\, the formation of compact objects\, such as neutron stars and black holes\, th at produce gravitational waves\, and the creation of rapid neutron capture (r-process) elements such as gold and platinum. Despite decades of resear ch\, our understanding of the final moments of the lives of massive stars is minimal. This is set to change as we enter the golden era of time-domai n and multi-messenger astronomy. The number of new transients discovered e ach year is rapidly increasing as new surveys employ novel approaches to i dentify young and interesting transients. Additionally\, gravitational wav e detections are combined with electromagnetic observations from space and ground-based telescopes\, shedding light on their progenitor systems. In this talk\, I will present an observational overview of the state of the f ield in i) the mass loss history of massive stars\, ii) the variety of exp losions and their progenitor systems\, iii) the fate of compact objects pr oduced from these explosions\, and iv) the production of r-process element s. LAST-MODIFIED:20260306T065110Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Lewis Miller) \nZoom: http s://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Manisha Shrestha (Monash U.) "Leveraging multi-messenger observatio ns to connect massive stars to their explosive ends" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240809T040000Z DTEND:20240809T043000Z DTSTAMP:20261011T152429Z UID:7t30tkh4v6aeufosoa95unq4b4@google.com CREATED:20240805T000609Z DESCRIPTION:Working as an engineering officer in the Australian Army provid ed many unique experiences and opportunities that translated into skills w hich have assisted in establishing a career in the Space engineering indus try. During my time in the military\, a significant amount of training was provided\, and practical experience gained in critical skills that are re quired to achieve organizational outcomes and develop technical competence . With some adaptation\, I found these skills to be very beneficial in my subsequent career as an engineering manager\, team lead and mission manage r at Skykraft\, a Canberra-based space start-up. This presentation will co nvey the skills and experiences I developed as a troop commander and engin eering officer in the Army\, explaining how their application can help pri vate industry and institutions better achieve organisational objectives. These include fundamental leadership and management principles required to develop high-performing teams and a positive workplace culture as well as management and planning skills to ensure that personal and organizational efficiency is maximized. I will also touch on complexity theory as a tool to help individuals and organisations achieve outcomes\, even when faced with apparently chaotic circumstances. In the latter part of my presentati on\, I will cover design practices and engineering processes that were req uired to take concepts from a whiteboard to flight model hardware in excee dingly short time frames. I will provide my impression on the different sy stems engineering approaches which are effective in a large\, risk averse organisation versus a highly time and resource constrained business. Fina lly\, I will share stories about working with companies like SpaceX\, and transitioning from Skykraft to start my own engineering company. LAST-MODIFIED:20240805T001110Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hana Benhizia) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Roger Dudziak (Clear Space Technologies) "Technical and Leadership Lessons Learned as A Defence and Space Engineer" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240130T000000Z DTEND:20240130T013000Z DTSTAMP:20261011T152429Z UID:h4nk6l600hctssa29eme9dt9og@google.com CREATED:20231212T003610Z DESCRIPTION:Studying the host galaxies of high-redshift quasars provides vi tal insights into the early growth of supermassive black holes and the bla ck hole-galaxy connection. JWST has launched a new era in this field\, pro viding the opportunity to observe the stellar components of these host gal axies for the first time\, due to its exquisite spatial resolution and inf rared spectral capabilities. I will present our latest results from a rang e of JWST programs aiming to measure high-z quasars and their host galaxie s\, including two z=6.8 quasars from the Galaxy Assembly with NIRSpec IFS GTO program. We have measured their black hole properties and a wide range of host properties\, for example their interstellar medium structure and kinematics\, star formation rates\, and outflows\, as well as discovering that both have merging companion galaxies. I will summarize our latest res ults and outline the plans for the rest of our upcoming observations study ing quasars and their host galaxies with JWST. LAST-MODIFIED:20240119T210606Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Stu Wyithe) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Madeline Marshall (Mertzberg Institute) "Observing the Host Galaxie s of High-z Quasars with JWST" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231017T000000Z DTEND:20231017T013000Z DTSTAMP:20261011T152429Z UID:4h3gt43vj3q8imnkqp7tfoo0dg@google.com CREATED:20230917T235113Z DESCRIPTION:The Parkes Pulsar Timing Array (PPTA) is a major project on the Parkes Radio Telescope (Murriyang)\, with the primary aim of detecting na nohertz-frequency gravitational waves (GWs). A background of GWs (GWB) mod ulates pulsar arrival times and manifests as a stochastic process\, common to all pulsars\, with a signature spatial correlation. In this talk I des cribe our recent search for an isotropic stochastic GWB using the third da ta release of the PPTA. We recover a noise process with a common spectrum among the pulsars\, which exhibits characteristics consistent with that ex pected of a GWB from supermassive black hole binaries. We also search for the spatial correlations expected from a GWB and estimate the significance of these correlations as 2 sigma in our data set. However\, contrary to e xpectations for the GWB from an isotropic population of inspiralling super massive black hole binaries\, we demonstrate that the apparent signal stre ngth is changing with time. I will discuss these results in the context of recent analyses from other international pulsar timing array collaboratio ns and describe the exciting outlook for nanohertz gravitational wave astr onomy with the sensitive new MeerKAT pulsar timing array. LAST-MODIFIED:20231008T225107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Sven) \nZoom: https://anu. zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Daniel Reardon (Swinburne U.) "Nanohertz-frequency gravitational wa ve astronomy with the Parkes Pulsar Timing Array and beyond" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230117T000000Z DTEND:20230117T004500Z DTSTAMP:20261011T152429Z UID:1bf69d5l6frntgl9bcnmph5ilo@google.com CREATED:20230111T054507Z DESCRIPTION:High resolution spectra of stars provide a wealth of informatio n regarding the composition and properties of their atmospheres. However\, the analysis of such spectra often requires normalization\, which involve s dividing the observed flux element-wise by a modeled pseudo-continuum. T he modeling of this pseudo-continuum is a non-trivial task\, as the shape is influenced by various factors such as the spectrum of the observed star \, interstellar absorption\, absorption in the Earth's atmosphere\, the re sponse function of the spectrograph\, and the reduction pipeline. These fa ctors can introduce numerous low- and high-frequency distortions that are difficult to model automatically\, resulting in time-consuming manual norm alization. One limitation of automatic methods is the assumption that the local flux maximum is a good approximation of the pseudo-continuum\, which is often not true in the case of spectra with emission features or wavele ngth ranges where spectral lines heavily blend. To address these challeng es\, we propose a method for stellar spectrum normalization based on a dee p convolutional neural network called SUPPNet. One of the key advantages o f this method is its ability to effectively handle spectra with both high and low signal-to-noise ratios\, various rotational velocities\, and spect rograph's resolutions. The algorithm is open source and available online: https://github.com/RozanskiT/suppnet. LAST-MODIFIED:20230117T005606Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Jo Ciuca) \nZoom: https:/ /anu.zoom.us/j/99785341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tomasz Rozanski (Wroclaw University) "SUPPNet: neural network for s tellar spectrum normalization" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151016T030000Z DTEND:20151016T034000Z DTSTAMP:20261011T152429Z UID:d8p1ememuc1ph4eu6rvftu25t0@google.com CREATED:20150824T070611Z DESCRIPTION:Time has come for me to move to a new longitude\, but not befor e following the tradition and updating you on the work I have been doing i n the latest stages of my PhD (and beyond). In particular\, I'll discuss m y various observations of galaxies in Hickson Compact Group 91\, and what these these (may) tell us about galaxy evolution in groups. This presentat ion would of course not be complete without a final attempt at convincing you of the potential of some excitingly new technology to publish multi-di mensional datasets in 3-D. Hence\, I shall also tell you about the newly d eveloped X3D pathway Chris Owen and I have been developing lately. LAST-MODIFIED:20151012T040618Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Frederic Vogt (RSAA) "Gas flows and star formation as a consequence of galaxy interaction in compact groups" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190124T000000Z DTEND:20190124T010000Z DTSTAMP:20261011T152430Z UID:4jq2le2eccdmvm1tkt8u8v3r60@google.com CREATED:20190117T235106Z DESCRIPTION:One of the outstanding problems in galaxy evolution studies is to link the evolution of the star formation rate of galaxies to their mole cular gas content. Observationally\, the last decade of studies have led t o a clear picture of the cosmic star formation history\, which peaked at z ~2 and has declined since then. However\, it is unclear whether the declin ing star formation rates are simply the result of lower molecular gas mass es\, or whether the star formation efficiency has also evolved. In this ta lk I will discuss how the molecular gas contents of galaxies are measured and highlight the difficulties of doing so at high redshift. I will descri be one of the most popular approaches\, which relies upon the dust continu um emission\, and will present our recent work where we test the validity of the this dust continuum calibration via a unique sample of z~2 galaxies with observations of both dust continuum and CO(1-0) line emission. LAST-MODIFIED:20190123T055104Z LOCATION:CSO Common Room (host: Zerjal) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Melanie Kaasinen (MPIA) "Weighing the Molecular Gas Reservoirs of H igh Redshift Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240806T010000Z DTEND:20240806T020000Z DTSTAMP:20261011T152429Z UID:o7nhntfa6l3604t4c84g8qo07o@google.com CREATED:20240417T012140Z DESCRIPTION:A key question has emerged in the wake of recent observations i n pulsar timing astronomy: what is the origin of the nanohertz gravitation al-wave background? If the background can be firmly linked to the mergers of supermassive binary black holes\, there will be important implications for cosmology: from the evolution of supermassive black holes over cosmic time to the formation of galaxies. On the other hand\, if the binary black hole hypothesis can be falsified\, this would likely imply new fundamenta l physics such as a phase transition in the early Universe. In this talk I argue that mapping the gravitational-wave sky is our most reliable method for testing the binary black hole hypothesis. I describe how to map the g ravitational-wave sky and present recent results from the MeerTime Collabo ration. LAST-MODIFIED:20240715T070613Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hilay Shah) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Eric Thrane (Monash U.) "Mapping the gravitational-wave sky: Result s from the 4.5 year MeerKAT Pulsar Timing Array Data Release" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200924T010000Z DTEND:20200924T013000Z DTSTAMP:20261011T152429Z UID:i1vcoq7gn73ls4s529j8a79f40@google.com CREATED:20200910T060511Z DESCRIPTION:TBD LAST-MODIFIED:20200910T060511Z LOCATION:ZOOM 997 8534 1005 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dávid Guszejnov (UT Austin (USA)) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150902T000000Z DTEND:20150902T010000Z DTSTAMP:20261011T152429Z UID:9jfd9n5nm3ku06ca379ab20ldk@google.com CREATED:20150714T123115Z DESCRIPTION:Women comprise more than half of science PhD graduates and earl y career researchers\, but less than 20% of senior academics in Australian universities and research institutes. The loss of women scientists is a s ignificant waste of expertise\, talent and investment\, and negatively imp acts on our nation's scientific productivity. Professor Jennifer Martin wi ll discuss the issues and roadblocks women face\, outline what universitie s and individuals can do to make change happen\, and highlight the current Academy of Science 'Science in Australia Gender Equity' (SAGE) pilot of t he UK Athena SWAN gender equity accreditation system. LAST-MODIFIED:20150715T133118Z LOCATION:Duffield Lecture Theatre (host: Celine d'Orgeville) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jenny Martin (UQ) "Gender Equity in Academia - Making it happen" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170324T030000Z DTEND:20170324T032000Z DTSTAMP:20261011T152429Z UID:voh4i97q87h7i82re8dbo2qmf8@google.com CREATED:20170313T232106Z DESCRIPTION:TBD LAST-MODIFIED:20170324T021604Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Laura McKemmish (University College London) "Original Research By Y oung Twinkle Students: involving high school students in research associat ed with a space mission" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240404T000000Z DTEND:20240404T013000Z DTSTAMP:20261011T152429Z UID:0s1agsuangmmdoq0ilf2rg9o9o@google.com CREATED:20240111T004623Z DESCRIPTION:Low mass stars retain the chemical imprint of the gas cloud the y were born from. Therefore\, stellar abundances provide insight into the evolution of stars and chemical elements throughout the life of galaxies\, such as our own Milky Way. Galactic archaeology uses stars and their chem ical fingerprints like fossils to trace cosmic history. Out of the known e lements\, lithium (Li) is a uniquely interesting element\, produced in Big Bang Nucleosynthesis and cosmic ray spallation\, and moderated in stellar evolution. Stellar abundances cannot be directly observed or measured\, i nstead they must be inferred from models. I will discuss the most physical ly realistic radiative transfer (3D NLTE) models\, how accurate they are c ompared to high fidelity observations\, and how these models can be applie d to large spectroscopic surveys to improve accuracy of abundances. Throug h this work\, I measure the lithium abundance of the Sun\, reject the seco nd cosmological lithium problem\, discover the evolution of the Li-dip up the subgiant branch\, and find no ubiquitous production of lithium in the He flash. LAST-MODIFIED:20240319T043613Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Sven Buder) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ella Wang (RSAA) "Spectroscopic Measurements of Lithium in Late-typ e Stars (End of thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200617T003000Z DTEND:20200617T021000Z DTSTAMP:20261011T152429Z UID:il3ftn3msb0k0ss53g4007u918@google.com CREATED:20200610T110105Z DESCRIPTION:Honours and Masters students will give their thesis talks. All welcome and encouraged to attend. Please see Chris' original email for zoo m details. LAST-MODIFIED:20200610T110105Z LOCATION:ZOOM (host: Wolf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Honours/Masters thesis talks (RSAA) "Honours/Masters thesis talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230322T000000Z DTEND:20230322T010000Z DTSTAMP:20261011T152429Z UID:f5nk5o19svk9kkmjhhmnjkihf0@google.com CREATED:20230317T025607Z DESCRIPTION:The baryon cycle regulates the ability of galaxies to form star s. Most galaxies\, however\, are too far away to resolve their gaseous inf lows and outflows. The nearby Milky Way and Magellanic Clouds offer unprec edented views of this cycle. In this talk\, we will survey a tidal remnant and a galactic wind that are both removing gas from the Magellanic Clouds . Additionally\, we will examine a high velocity cloud that is flowing tow ard the Galaxy. These spectroscopic emission- and absorption-line studies using radio\, optical\, and UV observations provide crucial insight on how these processes occur at greater distances where they cannot be explored in such great detail. LAST-MODIFIED:20230317T025607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Lindsey) \nZoom: https://a nu.zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kat Barger (Texas Christian University) "Gas flows of the Milky Way and Magellanic Cloud Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210212T030000Z DTEND:20210212T033000Z DTSTAMP:20261011T152430Z UID:v27rja6r7le2m88ttkf60rh9i4@google.com CREATED:20210108T205111Z DESCRIPTION:We start the weekend with our new open-mic talks. Ella: ADACS i nternship: the importance of testing your code Phil: Stromlo Garden and Co mpost LAST-MODIFIED:20210211T213605Z LOCATION:ZOOM and Duffield Lecture Theatre (host: Jung) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ella Wang and Phil Taylor (RSAA) "Feast of Facts" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260605T004500Z DTEND:20260605T023000Z DTSTAMP:20261011T152430Z UID:eeqehvgd6660i4749nkb1p48oo@google.com CREATED:20260503T113713Z DESCRIPTION:TBC LAST-MODIFIED:20260503T113714Z LOCATION:Zoom or Duffield Lecture Theatre (host: Chris Wolf) \nZoom: https: //anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA masters and honours students (RSAA) "Honours and masters end-o f-thesis talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191122T030000Z DTEND:20191122T033000Z DTSTAMP:20261011T152430Z UID:63vm2racpgictkfsn5gfc7kc2c@google.com CREATED:20191022T040713Z DESCRIPTION:We're all familiar with geostationary satellite antennas – th e Foxtel dishes atop many rooftops that point to a fixed location in space . The AITC has a number of programs\, however\, that rely on our ability to interact with satellites that freely zip across the sky under the influ ence of a plethora of perturbing forces. Understanding these forces is th e first step to being able to predict where any of the 20\,000+ catalogued orbital objects are at any particular instant so we know where – and wh en – to point our telescopes at them. In this talk I’ll outline how s atellites move\, how we find them and the challenges and opportunities the y afford to our communications and space environment research programs. LAST-MODIFIED:20191022T040713Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:James Webb (RSAA/AITC) "AITC Series – Space is big\, satellites a re (comparatively) small… the joys of finding\, tracking\, and using th em!" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161101T000000Z DTEND:20161101T010000Z DTSTAMP:20261011T152429Z UID:tjb1i6tbub958q8s6do3gmkvc0@google.com CREATED:20161017T025105Z DESCRIPTION:Most of the neutral Hydrogen in the Local Group is contained in the disks of the large spirals\, but there are important exceptions\, som e of which are tied to basic processes in galaxy evolution. After giving a brief survey of recent science with the Green Bank Telescope\, I'll disc uss the different populations of neutral hydrogen that are found outside t he disks of galaxies in the Local Group. The most puzzling are the clouds found between M31 and M33\, which have the mass of dwarf galaxies but con tain no stars. LAST-MODIFIED:20161031T233104Z LOCATION:Duffield Lecture Theatre (host: Helga Denes) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jay Lockman (US National Radio Astronomy Observatory) "Neutral Gas Outside the Disks of Local Group Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230719T230000Z DTEND:20230720T003000Z DTSTAMP:20261011T152429Z UID:nkud4mglr4halubtu9j3k6bhvo@google.com CREATED:20230718T060606Z DESCRIPTION:Supernovae are the explosive deaths of massive stars. Despite t heir rarity\, recent large-scale surveys have been able to discover them e n masse due to their extreme luminosity\, which enable us to study them fr om across intergalactic distances. Unfortunately\, studying their progenit ors is very difficult due to the distances involved. In this talk\, I will discuss an example showing what is currently possible to discern about su pernovae progenitors\, highlight the role that Australia's can play in upc oming large scale surveys\, and present work done in developing a new inst rument to provide rapid cadence observations of these transient events. LAST-MODIFIED:20230719T032605Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Bailey) \nZoom: https://an u.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Harrison Abbot (RSAA) "Supernova Surveys - From the ground up" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160610T040000Z DTEND:20160610T042000Z DTSTAMP:20261011T152429Z UID:9n954aig7ol95u90ngblc13hd8@google.com CREATED:20160503T003112Z DESCRIPTION:The presence of extended main-sequence turn-off (eMSTO) regions in intermediate-age\, 1–2 Gyr-old star clusters in the Large and Small Magellanic Clouds is often interpreted as resulting from extended star-for mation histories (SFHs) that last ≥ 300 Myr. This strongly conflicts wit h the traditional view of stellar clusters\, which are thought of as singl e-aged stellar populations. In this talk\, I will show our investigation i nto these issues by exploring the morphology of the sub-giant branch (SGB) of LMC and SMC clusters. We find that for most cases\, the width of the S GB favors the single-aged stellar population interpretation and rules out an extended SFH. For clusters that have a very low escape velocity\, they have unlikely undergone significant mass loss at an early stage\, thus ind icating that they may lack the capacity to capture most of their initial\, expelled gas from stellar evolutionary processes. LAST-MODIFIED:20160503T003112Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Chengyuan Li (Macquarie University) "Using the sub-giant branch to constrain the star formation history of intermediate-age clusters" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171214T000000Z DTEND:20171214T010000Z DTSTAMP:20261011T152429Z UID:9revimtrp55o65gqpd78rlkrlk@google.com CREATED:20171120T050511Z DESCRIPTION:The interpretation of images is at the heart of most investigat ions in astronomy\, and much effort is spent on designing and operating te lescopes and instruments that produce the sharpest and finest possible dat a-products. There are however a few important scenarios where despite thes e efforts\, the information one cares about remains clouded by residual in strumental effects. When looking for instance at AO corrected high-contras t images\, one needs to disentangle genuine astrophysical structures surro unding the target from residual diffaction features. The discrimination to ol is the fundamental measurement of the degree of coherence\, the usual d ata-product of interferometry. Looking at images as the result of an inter ferometric process makes it possible to ge beyond the conventional diffrac tion limit. I will describe one possible operating mode of this point of v iew that is currently being investigated in the context of a European proj ect called KERNEL and highlight two applications: the post-processing of m id-to-high Strehl images for high-precision relative astrometry of low-mas s binaries\; a focal plane based wavefront control loop successfully deplo yed on-sky by the extreme adaptive optics instrument SCExAO at the Subaru Telescope. LAST-MODIFIED:20171213T025206Z LOCATION:Duffield Lecture Theatre (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Frantz Martinache (Observatoire de la Cote dAzur) "The KERNEL proje ct" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260903T010000Z DTEND:20260903T020000Z DTSTAMP:20261011T152430Z UID:bgmi84r8t8l6m3bo2l02k0ald8@google.com CREATED:20260827T230005Z DESCRIPTION:Reverberation mapping (RM) of Active galactic nuclei (AGN) prov ides a direct probe of the geometry surrounding supermassive black holes ( SMBH). We correlate variations in the AGN disk brightness with its echoes in emission lines from further out in the system. The timescale of these r everberations gives us a ruler for the system's size\, letting us study AG N geometry well beyond the limits of direct imaging. From this\, we can co nstrain SMBH masses and population properties out to extreme redshifts.\n\ nWe live in the age of industrial scale RM\, where multi-year surveys like OzDES and SDSS (and in the future 4MOST and DESI)\, study 100’s to 1000 ’s of AGN at a time. The seasonal window function of these modern survey s inflicts the problem of aliasing: the appearance of false positive lag m easurements that confound our mass measurements and scaling relationships. This aliasing problem has been a dominant problem in modern RM. In this t alk\, I will walk through my end-to-end rebuilt of the industrial scale RM pipeline\; its new purpose-built statistical and numerical data analysis tools\, and what surprising results we get when we apply it to real data. LAST-MODIFIED:20260828T030006Z LOCATION:Zoom or Duffield Lecture Theatre (host: Chris Wolf) \nZoom: https: //anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Hugh McDougall (UQ) "Did I just hear something? Solving the problem of false positive detections in modern AGN reverberation mapping" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240516T010000Z DTEND:20240516T020000Z DTSTAMP:20261011T152429Z UID:2lcfo5m01nmd7vjp5vt09rp0k0@google.com CREATED:20240424T133612Z DESCRIPTION:Turbulence is one of the key architects of interstellar medium (ISM) structure\, and regulates many processes within galaxies\, from star formation on au scales\, to the mixing of metals on kpc scales. The way i n which turbulence is driven and energy is injected into the ISM has a sig nificant impact on these processes\, as has been well-described by computa tional studies of\, for example\, star formation in controlled (magneto-)h ydrodynamical simulations. From simulation work it has been shown that\, f or an isothermal\, compressible gas\, the volume density dispersion is pro portional to the sonic Mach number. The constant of proportionality\, b\, is known as the turbulence driving parameter\, and describes the ratio of solenoidal to compressive modes in the turbulent acceleration field of the gas. Theoretically\, the turbulence driving parameter ranges from b = 1/3 (purely solenoidal) to b = 1 (purely compressive)\, with b = 0.38 charact erising the natural mixture (1/3 compressive\, 2/3 solenoidal) of the two driving modes. In simulations we can dictate the value of b and observe it s influence. But what about in reverse? Can we observe b and therefore inf er how different physical processes in the ISM drive turbulence? The under lying challenge of this work is that turbulence is a distinctly three-dime nsional processes\, described using three-dimensional quantities. In obser vations we lack access to the third spatial dimension\, and therefore care ful assumptions need to be made in order to convert what we see on the pla ne of the sky to quantities that can diagnose turbulence. In this talk I w ill discuss a collection of works in which I have developed a robust set o f tools to extract turbulence characteristics from observations of primari ly HI emission\, focusing on recovering the turbulence driving parameter. I will present our findings from three studies carried out in different IS M environments and discuss their implications in the context of the physic al driving processes present in those environments. LAST-MODIFIED:20240506T035611Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Christoph Federrath) \nZoo m: https://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Bella Gerrard (RSAA) "Turbulence driving in the diffuse ISM (End-of -thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180111T223000Z DTEND:20180112T043000Z DTSTAMP:20261011T152429Z UID:uqha09l0bugneg704hbsef13f8@google.com CREATED:20171213T025207Z DESCRIPTION:Our 10 Summer Research Students will present seminars on the re search they performed over the summer. All Welcome and encouraged to atten d. LAST-MODIFIED:20171213T025207Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Summer Research Student Seminar Series (RSAA) "Summer Research Stud ent Seminar Series" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161028T030000Z DTEND:20161028T032000Z DTSTAMP:20261011T152429Z UID:6dpl25a8vbira1ogff72g2vb9o@google.com CREATED:20161019T233105Z DESCRIPTION:The Five Hundred Metre Aperture Spherical Telescope (FAST) was officially opened in Guizhou Province\, China in late September 2016. Las t week I had the opportunity to visit FAST. In this informal talk I will describe FAST and give a status report of where it is in its commissioning process. I will show pictures from my trip and discuss some of the scien ce I hope to do with FAST in the coming years. LAST-MODIFIED:20161025T230105Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Naomi McClure-Griffiths (RSAA) "A Visit to the World's Largest Tele scope: FAST" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221007T030000Z DTEND:20221007T033000Z DTSTAMP:20261011T152429Z UID:clliat2v36h1un3f0qb9sspqn0@google.com CREATED:20220926T013107Z DESCRIPTION:Gregory would present information on the opportunities provided by the ADACS Merit Allocation Program for accessing software support. LAST-MODIFIED:20221007T005607Z LOCATION:ZOOM ONLY (host: TBD) \nZoom: https://anu.zoom.us/j/99785341005?pw d=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Gregory Poole (Swinburne University) "ADACS Merit Allocation Progra m" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220329T000000Z DTEND:20220329T010000Z DTSTAMP:20261011T152430Z UID:589ej7laeqa2b7cbu3jchhiukc@google.com CREATED:20220201T005111Z DESCRIPTION:Advances in high-performance computing have enabled astronomers to simulate a variety of dark matter models beyond collisionless cold dar k matter\, in an effort to compare galaxy formation against observations a nd constrain the nature of dark matter and its parameters. In this talk\, I will present simulations of what the Universe would look like if DM were an ultra-light 10^-22 eV boson\, aka `fuzzy dark matter' (FDM). I explore the interplay between baryonic physics and unique quantum mechanical wave like features inherent to FDM. I describe the formation of first galaxies\ , which may be soon observable with the James Webb Space Telescope (JWST)\ , and how these objects give constraints on the small-scale nature of dark matter. LAST-MODIFIED:20220321T012611Z LOCATION:DLT & ZOOM (host: Neco Kriel) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Philip Mocz (Lawrence Livermore National Laboratory\, USA) "Invited Colloquium: Fuzzy Dark Matter Cosmology" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200306T030000Z DTEND:20200306T040000Z DTSTAMP:20261011T152429Z UID:utoku4dcdsk6b0r0241571a7vk@google.com CREATED:20200227T050105Z DESCRIPTION:Space debris poses a significant risk to safe operations in spa ce. Careful management of the space environment is required to prevent a K essler Syndrome where a cascade of debris can leave regions of space inope rable. Adaptive Optics Imaging (AOI) is an AO system for characterisation of satellites and debris in low Earth orbit (LEO)\, and tracking objects i n geostationary orbit (GEO). In this talk I will describe the work complet ed for my thesis which includes the design\, build and operation of AOI. LAST-MODIFIED:20200302T002606Z LOCATION:Duffield Lecture Theatre (host: Rey) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Michael Copeland (ANU) "Satellite and Debris Characterisation with Adaptive Optics Imaging (End-of-Thesis Colloquium)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201110T000000Z DTEND:20201110T010000Z DTSTAMP:20261011T152429Z UID:gkq151mvodqdku9m9im3i3p78o@google.com CREATED:20200923T022218Z DESCRIPTION:Direct imaging is the best detection method for exoplanets at w ide separations\, but it is limited by the large contrast difference betwe en stars and planets. The most promising direct imaging surveys are condu cted in near infrared wavelengths at young ages when a giant planet is sti ll self-luminous at these wavelengths. In this talk\, I summarize our sur vey of young stars in the Taurus Molecular Cloud and what this tells us ab out our experimental limits. Applying models of planet formation and brig htness evolution\, I also discuss how likely we are to detect accreting ex oplanets with future instruments and whether we can constrain the formatio n conditions of directly imaged planets. LAST-MODIFIED:20201109T010606Z LOCATION:DLT and ZOOM 997 8534 1005 (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alex Wallace (RSAA) "End-of-Thesis Talk: Searching for Young Exopla nets with High-Contrast Imaging" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190916T000000Z DTEND:20190916T020000Z DTSTAMP:20261011T152430Z UID:o973lv50fov9l4t9vl5gf4n8ck@google.com CREATED:20190725T162215Z DESCRIPTION:The AAT Council is holding a series of Town Hall Meetings to di scuss the future of the Anglo-Australian Telescope (AAT). As a member of t he ASA and as a potential future user of the AAT\, we’d like to encourag e you to have your say on the future of the AAT specifically\, and SSO mor e broadly. A short discussion paper (https://drive.google.com/file/d/1PTe JMF7uhOmImjK4UM0ieq9ozTtQQNX7/view) summarising current operations and lis ting a few discussion points has been prepared in advance of the meeting. The meeting will be streamed via zoom (id: 214 283 5158). For more details \, please contact seminars. LAST-MODIFIED:20190909T012603Z LOCATION:CSO Common Room (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:AAT town hall meeting (RSAA) "AAT and SSO: Current Operations and F uture Possibilities" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190809T040000Z DTEND:20190809T043000Z DTSTAMP:20261011T152430Z UID:cev145v153bgr4n6a21mcb2s94@google.com CREATED:20190710T050110Z DESCRIPTION:The use of remote sensing through free\, open and publicly avai lable satellite imagery for managing Australia's water resources has great ly increased in recent years\, for understanding the presence and changing behaviour of water across the landscape\, the extent and condition of nat ive vegetation as well as for helping ensure water users stay within the r ules. Such imagery provides a powerful tool\, with careful and tailored ap plication. This talk provides an overview of how such imagery is currently being used within the Murray-Darling Basin\, and outlines how big data\, programming and statistical analysis skills obtained from an Astrophysics career can play a big role in developing Australia's future water manageme nt under a drying climate. LAST-MODIFIED:20190730T042107Z LOCATION:Duffield Lecture Theatre (host: Zhang) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:David Weldrake (Murray-Darling Basin Authority) "Remote Sensing: Fr om Exoplanets to Water Management" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210219T030000Z DTEND:20210219T033000Z DTSTAMP:20261011T152429Z UID:f7l9r21jc5bct520t2sml3hr94@google.com CREATED:20210209T000608Z DESCRIPTION:Noelia will talk about her work at the RSPCA and will be sellin g chocolate to raise money and help the animals in the shelter. Bruce will talk about what evidence there is (or not) for an interstellar civilizati on. LAST-MODIFIED:20210215T211106Z LOCATION:Duffield Lecture Theatre and ZOOM (host: Kenchington Goldsmith) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Noelia Martinez Rey and Bruce Peterson (RSAA) "Helping (at) the RSP CA and Evidence for an Interstellar Civilization ... or not." TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220419T010000Z DTEND:20220419T020000Z DTSTAMP:20261011T152429Z UID:lv0q7nfu6cq3irm9j9061ep1rs@google.com CREATED:20220214T233113Z DESCRIPTION:The source of about half of the heaviest elements in the Univer se has been a mystery for a long time. Although the general picture of ele ment formation is well understood\, many questions about the astrophysical details remain to be answered. Here I focus on recent advances in our und erstanding of the origin of the heaviest and rarest elements in the Univer se. LAST-MODIFIED:20220324T221216Z LOCATION:DLT & ZOOM (host: Shyam Menon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Enrico Ramirez-Ruiz (iUniversity of California Santa Cruz\, USA) "I nvited Colloquium: Cosmic alchemy in the era of gravitational wave astrono my" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210222T230000Z DTEND:20210223T000000Z DTSTAMP:20261011T152430Z UID:k2l8q63v1tqbegm0no0s5gp6fg@google.com CREATED:20210214T234108Z DESCRIPTION:In this thesis we study the dynamical scaling relation between galaxy stellar mass M* and the general kinematic parameter S_K = sqrt( K V rot^2 + sigma^2) that combines rotation velocity Vrot and velocity dispers ion sigma and have previously shown potential for combining galaxies of al l morphologies in a single scaling relation. For the construction of this scaling relation\, we make use of the data from the Sydney-AAO Multi-objec t Integral-field spectroscopy (SAMI) Galaxy Survey. We investigate the app licability of the logM* - logS_K scaling relation on galaxies ranging from elliptical galaxies to late-type spiral galaxies\, we also investigate th e effect of using either the stars or the gas component of galaxies as the kinematic tracer\, we optimise the combination method of Vrot and sigma by varying the K value in the S_K parameter\, and we also compare t he kinematic measurements from IFS survey to single-fibre spectroscopy wit h the intention of applying the findings to large-scaling single-fibre spe ctroscopy galaxy surveys. Where the galaxy scaling relation from SAMI reac hes its limit\, we introduce the Study of H_alpha from Dwarf Emissions (SH aDE)\, a high spectral resolution (R=13500) H_alpha integral field survey of 69 dwarf galaxies with stellar masses 10^6< M* < 10^9 M_sol. We extend the study of logM* - logS_K scaling relation to include low-mass dwarf gal axy in an attempt of making the scaling relation truly universal. We find that ... * *for more exciting content\, be sure to tune in to the talk. LAST-MODIFIED:20210215T211108Z LOCATION:Duffield Lecture Theatre and ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dilyar Barat (RSAA) "End-of-Thesis Talk: Unified Kinematic Scaling Relation in the Local Universe using Integral Field Spectroscopy Surveys" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200924T010000Z DTEND:20200924T013000Z DTSTAMP:20261011T152429Z UID:js1l5kvsd2ieg43uilejup71lg@google.com CREATED:20200909T060510Z DESCRIPTION:TBD LAST-MODIFIED:20200909T060510Z LOCATION:ZOOM 997 8534 1005 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dávid Guszejnov (UT Austin (USA)) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20211214T000000Z DTEND:20211214T010000Z DTSTAMP:20261011T152429Z UID:bcbfro2sev1le88khpeq1osji4@google.com CREATED:20210927T081614Z DESCRIPTION:Star formation is messy! It spans many orders of magnitude in s patial scale and involves a variety of interconnected physical processes: gravity\, magnetic fields\, radiation and turbulence. Forming stars announ ce their presence by emitting radiation and ejecting high-velocity materia l. However\, identifying this stellar feedback is challenging\, so feedbac k signatures have traditionally been identified 'by eye' - either by astro nomers or by citizen scientists. In this talk I will show that supervised convolutional neural networks (CNNs) trained using numerical simulations\, provide a more reliable\, quantitative and faster alternative to visual s earches. I will present the results of our 3D Convolutional Approach to St ructure Identification (CASI-3D) method applied to observational data to i dentify stellar bubbles and outflows. I will show that CASI-3D uncovers mo re feedback than visual searches and significantly changes our understandi ng of how young stars shape the physical properties of their environment. LAST-MODIFIED:20211206T050108Z LOCATION:ZOOM (host: Amit Seta) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Stella Offner (University of Texas Austin\, USA) "Invited Colloquiu m: Harnessing Machine Learning to Study the Life Cycle of Stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260305T000000Z DTEND:20260305T010000Z DTSTAMP:20261011T152430Z UID:a11dnjhkf8qgkvq09q90ph2e7k@google.com CREATED:20260122T234611Z DESCRIPTION:One third of luminous red giant stars exhibit "long secondary p eriods" (LSPs) - brightness variations that occur on timescales far longer than their primary pulsations. Despite decades of study\, the physical or igin of these variations remains unresolved. Competing explanations includ e hidden binary companions and large-scale oscillatory convective modes wi thin the stellar envelope. Distinguishing between these scenarios requires going beyond integrated light measurements and directly probing stellar s tructure at high angular resolution. In this seminar\, I will first presen t the development of Baldr\, a Zernike wavefront sensor designed to improv e adaptive optics correction for a new visitor instrument called Asgard at the Very Large Telescope Interferometer (VLTI). I will also describe my c ontributions to the Manhattan II vibration-control upgrade as part of the Gravity+ project\, aimed at reducing optical path fluctuations in interfer ometric observations on the large 8m class telescopes at the VLTI. Togethe r\, these efforts form part of a broader push toward higher-contrast\, spe ctral and spatial resolution at the VLTI. I will then turn to the long sec ondary period problem. Using multi-wavelength VLTI observations of a nearb y LSP variable\, I spectrally and spatially test two leading explanations for these variations: oscillatory convective dipole modes and a dusty bina ry companion. The interferometric observables allow us to discriminate bet ween large-scale photospheric asymmetry and circumstellar structure. Addit ionally\, I will present a newly identified photometric harmonic signature that provides an additional diagnostic: the phase relationship between th e fundamental and second harmonic differs systematically between the conve ctive dipole and binary scenarios. This offers a population-level test tha t can distinguish between the two mechanisms. Ultimately\, this work highl ights the synergy between instrumentation and astrophysics: by refining th e stability and resolution of interferometric observations\, we gain the l everage needed to disentangle competing physical mechanisms in evolved sta rs. LAST-MODIFIED:20260223T112109Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mike Ireland) \nZoom: http s://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Benjamin Courtney-Barrer (RSAA) "Sharpening the VLTI: Wavefront Sen sing with Asgard\, Vibration Control for GRAVITY+\, and Probing Evolved St ars (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160205T030000Z DTEND:20160205T032000Z DTSTAMP:20261011T152429Z UID:e072e6eetfrpl0hdu3fgov9i7s@google.com CREATED:20160105T041606Z DESCRIPTION:To celebrate the impending start of the Super Rugby season\, I ’ll spend a short while describing some of the more interesting aspects of the physics of rugby union. Hopefully I’ll manage to convince you all that not only is rugby union a fascinating sport\, but there are lots of opportunities to use some of the more out-of-left-field applications of ph ysics in developing teaching and lesson plans for high school and undergra duate students. No prior knowledge of rugby necessary - I will give a brie f overview of the rules of the game before launching into the science. LAST-MODIFIED:20160205T020104Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Fiona Panther (RSAA) "Odd Shaped Balls - The physics of Rugby" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170908T040000Z DTEND:20170908T050000Z DTSTAMP:20261011T152429Z UID:ijktcj6d3es4po0en6dofkuqvg@google.com CREATED:20170903T234604Z DESCRIPTION:Prior to the year 2005\, the number of known "classical" Milky Way (MW) dwarf satellite galaxies (−8 mag > Mv > −18 mag) remained twe lve. However from 2005 to the present\, thanks to the high quality photome tric data from extremely well designed systematic surveys such as Sloan Di gital Sky Survey (SDSS\; York et al. 2000) or Dark Energy Survey (DES\; Ab bot et al. 2005)\, the number of newly discovered faint dwarf satellites h as dramatically increased: Now we have almost forty dwarf satellite galaxi es in the halo of the Milky Way (e.g.\, 15 ultra-faint dwarfs from SDSS\; 17 dwarf galaxy candidates from the first two-year data set of DES)\, and there might be more than tens of faint dwarf satellites still waiting to b e discovered in the near future (Koposov et al. 2007\; Tollerud et al. 200 8). In this talk\, I will give a quick guided tour on these near-field dwa rf galaxy populations. For in-depth review\, we will take a look at severa l specific case studies on the properties of dwarf satellite galaxies in t he Local Group and nearby Sculptor filament. Finally I will close my talk by introducing the usage of "RR Lyrae variable stars" as a versatile probe to "old stellar halos" of nearby galaxies. LAST-MODIFIED:20170903T234604Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Soung-Chul Yang (Korean Astronomy & Space science Institute) "Prop erties of Near-Field Dwarf Galaxies Revealed by their 'Resolved' Stellar P opulations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200904T040000Z DTEND:20200904T043000Z DTSTAMP:20261011T152430Z UID:09ahvsgin7ggnct2h4bgfh3020@google.com CREATED:20200825T234607Z DESCRIPTION:Our speakers have 15 minutes each to talk about topics of their choice. The idea of the new FoF is to get to know the many individuals th at work under the same roof\, allow newcomers to find friends easily\, and find new friends or colleagues with similar interests and hobbies. So fee l free to talk about some of your most favourite adventures\, memorable St romlo anecdotes\, your hobbies\, your last COVID-DIY project\, your volunt ary activities outside of Stromlo or whatever you are passionate about. LAST-MODIFIED:20200904T002105Z LOCATION:ZOOM 997 8534 1005 (host: Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ben Wibking and Sven Buder (RSAA) "Personal FoF: Memes & Nobel Priz es" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231212T000000Z DTEND:20231212T013000Z DTSTAMP:20261011T152429Z UID:f8nmaqcuq3mflber6eebf7ihkk@google.com CREATED:20230726T065120Z DESCRIPTION:The WST project aim to study and built an innovative 10-m clas s wide-field spectroscopic survey telescope (WST) in the southern hemisphe re with simultaneous operation of a large field-of-view (5 sq. degree) and high multiplex (20\,000) multi-object spectrograph facility with both med ium and high resolution modes (MOS)\, and a giant panoramic integral field spectrograph (IFS). The ambitious WST top-level requirements place it far ahead of existing and planned facilities. In just its first 5 years of op eration\, the MOS will target 250 million galaxies and 25 million stars at medium resolution + 2 million stars at high resolution\, and 4 billion sp ectra with the IFS. WST will achieve transformative results in most areas of astrophysics. The combination of MOS and IFS spectroscopic surveys is one of the key aspects of the project. It is very attractive because of th e high complementarity between the two approaches. I will detail this inno vative point using the example of the MOS and MUSE surveys performed in th e CDFS region. The project aims to be the next major post-ELT project. It is supported by a large consortium of very experienced institutes plus ESO \, representing 9 European countries and Australia. LAST-MODIFIED:20231206T224109Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hiep Nguyen) \nZoom: https ://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Roland Bacon (CRAL - Observatoire de Lyon) "WST - The Wide Field Sp ectroscopic Telescope" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170814T233000Z DTEND:20170815T003000Z DTSTAMP:20261011T152429Z UID:8re9qdmsd5qfsifh2a8pbd6i70@google.com CREATED:20170811T002105Z DESCRIPTION:SCExAO is the premier high-contrast system in the Northern Hemi sphere. It provides high Strehl ratios at near-IR wavelengths (y-K band) w ith stable pointing and coronagraphs with extremely small inner working an gles\, optimized for imaging faint exoplanets and brown dwarfs very close to their host stars. In the visible\, it has several interferometric image rs which offer polarimetric and spectroscopic capabilities and spectral di fferential imaging. The RHEA spectrograph obtains spatially resolved\, hig h resolution spectroscopy in the visible for the first time. A recent add ition to the NIR arm is the CHARIS integral field spectrograph\, which is nearing the end of commissioning. We also describe our single mode fiber i njection which is used to feed a compact photonic spectrograph that could be useful for future ELT instrumentation. New capabilities on the horizon include post-coronagraphic spectroscopy\, nulling interferometry and an MK ID array. Here we present the SCExAO instrument\, give an overview of the latest science results and outline a path to the future. LAST-MODIFIED:20170811T011105Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Nemanja Jovanovic (Caltech) "SCExAO: Prototyping new technologies a nd techniques for terrestrial planet characterization on ELTs" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181109T034000Z DTEND:20181109T040000Z DTSTAMP:20261011T152429Z UID:f8fk05p552o9a4ud7jhtbtd4fc@google.com CREATED:20181017T030107Z DESCRIPTION:Multi-conjugate adaptive optics (MCAO) aims to overcome the pro blem of anisoplanatism\, allowing astronomers to access large regions of t he sky with good adaptive optics correction. A source of error unique to M CAO systems is the generalised fitting error\, which is a consequence of t he finite number of deformable mirrors available to correct for a continuo us turbulence profile. I will present my work on a pedagogical approach to understanding the generalised fitting error and demonstrate the use of su ch an approach in analysis of MCAO design. LAST-MODIFIED:20181030T031108Z LOCATION:Duffield Lecture Theatre (host: Zerjal) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jordan Smith (AITC) "A Pedagogical Approach to the Generalised Fitt ing Error in MCAO" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220412T050000Z DTEND:20220412T060000Z DTSTAMP:20261011T152429Z UID:cr832nel647gc8ce8o1s4imkfk@google.com CREATED:20220201T005113Z DESCRIPTION:The oldest\, most metal-poor stars we find in the Milky Way tod ay were born in pristine environments in the early Universe. They contain unique clues about the First Stars and the early formation and evolution o f our Galaxy. Most metal-poor stars are found in the Galactic halo\, but t he central halo overlapping with the Galactic bulge has often been avoided - it is challenging to identify metal-poor stars in this dusty\, crowded area of the sky. In this talk\, I will introduce the Pristine Inner Galaxy Survey (PIGS) which has reached unprecedented efficiency in finding very metal-poor stars in the Galactic bulge region. I will present recent PIGS results on the chemistry and the kinematics the metal-poor inner Galaxy\, and discuss what they can teach us about this ancient component of the Mil ky Way. Of particular interest in Galactic Archaeology are the carbon-enha nced metal-poor (CEMP) stars\, which are thought to be probes of the First Stars\, early chemical evolution and binary interactions. I will also pre sent some recent results on these CEMP stars. LAST-MODIFIED:20220403T220109Z LOCATION:DLT & ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anke Arentsen (Observatoire and University Strasbourg\, France) "In vited Colloquium: Galactic Archaeology with the oldest stars in the Milky Way" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251120T000000Z DTEND:20251120T010000Z DTSTAMP:20261011T152430Z UID:jcsrckfklsshh32smebdqoadt0@google.com CREATED:20251104T232112Z DESCRIPTION:The MCAO-Assisted Visible Imager and Spectrograph (MAVIS) will deliver high-resolution optical imaging and spectroscopic capabilities onc e it goes on sky at the ESO VLT in the early 2030's. As MAVIS moves toward s closure of its final design review (FDR) with ESO\, planning for the nex t steps of MAVIS are underway. In this talk\, I will provide an overview o f the MAVIS design and capabilities\, highlight some of the key science th at it aims to address\, and provide an update of the FDR process and its o utcomes. LAST-MODIFIED:20251109T225609Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Trevor Mendel (RSAA) "MAVIS at FDR and beyond" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250220T000000Z DTEND:20250220T010000Z DTSTAMP:20261011T152430Z UID:818indmbctsmcr3l6rejhhe5l4@google.com CREATED:20240927T022130Z DESCRIPTION:Integral field spectroscopy has allowed astronomers to probe th e local variations of properties within galaxies revealing the physical pr ocesses governing their local and global star formation activity. Large ga laxy surveys (e.g.\, MaNGA)\, as well as simulations (e.g.\, IllustrisTNG) \, have revealed radial trends in star formation with respect to the star- forming main sequence (SFMS). However\, unifying observational and theoret ical results is challenging. Utilizing adaptive optics with MUSE\, the MAG PI survey allows us to extend results in the local universe\, to a crucial time of 4 Gyr ago (z ~ 0.3) when simulations predict the greatest diversi ty in evolutionary pathways for central and satellite galaxies. Furthermor e\, MAGPI aims to bridge the gap between observations and simulations by c reating MUSE-matched mock data cubes from a suite of simulations as a mean s of direct comparison. In this end-of-thesis talk\, I will discuss the ph ysical processes governing the star formation activity of galaxies at z ~ 0.3 as seen with MAGPI and three cosmological simulations - EAGLE\, Magnet icum\, and IllustrisTNG. LAST-MODIFIED:20250212T113107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Emily Wisnioski) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Marcie Mun (RSAA) "Spatially resolved star formation and quenching: insights from observations and simulations (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160826T040000Z DTEND:20160826T042000Z DTSTAMP:20261011T152430Z UID:7p61mqpfesmhmu0evtha3ckrg8@google.com CREATED:20160825T103604Z DESCRIPTION:I briefly review recent developments in Galactic bulge science for non-bulge Astronomers. Recent years have seen a precision mapping of t he global parameters of the Galactic bulge such as the distance\, structur e\, extinction\, and metallicity-distribution function of the bulge. New a reas of investigation including chemical tagging\, chemodynamical families \, dark matter mapping\, and the search for the oldest stars in the Galaxy . In most of these areas\, and in Galactic bulge research as a whole\, ANU astronomers have played a leading role in defining\, redefining\, and lea ding bulge-related research. LAST-MODIFIED:20160825T103604Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:David Nataf (RSAA) "Galactic Bulge Review Talk for non-Bulge Astron omers" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260721T010000Z DTEND:20260721T020000Z DTSTAMP:20261011T152430Z UID:4is44e9clmtc5oo2f8pcu8ufc8@google.com CREATED:20260503T114413Z DESCRIPTION:In this talk I will discuss recent results and upcoming prospec ts for observing distant supernovae. I will begin with a brief review of p revious supernova surveys and the use of Type Ia supernovae in cosmology. Recent results suggest that the properties of dark energy may be changing with time\, in contrast to the cosmological constant explanation for dark energy. This provides new impetus for improving our measurements of the co smological parameters. I will describe prospects for supernova observation s from the Time Domain Extragalactic Survey (TiDES) which will use the 4MO ST instrument to obtain spectra tens of thousands of supernovae and their host galaxies discovered by the Rubin Observatory's Legacy Survey of Space and Time (LSST). I will also describe some early results and prospects fo r supernova science with the Euclid mission\, and discuss how the combinat ion of Rubin/LSST\, TiDES and Euclid will advance supernova cosmology. LAST-MODIFIED:20260716T040005Z LOCATION:Zoom or Duffield Lecture Theatre (host: Chris Lidman) \nZoom: http s://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Isobel Hook (U. Lancaster) "Supernova cosmology with Euclid\, Rubin and TiDES" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170526T040000Z DTEND:20170526T042000Z DTSTAMP:20261011T152429Z UID:9lo74fhgrpgn28cf8n1tu8plfo@google.com CREATED:20170511T064611Z DESCRIPTION:The SkyMapper Transient team launched a citizen science project last week. In this talk\, I will present the motivation behind this proje ct\, explain the process\, goals and early results. For some context\, in our survey\, the transient detection procedure includes pre-processing Sky Mapper images\, extracting sources\, classifying Real and Bogus candidates based on a machine learning algorithm and then visual confirmation by a m ember of our team. Now\, we incorporate in this last part citizen scientis ts which\, in less than 24 hours performed 30\,000 classifications! LAST-MODIFIED:20170523T133605Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anais Moller (RSAA) "Supernova Sighting" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151008T000000Z DTEND:20151008T010000Z DTSTAMP:20261011T152429Z UID:urum1v5hfd0oj5kcpm4he506u4@google.com CREATED:20150826T073108Z DESCRIPTION:The first stars\, known as Population III\, produced the first heavy elements\, thereby enriching their surrounding pristine gas. Howeve r\, all previous detections of metals in intergalactic gas clouds find a h eavy element enrichment at least 1/1000 times that of the solar environmen t\, which is higher than expected for remnants of Population III stars. In this talk I will describe our search for gas clouds with enrichment level s below this metallicity 'floor' of 1/1000th solar\, and outline the chall enges involved in finding such systems and measuring their metallicity. Ou r search has discovered a cloud at redshift 3.5 with metallicity 1/2500th solar\, the lowest value yet seen in a single cloud containing metals\, an d at the level expected for Population III remnants. I will discuss how re lative abundance measurements in this extremely metal-poor regime enable u s to test models of Population III star formation\, early gas enrichment a nd metal mixing. Finally\, I will summarise the prospects for finding simi lar systems in future surveys. LAST-MODIFIED:20151001T034107Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Neil Crighton (Swinburne) "Near Pristine Gas in the Early Universe" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151126T000000Z DTEND:20151126T010000Z DTSTAMP:20261011T152429Z UID:gn0cd67tnaopkvp3fjkdek0rug@google.com CREATED:20150902T015612Z DESCRIPTION:In 2011 the Nobel Prize in Physics was awarded "for the discove ry of the accelerating expansion of the Universe through observations of d istant supernovae". These Type Ia supernovae (SNe Ia) are also the dominan t contributor to iron-group nucleosynthesis and leading candidates for the elusive sites of high energy cosmic rays\, the p-process isotopes\, and t he positrons responsible for the 511 keV annihilation signal in our Galaxy . SNe Ia are thought to be thermonuclear explosions of white dwarf stars. Despite their ubiquitous importance to cosmology and astronomy\, their pro genitor systems and the explosion mechanism(s) are still largely unknown. This "SN Ia progenitor and explosion mechanism problem" is one of the grea t unsolved problems in astrophysics\, complicated by the fact that in rece nt years several unique sub-classes of SNe Ia have been described. I will discuss leading explosion models for SNe Ia\, present results from multi-d imensional hydrodynamical simulations of the final seconds of the star's l ife\, and highlight our quest to predict testable observables for the diff erent suggested progenitor and explosion mechanisms of SNe Ia. LAST-MODIFIED:20151122T101105Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ivo Seitenzahl (RSAA) "Modelling thermonuclear supernovae - explosi on simulations\, nucleosynthesis\, observables" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151112T000000Z DTEND:20151112T010000Z DTSTAMP:20261011T152429Z UID:ceibse0lshcvcb5qgf218o6kpc@google.com CREATED:20150830T042611Z DESCRIPTION:Sub-millimeter galaxies (SMGs) are the most dusty galaxies in t he high-redshift Universe\, with large infrared luminosities powered by in tense star formation activity. Although these galaxies are relatively rare \, they are a crucial population to understand the broad picture of galaxy evolution. SMGs contribute up to half of the star formation rate density at z>1\, and they are possibly the progenitors of the most massive galaxie s found in the local Universe. Their large amounts of dust make them ideal objects to study how dust forms in the high-redshift interstellar medium (ISM)\, and to study the interplay between star formation activity\, gas a nd dust. Up until recent interferometric observations with PdBI and ALMA\, the full characterisation of SMGs had been hindered by the large beams of single-dish observations that made it challenging to identify their optic al and infrared counterparts. The ALESS survey has followed-up a sample of 122 SMGs in the Chandra Deep Field South with ALMA\, allowing us to compi le the multi-wavelength spectral energy distributions (SEDs) of the most u nbiased and statistically reliable survey of SMGs to date. I will present a new calibration of the MAGPHYS SED modelling code that is optimised to i nterpret these ultraviolet-to-radio high-redshift observations simultaneou sly. With this code\, we derive statistically and physically robust estima tes of the photometric redshifts and physical parameters (e.g. stellar mas ses\, star formation rates\, dust masses) for the ALESS SMGs. Our modellin g shows that our energy balance technique still successfully reproduces th e observed SEDs in this highly obscured regime. To put the ALESS SMGs into context\, we compare their stellar masses and star formation rates with t hose of mass-selected galaxies at the same redshifts\, to understand where they are located in comparison to the observed 'star-forming main sequenc e' of galaxies. Finally\, I will discuss new avenues in understanding this population of galaxies with future ALMA programmes. LAST-MODIFIED:20151030T050107Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Elisabete da Cunha (Swinburne) "Understanding the most dusty galaxi es in the Universe with ALMA" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200924T010000Z DTEND:20200924T013000Z DTSTAMP:20261011T152430Z UID:3ajf1ohshc6oo4qeal8taa8kc8@google.com CREATED:20200908T060509Z DESCRIPTION:TBD LAST-MODIFIED:20200908T060509Z LOCATION:ZOOM 997 8534 1005 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dávid Guszejnov (UT Austin (USA)) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170209T000000Z DTEND:20170209T010000Z DTSTAMP:20261011T152429Z UID:e0f7p4u5ch5hhj67pj0hfna3m4@google.com CREATED:20170111T010605Z DESCRIPTION:The Dark Energy Survey aims to make the most precise test yet o f our cosmological model\, dark energy\, dark matter\, and our laws of gra vity. The four main probes we use are baryon acoustic oscillations\, weak lensing\, galaxy clusters\, and type Ia supernovae. We have just finishe d the fourth year of a five-year\, 525 night observing program and have al ready discovered thousands of supernovae\, are monitoring almost 800 activ e galaxies\, and by next year expect to have mapped approximately 300 mill ion galaxies. The wealth of data DES produces can do a lot more than just dark energy. Using reverberation mapping we’re aiming to measure how s upermassive black holes have evolved over the last 12 billion years\; usin g microlensing we’re looking for massive black holes in our galaxy\; usi ng the 3 square degree field and 570 Mega-pixels of the Dark Energy Camera we are following up gravitational wave discoveries\; and similarly watchi ng for Kuiper belt objects and potentially planet nine. This talk will gi ve an overview of DES and highlight the role of our 100 night spectroscopi c follow-up program\, OzDES\, that we are running at the Anglo-Australian Telescope. LAST-MODIFIED:20170123T032606Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tamara Davis (University of Queensland) "The Dark Energy Survey: mo re than dark energy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171124T030000Z DTEND:20171124T032000Z DTSTAMP:20261011T152429Z UID:t2h25701p4q2hq3a2ve87a1l94@google.com CREATED:20171101T231116Z DESCRIPTION:Recent research has shown that a planet’s ability to maintain liquid water and potentially host life depends on the type of star\, the planet’s density\, atmospheric composition and planet-star interactions. Additionally\, there are a variety of previously undefined factors such a s magnetic field\, albedo\, tidal locking\, impact events\, and plate tect onics that could also affect habitability. This thesis proposes to investi gate the effect these diverse parameters have on an exoplanet’s ability to sustain liquid water. I will analyse the interrelatedness of these fact ors and combine them into a code to estimate the degree of habitability of exoplanets in a variety of situations. In conjunction with the rapidly in creasing information from exoplanet databases expected within the next 2 y ears\, this research will help determine optimal targets for near-future g round- and space-based observations of planetary atmospheres and the poten tial detection of life in space. LAST-MODIFIED:20171115T230112Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sarah McIntyre (ANU) "A many-parameter approach to exoplanet habita bility" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180223T030000Z DTEND:20180223T032000Z DTSTAMP:20261011T152429Z UID:c5q0k1orgn3lbjef54be0d53ck@google.com CREATED:20180130T061612Z DESCRIPTION:The space committee will present plans for a renovation of lowe r Duffield\, including a timetable for the work. Comments on the plans fro m all school members are welcome\, but students and anyone whose office is in Duffield are particularly encouraged to attend. LAST-MODIFIED:20180131T001612Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:The Space Committee (RSAA) "Plans for the Renovation of Lower Duffi eld" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181108T000000Z DTEND:20181108T010000Z DTSTAMP:20261011T152429Z UID:3do44a8lmdekcaacsk9id1lh5o@google.com CREATED:20181105T001605Z DESCRIPTION:The origin of the stars with coherent velocities discovered in the solar neighborhood remains uncertain\, but their dynamics and evolutio n are key to understanding the dynamics of the Galactic stellar disk and u ltimately the history of the Milky Way. The Gaia satellite is currently ma pping the phase-space of a few million stars in the solar neighborhood. Ab out 3.5 million stars within ~5\,000 light-years from the Sun are identifi ed in streams\, bundles of stars that move together in the same direction with a velocity that is distinct from neighboring stars. The most prominen t among them is the Hercules stream. This study performs action and phase- space analysis to reveal the origin of this stream. We show that Hercules stars originate in the inner part of the Galaxy with stars that have the e ccentricity to reach the solar neighborhood. Contrary to previous theories \, our analysis\, based on a fully consistent simulation of the Milky Way\ , indicates that the Hercules Stream does not originate in resonances\, su ch as the Lindblad resonances\, or at co-rotation with spiral arms. We ant icipate the existence of a twin of the Hercules Stream being located in a patch with 180 degrees symmetry from the solar vicinity. Furthermore\, ou r model predicts that Hercules extends to stars moving faster than the Lo cal Standard Rest\, a prediction that can be tested by the upcoming releas es of Gaia\, Galah and SDSS-V. LAST-MODIFIED:20181105T232107Z LOCATION:Duffield Lecture Theatre (host: Ponomareva) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Elena D'Onghia (University of Wisconsin) "The Hercules Stream: reso nant stars visiting the Solar vicinity from the inner Galaxy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170420T010000Z DTEND:20170420T020000Z DTSTAMP:20261011T152429Z UID:7protahrkaj540qc6kl63jsbb0@google.com CREATED:20170409T233605Z DESCRIPTION:The ΛCDM model of cosmology predicts inevitable\, weak distort ions in the spectrum of the Cosmic Microwave Background (CMB) from that of a blackbody. However\, no such deviations have been measured to date. In this talk\, I focus on CMB spectral distortions arising from the cosmologi cal epochs of recombination and cosmic dawn &\; reionization (collectiv ely called EoR henceforth). A detection and measurement of these CMB spec tral distortions will enable a better understanding of the thermal and ion ization history of the Universe and help us probe redshifts that have neve r been directly observed thus far. I present a feasibility study for a gr ound-based detection of extremely weak\, ripple-like additive features in the CMB spectrum created by photons emitted during cosmological recombinat ion (900 < z < 7000). I introduce the Maximally Smooth (MS) function\, an algorithm to distinguish smooth foregrounds from the ripple like signal. Using synthetic spectra\, I demonstrate the efficacy of using MS function s over polynomials to separate foregrounds from the cosmological recombina tion signal. I also present GMOSS: Global model for the radio sky spectrum \, a physically motivated model of the low-frequency radio sky. Using GMOS S I investigate the spectral complexity expected in foregrounds and the ef fect of the same on detection of the global redshifted 21-cm signal from E oR (6 < z < 150). Once again\, I demonstrate the advantage of using MS fun ctions over polynomials to separate foregrounds from the global EoR signal in mock-sky spectra. I conclude the talk with a brief discussion on desig n criteria for radio-telescopes seeking to detect distortions in the CM B spectrum arising from the epochs of recombination through reionization. LAST-MODIFIED:20170410T035605Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mayuri S. Rao (RSAA) "On the detection of spectral distortions in t he CMB: recombination to reionization" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171201T020000Z DTEND:20171201T030000Z DTSTAMP:20261011T152430Z UID:olh2vkvcuh8qf168ekqdpi911g@google.com CREATED:20171129T005106Z DESCRIPTION:AGN are episodic in nature\, cycling through periods of activit y and quiescence. Their life-cycle is key for understanding the impact the y have on their host galaxy. In this talk\, I will present our studies aim ed at understanding the life-cycle and the role of the gas in a particular class of active nuclei: the radio-loud AGN. These studies make use of the exciting possibilities offered by the new generation of radio telescopes. For radio AGN\, their evolutionary stage (young\, adult\, dying\, restart ed) can be derived from the radio spectra and morphology\, in particular b y using the capabilities of new low-frequencies radio telescopes. Our sear ch of dying and restarted sources aims at understanding the time-scale of their evolution. The study of their duty-cycle has been done in the MHz-do main using the LOFAR radio telescope and the continuum surveys that are no w in progress. I will summarise the results and compare them with evolutio nary models of radio sources developed by our group. In the second part o f the talk\, I will present the results of our study on the effect of the radio plasma on the surrounding medium. Surprisingly\, and despite the ext remely energetic phenomena\, these effects can be traced by the cold compo nent of the gas using the atomic HI-21cm and the molecular (CO) components . I will describe the presence and characteristics of these fast and massi ve outflows and discuss the important connection between the evolutionary stage of the radio source and the effect of the radio plasma on the surrou nding ISM. The results presented represent and important starting point fo r the large surveys (in particular of HI absorption) that are about to sta rt with SKA pathfinders and\, in the near future\, with SKA. LAST-MODIFIED:20171129T005106Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Raffaella Morganti (ASTRON\, the Netherlands Institute for Radio As tronomy and Kapteyn Astronomical Institute\, University of Groninge) "Cold gas outflows and life-cycle of radio galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191011T030000Z DTEND:20191011T040000Z DTSTAMP:20261011T152429Z UID:gi25hr17e1m9asstc4pv7jntak@google.com CREATED:20191004T033105Z DESCRIPTION:NCI Australia is the nation's most highly integrated high-perfo rmance research computing environment\, providing world-class services to government\, industry\, and researchers. NCI User Support Manager Dr Roger Edberg will go into detail about Gadi\, Australia's newest and fastest su percomputer\, as well as discuss the ANU Merit Allocation Scheme (ANUMAS)\ , which is used to allocate compute time at NCI. LAST-MODIFIED:20191008T035605Z LOCATION:Duffield Lecture Theatre (host: Pingel) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Roger Edberg (National Computational Infrastructure) "NCI's newest and fastest Tier-1 high-performance supercomputer" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151106T030000Z DTEND:20151106T032000Z DTSTAMP:20261011T152429Z UID:2qbfvcjm4nel5fi8pt4r2p4blk@google.com CREATED:20151027T001106Z DESCRIPTION:For about forty years it has been known that something in the G alactic bulge is a prodigious source of positrons. The bulge outshines the disk in diffuse 511 keV positron annihilation radiation despite the fact that it is both less massive and has much less on-going star-formation. I will discuss -- and invite comments on -- our hypothesis that the positron s originate in the decay of radioactive 56Ni synthesised in a peculiar cla ss of underluminous Type I supernovae. These supernovae likely result from collisions between ~0.6 solar white dwarfs in perturbed binaries inhabiti ng the bulge. These white dwarfs originate from >10 Gyr old ~solar mass st ars which have only recently run through their main sequence lifetimes. In our scenario\, then\, the positrons are echoes of the last big burst of b ulge star-formation at z ~ 2. Similar WD-WD collisions\, occurring in the thick disk\, ultimately supply much of the 511 keV radiation emission exte nding along the Galactic plane. LAST-MODIFIED:20151102T114605Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Roland Crocker (RSAA) "A connection between the ancient bulge stars and a high-energy astrophysical anomaly" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240718T010000Z DTEND:20240718T020000Z DTSTAMP:20261011T152429Z UID:baeev9fiskm8qbka8p9mqopng8@google.com CREATED:20240711T064606Z DESCRIPTION:Recent JWST observations have unveiled a double-peak feature in the mass function of quiescent galaxies at high redshift (2.0 < z < 2.5). To explore the nature of these quiescent galaxies\, we utilize the Meraxe s semi-analytical galaxy-formation model. Our analysis reveals that active galactic nucleus feedback is the primary mechanism for quenching in massi ve quiescent galaxies. In contrast\, less massive quiescent galaxies exhib it stochastic star formation histories characterized by oscillating star f ormation rates. Intriguingly\, a similar pattern is also observed in star- forming galaxies. We quantify that\, in the low-mass end\, quiescent and s tar-forming galaxies may belong to a single population\, differing only in their observed episodes of star formation activity. Our results highlight the importance of temporal variations in star formation rates in understa nding the evolutionary pathways of galaxies. LAST-MODIFIED:20240711T064606Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Yuxiang Qin) \nZoom: https ://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Novan Saputra Haryana (Institut Teknologi Bandung) "Stochastic Star Formation Histories in Less Massive Quiescent and Star-Forming Galaxies a t High Redshift from Meraxes" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260409T013000Z DTEND:20260409T023000Z DTSTAMP:20261011T152430Z UID:6ujp6otaju3gnoi7vls5pfck9o@google.com CREATED:20260323T222609Z DESCRIPTION:Since 2010\, pioneering time-domain photometric missions (CoRoT \, Kepler\, and TESS) together with extreme-precision radial-velocity inst ruments (VLT/ESPRESSO and Keck/KPF)\, have revealed a rich spectrum of low -amplitude stellar variability driven by rotation\, convection\, and oscil lations. Among these phenomena\, stellar oscillations provide a powerful p robe of stellar interiors\, enabling unique inferences of fundamental prop erties and internal physics of stars. These constraints provide direct kno wledge of internal composition\, angular momentum transport\, convection\, and magnetism. These new constraints\, however\, also reveal significant deviations from our theoretical expectations. In this talk\, I will presen t a few recent technical\, observational\, and theoretical advances enable d by these data\, including applications to exoplanet host characterizatio n\, post-mass-transfer systems\, and mass-loss mechanisms in red giant sta rs. The coming decade--driven by ongoing and forthcoming facilities such a s TESS\, Rubin\, Roman\, PLATO\, and Earth2.0--will continue to revolution ize stellar\, Galactic and exoplanetary science. LAST-MODIFIED:20260323T222610Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Claudia Reyes) \nZoom: htt ps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Yaguang Li (U. Hawaii) "Probing Stellar Interiors in the Era of Pre cision Stellar Astrophysics" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210910T040000Z DTEND:20210910T043000Z DTSTAMP:20261011T152429Z UID:lv1rnv03cm7adetvgmtigs59t0@google.com CREATED:20210830T033607Z DESCRIPTION:The Feast-of-Facts are an informal open-mic format from RSAA me mbers for RSAA members. LAST-MODIFIED:20210830T033607Z LOCATION:ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Francois Rigaut (RSAA) "Optimising online live lecture delivery wit h OBS studio" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230817T060000Z DTEND:20230817T070000Z DTSTAMP:20261011T152429Z UID:tmjb2k2rc9lkmjlrsp213uq1q4@google.com CREATED:20230813T234107Z DESCRIPTION:The pursuit of understanding and detecting close-binary superma ssive black hole binaries (CB-SMBHs\, with subparsec mutual separation) is essential for progressing theories of galaxy formation and pinpointing po tential sources of nanohertz gravitational waves. This endeavor necessitat es an amalgamation of various observational techniques and simulation mode ls. Initially\, the current observational strategies employed for CB-SMBH detection are presented\, with an emphasis on the combination of diverse t ime-domain techniques. Following this\, the potential of comparing observa tional and simulated data of CB-SMBHs through the phase space of system dy namics is discussed. Highlighted next are quasar light curves from the Ver a C. Rubin Legacy Survey of Space and Time AGN Data Challenge database (Ri chards & Yu\, 2021\, 2022). The analysis concludes with an examination of specific features that might be indicative of microlensing events\, and a demonstration of the application of a time-domain technique for periodic v ariability mining\, which could be informative for simulations. It is envi saged that the synergy be-tween observational data and insights gleaned fr om simulations will accelerate the discovery and understanding of CB-SMBHs in the coming years. LAST-MODIFIED:20230813T234107Z LOCATION:TBD (host: Lilli) \nZoom: https://anu.zoom.us/j/83410388355?pwd=Qm 9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Andjelka Kovacevic (University of Belgrade) "Unraveling close binar y supermassive black holes: Interplay of time-domain observations and simu lations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231026T000000Z DTEND:20231026T013000Z DTSTAMP:20261011T152429Z UID:5dmeb22772kpu4bgc0727clkhs@google.com CREATED:20231019T131107Z DESCRIPTION:The evolution of wireless communication networks\, from present to the emerging fifth-generation (5G) new radio (NR)\, and sixth-generati on (6G) is inevitable\, yet propitious. The first part of the study evolve s around artificial intelligence (AI)/machine learning (ML) techniques to problems in spectrum management\, internet-of-things (IoT)\, physical laye r security\, and intelligent reflecting surface (IRS). Hence\, leading tow ards efficient\, secure\, and smart communication for complex wireless net works. Following on the prior research experience of applied AI/ML\, the s econd part of study highlights intelligence-based approaches for high dime nsional\, complex\, and dynamic problems in space networks. The current gl obal space traffic management must evolve into an updated\, automated\, an d adaptive system to meet the needs of the exponentially growing populatio n of Resident Space Objects (RSO) launched into orbit each year. However\, achieving this autonomous adaptability comes with complex space domain aw areness issues. Therefore\, more sophisticated models based on machine lea rning methods and deep neural networks are explored to ensure autonomous\, safe\, and secure navigation of space objects. LAST-MODIFIED:20231019T131107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: David Brodrick) \nZoom: ht tps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rabbia Saleem (UNSW Canberra) "Artificial intelligence/machine lear ning-driven wireless communication networks and space mission systems" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190320T000000Z DTEND:20190320T010000Z DTSTAMP:20261011T152429Z UID:ju3d06spmq0ekvr13k1tq0kfh8@google.com CREATED:20190314T233105Z DESCRIPTION:Since it's inception NASA has promulgated a vision of human exp loration that involves missions and outposts in Earth orbit\, the lunar su rface and Mars\, with supplies delivered from Earth's surface. When in-spa ce resources are considered\, they are assumed to be derived from the surf ace of the Moon or Mars\, with some consideration of Phobos and Deimos. I will describe the vision of TransAstra Corporation that promotes a scenari o in which humans live in space supported by asteroid resources beginning with the most accessible Near Earth Objects (NEOs). NEO resources are a co st-effective approach because they contain available\, exploitable extrate rrestrial material that are delivered to the inner solar system by gravita tional perturbations from the planets\, they have been naturally preproces sed into objects the ideal size for industrial operations\, and they conta in critical materials for cost-effective self-sustaining activities in spa ce. TransAstro corporation's proposed Sutter Survey spacecraft mission wil l demonstrate technologies critical to prospecting for the most promising NEOs for in-space resource utilization. LAST-MODIFIED:20190315T024105Z LOCATION:CSO Common Room (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Robert Jedicke (IfA Hawaii) "First Steps on the Path to Asteroid Mi ning" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150730T010000Z DTEND:20150730T020000Z DTSTAMP:20261011T152429Z UID:ciohj1qp3satk7s0h4cd0ccp3k@google.com CREATED:20150709T062107Z DESCRIPTION:Ladies and Gentlemen\, I would like to bring to your attention a momentous occasion. The first SkyMapper Ph.D. is (almost) complete! I kn ow some feared this day would never come\; for many students have come bef ore me\, and SkyMapper thwarted all their plans. I hope you'll all join me to celebrate SkyMapper's achievement by coming to my Final Thesis Talk. I 've spent the past 3.7 years searching for the oldest stars in the Milky W ay\, using SkyMapper photometry to hunt for metal-poor stars in the Galact ic bulge. Cosmological simulations of galaxy formation predict that the ve ry first stars formed at redshits z>15 in the largest overdensities\, whic h over time grew into the central regions of large galaxies such as the Mi lky Way. The remnants of these oldest stars should be observable today as metal-poor stars on tightly bound orbits close to the Galactic centre. The EMBLA survey made use of SkyMapper's unique filter system to hunt through more than 5 million stars in the Galactic bulge\, picking out metal-poor candidates to observe using AAOmega/2dF at the AAT. Three years of observa tions and 14\,000 stars later\, and we've found at least 10 stars with [Fe /H]<-3\, and using the latest OGLE astrometry\, we have been able to confi rm most of them lie on tightly bound objects. These could well be the olde st known objects in the Universe! LAST-MODIFIED:20150719T122106Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Louise Howes (RSAA) "Final Thesis Talk" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191015T000000Z DTEND:20191015T010000Z DTSTAMP:20261011T152429Z UID:4tbchk6ibkm5v6k7a06fgk0qik@google.com CREATED:20190801T011116Z DESCRIPTION:In this talk i describe new efforts to model radio AGN in a cos mological context using the SAGE semi-analytic galaxy model and a number o f large cosmological N-body simulations. Our new method tracks the physica l properties of radio jets in massive galaxies\, including the evolution o f radio lobes and their impact on the surrounding gas. Unlike most previou s efforts\, we now self consistently track the cooling-heating cycle that significantly shapes the life and death of many types of galaxies. Adding jet physics to SAGE adds new physical properties to the model output\, whi ch in turn allows us to make more detailed predictions for the AGN and gal axy populations\, and build customised AGN-focused mock survey catalogues for comparison with observations. LAST-MODIFIED:20191008T021106Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Darren Croton (Swinburne University) "The many lives of AGN: the fo rmation and evolution of radio jets and their impact on galaxy evolution" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220713T232000Z DTEND:20220714T034000Z DTSTAMP:20261011T152430Z UID:2le383lth0lk09k1v1ob69jdq4@google.com CREATED:20220705T052108Z DESCRIPTION:Schedule available at : https://anu365-my.sharepoint.com/:x:/g/ personal/u1057001_anu_edu_au/EX00_zlqLHdKpjR-rZiRGBABRC1a20hn3dM4wEmmIMyoT Q?e=DpJnwu LAST-MODIFIED:20220705T052108Z LOCATION:DLT & ZOOM (host: Tony Travouillon) \nZoom: https://anu.zoom.us/j/ 99785341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA HDR Students (RSAA) "RSAA HDR Students Thesis Proposals and An nual Reviews" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160308T000000Z DTEND:20160308T010000Z DTSTAMP:20261011T152429Z UID:4ej0pv7m8u6qp50ktndulas2b8@google.com CREATED:20160129T023114Z DESCRIPTION:Pulsars are great probes for exploring theories of gravitation and detection of gravitational waves. Observations of binary pulsar syste ms\, particularly the Double Pulsar system\, have provided the most string ent tests of relativistic gravity in strong-field situations\, confirming the accuracy of Einstein¹s general theory of relativity. Pulsar Timing Ar rays (PTAs) have as a main aim the detection and study of nanohertz gravit ational waves (GWs). With the exciting detection of audio-frequency GWs by the LIGO-Virgo team\, the challenge for PTAs now is to complement this de tection at nanohertz frequencies. Current limits on the background level o f nanohertz GWs are significantly constraining models for the evolution of supermassive black holes in the cores of distant galaxies. Future develop ments \, including progress on the International PTA and planned new instr uments will be discussed. LAST-MODIFIED:20160307T024105Z LOCATION:Duffield Lecture Theatre (host: Helga Denes) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dick Manchester (CSIRO) "Pulsars and Gravity" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261008T000000Z DTEND:20261008T010000Z DTSTAMP:20261011T152430Z UID:2b32g3n7pd44iirj3ur3rflsso@google.com CREATED:20260915T000009Z DESCRIPTION:The first generation of stars\, often called Population III (or Pop III)\, form from metal-free primordial gas at redshifts z ~ 30 and be low. They dominate the cosmic star formation history until z ~ 20-15\, at which point the formation of metal-enriched Pop II stars takes over. I rev iew current theoretical models for the formation\, properties and impact o f Pop III stars\, and discuss observational constraints. I argue that prim ordial gas is highly susceptible to fragmentation and Pop III stars form a s members of small clusters with a logarithmically flat mass function. Fee dback from massive Pop III stars plays a central role in regulating subseq uent star formation\, but major uncertainties remain regarding its immedia te impact. Direct observations of Pop III stars in the early Universe rema in extremely challenging\, whereas stellar archeological surveys allow us to constrain both the low-mass and the high-mass ends of the Pop III mass distribution. Observations suggest that most massive Pop III stars end the ir lives as core-collapse supernovae rather than as pair-instability super novae. I also speculate about the formation of supermassive stars\, which under very specific circumstances can get as massive as several 100.000 so lar masses. They have observable signatures similar to Little Red Dots\, a nd can become the seeds of the supermassive black holes observed in the hi gh-redshift Universe. LAST-MODIFIED:20260915T000009Z LOCATION:Zoom or Duffield Lecture Theatre (host: Christoph Federrath) \nZoo m: https://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ralf Klessen (U. Heidelberg) "The First Stars: Formation\, Properti es\, and Impact" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141121T030000Z DTEND:20141121T032000Z DTSTAMP:20261011T152430Z UID:kuh8gd9d6l1ve7ugjmnnr1jp1o@google.com CREATED:20141117T060336Z DESCRIPTION:Sophisticated chemical evolution models have been successful in reproducing the current abundance gradient in our Milky Way and other nea rby galaxies\, but these models produce dramatically conflicting predictio ns for galaxies at intermediate distances and in the early universe. One m ajor problem with this work is that metallicity calibrations have been hin dered by large discrepancies\, particularly between diagnostics that use d ifferent sets of emission-lines\, and these discrepancies are not well und erstood. Fortunately\, large integral field spectroscopic surveys offer t he first large local datasets to resolve this issue and in this project\, 6 different metallicity calibrations were applied to a star-forming galax ies from the SAMI galaxy survey. LAST-MODIFIED:20141119T225619Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Diane Salim (RSAA) "Metallicity Calibrations and Gradients in SAMI Star-forming Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150213T030000Z DTEND:20150213T032000Z DTSTAMP:20261011T152429Z UID:7uv9o6r97frmg4660i5knl3b14@google.com CREATED:20150119T064109Z DESCRIPTION:The evolution of galaxies is driven by the intricate power play between magnetically driven turbulence and the mass and gravity of its co mprising gas and dust\, a system which governs the formation of stars in t he dense cores of the interstellar medium's giant molecular clouds. The ra te at which such stars form is hence a pivotal quantity in tracing a galax y's fundamental properties and distribution of matter and activity. Howeve r\, the parameterisation of the column density of star formation (Sigma_SF R) of a molecular cloud of gas in a galaxy has been a highly debatable top ic for more than two decades\, with historical parameterisations including the mean column density of available gas (Sigma_gas)\, as well as the rat io between Sigma_gas and the mean free-fall time (time it would take the m olecular cloud to collapse under its own gravitational attraction) of the medium. Both these attempts at describing the Sigma_SFR have resulted in s ignificant intrinsic scatter\, and follow-up analysis of these models via computer simulations have determined that the observed scatter may be prim arily attributed to the physical variations in the Mach number of the turb ulence. This results in separate relations for the star formation rate de pending on the Mach number of the medium\, differing from each other by up to an order of magnitude. This discrepancy has shed light on the need for a more global description of the behaviour of the molecules in a gas clou d\, illuminating the incompetency of a mere mean of the gas column density and free-fall time in accurately predicting the star-formation rate of a galactic medium. Instead\, a cloud of gas would enclose molecules with a d istribution of these two fundamental parameters\, and the probability dens ity function of volume densities and corresponding free-fall times as well as the Mach number of turbulence need be considered when endeavouring to construct a universal law for star formation rate. Addressing such concern s\, we incorporate the distribution of probability densities to formulate a more universally encapsulating star formation rate law. We apply resolve d observations from Milky Way molecular clouds to identify this relationsh ip\, and discern a correlation in which the star formation rate is equal t o ~0.4% of molecular gas mass per multi-free-fall time. Employing our newl y discovered relationship\, we make sonic Mach number predictions for kpc- scale observations of Local Group galaxies as well as unresolved observati ons of local and high-redshift disk and starburst galaxies that do not hav e reliable estimates for such values. LAST-MODIFIED:20150202T051609Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Diane Salim (RSAA) "An Even More Universal Star Formation Law in Mo lecular Clouds and Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150512T010000Z DTEND:20150512T020000Z DTSTAMP:20261011T152429Z UID:n17e2r4nr79oigud5i4gc23t74@google.com CREATED:20150506T020607Z DESCRIPTION:Despite many decades of progress in understanding the evolution of star formation and stellar populations in galaxies\, we have still fun damental questions that have remained unanswered. These include: how do st ars cluster in galaxies\, and how do these structures evolve in time? Do w e actually have a 'clustered' and 'diffuse' mode of star formation? When s tructures remain bound (star clusters)\, how do their populations evolve? Is the stellar Initial Mass Function universal? How are popular star forma tion rate indicators affected by the recent star formation history of a ga laxy? How are these effects impacting our understanding of the scaling law s of star formation with the gas reservoir? The answers to these questions inform our theories for the evolution of galaxies through cosmic times. M any of these questions are being addressed by recent projects that combine UV and high-angular resolution with the Hubble Space Telescope\, and whic h I will describe together with the results they have obtained so far. LAST-MODIFIED:20150508T093107Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Daniela Calzetti (UMass Amherst) "Star Formation Across Space" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170516T010000Z DTEND:20170516T020000Z DTSTAMP:20261011T152429Z UID:1hve4s34v0hm86rdbd3neuik84@google.com CREATED:20170131T232113Z DESCRIPTION:ITSO symposium LAST-MODIFIED:20170131T232113Z LOCATION:Duffield Lecture Theatre (host: Joao) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:ITSO symposium (ITSO) "ITSO symposium" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201016T030000Z DTEND:20201016T033000Z DTSTAMP:20261011T152429Z UID:mru8uen5316mrcdvpgfnv54u40@google.com CREATED:20201008T052109Z DESCRIPTION:The new FoF format is like an Open Mic: Our speakers have 15 mi nutes each to talk about topics of their choice. The idea of the new FoF i s to get to know the many individuals that work under the same roof\, allo w newcomers to find friends easily\, and find new friends or colleagues wi th similar interests and hobbies. So feel free to talk about some of your most favourite adventures\, memorable Stromlo anecdotes\, your hobbies\, y our last COVID-DIY project\, your voluntary activities outside of Stromlo or whatever you are passionate about. Science talks (about a scientific to pic/question that you are interested in) are also welcome\, but be mindful of your audience (astronomers\, students\, engineers\, professional staff ). LAST-MODIFIED:20201012T002114Z LOCATION:ZOOM 997 8534 1005 (host: Menon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Michael Ireland and Francois Rigaut (RSAA) "Observation and instrum entation used for the Physics Nobel Prize 2020 research (Black Holes)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190403T000000Z DTEND:20190403T010000Z DTSTAMP:20261011T152429Z UID:6i1i2gtnv29o60uog67bg4pn1s@google.com CREATED:20190317T232612Z DESCRIPTION:Globular clusters are the relics of extreme star formation in h igh-redshift galaxies. Their enormous potential as tracers of high-redshif t galaxy formation is broadly recognised\, but concrete applications of th is link have remained out of reach. The key missing ingredient has been to construct an end-to-end model for star cluster formation and evolution in a cosmological context. I will present results from the E-MOSAICS project \, in which we carry out fully self-consistent\, cosmological zoom-in hydr odynamics simulations of the co-formation and evolution of globular cluste rs and their host galaxies. This work has led to two crucial insights. The first is that the formation of young massive clusters and old globular cl usters can be described by a single modelling framework\, showing that glo bular clusters are the relics of regular star formation in high-redshift e nvironments. The second is that the high-pressure formation environment of globular clusters has shaped a wide range of their present-day properties \, enabling their direct use as tracers of high-redshift galaxy growth. I will show how globular cluster metallicities\, masses\, ages\, kinematics\ , and spatial distributions provide a new and exciting window for reconstr ucting the host galaxy merger history\, distinguishing between in-situ and ex-situ galaxy growth\, and probing the conditions of cloud-scale star fo rmation and feedback at high redshift. Specifically\, I will demonstrate t he power of unifying cluster formation and destruction processes across co smic time by using the E-MOSAICS simulations to derive the formation and a ssembly history of the Milky Way\, culminating in the reconstruction of it s merger tree. I will conclude with a discussion of current shortcomings o f these simulations\, and how we are combining observational\, theoretical \, and numerical work to remedy these through improved subgrid models for star formation\, feedback\, and globular cluster formation and evolution. LAST-MODIFIED:20190324T003608Z LOCATION:CSO Common Room (host: Oh) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Diederik Kruijssen (Heidelberg University) "Globular clusters revea ling the formation and assembly history of the Milky Way" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151216T000000Z DTEND:20151216T010000Z DTSTAMP:20261011T152429Z UID:tnukh7hq255oquknaa4uafcmt4@google.com CREATED:20151110T031617Z DESCRIPTION:Subaru Telescope is an 8.2m telescope on top of Maunakea\, Hawa ii. The telescope has suites of state-of-art instruments which cover almos t entire wavelength range in optical to mid-infrared and various spectral resolutions. We will briefly introduce some scientific highlights using Su baru Telescope to show its capabilities. Recently a new prime focus optica l imager Hyper Suprime-Cam (HSC) started its science operations. HSC has 1 .5 deg. field-of-view with excellent image quality\, and the international collaboration team is conducting a large survey using HSC with 300 nights in total which aims at covering about 1\,400 sq. degrees. We will also in troduce some new instrument projects such as Prime Focus Spectrograph (PFS ) which employs 2\,400 fibres over 1.3 sq. degree FoV\, new exoplanet inst ruments\, a wide-field near-infrared instrument concept with Ground-Layer Adaptive Optics on which we are working with AAO team\, and the strategic plan of Subaru Telescope toward 2020s. We would like to discuss the possib ilities of extending collaborations with Australian astronomical community . LAST-MODIFIED:20151215T224605Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Nobuo Arimoto & Ikuru Iwata (Subaru Telescope NAOJ) "Subaru Telesco pe: current status and strategy toward future" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141125T000000Z DTEND:20141125T010000Z DTSTAMP:20261011T152430Z UID:h6qq66up93r4f779p0j6gln3bs@google.com CREATED:20141117T060337Z DESCRIPTION:Dark matter forms the foundation for all cosmic structure\, and its annihilation\, decay\, or other particle interactions have the potent ial to affect early structure formation by injecting energy into local gas . I will discuss the status of the quest to identify dark matter\, major u nsolved problems relevant to the abundance and structure of dark matter ha los\, and how dark matter annihilation energy can affect the binding of ga s within the earliest cosmic structures. [Papers: arXiv: 1309.7783\, 1411. 3783] LAST-MODIFIED:20250925T231021Z LOCATION:Duffield Lecture Theatre (host: Richard Scalzo) \nZoom: https://an u.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Katie Mack (University of Melbourne) "Dark Matter in the Cosmic Con text" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250516T040000Z DTEND:20250516T050000Z DTSTAMP:20261011T152429Z UID:ij48ujbq8ub7f38a2f6o113dsg@google.com CREATED:20250507T215607Z DESCRIPTION:The Unstable Neutral Medium results from the multiphase nature of the Interstellar medium\, in order to have both stable warm and cold ph ases an unstable transitionary phase must exist between them. Despite havi ng known of this phase through modelling for decades it has appeared less abundant than expected when conducting observations. Here we present one o f the deepest observations of 21cm HI in absorption to date. Using these o bservations and gaussian decomposition techniques we are able to detect so me of the warmest HI components published. This provides much needed data to a scarcely sampled phase of the Interstellar medium which will improve our understanding of how gas transitions between these phases its abundanc e and temperature. LAST-MODIFIED:20250507T215607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Naomi McClure-Griffiths) \ nZoom: https://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQ T09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Nicholas Killerby-Smith (RSAA) "A sensitive search for the Unstable Neutral Medium (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20211202T000000Z DTEND:20211202T003000Z DTSTAMP:20261011T152429Z UID:arb981m7aacm57ei7kn6uq3frk@google.com CREATED:20211014T034612Z DESCRIPTION:During the next decade\, the Vera C. Rubin Observatory will obt ain high-resolution optical images of the Southern Sky at unprecedented de pths. Rubin public alert stream will communicate the detection of up to 10 million potential transient objects every night. Given the large data vol umes of Rubin\, it will be crucial to select promising events and automati cally connect them with follow-up facilities and science teams. I will int roduce the Fink broker which has been selected to receive the full Rubin a lert stream. Fink is built on high-end technology that enables real-time s election of promising transients using machine learning and combining info rmation from catalogues and surveys. Fink is already processing ZTF data a nd have ongoing collaborations in a wide science range. I will discuss the potential of connecting Rubin time-domain data with Australian facilities and the opportunities for cosmology and multi-wavelength and messenger as tronomy. LAST-MODIFIED:20211201T224607Z LOCATION:DLT and ZOOM (host: Sven Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anais Moeller (Swinburne) "Fink broker enabling time-domain science with Rubin Observatory" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191114T020000Z DTEND:20191114T040000Z DTSTAMP:20261011T152429Z UID:hu0j0cgl92c8dmojfvi0ctk940@google.com CREATED:20191111T090604Z DESCRIPTION:Masters students will give their thesis talk. All Welcome and e ncouraged to attend. LAST-MODIFIED:20191112T144706Z LOCATION:Duffield Lecture Theatre (host: Wolf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Masters thesis talks (RSAA) "Masters thesis talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151020T000000Z DTEND:20151020T010000Z DTSTAMP:20261011T152429Z UID:d4jlpferfmveggd90vc17vvbog@google.com CREATED:20151007T053608Z DESCRIPTION:I will present some new results pertaining to our current under standing of the structure and substructure of the stellar components of th e Milky Way\, including possible relations between them and insight gained into Galaxy evolution. LAST-MODIFIED:20151009T055608Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rosemary Wyse (Johns Hopkins University) "The Structure and Substru cture of the Milky Way Galaxy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190523T010000Z DTEND:20190523T020000Z DTSTAMP:20261011T152429Z UID:hkmg0cdaqoovfe32ro83cmds0c@google.com CREATED:20190517T073604Z DESCRIPTION:Metal-poor stars can provide important diagnostics on the masse s and nucleosynthetic yields from the first generation of stars\, the univ ersality of the initial mass function\, and on the early formation stages of galaxies. However\, these are rare stars and have required special tec hniques to find them\, ranging from narrow-band photometry (e.g.\, SkyMapp er and Pristine) to blind spectroscopic surveys (e.g.\, SDSS and LAMOST). Several hundred metal-poor stars are now known in the Galactic halo and n earby dwarf galaxies\, and we are starting to uncover these objects in the Galactic disk and bulge\, the latter being the preferred location for the formation of the first stars. I will discuss some of the recent highlight s from the search for and analyses of the most metal-poor stars\, particul arly from the Pristine survey team. These results range from carbon-enha ncements\, binary fractions\, and r-process element abundances\, to some o f the unexpected kinematics found in their Gaia DR2 data. LAST-MODIFIED:20190517T073604Z LOCATION:Duffield Lecture Theatre (host: Cultinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kim Venn (University of Victoria) "Metal-poor stars and results fro m the Pristine Survey" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190917T010000Z DTEND:20190917T020000Z DTSTAMP:20261011T152429Z UID:vi8vpch89g2kmthij3j5nbjm60@google.com CREATED:20190624T011111Z DESCRIPTION:Fast stars are the smoking guns of extreme stellar collisions a nd explosions\, but seeing a fast star in your catalogue is more likely a sign that your methodology has fallen down. I will give a brief history of fast stars from the first detection of proper motion to the discovery of stars escaping our Milky Way. These latter stars are known as hypervelocit y stars and the focus of this talk will be on the huge open questions conc erning them. Why are they moving so fast? Where do they come from? What st ars can be hypervelocity stars? The Gaia space telescope has been transfor mative and I will present both the successes and failures of the hunt for hypervelocity stars with Gaia. I will discuss the discovery of white dwarf s moving at 1000s of km/s and the proof of a massive star having been ejec ted from the Large Magellanic Cloud at 870 km/s. I will walk you through t he mystery of the highest radial velocity star in Gaia and introduce the c rucial discovery of a star in the halo moving at 1700 km/s that can be tra cked back to the centre of the Milky Way. LAST-MODIFIED:20190909T033104Z LOCATION:Duffield Lecture Theatre (host: Monty) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Douglas Boubert (University of Oxford) "Hypervelocity discoveries w ith the Gaia space telescope" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240502T010000Z DTEND:20240502T023000Z DTSTAMP:20261011T152429Z UID:gfkiqhsj2dfbrariadlctktkm4@google.com CREATED:20240220T233632Z DESCRIPTION:Giant molecular clouds (GMCs) are the birthplaces of stars. Mul tiple physics mechanisms including gravity\, magnetic fields\, and radiati on interplay within these clouds\, and set the initial conditions for star formation. However\, the exact role of each mechanism is still unclear\, largely due to observational biases arising from projection\, chemical\, a nd excitation effects. Simulations and simulated observations and therefor e necessary for realistic interpretation of observations of the GMC format ion and evolution processes. This thesis focuses on building a comprehensi ve picture of the structure of GMCs using this approach. The first part of the thesis provides a theoretical model that can predict the 3d density s tructure of GMCs that are observed only in projection\, and applies it to nearby GMCs. The second part of the thesis examines measurements of magnet ic field strengths\, and points out that due to chemical and excitation bi ases the role of magnetic fields in GMC formation is less important than s uggested by earlier interpretations of observations. The final part of thi s thesis reveals a significant discrepancy between two main star formation rate measurement methods\, young stellar object counting and recombinatio n lines\, and demonstrates how this discrepancy changes with local GMC con ditions. LAST-MODIFIED:20240421T234609Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Zipeng Hu (RSAA) "Make the clouds less cloudy: modelling the ISM wi th simulations and synthetic observations (End of thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250204T000000Z DTEND:20250204T010000Z DTSTAMP:20261011T152430Z UID:t4cropj3q89aerrcd6t47pu128@google.com CREATED:20250106T225606Z DESCRIPTION:MANIFEST (Many-Instrument Fiber System) will be one of the grou ndbreaking instrument on the Giant Magellan Telescope (GMT)\, empowering a stronomers to study the universe in incredible detail. This advanced fiber -optic positioning system allows the GMT to connect with multiple instrume nts and capture light from multiple objects simultaneously across the vast field of view of the GMT. For Australian astronomy\, MANIFEST opens new o pportunities to explore distant galaxies and stars with unmatched precisio n and resolution. This talk will delve into MANIFEST innovative design and capabilities\, its integration with the GMT and implications for advancin g cosmology\, stellar evolution\, and our quest to understand the galaxy e volution. LAST-MODIFIED:20250113T014608Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Maya Jablonska) \nZoom: ht tps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tayyaba Zafar (Macquarie U.) "MANIFEST: A Versatile Multi-Interface Instrument for the Giant Magellan Telescope" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240627T010000Z DTEND:20240627T020000Z DTSTAMP:20261011T152429Z UID:tr92d1a01p9nt2b7640ebr6reo@google.com CREATED:20240415T051633Z DESCRIPTION:In the context of hierarchical galaxy assembly\, both globular clusters and dwarf galaxies serve as indispensable probes of the formation of our Milky Way. The chemical composition of stars within these ancient structures plays a pivotal role in constraining their chemical enrichment history. Each possesses its own chemical peculiarities\; for instance\, dw arf galaxies contain stars with low [alpha/Fe] compared to Galactic halo o bjects of the same metallicity. Meanwhile\, globular clusters house multip le stellar populations characterized by their light element abundances. To date\, most studies have focused almost exclusively on elemental abundanc es\, however\, nucleosynthesis operates at the isotopic level. This thesis will discuss how Mg isotope ratios shed light on both the accreted dwarf galaxy component of our Milky Way and the light element enhanced populatio ns within globular clusters. This reveals contributions from supernova and low-mass stars that cannot be discerned through element abundances alone. LAST-MODIFIED:20240624T043109Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Madeleine McKenzie (RSAA) "Nucleosynthesis at the isotopic level: h ow chemical abundances enhance our understanding of globular clusters and dwarf galaxies (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260212T000000Z DTEND:20260212T010000Z DTSTAMP:20261011T152430Z UID:sacrfhup1sfrramq1umvrnp6a8@google.com CREATED:20260122T000207Z DESCRIPTION:Stellar streams are one of the most powerful tracers to determi ne the mass and profile of the Milky Way as well as constrain the properti es of dark matter. In this talk\, I will discuss two ongoing spectroscopic programs to study the stellar streams in our Milky Way and highlight a fe w latest scientific results from these two programs. The Southern Stellar Stream Spectroscopic Survey (S5)\, started in 2018\, is the first systemat ic program pursuing a complete census of known streams in the Southern Hem isphere using the fiber-fed AAOmega spectrograph on the Anglo-Australian T elescope. The Milky Way Survey of the Dark Energy Spectroscopic Instrument (DESI)\, on the other hand\, is a recently started 5-yr spectroscopic pro gram in the Northern Hemisphere. We are entering an extremely data-rich er a in the next decade\, with full 6D+chemistry information on dozens of ste llar streams\, to shape our understanding on the chemo-dynamical evolution of the Milky Way\, as well as the nature of dark matter. LAST-MODIFIED:20260127T024608Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Melissa Ness) \nZoom: http s://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ting Li (U. Toronto) "Tidal Streams in the Era of Spectroscopic Sur veys" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210205T030000Z DTEND:20210205T033000Z DTSTAMP:20261011T152429Z UID:64e02bm30pc6l89mfi6jkgbd54@google.com CREATED:20210105T061108Z DESCRIPTION:We start the weekend with our new open-mic talks. LAST-MODIFIED:20210129T030106Z LOCATION:ZOOM and Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Matthew Colless\, Jonah Hansen (RSAA) "Science & Beauty and Interns hip at HEO Robotics" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190530T010000Z DTEND:20190530T020000Z DTSTAMP:20261011T152429Z UID:0arl3doi6af76rs52r8h1b3s00@google.com CREATED:20190320T091119Z DESCRIPTION:Stellar kinematics is a fossil record of galaxy formation and e volution. In particular\, the fraction of stars on near-circular orbits co mpared to the fraction of stars on kinematically hotter and geometrically rounder orbits\, speaks directly to the slowly accretion of gas flow or vi olent merging/feedback of the galaxies’ past. On the other hand\, stella r chemistry is conserved\, thus a timing clock of the galaxies' formation. The combination of stellar kinematics and stellar chemistry may provide u s unprecedented information to understand the formation of galactic struct ures. The IFU surveys\, like CALIFA\, MaNGA\, SAMI\, provide us informatio n integrated along the line-of-sight\, including kinematic maps\, mean age and metallicity maps. Using the orbit-superposition Schwarzschild method\ , we have been able to derive the internal stellar orbit distribution for a sample of 300 CALIFA galaxies\, which form an orbit-based ‘dynamical H ubble sequence’. Decomposition of galaxies is thus possible based on the ir orbit distribution. We further developed a population-orbital model by tagging age and metallicities to the orbits in the Schwarzschild model. Wh ich has been applied to FCC 167 with MUSE observations as a first case-stu dy. Based on the model\, we obtain the distribution of stellar orbits on p hase space of angular momentum vs. stellar age\, thus are able to present the formation history of different galactic structures in a quantitative w ay. LAST-MODIFIED:20190520T093608Z LOCATION:Duffield Lecture Theatre (host: Oh) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ling Zhu (Shanghai Astronomical Observatory) "Disentangling galaxy formation history through a population-orbit superposition model" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200924T010000Z DTEND:20200924T013000Z DTSTAMP:20261011T152429Z UID:903bs54j7vkjln7vmrc4mlieig@google.com CREATED:20200909T205109Z DESCRIPTION:TBD LAST-MODIFIED:20200909T205109Z LOCATION:ZOOM 997 8534 1005 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dávid Guszejnov (UT Austin (USA)) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151120T030000Z DTEND:20151120T032000Z DTSTAMP:20261011T152429Z UID:icr659f2pmnd4me5stmuuvg3l4@google.com CREATED:20151029T022611Z DESCRIPTION:For around forty years\, astrophysicists have observed the anni hilation of positrons in the Galaxy at a prodigious rate. Around 2 x 10^43 positrons annihilate every second\, giving rise to diffuse emission of so ft 511 keV gamma rays\, which have been mapped most recently by the SPI sp ectrometer on board ESA’s INTEGRAL satellite observatory. Despite years of study and the ubiquity of positron annihilation in astrophysical enviro nments\, these long-standing observations are hard to explain. The fact th e Galactic bulge far outshines the disk in annihilating positrons which ar e injected into the ISM at low energies makes the source of the positrons difficult to identify\, as the main source of such positrons are prima fac ie located in the Galactic disk. I will present my PhD thesis proposal: An ancient stellar source of the Galactic bulge positron excess\, and descri be the work we intend to carry out to investigate the plausibility of the positrons originating in sub-luminous supernovae associated with the ancie nt stars of the Galactic bulge. LAST-MODIFIED:20151117T024605Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Fiona Panther (RSAA) "Thesis proposal talk: An ancient stellar sour ce of the Galactic bulge positron excess" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160909T040000Z DTEND:20160909T050000Z DTSTAMP:20261011T152430Z UID:vn9hp6208cradd9lqu1i94skh8@google.com CREATED:20160902T014109Z DESCRIPTION:The evolution of galaxies is directly linked to the gas reservo irs surrounding them\, known as the circumgalactic medium (CGM). CGM gas f lows into galaxies along filaments and forms new stars. Eventually stars e xplode as supernovae and gas is ejected\, feeding back into the CGM. This feedback loop continuously affects the morphology\, mass growth and chemic al make-up of galaxies. Understanding this gas cycle is key to determining how galaxies evolve. In this talk\, I will present our latest results and provide an overview of our current understanding of the CGM-galaxy relati onship. I'll further show how these gas flows directly affect well known e mpirical relations that are commonly used to interpret how galaxies evolve . LAST-MODIFIED:20160904T234605Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Glenn Kacprzak (Swinburne University) "The Circumgalactic Medium an d its Role in Galaxy Evolution" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250519T033000Z DTEND:20250519T043000Z DTSTAMP:20261011T152429Z UID:8h5vlmpkoe98j2d29p0me7llmc@google.com CREATED:20250515T024606Z DESCRIPTION:1:30pm-2:00pm: Allison Blum\, "[OIII] as a Proxy for Virial Mas s: A Single Epoch Approach Unaffected by AGN Variability"\; 2:00pm-2:30pm: Adrian Lehane\, "Modelling chemical abundances of dwarf galaxies to study the Milky Way halo" LAST-MODIFIED:20250516T023207Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Helmut Jerjen) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:ASTR3005 Student Talks (RSAA) "ASTR3005 Student Talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150911T010000Z DTEND:20150911T020000Z DTSTAMP:20261011T152430Z UID:if10qeqcaqeimi8pc57ecg7iao@google.com CREATED:20150822T134609Z DESCRIPTION:Diffuse interstellar bands (DIBs) and atomic lines are observed as interstellar absorptions in GALAH and other massive spectroscopic stel lar surveys. By observing a given DIB toward many stars which are nearly i n the same direction\, but at different distances\, one can reconstruct ab sorption sites along the line of sight. Joining observations in many direc tions on the sky finally leads to their spatial distribution\, while measu rement of radial velocities adds the fourth dimension for each interstella r absorption. In special cases a complete velocity vector can be reconstru cted which makes the dynamical picture of the interstellar medium equivale nt to the one collected for stars by Gaia. LAST-MODIFIED:20150902T000105Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tomaz Zwitter (University of Ljubljana) "Dynamical interstellar med ium with Gaia and ground-based massive spectroscopic stellar surveys" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201027T000000Z DTEND:20201027T010000Z DTSTAMP:20261011T152429Z UID:7pgsi3isnee9ilkctipsthql60@google.com CREATED:20200916T021114Z DESCRIPTION:There are two potentially paradigm-shifting trends taking place in astronomical research. The first is the move away from individuals or groups of observers obtaining data for a narrow scientific experiment\, to wards the use of surveys\, large datasets and catalogs that enable a wide range of topics to be studied. The second trend is the recognition that th e astronomical and astrophysical community of researchers must become more inclusive in order to realize the best scientific innovation and producti vity. In this talk\, I will discuss how leveraging these trends provides the field with a unique opportunity for both to be mutually supportive in the quest to advance discovery! I will also show how the Community Science and Data Center (CSDC) at NOIRLab is supporting this effort. LAST-MODIFIED:20201019T231607Z LOCATION:ZOOM 997 8534 1005 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dara Norman (Community Science and Data Center/NOIRLab\, USA) "Invi ted Colloquium: Can Big Data Lead an Astronomical Inclusion Revolution?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160901T010000Z DTEND:20160901T020000Z DTSTAMP:20261011T152430Z UID:5snr0n7875j5giku1fde77frv0@google.com CREATED:20160725T002614Z DESCRIPTION:I recently had the rare opportunity to fly on NASA's Stratosphe ric Observatory For Infrared Astronomy (SOFIA)\, a Boeing 747 with a 2.5m telescope that flies above 40\,000 ft and most of the atmospheric water va pour that absorbs far-infrared radiation. In this talk I will outline what it took to get SOFIA off the ground\, and give an inside look at what obs erving with the world's only flying telescope is like. LAST-MODIFIED:20160725T003116Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Stuart Ryder (AAO) "A Night on SOFIA" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230525T010000Z DTEND:20230525T020000Z DTSTAMP:20261011T152429Z UID:anua1ldcig778c7j30v3pk3lrk@google.com CREATED:20230506T091108Z DESCRIPTION:Flows with high Knudsen number\, due either to low density or s mall scale\, can present significant challenges for experimental measureme nts. Laser diagnostics\, when used appropriately\, can assist both in vis ualising and in making measurements in such flows. In this talk I will pr esent some measurement techniques we have developed for low-density plasma s and hypersonic flows\, and will present a proposal for measurements usin g electron beam fluorescence at the very low densities characteristic of l ow-earth orbit. LAST-MODIFIED:20230524T005108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hiep) \nZoom: https://anu. zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sean O'Byrne (UNSW Canberra) "Measurements in low-density flows (As tralis seminar series)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150227T030000Z DTEND:20150227T032000Z DTSTAMP:20261011T152429Z UID:cmnkte83adj9e1l5i5i4bjtabc@google.com CREATED:20150223T003105Z DESCRIPTION:Transits are key to our understanding of exoplanets. In this ta lk\, I will describe a novel technique we have developed to measure the sh ape and rotation of exoplanets from their Kepler transit light curves. Jup iter and Saturn have about 10 hour days. This rapid rotation causes their shapes to become oblate. Do other planets have similar rotation rates? I p resent the first search for rotationally oblate gas giants in the Kepler d ataset\, and a tentative detection for the oblateness of Kepler-39b\, a br own dwarf in a 21-day period orbit. LAST-MODIFIED:20150223T065604Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:George Zhou (RSAA) "Measuring the rotational oblateness of exoplane ts with Kepler" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181030T000000Z DTEND:20181030T010000Z DTSTAMP:20261011T152430Z UID:5j6r14d15ak1oe1gndi87462j8@google.com CREATED:20180822T015207Z DESCRIPTION:Astronomers will increasingly rely on AI and machine learning c ode to sift and sort through the mountains of data that are now upon us\, growing in volume and complexity by the day. As the diamonds in the rough are identified\, it will still come down to careful and close inspection t o disentangle the natural secrets within. Astrophysical data is inherently multi-parameter\, with the spatial dimensions at the core centre of imagi ng\, spectral\, time-domain and simulation data. With the dawn of powerful GPUs and virtual-reality (VR) technology we are no longer limited to flat screens to emulate 3-D cosmic views. Leveraging the significantly improve d VR headsets with the powerful programming tools developed for visualisat ion gaming\, the time is right for astronomers to deploy such technology t o interrogate and interact with complex multidimensional data. Here I will present the development work in our visualisation laboratory - using HTC VIVE-PRO and Samsung Odyssey VR tech\, the Unreal Engine C++ and Unity pro gramming C# foundations - that supports our research on galaxy evolution\, cosmic web large scale structure\, galaxy-galaxy interaction simulations\ , and gas/kinematics of nearby galaxies. The Big Data Era ushered in by th e SKA and its Pathfinders challenges our storage\, calibration\, reduction and refinement methods\, and it also demands innovative ways to interroga te the data at intuitive - visualisation - levels necessary for new discov ery. LAST-MODIFIED:20181022T011608Z LOCATION:Duffield Lecture Theatre (host: Oh) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Thomas Jarrett (University of Cape town) "The Future is Here\, Astr ophysics with Virtual Reality" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230201T000000Z DTEND:20230201T010000Z DTSTAMP:20261011T152429Z UID:5umsgluokit7hpk0vjnqi3fipo@google.com CREATED:20230125T071607Z DESCRIPTION:The presence of atmospheric turbulence degrades the image quali ty of ground-based telescopes. Adaptive Optics (AO) is a powerful method t o partially correct the wavefront distortion caused by atmospheric turbule nce in real-time. MAVIS is a visible band\, general purpose MCAO instrumen t with ambitious goals and a tight error budget\, motivating the research of an optimised control scheme. In this talk\, we present the development of the optimised Learn and Apply (L&A) method - a model-driven\, predictiv e MCAO supervisory solution. We derive a generalised model that combines l ow-order and high-order measurements from different wavefront sensors to e nable a global reconstruction. Based on that\, we develop a second order s tochastic algorithm for the pseudo-real-time identification of atmospheric turbulence profile (Learn)\, and an integrated controller that simplifies the MCAO control into a single loop (Apply). Finally\, we implement the o ptimised L&A into a closed supervisory loop with realistic error sources t aken into consideration. As shown by the numerical simulation results\, ou r control scheme brings substantial improvement to the system performance\ , and only introduces marginal increase in real-time computational load. LAST-MODIFIED:20230130T001108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Takafumi Tsukui) \nZoom: h ttps://anu.zoom.us/j/99785341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Hao Zhang (RSAA) "Laser tomography in high-order adaptive optics" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220722T040000Z DTEND:20220722T043000Z DTSTAMP:20261011T152429Z UID:hstluo4759gg0rfvgegfmst2ms@google.com CREATED:20220718T143705Z DESCRIPTION:JWST is now operating and has the mission has already delivered spectra of transiting exoplanet atmospheres that are significantly advanc ing the field. In parallel\, ground-based observations of exoplanets with large facilities have also matured and providing detailed pictures of exo- worlds. I present comparative exoplanetology programs that aim at characte rising planetary systems transiting nearby stars through the observations of their atmospheres. Our findings on the atmospheric composition and phys ical properties provide insights into the formation and evolution of plane tary systems and enhance our understanding of our own Solar System's forma tion. LAST-MODIFIED:20220718T143705Z LOCATION:DLT & ZOOM (host: TBD) \nZoom: https://anu.zoom.us/j/99785341005?p wd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jean-Michel Desert (University of Amsterdam) "Transiting exoplanet atmospheres in the JWST era" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260813T010000Z DTEND:20260813T020000Z DTSTAMP:20261011T152430Z UID:18lfu79a2d1n136ljm8asrarhs@google.com CREATED:20260629T120013Z DESCRIPTION:ULTIMATE-Subaru is the next-generation instrument suite for the Subaru telescope. It comprises a Ground Layer Adaptive Optics system and a Wide Field Imager. At ANU\, we’re responsible for two out of four work packages of GLAO: the Laser Guide Star Facility and the Wavefront Sensor module. Four laser beams are launched from the telescope’s central secti on\, each paired with a corresponding Laser Guide Star Wavefront Sensor (4 units) working together with 4 Natural Guide Star Wavefront Sensors. I’ ll present the project’s status\, ready to transition from design to rea l hardware and begin production. LAST-MODIFIED:20260716T040015Z LOCATION:Zoom or Duffield Lecture Theatre (host: N/A) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Noelia Martinez (RSAA) "ULTIMATE-Subaru GLAO enters production phas e at the ANU" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250909T010000Z DTEND:20250909T020000Z DTSTAMP:20261011T152429Z UID:n9khj1bt443koms516jjke4ue0@google.com CREATED:20250520T123620Z DESCRIPTION:The long-period radio transients are a newly-discovered class o f Galactic radio sources that produce pulsed emission lasting tens of seco nds to several minutes\, repeating on timescales of tens of minutes to hou rs. Such cadence is unprecedented\, and there is currently no single emiss ion mechanism or progenitor that can explain the observations\, which incl ude complex polarisation behaviour\, pulse microstructure\, and activity w indows that range from hours to decades. Could they be ultra-long period m agnetars\, and connected to the phenomenon of Fast Radio Bursts? Could the y be white dwarf pulsars\, defying the expectations of the magnetic field evolution of these stellar remnants? In this talk I will describe the ten discoveries made so far\, informative simulations of their evolution\, the potential physical explanations\, and the prospects for detecting more of these sources in ongoing and upcoming radio surveys\, that will help unco ver their true nature. LAST-MODIFIED:20250909T030105Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Eric Muller) \nZoom: https ://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Natasha Hurley-Walker (Curtin U) "The enigmatic long-period radio t ransients" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230822T010000Z DTEND:20230822T023000Z DTSTAMP:20261011T152429Z UID:s8ookn9nciei85jck48t4horp0@google.com CREATED:20230724T065613Z DESCRIPTION:NFW would have us believe that dark matter dominates the centre s of galaxies\, but this has never been observed in massive galaxies\, and certainly not in the Milky Way and M31 where baryons dominate out to at l east 10 kpc in radius. So what about early galaxies? Can we find NFW cusps here that were subsequently wiped out? This is looking increasingly unlik ely as well -- baryons may have always dominated the inner parts of galaxi es. I will examine implications of baryon domination that will be testable with JWST deep fields (e.g. JADES) in the coming months. LAST-MODIFIED:20230724T065613Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark) \nZoom: https://anu. zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Joss Bland-Hawthorn (U. Sydney) "Do baryons dominate the centres of high-redshift galaxies?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180608T040000Z DTEND:20180608T042000Z DTSTAMP:20261011T152429Z UID:8d5o6vict20k363o5emc2shsoc@google.com CREATED:20180518T002112Z DESCRIPTION:As near-infrared instrumentation comes into widespread use in e xtragalactic astronomy\, we can observe the rest-frame properties of galax ies in over-dense or proto-cluster environments. These observations provid e valuable information on the early affects of environmental density on ga laxy evolution\, and provide constraints on advanced cosmological simulati ons such as FIRE and Illustris-TNG. The ZFIRE survey has spectroscopically confirmed two such proto-clusters\, at z=2.095 in COSMOS\, and at z=1.65 in UDS\, using the MOSFIRE instrument on Keck 1. In the COSMOS cluster\, w e measure gas kinematics from the Hydrogen alpha emission line\, and find no cluster-wide effects on kinematics\, and a minor correlation between ir regular morphology and angular momentum. In addition\, we measure gas-phas e metallicity on the group scale\, attempting to measure indications of ga s accretion or metal enrichment in the merging groups that define this pro to-cluster. We determine if and when environmental density plays a role in early galaxy properties\, which evolutionary processes are affected\, and at what scale these processes act on members of over-dense regions at z~2 . LAST-MODIFIED:20180606T003611Z LOCATION:Duffield Lecture Theatre (host: Battisti) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Leo Alcorn (Texas A&M) "The Proto-cluster Environment at z~2: Kinem atics\, Metallicity\, and Merging Groups" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240402T000000Z DTEND:20240402T013000Z DTSTAMP:20261011T152429Z UID:lj6c6bpa7ial2kffjm9m2t28j4@google.com CREATED:20231212T120225Z DESCRIPTION:If you stir a hot plasma\, where does the energy go? This quest ion -- relatively simple for cooler gas in thermal equilibrium (the energy becomes heat) -- remains mysterious and non-intuitive\, depending sensiti vely on the plasma's parameters and even how it is stirred. It is also cru cial for understanding many high-energy astrophysical systems. For example \, in solar-coronal heating\, the partition of energy between ions and ele ctrons\, and between heat in different directions\, can change the efficie ncy of solar-wind acceleration by large factors\; in black-hole accretion\ , low-luminosity states (like those observed by the EHT) are possible only if most of the energy reaches ions\, not electrons\, creating a two-tempe rature plasma. In this talk I will explore plasma heating via turbulence. A particular focus will be the solar wind and corona\, which provide us wi th a resource unrivalled in most of the rest of astrophysics: a natural wi nd tunnel where measurements can be taken in situ. Later this year\, NASA' s Parker Solar Probe (PSP) spacecraft will fly through regions closer to t he Sun than ever before (0.046AU)\, yielding precision measurements from i nside some of the most extreme conditions in our solar system. I will disc uss some of the theoretical approaches and new insights that have led to r ecent progress in understanding heating across a variety of systems\, and how we can test them using PSP and other spacecraft. LAST-MODIFIED:20240318T222610Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jono Squire (U. Otago) "Our natural plasma wind tunnel: learning ab out black-hole accretion from the solar wind" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210706T010000Z DTEND:20210706T020000Z DTSTAMP:20261011T152429Z UID:lmuoduq14hp4hhpt4f9kqn3d4s@google.com CREATED:20210210T061118Z DESCRIPTION:The chemical evolution of the Universe is governed by the nucle osynthesis contribution from stars\, which in turn is determined primarily by the initial stellar mass. In this talk I want to focus on one key outs tanding question related to stellar nucleosynthesis and chemical enrichmen t: the problem of binary stars. We know that most stars in the Universe ha ve a gravitationally bound companion but this is not reflected in the stel lar yields used as input into most models of Galactic chemical evolution. Type Ia supernovae are historically the one exception because these explos ions can only happen in a binary system. Nowadays we also need to consider neutron star mergers as a source of heavy r-process elements. How else ca n binary evolution affect stellar evolution and the resultant stellar yiel ds? I discuss results from new binary population synthesis models of accre ting white dwarfs and discuss new projects which will examine the effect o f binary evolution on the advanced evolutionary phases of low and intermed iate-mass stars. LAST-MODIFIED:20220618T125714Z LOCATION:ZOOM and Duffield Lecture Theatre (host: Sven Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Amanda Karakas (Monash University) "Invited Colloquium: Galactic ch emical evolution and the problem of binary stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250318T020000Z DTEND:20250318T030000Z DTSTAMP:20261011T152430Z UID:qknvvkbjkkitpr3ugfr9r2i3ng@google.com CREATED:20250317T014106Z DESCRIPTION:Brady will describe the current state of ground-based\, gravita tional-wave astronomy and the prospects for the future. He will present hi ghlights from LIGO-Virgo-KAGRA observations including recent findings on c ompact object mergers. Gravitational waves from black-hole-binary mergers are now being detected about twice per week and astronomers are eagerly aw aiting the next multi-messenger event. Over the next decade\, a sequence o f upgrades will more than double the amplitude sensitivity of the most sen sitive gravitational-wave detectors and increase the rate of compact binar y detections by about a factor of ten. Brady will discuss how the improved signal-to-noise ratio will also enable unprecedented measurements of mass es\, spins\, and other properties of black holes and neutron stars in bina ry systems. The upgrades may also bring the discovery of other gravitation al-wave sources. The talk will end with a discussion of future directions for ground-based gravitational-wave astronomy\, highlighting the opportuni ties for multimessenger astronomy in the early 2030s and how operations of the current detector network can dovetail with operations of next-generat ion facilities. NOTE THAT THIS TALK WILL NOT BE BROADCAST ON THE STANDARD RSAA SEMINARS LINK\, AND WILL INSTEAD BE AVAILABLE ON ZOOM WITH MEETING ID 852 6712 3867\, PASSWORD 829438. LAST-MODIFIED:20250317T014106Z LOCATION:ZOOM or Finkel Lecture Theatre\, JCSMR Building (host: N/A) \nZoom : https://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Patrick Brady (University of Wisconsin-Milwaukee) "Gravitational-wa ve physics and astronomy: progress & prospects" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150731T040000Z DTEND:20150731T043000Z DTSTAMP:20261011T152429Z UID:2rj6jmoq6e89n8allusfrjki7g@google.com CREATED:20150525T123114Z DESCRIPTION:Two members of the RSAA Access and Equity Committee\, Adam Thom as and Celine d'Orgeville\, have been trained as part of the ALLY program\ , which supports LGBTI+ people in the workplace. Come along to the Feast o f Facts talk on 31 July to learn about the surprising nature of the divers ity that's out there and why LGBTI+ inclusion is important for individuals and organisations. LAST-MODIFIED:20150721T101608Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Celine D'Orgeville & Adam Thomas (RSAA) "ALLY program at RSAA" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190225T004000Z DTEND:20190225T012000Z DTSTAMP:20261011T152429Z UID:d44juvdapf5alse0sj2467vajg@google.com CREATED:20190110T003815Z DESCRIPTION:The development and application of cutting-edge technologies is a major part of the historical and current success of ESO Instrumentation . Although some technologies have significant in-house programmes\, most d evelopments occur outside either in industry or with partner-institutes an d universities. In this talk I will give a brief overview of some of the r ecent and ongoing developments in areas such as adaptive optics\, detector s and ELT sub-systems. LAST-MODIFIED:20190217T005108Z LOCATION:CSO Common Room (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mark Casali (ESO) "Instrumentation Technology at ESO" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260623T013000Z DTEND:20260623T023000Z DTSTAMP:20261011T152430Z UID:pe7v67881h9mqivuo3bhb3q2ss@google.com CREATED:20260503T114410Z DESCRIPTION:The journey to 6000 exoplanets began with giant planets found v ia the\nradial-velocity method. In the three decades since\, advancements have made\nEarth-size planet discoveries commonplace. While much attention is being\ngiven to ever-smaller planets\, I argue that our forgotten gian t friends are\ndue for a renaissance. To find and truly understand Earth- like planets\, we\nmust first understand Jupiter-like planets.\n\nEvidence from our own Solar system\, alongside long-term monitoring of\nKepler and TESS systems\, supports a growing consensus that cold\, outer\ngiant plan ets are correlated with small\, inner rocky worlds. Yet\, the\nexact caus e of this correlation\, and how the presence or absence of an\nouter giant dictates the properties of inner planets\, remain unknown. Key\nopen que stions include: How do the mass\, radius\, and atmospheric\ncompositions o f inner planets vary with a giant companion? And how does an\nouter giant influence the orbital architecture and multiplicity of these\ninner world s?\n\nWhile over 200 cold giant planets have been discovered via radial ve locity\,\ntheir true masses and 3-dimensional architectures remain unconst rained due\nto the limitations of the technique. Pairing radial velocitie s with Gaia\nastrometry offers a solution to unlock these systems\, alread y yielding new\nrevelations for known Jupiter analogs. I present a resear ch program\ndesigned to address these critical science gaps\, leveraging A ustralian\nfacility access to the Magellan and Giant Magellan Telescopes. This \nproject\, in collaboration with key international partners\, promi ses to\ndeliver unprecedented new understanding of the composition\, archi tectures\, \nand atmospheres of planets orbiting nearby stars using the la test\nhigh-precision data from ground and space-based telescopes. LAST-MODIFIED:20260605T070006Z LOCATION:Zoom or DLT (host: Tomasz Rozanski) \nZoom: https://anu.zoom.us/j/ 82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rob Wittenmyer (U. Southern Queensland) "A reunion of old friends: Giant planets in the Gaia era" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170301T000000Z DTEND:20170301T010000Z DTSTAMP:20261011T152429Z UID:t3mh94ua1pkoiofq6cfo3j2voc@google.com CREATED:20170206T222608Z DESCRIPTION:I will review efforts being made to detect and explore the neut ral hydrogen signal from the first billion years of the universe. Neutral hydrogen acts as a tracer of the growth of structure\, and encodes key inf ormation about the astrophysical conditions in the intergalactic medium wh ile the first ionising sources illuminated the universe. The spatial distr ibution and evolution of hydrogen can be used to constrain models of the g rowth of the first structures\, their radiation fields and source type\, a nd physical conditions of the gas medium. Despite this promise of great di scovery\, detection of the weak cosmological signal is a major challenge f or current and future low-frequency radio telescopes. Beyond the simple we akness of the signal\, the need to extract information from contaminated d ata observed through complex instrument\, is proving a major hurdle. I wil l describe the progress we have made with the Murchison Widefield Array\, leading to the design of the future SKA-Low\, to extract this information\ , and prospects for the future of EoR science. I will also describe exciti ng prospects for connecting this information to the low redshift universe\ , providing a full history of the evolution of structure in the universe. LAST-MODIFIED:20170208T115609Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Cathryn Trott (Curtin University) "Exploring the Epoch of Reionisat ion with current and future low-frequency radio telescopes" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230919T010000Z DTEND:20230919T023000Z DTSTAMP:20261011T152429Z UID:n52u216jfcgvbpmgtditbk42to@google.com CREATED:20230806T233119Z DESCRIPTION:Ultra Diffuse Galaxies (UDGs)\, have the sizes of giant galaxie s but the luminosities of dwarfs. So far\, simulations are not able to re produce all of their characteristics and observations suggest multiple for mation pathways. Many UDGs are overabundant in globular star clusters for reasons which are likely linked to their early formation times. Globular clusters allow the determination of UDG properties\, such as stellar popul ations and total masses\, that are otherwise very challenging to obtain fo r these low surface brightness objects. I'l describe our observations of UDGs in a variety of environments and with a range of fundamental properti es. I'll draw comparisons with simulations of dwarf galaxy and UDG formati on and describe predictions from simulations of their globular cluster sys tems. LAST-MODIFIED:20230917T234105Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hiep) \nZoom: https://anu. zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jean Brodie (Swinburne University) "The Origins of Ultra Diffuse Ga laxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210506T010000Z DTEND:20210506T020000Z DTSTAMP:20261011T152429Z UID:u28vkqgptmmj7hh6qjikalrcjo@google.com CREATED:20210325T011114Z DESCRIPTION:David will visit to give us an overview of CGA. He and colleagu es arrive at 10:30 for morning tea in Possum Hall. LAST-MODIFIED:20210427T024607Z LOCATION:Duffield Lecture Theatre and ZOOM (host: Sven Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:David McClelland (CGA at ANU) "Joined Seminar of CGA and ANU: An Ov erview of CGA" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150501T040000Z DTEND:20150501T044000Z DTSTAMP:20261011T152429Z UID:ip6vdm3jbe950gsvpjso10q4ss@google.com CREATED:20150129T040633Z DESCRIPTION:This tour is for people who have wondered what goes on behind t he locked doors in Possum Hall. This walking Feast of Facts will give you an insiders view and brief you of some of the astronomy and space projects the AITC is supporting\, and our aspirations for the future. You don't ne ed to don a clean suit but you will need to leave all food and drink behin d. LAST-MODIFIED:20150421T023607Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Naomi Mathers (RSAA) "What's Hiding Behind the Locked Doors? An Ins iders Tour of the Advanced Instrumentation and Technology Centre (AITC)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171129T220000Z DTEND:20171130T060000Z DTSTAMP:20261011T152430Z UID:9diojn97bms4va1gnme0328qlc@google.com CREATED:20170811T014115Z DESCRIPTION:Mt. Stromlo Student Seminars LAST-MODIFIED:20171120T233107Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mt. Stromlo Student Seminars (ANU) "Mt. Stromlo Student Seminars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260922T010000Z DTEND:20260922T020000Z DTSTAMP:20261011T152430Z UID:0g8fnj9an5u5fgmaqmcd6of3jo@google.com CREATED:20260605T021624Z DESCRIPTION:High-precision cosmological surveys are expected to deliver mea surements at sub-percent precision. In order to ensure we correctly interp ret these data\, we need to be sure that our theoretical model is accurate . Within general relativity\, the standard cosmological model adopts many approximations for gravitational interactions and geometry. These approxim ations have served us well so far\, but as our error bars grow smaller and smaller we need to know at exactly what point they fail. Numerical relati vity is a computational method which allows us to relax simplifying assump tions for gravity and geometry and consider the full interaction of matter and space-time as described by general relativity. I will provide some ba ckground on the use of numerical relativity for cosmological simulations b efore discussing the generation of synthetic observables in these simulati ons which are also free from common simplifying assumptions. This from-fir st-principles framework is exciting in its potential to quantify exactly w hen our approximations fail and might begin to bias our cosmological const raints. LAST-MODIFIED:20260820T020014Z LOCATION:Zoom or Duffield Lecture Theatre (host: Daniela Montes Doria) \nZo om: https://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Haley McPherson (U. Melbourne) "Numerical relativity as a tool for precision cosmology" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141128T032000Z DTEND:20141128T034000Z DTSTAMP:20261011T152429Z UID:sltekgi1ch6qm6is4l0bcdbajg@google.com CREATED:20141117T060339Z DESCRIPTION:In the recent years\, the interest on studying the outer parts of spiral galaxies is rising. To better understand galactic formation and evolution\, simulations and observations are working together to understan d the different behaviours that the disc light distribution displays in th e outer parts of these systems. During this talk I will speak about my cur rent work as part of my PhD project focused on the stellar content in thes e outer regions. We have implemented a new methodology to analyse the stel lar content from spectroscopic data based on the state-of-art full spectru m fitting techniques (using GANDALF and STECKMAP). We have tested such met hodology on the LMC bar region\, where high quality integrated spectra can be obtained as well as Color-Magnitude Diagrams reaching the oldest Main Sequence Turnoff. I will also show the first results that we are obtaining when applying such methodology to the smallest galaxies observed in the C ALIFA (Sanchez et al. 2012) and SAMI (Croom et al. 2012) surveys. I will c ompare such observational results with what recent simulations (RaDES\, Fe w et al. 2012) suggest. I will finish showing the effect that satellite ac cretion has on shaping the chemical and kinematic properties of the outski rts of simulated galaxies\, as well as the effect of such accretion in the shape of the stellar age profile as shown by the RaDES set of galaxies. LAST-MODIFIED:20141119T225624Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tomas Ruiz-Lara (University of Granada) "Unveiling the stellar cont ent in the outer parts of spiral galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251021T000000Z DTEND:20251021T010000Z DTSTAMP:20261011T152430Z UID:i4dt9etrambdenqe9dkde6k1mk@google.com CREATED:20250520T123622Z DESCRIPTION:It's never been easier to launch something into space. It's nev er been cheaper to get a spacecraft. In this new era of space accessibilit y\, the astronomical community has an exciting opportunity to advance spac e sciences through small payloads and telescopes on small sats. In this ta lk\, I will describe a bit about the current landscape\, provide some exam ples from a cost and schedule perspective\, and describe my own involvemen t in several smaller missions\, both at the concept stage and being built. I will touch on how missions of this type can contribute to science quest ions across astronomy\, with a focus on my own interests in CGM science an d molecular cloud lifetimes and formation\, and how those interests can be explored now with smallsats. I will focus especially on the Aspera Missio n\, a $20M USD mission funded by NASA to observe nearby galaxy circumgalac tic media via extreme ultraviolet OVI emission. LAST-MODIFIED:20250923T021611Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Arunima) \nZoom: https://a nu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Erika Hamden (U Arizona) "Discovery potential in the era of Small S ats" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230804T040000Z DTEND:20230804T043000Z DTSTAMP:20261011T152429Z UID:7dn7dh593aqnt4o936h5fnen24@google.com CREATED:20230703T013112Z DESCRIPTION:AAL will be presenting a member update to ANU\, introducing AAL and describing who we are and what we do for those who haven't come acros s us before (while also providing a refresher to those who have). Informat ion on how AAL makes funding decisions will also form part of the update. Presenters from AAL will then open up the floor to discussion\, allowing p lenty of time for the audience to ask questions or talk about matters that are important to them. We will be utilising WooClap (a Q&A online platfor m) for part of the session\, so it would be great if everyone can have a d evice on hand (a phone will do!) to jump online and participate. LAST-MODIFIED:20230726T053609Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBA) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Orsola De Marco (AAL Board Chair) "Annual AAL Update" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250603T010000Z DTEND:20250603T020000Z DTSTAMP:20261011T152429Z UID:uibogmjukmmcjaor60rtuqqg28@google.com CREATED:20250312T111617Z DESCRIPTION:The quest for radio transients has evolved into a thriving fiel d\, driven by the rise of wide field-of-view telescopes. In recent years\, two remarkable classes of extreme coherent radio transients have emerged: long-period transients\, with pulse durations from minutes to hours\, and fast radio bursts\, with pulse durations from microseconds to tens of mil liseconds. Intriguingly\, the long-period transients are lighting up from the compact object "graveyard\," where traditional models predict they sho uld no longer be detectable in the radio. Zombie stars\, anyone? Emerging theories\, coupled with observational data\, reveal striking similarities in the spectral\, temporal\, and polarimetric properties of long-period tr ansients and fast radio bursts. While the exact origins of FRBs remain unc lear\, the 2020 detection of a fast radio bursts-like pulse from the Galac tic magnetar SGR 1935+2154 confirmed that magnetars can produce such burst s\, at least in some cases. But many questions remain: Are all fast radio bursts from magnetars? What powers their extreme emission? And could long- period transients be their evolutionary cousins? In this talk\, I will hig hlight recent discoveries from the ASKAP and MeerKAT telescopes that are r eshaping our understanding of the fast radio burst and long-period transie nt populations. Early JWST follow-up has begun to uncover fast radio burst s in distant\, high-redshift environments\, offering new clues about their origins and strengthening their potential as cosmological probes. I will also discuss how next-generation facilities like the SKA will revolutionis e the field through population studies and new tests of fundamental physic s. LAST-MODIFIED:20250507T015610Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Manisha Caleb (U. Sydney) "Milliseconds\, Minutes\, and Mysteries: The New Era of Radio Transients" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160913T010000Z DTEND:20160913T020000Z DTSTAMP:20261011T152429Z UID:s85vla61kfqbgial49nitdn76o@google.com CREATED:20160516T014118Z DESCRIPTION:There is now little doubt that Lenticular (S0) galaxies are the descendants of spiral galaxies whose star-formation ceased. In this talk I will present some of the evidence we have gathered in support of this hy pothesis and the physical mechanisms driving the transformation. I will al so discuss some recent and ongoing work on applying spectroscopic bulge-di sk decomposition techniques to multiple IFU surveys such as MaNGA. LAST-MODIFIED:20160913T042105Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alfonso Aragon-Salamanca (University of Nottingham) "Transforming S pirals into S0s" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221018T000000Z DTEND:20221018T010000Z DTSTAMP:20261011T152429Z UID:q4gd7g19vfkqa16ng925fg56mo@google.com CREATED:20220929T030512Z DESCRIPTION:One of the last great unknowns in our history of the Universe i s when and how the first galaxies emerged after the Big Bang. These galaxi es transformed the cosmos -- they illuminated the invisible scaffolding o f dark matter that underpins the Universe\, they ionized the intergalactic reservoirs of hydrogen\, and they synthesized the elements that would one day seed life on Earth. Thanks to JWST\, these enigmatic galaxies are fin ally coming into view. In this talk I will present early JWST results on t hese systems\, and preview upcoming Cycle 1 programs I am leading. I will discuss: (i) emerging constraints on the nature of the first galaxies both via direct searches for the most distant galaxies as well as via archaeol ogical methods\; (ii) outstanding questions around how these early galaxie s reionized the Universe\, and the pathway to settle them with JWST (e.g.\ , was reionization driven by numerous faint galaxies\, or by rare\, bright 'oligarch' galaxies?). LAST-MODIFIED:20221010T235610Z LOCATION:DLT & ZOOM (host: TBD) \nZoom: https://anu.zoom.us/j/99785341005?p wd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rohan Naidu (CFA\, Harvard) "The First Glimpse of the First Galaxie s with JWST" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230202T000000Z DTEND:20230202T010000Z DTSTAMP:20261011T152429Z UID:e4i9heuft9k5c7gpmkosgjhldk@google.com CREATED:20221201T030318Z DESCRIPTION:Reverberation mapping (RM) is the leading technique used to mea sure direct black hole masses in active galactic nuclei (AGN) outside of t he local Universe. The strength of RM lies in its ability to resolve the i nnermost regions of AGN in the time-domain\, rather than spatially\, allow ing us to study these compact cores out to high redshifts. Additionally\, reverberation measurements calibrate secondary mass-scaling relations used to estimate single-epoch virial black hole masses. However\, the RM techn ique is observationally intensive and consequently few measurements have b een made\, particularly at z>0.3. The Australian Dark Energy Survey (OzDES ) RM Program leveraged high-multiplexed spectroscopy to monitor over 700 A GN up to z~4\, probing new regions of the AGN luminosity-redshift paramete r space. In this thesis\, I deliver results from the OzDES RM Program and explore the complexities of performing reverberation mapping on this `indu strial-scale'. LAST-MODIFIED:20230201T122707Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hiep Nguyen) \nZoom: https ://anu.zoom.us/j/99785341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Umang Malik (RSAA) "Supermassive black hole masses with multi-objec t Reverberation Mapping (End of Thesis Talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190726T040000Z DTEND:20190726T043000Z DTSTAMP:20261011T152429Z UID:9oetv16qsov17fnf8c60sd56co@google.com CREATED:20190624T020608Z DESCRIPTION:The Large and Small Magellanic Clouds (LMC/SMC)\, as two of the closest and most massive satellites of the Milky Way\, have significant e ffects on the local Universe\; including the distribution of ultra-faint s atellites\, and the orbits of tidal streams. Ongoing survey efforts with t he Dark Energy Camera have revealed a wealth of low-surface-brightness ste llar substructures in the periphery of the Clouds\; characterising these s tructures will provide significant insight into the currently poorly-const rained masses and interaction history of the Clouds. In order to elucidate the properties of the structures\, we have used 2df+AAOmega at the Anglo Australian Telescope to instigate a large-scale spectroscopic follow-up of stars across the Magellanic periphery. We are able to detect the kinemati c signature of the Clouds up to projected distances of 23 degrees from the centre of the LMC. Combining our spectroscopically derived radial velocit ies with Gaia DR2 astrometry provides the first 3D kinematics for these re gions. Our initial set of measurements\, along a large substructure to the north of the LMC\, reveal radial velocities near the extremity of the sub structure are significantly different from those expected from an extrapol ation of the LMC rotation curve\; this discrepancy may indicate a strong w arp in the LMC disk. Our ultimate aim is to use these 3D kinematics to ass ess dynamical models of the Clouds\; this will shed new light on the origi n of the substructures\, and the evolution of the Magellanic/Milky Way sys tem. LAST-MODIFIED:20190718T021609Z LOCATION:Duffield Lecture Theatre (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Lara Cullinane (RSAA) "3D kinematics of stellar substructures in th e Magellanic periphery (Annual review talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171109T000000Z DTEND:20171109T010000Z DTSTAMP:20261011T152429Z UID:53hq0n37d8u3urenab8m0b2uf8@google.com CREATED:20171106T045106Z DESCRIPTION:Thanks to nuclear astro-physics collaboration\, we now have goo d understanding of the origin of elements from carbon to zinc\, and theore tical models have well reproduced the observations of these elemental abun dances in the Milky Way Galaxy. Now we can constrain galaxy formation proc esses such as supernova and AGN feedback using metallicities and elemental abundances. Our cosmological simulations are in good agreement with many observations\, namely\, mass-metallicity relations of galaxies (which evol ve with a steeper slope at higher redshifts) and metallicity radial gradie nts within galaxies (which can trace the merging history of the galaxies). Stellar [alpha/Fe] ratios of early-type galaxies become closer to observa tions with AGN feedback (where the seed blackholes originate the first sta rs). The gas-phase C\, N and O abundances can constrain the star formation history of disk galaxies\, which can be used for future observations with JWST. In the Milky-Way simulations\, we also show neutron-capture element s\, including the recent discovery of kilonova (GW170817) as one of the r- process sources. LAST-MODIFIED:20171106T094107Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Chiaki Kobayashi (University of Hertfordshire) "Elemental Abundance s across Cosmic Time" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161215T000000Z DTEND:20161215T010000Z DTSTAMP:20261011T152429Z UID:ni3pklpruq36na38sgo92cpkr4@google.com CREATED:20161031T233115Z DESCRIPTION:Our view and understanding of globular clusters in the Milky Wa y have undergone massive changes over the past few decades. No longer are globular clusters seen as the perfect example of simple stellar population s\, as almost all galactic globular clusters contain star-to-star light el ement abundance variations\, and a small subset contain heavy element abun dance ranges. However\, not only can a lot be learnt from studying the sta rs within globular clusters\, but from the stars outside the globular clus ters\, beyond the tidal radius. Whether the structure is in the form of ti dal tails such as the iconic tails of Palomar 5\, or part of a much larger scale stellar structure such as the stellar stream belonging to the disru pting dwarf galaxy Sagittarius or the wealth of streams in the halo of M31 \, the environs of Galactic globular clusters can be used as insights to t he formation of the globular clusters themselves\, or the shape and format ion of the Milky Way's halo. This thesis focuses on exploring extended fea tures of Milky Way globular clusters. Firstly\, by increasing the spatial coverage and kinematics of the tidal tails of Palomar 5 through low to int ermediate resolution spectroscopy from the 2DF AAOmega Spectrograph on the Anglo-Australian Telescope. We identify 39 new and recover 8 previously d etermined members in the tidal stream through radial velocities\, line str engths and photometric information. Secondly\, we performed a wide field p hotometric survey of southern Galactic globular clusters with the compleme ntary photometric cameras MegaCam and the DECam. We present the results fo r the four clusters analysed during the PhD candidature: NGC 1261\, NGC 18 51\, NGC 5824 and NGC 7089 (M2). We find diffuse large low surface brightn ess stellar envelopes embedding NGC 1261\, NGC 1851 and M2\, with a tentat ive detection of an envelope embedding NGC 5824. We will discuss the origi ns of the envelopes and how the features we have uncovered\, along with Pa lomar 5's tidal tails\, may influence our understanding of the Galactic ha lo and globular cluster formation. LAST-MODIFIED:20161206T232107Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Pete Kuzma (RSAA) "Extended Structures in Globular Clusters - End o f Thesis Colloquium" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150320T030000Z DTEND:20150320T032000Z DTSTAMP:20261011T152429Z UID:hgbivc9f030s0gq5bv36gekmj0@google.com CREATED:20150119T064116Z DESCRIPTION:The Gemini multi-conjugate adaptive optics system (GeMS) deploy s five laser guide stars and up to three natural guide stars\, for better- than-Hubble resolution of ~ 90 milli-arcseconds in Ks-band across the fiel d of view of the RSAA-built Gemini South adaptive optics imager (GSAOI). I will present a user's view of observing with this complex instrument\, an d make recommendations for getting the most out of your GeMS/GSAOI data. LAST-MODIFIED:20150316T234106Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sarah Sweet (RSAA) "Hidden GeMS: observing with the Gemini multi-co njugate adaptive optics system" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200929T010000Z DTEND:20200929T020000Z DTSTAMP:20261011T152429Z UID:qloff61tcol2g7b3l0780uiqto@google.com CREATED:20200829T040312Z DESCRIPTION:Half of the heaviest elements in the periodic table are synthes ized in the rapid neutron-capture process (r-process)\, but the astrophysi cal origin of these elements has been debated for over 60 years. The curre nt debate centers around whether r-process elements are mostly synthesized by neutron star mergers or rare core-collapse supernovae. The recent obse rvation of a neutron star merger in both gravitational waves and electroma gnetic radiation (GW170817 and its associated gamma ray burst/kilonova) di d not resolve this debate\, but it does emphasize the close connection bet ween elemental abundances of stars and direct observations of astrophysica l transients. In this talk\, I will show two examples of how chemical abun dances in metal-poor stars can be combined with observations of astrophysi cal transients to understand r-process nucleosynthesis. First\, I will use abundance ratios in metal-poor stars to predict the expected composition of future kilonovae. Second\, I will use long gamma ray bursts to motivate a new model for explaining r-process scatter in metal-poor stars. These e xamples highlight the importance of stellar spectroscopy in the upcoming e ra of multimessenger astronomy. LAST-MODIFIED:20200923T022210Z LOCATION:ZOOM 997 8534 1005 (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alex Ji (Carnegie\, USA) "Invited Colloquium: Understanding R-Proce ss Nucleosynthesis with Stellar Abundances and Astrophysical Transients" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180503T010000Z DTEND:20180503T020000Z DTSTAMP:20261011T152429Z UID:d259l9q2nhsvndajlgufr1ds04@google.com CREATED:20180109T011609Z DESCRIPTION:The adventure of catching up with new stellar clusters in the M agellanic System has been recently fueled from the ongoing relatively deep and extensive photometric surveys. Particularly\, the presence of stellar clusters in the periphery of the Magellanic Clouds and beyond is currentl y an exciting issue. We present here a review of recently discovered stell ar clusters in the Magellanic System. Particularly\, we focus on the use o f a wealth of wide-field high-quality images released in advance to the as tronomical community. Additionally\, we show the performance of searching techniques for new stellar cluster candidates using suitable kernel densi ty estimators for appropriate ranges of cluster radii and stellar densitie s. LAST-MODIFIED:20180419T232611Z LOCATION:Duffield Lecture Theatre (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Andres Piatti (Universidad Nacional de Cordoba) "The growing number of (new?) star clusters in the Magellanic System" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141128T032000Z DTEND:20141128T033500Z DTSTAMP:20261011T152430Z UID:1im4rl79fk0ffkr2b6p4qfh86c@google.com CREATED:20250925T231022Z DESCRIPTION:In the recent years\, the interest on studying the outer parts of spiral galaxies is rising. To better understand galactic formation and evolution\, simulations and observations are working together to understan d the different behaviours that the disc light distribution displays in th e outer parts of these systems. During this talk I will speak about my cur rent work as part of my PhD project focused on the stellar content in thes e outer regions. We have implemented a new methodology to analyse the stel lar content from spectroscopic data based on the state-of-art full spectru m fitting techniques (using GANDALF and STECKMAP). We have tested such met hodology on the LMC bar region\, where high quality integrated spectra can be obtained as well as Color-Magnitude Diagrams reaching the oldest Main Sequence Turnoff. I will also show the first results that we are obtaining when applying such methodology to the smallest galaxies observed in the C ALIFA (Sanchez et al. 2012) and SAMI (Croom et al. 2012) surveys. I will c ompare such observational results with what recent simulations (RaDES\, Fe w et al. 2012) suggest. I will finish showing the effect that satellite ac cretion has on shaping the chemical and kinematic properties of the outski rts of simulated galaxies\, as well as the effect of such accretion in the shape of the stellar age profile as shown by the RaDES set of galaxies. LAST-MODIFIED:20250925T231023Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) \nZoom: https://anu.zoo m.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tomas Ruiz-Lara (University of Granada) "Unveiling the stellar cont ent in the outer parts of spiral galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150416T010000Z DTEND:20150416T020000Z DTSTAMP:20261011T152429Z UID:5f5jhmu4la1ipabt15o7avr4us@google.com CREATED:20150329T111110Z DESCRIPTION:One of the major unknowns in the history of Earth is concerned with the effects on the Earth of the Late Heavy Bombardment\, documented o n the moon during ~3.95-3.85 billion years. To date pre-3.6 billion years- old terrains disclose little evidence for asteroid impacts\, likely due to the masking of their textural\, mineralogical and geochemical signatures by high grade metamorphism. However\, since 1986 the progressive discovery of asteroid ejecta and associated tsunami events in Archaean sediments in dicates ongoing bombardment by asteroids on the scale of tens of kilometre in diameter. To date at least 15 such events are recorded in South Africa and Western Australia. It is estimated that\, due to erosion and removal of asteroid ejecta units across unconformities and the difficulty in ident ifying such units in the field\, no more than one in ten asteroid impact u nits have been found. The seminar will report a number of new discoveries and consider their implications for the nature and evolution of the early Earth crust and mantle. LAST-MODIFIED:20150409T004108Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Andrew Glikson (Planetary Science Institute\, ANU) "Evidence of ear ly heavy asteroid bombardment of Earth during 3.5-2.5 billion years ago" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191011T003000Z DTEND:20191011T013000Z DTSTAMP:20261011T152429Z UID:k10m1f7qr870ltenbu6aeiejeg@google.com CREATED:20190913T013606Z DESCRIPTION:The Kepler Mission has fueled a revolution in the understanding of the demographics and composition of exoplanets. As a transiting planet mission\, Kepler fundamentally enables the derivation of the planetary ra dius. The sizes of these planets are ascertained directly from the transi t depth and the determination of the stellar radii. But the radii also dep end strongly on the amount the transit depth is diluted by the addition of light from stars blended into the photometric aperture. Without properly accounting for the flux dilution from bound and line-of-sights stars\, pre cise planetary radii cannot be determined. Determination of the bulk compo sition and atmospheric abundances\, requires accurate and precise knowledg e of the planetary bulk density and surface gravity\, which relies on know ledge of the planetary radii. Because of the presence of stellar companion s\, both known and unknown\, the derivation of planetary radii can be bias ed towards smaller radii and\, therefore\, the densities are biased toward s higher densities once the masses are determined. Thus\, characterizing the stellar multiplicity of planetary systems is critical to understanding the sizes\, densities\, and frequency of planets. LAST-MODIFIED:20191008T035604Z LOCATION:Duffield Lecture Theatre (host: Zerjal) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:David Ciardi (NASA Exoplanet Institute/IPAC/Caltech) "Characterizin g Exoplanets Means Characterizing Stellar Multiplicity" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250821T010000Z DTEND:20250821T020000Z DTSTAMP:20261011T152429Z UID:5a2v23dq6nsvi9f7vgqvebg1sk@google.com CREATED:20250623T121111Z DESCRIPTION:Molecular gas\, the fuel for star formation\, is often traced b y CO emission\, whose observations become challenging for metal-poor dwarf galaxies. I will discuss the role of kinematically cold atomic hydrogen ( colder HI) as an alternative tracer of star-forming gas. Using seven nearb y galaxies with a wide range of metallicities\, we identify and map the co lder HI components\, which appear to trace regions associated with star fo rmation\, especially for dwarf galaxies. We highlight their importance in the interstellar medium (ISM) and the need for high-resolution HI observat ions. Alongside this gas-phase view\, I also investigate the dust componen t of the ISM through the relationship between the dust-to-gas mass ratio ( DGR) and gas-phase metallicity (Zgas). This relation provides key insights into the dust cycle in the ISM and is a valuable tool for estimating gas masses in high-redshift galaxies. While the DGR-Zgas relation is well cons trained and approximately linear at high metallicities\, its behaviour at low metallicities (Z < 0.3 Zsolar) remains uncertain. I will present a spa tially resolved DGR-Zgas relation in nearby galaxies (0.07-1 Zsolar)\, com bining multi-wavelength observations with wide-field pseudo-integral field spectroscopic data from the TYPHOON/PrISM survey and VLT/MUSE. LAST-MODIFIED:20250818T084805Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Naomi McClure-Griffiths) \ nZoom: https://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQ T09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Hye-Jin (Hayden) Park (RSAA) "Linking optical IFS data with multi-w avelength data: Probing the interplay of gas\, metals\, and dust in galaxi es (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180301T000000Z DTEND:20180301T010000Z DTSTAMP:20261011T152429Z UID:j69cnd6u1e56t6paicvfqfbkbo@google.com CREATED:20180102T234608Z DESCRIPTION:Globular clusters are important tools to help us understand how galaxies form and evolve. Globular cluster formation tells us about the c onditions of extreme star formation while their survival from high redshif t tell us about the processes of galaxy assembly. Being much brighter than red giant stars\, globular clusters allow the stellar populations of gala xies to be studied at much greater distances. Thus a wider range of galaxy masses\, environments and morphologies to be studied than can be with res olved stars. Using data from the WAGGS survey of massive star clusters in the Milky Way and its satellite galaxies and the SLUGGS survey of the glob ular cluster systems of massive early-type galaixes\, I will talk about ho w we can measure the metallicities of globular clusters using the strength of the calcium triplet in integrated light. Using globular cluster metall icity distributions and the relationships between globular cluster colour and metallicity\, I will present evidence that different galaxies with sim ilar masses experienced different formation histories. I will compare thes e observations with the predictions of the E-MOSAICS cosmological simulati ons of the formation of globular cluster systems. I will also talk about h ow the E-MOSAICS simulations have allowed to us to understand how globular cluster colour distributions vary with globular cluster luminosity (the ' blue tilt'). LAST-MODIFIED:20180218T232609Z LOCATION:Duffield Lecture Theatre (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Christopher Usher (Liverpool John Moores University) "Using Globula r Cluster Stellar Populations to Understand Galaxy Formation" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261203T000000Z DTEND:20261203T010000Z DTSTAMP:20261011T152430Z UID:5p7q1jc8j2u7s04v8kin9i0u1o@google.com CREATED:20260504T083236Z DESCRIPTION:TBC LAST-MODIFIED:20260716T070029Z LOCATION:Zoom or Duffield Lecture Theatre (host: TBC) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Maja Jablonska (RSAA) "TBC (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160301T000000Z DTEND:20160301T010000Z DTSTAMP:20261011T152429Z UID:vucb64lgi32bcc5uaf10sts5mc@google.com CREATED:20151222T081113Z DESCRIPTION:Since the first stars and then galaxies formed the Universe has been an immense factory converting neutral gas into stellar material. The distribution of this stellar material is key to our understanding of gala xy formation and evolution as it is the primary baryonic component we can observe in galaxies over the last 13Gyr. However\, the changing distributi on of stars at a given epoch is dependant on many different processes such as: i) in-situ star-formation rates\, ii) merger rates\, iii) the neutral gas reservoirs available for future star-formation episodes\, iv) the eff ect of galaxy-galaxy interactions on both star-formation and neutral gas c ontent and v) AGN activity. These processes occur in different measures to all galaxies over the history of the Universe\, ultimately resulting in t he distribution of stellar material we see today. If we wish to understand the assembly of stellar mass in the Universe we must aim to probe all of these process\, and build a complete and consistent picture of their inter play over cosmic timescales. In this seminar I will discuss recent result s from the Galaxy And Mass Assembly (GAMA) survey\, probing the assembly o f stellar mass though both in-situ star formation (as traced by multiple S FR indicators) and interactions (both mergers and interaction induced star -formation) - in galaxies spanning ~4 decades in stellar mass. I will disc uss upcoming HI surveys which are aligned with the current state-of-the-ar t multi-wavelength\, spectroscopic surveys - allowing us to simultaneous p robe both star-formation and neutral gas reservoirs in a consistent and st atistically robust sample of galaxies. Lastly\, I will discuss how large a rea surveys of the coming decade\, such as the Wide Area VISTA Extragalact ic Survey (WAVES)\, will help revolutionise our understanding of the assem bly of stellar mass is galaxies. LAST-MODIFIED:20160225T041606Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Luke Davies (University of Western Australia) "Star Formation\, Mer gers and the Assembly of Stellar Mass in Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171013T033000Z DTEND:20171013T035000Z DTSTAMP:20261011T152429Z UID:mvr91hvld6nod5kkv327q6uu48@google.com CREATED:20170915T054111Z DESCRIPTION:Be stars are main­ sequence fast-rotating stars that display a circumstellar emission. This emission is regarded as originated from a di sk\, formed by episodic mass-loss from the star. I will present the curren t modeling efforts and recent achievements of the BeACoN group at the IAG/ ­USP (Brazil)\, which aims at understanding the rich Be phenomenology and the physical processes driving It. Based on the VDD (Viscous Decretion Di sk) model and radiative transfer simulations\, I will report (i) the obser vational campaign of the Be star Achernar over a full active phase\, that started in 2013 and ended in 2016\; (ii) the measurement of the Be disks v iscosity from a sample in the Magellanic clouds and (iii) some predicted a nd observed binarity effects in these systems. LAST-MODIFIED:20170916T054608Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Daniel Faes (Institute of Astronomy and Geophysics - University of Sao Paulo) "Be stars - fast rotators and circumstellar disks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220916T040000Z DTEND:20220916T043000Z DTSTAMP:20261011T152429Z UID:j5ng0khu5n1c93p0p7v98rvfc8@google.com CREATED:20220902T015611Z DESCRIPTION:This will be a repeat of the presentation Celine gave late July 2022 at the SPIE Astronomical Telescope and Instrumentation conference in Montreal\, Canada LAST-MODIFIED:20220902T015611Z LOCATION:DLT & ZOOM (host: TBD) \nZoom: https://anu.zoom.us/j/99785341005?p wd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Celine D'Orgeville (RSAA) "Through fires\, smoke\, hail\, austeriti es and COVID-19: The successful operation of the ANU's Advanced Instrument ation Technology Centre (AITC)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250415T010000Z DTEND:20250415T020000Z DTSTAMP:20261011T152430Z UID:4bahrfjukqm95lcqr9p7qubf94@google.com CREATED:20250106T230125Z DESCRIPTION:Direct detection experiments are crucial in the search for dark matter\, particularly targeting elusive particles such as weakly interact ing massive particles (WIMPs)\, axions\, and axion-like particles (ALPs). To detect WIMP-like particles\, experiments use detectors placed deep unde rground\, shielding them from cosmic radiation and background noise to enh ance sensitivity to rare interactions that could signal dark matter's pres ence. In contrast\, ALP detection relies on highly sensitive instruments\, such as resonant cavities and superconducting sensors\, to detect axion-p hoton interactions. This talk will provide an overview of the dark matter direct detection field\, emphasizing the Australian role\, supported by th e ARC Centre of Excellence for Dark Matter Particle Physics (CDM). The Sou thern Hemisphere\, with Australia’s Stawell Underground Physics Laborato ry (SUPL)\, offers a unique platform for dark matter searches. Notably\, t he SABRE South experiment\, operating in tandem with its Northern Hemisphe re counterpart\, aims to validate dark matter signatures\, including seaso nal modulation. In a more recent development\, a new facility at SUPL (CEL LAR) will house a dilution refrigerator\, which can be used for dark matte r detector R&D and low-mass dark matter experiments. In addition to WIMP s earches\, Australia’s dark matter direct detection efforts focus on axio n-photon interactions\, with ongoing experiments like ADMX and ORGAN\, as well as other innovative techniques\, being conducted through both interna tional and Australian-based collaborations. Finally\, I will discuss the f uture of dark matter detection technologies and experiments\, focusing on new technologies. I will emphasize where Australia may have strategic adva ntage in future and upcoming experiments. LAST-MODIFIED:20250410T112106Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Vanhiep Nguyen) \nZoom: ht tps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Elisabetta Barberio (U. Melbourne) "Dark Matter Detection in the So uthern Hemisphere" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190613T010000Z DTEND:20190613T020000Z DTSTAMP:20261011T152429Z UID:seram2918vsesr4qme724h9k64@google.com CREATED:20190320T091120Z DESCRIPTION:Driven by gravity\, galaxies continuously grow through accretio n of smaller systems. Stellar streams are nice illustrations of this hiera rchical build-up\, but the accreted stars quickly disperse. I will present advanced dynamical models that can convert the observed positions and vel ocities of the accreted stars to phase-space quantities like energy and an gular momentum which remain conserved. In addition\, these models can incl ude the observed chemical properties of stars which are also conserved. Th e resulting population-dynamical models allow us then to uncover even thos e accretion events which are now fully dispersed. At the same time\, these models also accurately constrain the total mass distribution\, including a central black hole and dark matter halo. I will illustrate how these mo dels make optimally use of observations to unveil the colourful past and d ark side of galaxies: from unveiling their complex orbital distribution\, to uncovering the satellite accretion history\, to dark-matter dominated d warf spheroidal galaxies having suffered interactions and even mergers. By the end\, I aim to have demonstrated that these models provide a unique b ridge between the studies of resolved stars in the Milky Way and integrate d-light of high-redshifts galaxies. Together with direct coupling to state -of-the-art galaxy formation simulations\, these population-dynamical mode ls enable us to uncover the hierarchical build-up of galaxies in a cosmolo gical context. LAST-MODIFIED:20190530T162106Z LOCATION:Duffield Lecture Theatre (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Glenn van de Ven (University of Vienna) "The colourful past and dar k side of galaxies unveiled through population-dynamics of their stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230615T010000Z DTEND:20230615T020000Z DTSTAMP:20261011T152430Z UID:jh3boe5ftrel8s1j9495ifn33c@google.com CREATED:20230521T073611Z DESCRIPTION:The study of exoplanets is one of the fastest growing sub-field s in astronomy\, and in particular one question stands above the rest: "Is Earth the only planet to harbour life? Are we alone?" While there have be en numerous proposed missions to answer this question\, none hold as much promise as a mid-infrared (MIR) nulling space interferometer as it concurr ently provides the contrast\, sensitivity and angular resolution to charac terise many Earth-sized planets inside their star's habitable zone (HZ). I n this thesis talk\, I present advances towards making a MIR space interfe rometry mission\, such as the Large Interferometer For Exoplanets (LIFE) f easible. This comes in two parts: First\, I introduce and discuss the grou nd-based pathfinder interferometer Pyxis\, the only visible light combiner in the Southern Hemisphere which consists of three autonomous robotic pla tforms. These platforms are used as placeholders for satellites\, where Py xis demonstrates the metrology\, pointing and fringe tracking precision ne eded for a small space interferometry mission. I also show some of the fir st light science results from our commissioning run. Secondly\, I describe configuration and architecture options for a large-scale multi-aperture m ission such as LIFE. Using the paradigm of kernel-nulling\, I find that a pentagonal array of five telescopes is superior to the incumbent Emma X-ar ray configuration in the photon limited regime. Taking this array configur ation\, I present a possible implementation of the beam combiner using an adaptive nuller and a cascade of beam splitters\, as well as a discussion on a few alternative implementations. Together\, this work demonstrates th at formation-flying interferometry is indeed feasible\, and is a step towa rds a future space demonstrator mission. LAST-MODIFIED:20230605T005109Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Callum) \nZoom: https://an u.zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jonah Hansen (RSAA) "Preparing for LIFE (End of Thesis Talk): Towar ds Optical & Infrared Interferometry From Space" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251118T223000Z DTEND:20251119T040000Z DTSTAMP:20261011T152430Z UID:iqbmllf0pbjps4hnnptq54are0@google.com CREATED:20250917T113217Z DESCRIPTION:09:30 - 10:00: James McGregor (PhD chair: Kaasinen\, CRP chair: Martinez Rey)\; 10:00 - 10:30: Daniela Montes Doria (PhD chair: Qin\, CR P chair: Federrath)\; 10:30 - 11:00: morning coffee\; 11:00 - 11:30: Patri ck O'Connor (PhD chair: Mendel\, CRP chair: Colless)\; 11:30 - 12:00: Fat ma Shaban (PhD chair: Wyithe\, CRP chair: Ness)\; 12:00 - 12:30: Zachary Steyn (PhD chair: Wolf\, CRP chair: Martinez Rey)\; 12:30 - 13:30: lunch break\; 13:30 - 14:00: Ashley Tan (PhD chair: Wolf\, CRP chair: Anderson)\ ; 14:00 - 14:30: James Watt (PhD chair: Krumholz\, CRP chair: Colless)\; 1 4:30 - 15:00: Thimo Timmermans (PhD chair: Colless\, CRP chair: Buder) LAST-MODIFIED:20251118T011106Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Christoph Federrath) \nZoo m: https://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Various (RSAA) "Confirmation of Candidature Talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150226T000000Z DTEND:20150226T010000Z DTSTAMP:20261011T152429Z UID:ne6i9te6po82gaac1h54v74tas@google.com CREATED:20150112T031108Z DESCRIPTION:The early chemical evolution of the Galaxy and the Universe is vital to our understanding of a host of astrophysical phenomena. Since the oldest\, most metal-poor stars are relics from the high-redshift universe \, they probe the chemical and dynamical conditions of a time when large g alaxies first began to assemble. Recent works have shown that the ultra-fa int dwarf galaxies (with L<10^5Lsun) contain a relatively large fraction o f extremely metal-poor stars and are devoid of solar-metallicity stars. Th is reflects a rather short or truncated star formation history similar to what one would expect to occur in a first/early galaxy. Indeed\, a spectro scopic study of the faintest dwarf galaxy Segue 1 shows a metallicity rang e from -4 < [Fe/H] < -1 and abundance patterns like those of other metal-p oor halo stars. The over chemical signature of Segue 1 and other ultra-fai nt dwarfs thus supports the concept that small systems analogous to the su rviving ultra-faint galaxies were the building blocks of the Milky Way's l ow-metallicity halo. This suggestion is in line with recent age measurment s for similar ultra-faint dwarf which showed these galaxies to be single-a ge stellar systems that are about as old as the universe itself. This open s a new window for studying galaxy formation with the means of stellar che mical analyses. LAST-MODIFIED:20150126T234617Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anna Frebel (MIT) "The ultra-faint dwarf galaxy Segue 1: Is it a su rviving first galaxy?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240229T000000Z DTEND:20240229T010000Z DTSTAMP:20261011T152429Z UID:h430pgs6hts79skbdjgor54qg8@google.com CREATED:20231211T052613Z DESCRIPTION:Photometric and spectroscopic observations unveil important ste llar properties\, including chemical abundance\, radial velocity\, multipl icity\, mass\, distance\, and age. Open clusters provide a homogeneous ste llar sample with uniform age and similar metallicity\, enabling systematic exploration of diverse stellar mechanisms. Lithium is destroyed in hot st ellar interiors with an effective temperature exceeding 2.5 MK\, while it can be produced in certain red giants and AGB stars. Thus\, Lithium become s pivotal in tracing internal stellar processes. Additionally\, host stell ar chemical compositions play a crucial role in shaping planetary systems. This talk explores the Lithium pattern in dwarfs\, supporting the role of rotational mixing\, and investigates the internal and external factors co ntributing to the formation of Lithium-rich giants. Furthermore\, it discu sses the correlation between the atmospheric abundance of planets and thei r host stars\, and examines the planet engulfment signatures in stellar ch emical abundances\, especially Lithium. LAST-MODIFIED:20240218T224111Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Trey Yang) \nZoom: https:/ /anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Qinghui Sun (Tsinghua University) "Exploring Stellar Physics and St ar-Planet Interaction through the Lens of stellar Chemical Abundance" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230808T010000Z DTEND:20230808T023000Z DTSTAMP:20261011T152429Z UID:lvl9ga6l2sc538dd82nrkdabec@google.com CREATED:20230730T235607Z DESCRIPTION:The historical multi-messenger firework SN1987A confirmed the i mportance of neutrinos in a core-collapse supernova. However\, there has b een no confirmed supernova neutrinos since\, leaving many open questions i n stellar collapse. The diffuse flux of supernova neutrinos provides an im mediate opportunity to detect stellar core-collapse neutrinos. This signal is spatially isotropic and temporally constant\, arising from the combine d fluxes of neutrinos emitted from all distant stellar core collapses. It has not been detected yet\, but the Super-Kamiokande detector\, now upgrad ed with gadolinium\, has a real shot at its first discovery. In this talk\ , I will review predictions of the diffuse supernova neutrino flux and dis cuss the detection prospects in the coming decade. Inputs from both the th eoretical\, observational\, and experimental communicates are crucial\, an d I will cover recent insights gained from both simulations and observatio nal surveys. I will close with some promising probes which would become po ssible in the precision phase during the Hyper-Kamiokande era. LAST-MODIFIED:20230808T003604Z LOCATION:TBD (host: Roland) \nZoom: https://anu.zoom.us/j/83410388355?pwd=Q m9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Shunsaku Horiuchi (Virginia Tech.) "Towards the discovery of diffus e supernova neutrinos" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240209T040000Z DTEND:20240209T050000Z DTSTAMP:20261011T152429Z UID:h6u59bgocbg3idf0v9uacek42o@google.com CREATED:20240206T104710Z DESCRIPTION:TBC LAST-MODIFIED:20240206T104710Z LOCATION:Duffield Lecture Theatre (host: Emily Wisnioski) \nZoom: https://a nu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Emily Wisnioski (RSAA) "Thesis oversight committee information sess ion" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260630T013000Z DTEND:20260630T023000Z DTSTAMP:20261011T152430Z UID:43dgpslceh68j481o2ft399ojg@google.com CREATED:20260503T114411Z DESCRIPTION:Gas-phase metallicity is a fundamental tracer of galaxy evoluti on\, yet strong-line calibrations derived from local galaxies become biase d at high redshift due to evolving interstellar medium (ISM) conditions. W ith JWST now enabling direct metallicity measurements via auroral lines at z>2\, a consistent theoretical framework for interpreting strong-line dia gnostics across cosmic time is urgently needed. We present a first-princip les framework to derive redshift-dependent metallicity calibrations for ga laxies at z=2-7. Our approach combines the cosmological simulation ASTRID with stellar population synthesis and MAPPINGS V photoionization modeling. HII region properties are computed self-consistently for young star clust ers using an analytic feedback model\, capturing the coupled evolution of stellar feedback\, ionization parameter\, and local ISM density. The resul ting emission-line predictions are validated against observed star-formati on rate indicators and the [OIII] luminosity function. From this model\, w e derive calibrations for common optical (R23\, O3N2\, N2\, O32) and UV (C 3O3\, N3O3) diagnostics. We find significant redshift evolution in these r elations\, driven primarily by changing ionization conditions. A Bayesian analysis quantifies calibration performance under varying signal-to-noise\ , enabling diagnostic recommendations as a function of redshift and data q uality. The R23 calibration has the lowest scatter\, lowest sensitivity to S/N\, and weakest redshift evolution. These results provide a practical f ramework for interpreting JWST spectroscopy and tracing chemical evolution from cosmic noon to the epoch of reionization. LAST-MODIFIED:20260605T070008Z LOCATION:Zoom or DLT (host: TBD) \nZoom: https://anu.zoom.us/j/82974980739? pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Yao Yao (RSAA) "Theoretical emission lines and metallicity calibrat ions of H II regions in Astrid simulation" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180427T040000Z DTEND:20180427T042000Z DTSTAMP:20261011T152429Z UID:7dp1cfu0s0hk3pkgq24gmcn3hc@google.com CREATED:20180419T032607Z DESCRIPTION:The ATLAS All-sky Survey System is carefully optimized to maxim ize survey capability for transient and moving objects per unit cost - in this regard it out-performs every other survey around. I will describe the ATLAS system: purchased hardware\, custom-built hardware\, software\, and personnel\, explaining some of the design choices that make ATLAS particu larly effective. LAST-MODIFIED:20180419T045609Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:John Tonry (University of Hawaii) "The ATLAS All-sky Survey System" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251204T000000Z DTEND:20251204T010000Z DTSTAMP:20261011T152430Z UID:q5heqr46094sasdfreabhhf988@google.com CREATED:20250902T070120Z DESCRIPTION:Observations of dwarf satellite galaxies in the nearby universe find they orbit their hosts in flattened\, co-rotating structures called 'satellite planes'. Similar coherent structures are rarely observed in cos mological simulations. Attempts to resolve this discrepency known as the ' satellite planes problem' have been ongoing for decades. Some hypotheses s uggest that unique formation conditions in the Local Sheet\, a cosmic stru cture containing galaxy groups out to 7 Mpc\, may be leading to this perce ived discrepancy. During my PhD\, I have undertaken a multi-year observing program of the M104 system (D=9.55 Mpc) with deep-optical imaging and IFU spectroscopy. This extensive survey finds M104 is one of the most heavily systems within 10 Mpc\, reveals the first possible satellite plane discov ered outside of the Local Sheet\, and evidence of a recent merger event as sociated with a system-wide starburst in the stellar populations of the sa tellites. LAST-MODIFIED:20251130T225107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Helmut Jerjen) \nZoom: htt ps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ethan Crosby (RSAA) "Near-Field Cosmology and the Satellite Galaxy System of M104 (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250218T000000Z DTEND:20250218T010000Z DTSTAMP:20261011T152429Z UID:urk6sridqcf6qbpo0ik7s5f4vs@google.com CREATED:20250106T225609Z DESCRIPTION:The now-well-known "Hubble tension" is the difference between t he expansion rate measured locally and that predicted from Cosmic Microwav e Background (CMB) measurements extrapolated to the present-day assuming t he Lambda Cold Dark Matter cosmological model. Similar\, but less well kno wn\, is the "S8 tension" which is related to the smoothness of the Univers e. This tension is most strongly felt comparing recent weak gravitational lensing measurements to the CMB. The same S8 tension is also present when using other probes of the homogeneity of the nearby Universe. In particul ar\, peculiar velocities - deviations from Hubble expansion - probe the gr owth rate of matter density fluctuations on large scales. I will discuss recent measurements of cosmological parameters based on our approach of pr edicting peculiar velocities from the density field. Time permitting\, I w ill also describe results from our new weak lensing survey\, the Ultraviol et Near-Infrared Optical Northern Survey (UNIONS)\, which should have an i mpact on this topic. LAST-MODIFIED:20250106T225609Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Matthew Colless) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mike Hudson (U. Waterloo) "Cosmic flows and weak gravitational lens ing crank up the tension in cosmology" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240729T060000Z DTEND:20240729T070000Z DTSTAMP:20261011T152429Z UID:dv07ss92d76483gm4jims1bmdk@google.com CREATED:20240724T045109Z DESCRIPTION:Three fiber feed integral field units (IFU) are being developed in the SAAO fiber-lab for the Robert Stobie Spectrograph's visible arm an d the future red arm. The smaller\, 200 micron fibre IFU has 309 x 0.9 arc sec diameter spatial elements covering an elongated hexagonal footprint of 18 x 23 arcsec is now being commissioned. The larger\, 300 (400) micron f iber IFU has 21 x 1.35 arcsec (178 x 1.8 arcsec) diameter spatial elements covering an on-sky area of 18 x 29 sq. arcsec (21 x 44 sq. arcsec). In al l cases there are two groups of 13 fibres offset by roughly 50 arcsec on e ither side of the primary array to sample sky. The 0.9 arcsec spatial reso lution SMI provides a median spectral resolution of 2400 at H-alpha wavele ngths in the low resolution mode simultaneously covering 320 to 740 nm. At a higher grating angles the SMI will deliver spectral resolution up to 10 000 with 0.9 arcsec sampling on sky. A future red spectrograph arm which w ill extend the wavelength coverage up to 900 nm at a median resolution of 6000 for the same IFU. Each IFU sits in its own slit-mask cassette and is referred to as a slit-mask IFU (SMI). These are inserted in the same fashi on as the existing long-slit cassettes at the SALT focal plane. In this ta lk I will report the laboratory characterization and on-sky commissioning- performance of the first Slit Mask IFU\, as well as data reduction pipelin e. (IMPORTANT NOTE: this seminar will not be broadcast on the usual semina rs zoom link\, and will instead be broadcast on the alternative link locat ed above)). LAST-MODIFIED:20240724T050110Z LOCATION:ZOOM or Duffield Lecture Theatre\, zoom link https://anu.zoom.us/j /89603793950?pwd=zt1CybgCwhazVKiykjzfSg4OFj2MFh.1 (host: N/A (speaker pres enting remotely)) \nZoom: https://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QS tWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sabyasachi Chattopadhyay (South African Astronomical Observatory/So uth African Large Telescope (SAAO/SALT)) "Early commissioning results of t he Slit Mask Integral Field Unit on Southern African Large Telescope (Astr alis Seminar)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220920T010000Z DTEND:20220920T020000Z DTSTAMP:20261011T152430Z UID:4mh49v491vn2tasjo0uik6qdso@google.com CREATED:20220809T022112Z DESCRIPTION:Most stars are born with one or more companions. Observational advances over the last decade have enabled high-resolution\, interferometr ic studies of forming multiple systems and statistical surveys of multipli city in star-forming regions. These have yielded new insights into how suc h systems form and how multiplicity affects disk evolution and planetary a rchitectures. In this talk\, I will review recent observational discoverie s of the youngest multiple systems. I will present the results of star clu ster simulations modeling the formation and evolution of multiple systems\ , and I will discuss the role of dynamics and environment in setting stell ar multiplicity. Finally\, I will highlight remaining numerical and obser vational challenges. LAST-MODIFIED:20220913T005110Z LOCATION:DLT & ZOOM (host: Shyam) \nZoom: https://anu.zoom.us/j/99785341005 ?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Stella Offner (University of Texas Austin\, USA) "Our Lonely Sun: H ow Multiple Star Systems Form (or don't)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161118T030000Z DTEND:20161118T032000Z DTSTAMP:20261011T152429Z UID:foa2h5ol47cv69762f09dqst9k@google.com CREATED:20161103T055608Z DESCRIPTION:This paper covers the design\, construction and testing of a ca mera latency measurement device. As the latency of a camera used in an ada ptive optics system could be the limiting factor to the speed at which the system can operate\, and the latency is not readily available from the ma nufacturers\, a device is required to measure this latency. The initial sp ecifications for the device were to deliver a measurement with sub millise cond resolution and measurement uncertainty on the order of tens of micros econds. A system was designed which consisted of a computer sending a sign al\, via its in built sound card\, through some interface circuitry to mod ulate a LED. The detected light modulation is then time synchronised with the electronic signal by use of the computer’s serial port and the corre lation between the two signals used to extract the latency. A proof of con cept test was performed and the latency of a Nuvu Hnu 128 was measured as 1.160+/-0.057\, 1.202+/-0.042\, and 1.227+/-0.045 ms for frame rates of 20 0\, 400 and 900 frames per second\, respectively. A proposed next stage of testing is to use the system on a camera with known latency to verify its accuracy. However\, to do this test the measurement uncertainty needs to be reduced. Ways to reduce this uncertainty are discussed with the most si gnificant being to change the form of the initial pulse used to time synch ronise the signals so as to avoid contraction effects and to replace the L M741 op-amp using in interface circuitry with a better\, low noise alterna tive. LAST-MODIFIED:20161114T003706Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alexander Stuchbery (RSAA) "Design Construction and Test of a Camer a Latency Measurement Device" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230217T000000Z DTEND:20230217T010000Z DTSTAMP:20261011T152429Z UID:dtpf8sb7mtleuua53j17ht4oqk@google.com CREATED:20230130T230112Z DESCRIPTION:Schedule: 11:00-11:15am Dinguan Cao: Post-processing tool to cr eate synthetic IR images from star formation simulations 11:15-11:30am Ani ka Chan: Exploring Mg II and Fe II Wind Signatures in Star- Forming Galaxi es With The MAGPI Survey 11:30-11:45am Paris Gordon-Hall: Using Reverberat ion Mapping from the OzDES and SDSS AGN/Black Hole Measurements as a New C osmological Distance Method LAST-MODIFIED:20230205T000114Z LOCATION:DLT and ZOOM (host: Emily Wisnioski) \nZoom: https://anu.zoom.us/j /84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:ASTR3005 Student Presentations (RSAA) "ASTR3005 Student Presentatio ns" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201120T030000Z DTEND:20201120T033000Z DTSTAMP:20261011T152429Z UID:bqkgi7k06kgohe7qr9g7orps5c@google.com CREATED:20200923T022220Z DESCRIPTION:The new FoF format is like an Open Mic: Our speakers have 15 mi nutes each to talk about topics of their choice. The idea of the new FoF i s to get to know the many individuals that work under the same roof\, allo w newcomers to find friends easily\, and find new friends or colleagues wi th similar interests and hobbies. So feel free to talk about some of your most favourite adventures\, memorable Stromlo anecdotes\, your hobbies\, y our last COVID-DIY project\, your voluntary activities outside of Stromlo or whatever you are passionate about. Science talks (about a scientific to pic/question that you are interested in) are also welcome\, but be mindful of your audience (astronomers\, students\, engineers\, professional staff ). LAST-MODIFIED:20201117T230107Z LOCATION:ZOOM 997 8534 1005 (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alex Wallace and Eloise Birchall (RSAA) "FoF: "Great Australian Roa d Trips" and "What I've learnt at Geoscience Australia"" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250306T000000Z DTEND:20250306T010000Z DTSTAMP:20261011T152429Z UID:a72k4fqeihtf0dk74bp2oic3fc@google.com CREATED:20250131T012122Z DESCRIPTION:A density field mapped from a galaxy redshift survey can be use d to predict the peculiar velocity field\, up to normalisation and any ext ernal tidal field. Fitting such a model for the predicted peculiar velocit ies to those measured using a distance estimator such as the Tully-Fisher relation provides a test for theories of gravity via a measurement of the growth factor. In this end-of-thesis talk\, I will present a Bayesian forw ard-modelling method that simultaneously determines the parameters of both the Tully-Fisher relation and the peculiar velocity field\, while incorpo rating a selection function and an intrinsic Tully-Fisher scatter model. I will also show how this methodology can be applied to improve upon Tully- Fisher measurements of the Hubble constant and directly measure possible v ariations of H_0 on the sky. The former is currently limited by uncertaint ies in the absolute calibration\, but the latter is only limited by sample size and sky/redshift coverage. These methods were applied to the Cosmicf lows-4 Tully-Fisher dataset to obtain measurements on the growth rate\, H_ 0\, and a possible dipole in H_0. Using Tully-Fisher mocks of the ongoing WALLABY survey\, I show the extent to which each of these constraints will be improved by next-generation datasets. LAST-MODIFIED:20250226T222607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Matthew Colless) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Paula Boubel (RSAA) "Cosmological tests from large-scale motions an d the Tully-Fisher relation (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191115T003000Z DTEND:20191115T010000Z DTSTAMP:20261011T152429Z UID:0k992l20h5v9ifndc0og0tisko@google.com CREATED:20191105T083605Z DESCRIPTION:The presentation will focus on introducing the Australian Natio nal Fabrication Facility - ACT Node structure and its various capabilities /equipment highlighting the various technological capabilities/processes a vailable/achieved at the node. That includes examples from E-beam lithogra phy\, deposition\, etching\, focused ion beam experiments\, SEM\, etc. LAST-MODIFIED:20191105T083605Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Fouad Karouta (Australian National Fabrication Facility) "Introduci ng ANFF fabrication capabilities at your doorstep at the ACT node" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190709T010000Z DTEND:20190709T013000Z DTSTAMP:20261011T152429Z UID:743b74et3etepddo765jfgpcps@google.com CREATED:20190708T041104Z DESCRIPTION:The Milky Way is a unique laboratory\, where stellar properties can be measured and analyzed in detail. In particular\, stars in the olde r populations encode information on the mechanisms that led to the formati on of our Galaxy. In this talk\, I will discuss the kinematics\, spatial d istribution\, and chemistry of a large number of stars in the Solar Neighb orhood\, where all of the main Galactic components are well-represented. W e used the accurate parameters delivered by Gaia DR2 and we found evidence that the thick disk comprises two distinct and overlapping stellar popula tions\, with different kinematic properties and chemical compositions. The metal-weak thick disk (MWTD) contains two times less metal content than t he canonical thick disk and exhibits enrichment of light elements typical of the oldest stellar populations of the Galaxy. The rotational velocity o f the MWTD around the Galactic center is 150 km s-1\, corresponding to a r otational lag of 30 km s-1 relative to the canonical thick disk (180 km s- 1)\, with velocity dispersion of 60 km s-1. Some formation scenario will b e also discussed. LAST-MODIFIED:20190708T071604Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Daniela Carollo (INAF - Astrophysical Observatory of Turin) "Eviden ce for the third stellar population in the Milky Way's disk" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230508T010000Z DTEND:20230508T020000Z DTSTAMP:20261011T152429Z UID:rtg2b16ac14ehadov3qqbd6g2k@google.com CREATED:20230501T020307Z DESCRIPTION:The upcoming fourth observing run (O4) of the global LIGO-Virgo -KAGRA network of gravitational wave (GW) detectors is set to begin later this month. Joint detections of GWs and electromagnetic counterparts are n ecessary in advancing our understanding of the universe and the use of rap id wide-field optical telescopes has become increasingly important for the detection and characterisation of cosmic events. I will explore the role of the newly commissioned Gravitational-wave Optical Transient Observer (G OTO) network in this endeavor by providing rapid and precise follow-up obs ervations of GW events. GOTO is a network of wide-field small robotic tele scopes located in the northern (ROM\, La Palma) and southern (Siding Sprin g Observatory\, Australia) hemispheres that can rapidly and autonomously o bserve the sky in response to alerts from GW and gamma-ray detectors. I w ill also discuss outstanding scientific puzzles that can be addressed with joint GW and electromagnetic counterpart searches\, including the measure ment of the Hubble constant using standard sirens\, constraints on the neu tron star equation of state\, and constraints on (non)deviations from gene ral relativity. Additionally\, I will examine realistic scenarios of what we might expect observationally during O4\, and the exciting possibilities that lie ahead for GW astronomy with the O4 run and beyond. LAST-MODIFIED:20230501T045107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Lilli) \nZoom: https://anu .zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kendal Ackley (Warwick) "Exploring the Universe with Joint Gravitat ional Wave and Electromagnetic Counterpart Searches" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191121T000000Z DTEND:20191121T010000Z DTSTAMP:20261011T152429Z UID:bk5vbds01rjse658r6jrfvtdu4@google.com CREATED:20190905T072111Z DESCRIPTION:This informal seminar will highlight results obtained recently with the GRAVITY instrument on ESO's Very Large Telescope Interferometer. These include the detection of the gravitational redshift and relativistic transverse Doppler motion in the highly-elliptical 16-year-period orbit o f the star S2 near Sgr A*\, the detection of looped motion of flares in Sg r A* at 30% of the speed of light near the innermost stable circular orbit of the central black hole\, the measurement of the size of the broad-line region in 3C273\, as well as direct spectroscopic measurements of the pro perties of the atmosphere of bright young exoplanets. LAST-MODIFIED:20191104T114107Z LOCATION:Duffield Lecture Theatre (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tim de Zeeuw (Leiden Observatory/MPE) "Gravity on the VLT" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151013T000000Z DTEND:20151013T003000Z DTSTAMP:20261011T152429Z UID:22g1s7qpravitjdtcgs3oaaslo@google.com CREATED:20151004T121107Z DESCRIPTION:I will review the outcomes from our recent researches of mappin g star forming activities during the peak epoch of galaxy formation and ac ross various environments through our Mahalo-Subaru project. I will then a ddress remaining key questions and future prospects with new facilities. LAST-MODIFIED:20151012T040608Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tadayuki Kodama (NAOJ) "Early Environmental Effects in Proto-Cluste rs at the Cosmic High Noon" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150409T010000Z DTEND:20150409T020000Z DTSTAMP:20261011T152429Z UID:njvh6ebibbd4so4482e5lhvf2s@google.com CREATED:20150310T094114Z DESCRIPTION:Sun-like stars end their lives in a phase of catastrophic mass loss. Between 30% and 80% of the mass of the star is lost in an extreme st ellar wind. The ejecta are briefly visible as an ionized\, expanding plane tary nebula surrounding a hot pre-white dwarf star. The mass loss of Sun-l ike stars is crucial to both stellar and galactic evolution: it is respons ible for the mass distribution of white dwarfs\, about half the local ISM\ , most of the carbon in the Universe\, much of the dust and half of all el ements heavier than iron. But planetary nebulae\, the death shrouds of th eir stars\, are also important as tracers of older stellar populations. Th ey are the most luminous phase in the evolution of their host stars\, and emit much of their energy in just a few bright emission lines. About 400 p lanetary nebulae are known in the Galactic bulge. In this talk I will disc uss this population. Planetary nebulae present indications for a younger c omponent to the bulge than the accepted age of 10Gyr. For globular cluster s\, there is a discrepancy between the presence of mass losing stars and t he absence of any interstellar medium. The talk will discus how globular clusters rid themselves of the ejecta. LAST-MODIFIED:20150329T225106Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Albert Zijlstra (Jodrell Bank Centre for Astrophysics) "Life in ret irement: old stars in old stellar populations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230331T030000Z DTEND:20230331T031500Z DTSTAMP:20261011T152429Z UID:3vmrq5h7ib0j8q59o58l7m25oc@google.com CREATED:20230222T040810Z DESCRIPTION:TBD LAST-MODIFIED:20230222T040810Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ella Wang (RSAA) "Ella's objective list of the best Australian citi es" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260825T010000Z DTEND:20260825T020000Z DTSTAMP:20261011T152430Z UID:80e79ds84lnnfb60c4s3fp8l1s@google.com CREATED:20260503T114410Z DESCRIPTION:The First Large Absorption Survey in HI (FLASH) is a wide-area\ , untargeted survey with ASKAP designed to systematically probe cold neutr al gas in galaxies beyond the local Universe. By detecting HI 21-cm absorp tion at redshifts 0.42 < z < 1.0\, FLASH provides a unique window into the evolution of the cold gas reservoir and the role of AGN feedback in galax y evolution.\n\nThe ASKAP-FLASH survey commenced its observing program in 2023 and has recently completed observations\, covering 24000 square degre es. In this talk I will present an overview of the survey\, highlighting e arly results and showcasing some interesting\, new HI absorption detection s. I will also present follow-up observations of FLASH detections with Mee rKAT\, searching for evidence of fast outflows of cold gas at intermediate redshifts. These results demonstrate the complementarity of ASKAP and Mee rKAT in detecting and characterising HI absorbers\, providing insight into how radio jets interact with the interstellar medium in AGN host galaxies . By studying these systems at a critical stage in the lifecycle of radio galaxies\, we can further understand the impact of AGN-driven feedback on galaxy evolution. LAST-MODIFIED:20260722T060013Z LOCATION:Zoom or Duffield Lecture Theatre (host: Hiep Nguyen) \nZoom: https ://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:2 STATUS:CONFIRMED SUMMARY:Elizabeth Mahony (CSIRO) "Searching for cold gas in distant galaxie s: Early results from the ASKAP-FLASH Survey" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261112T000000Z DTEND:20261112T010000Z DTSTAMP:20261011T152430Z UID:6794dokbsu19637re5gcl6ma8c@google.com CREATED:20261006T060012Z DESCRIPTION:TBC LAST-MODIFIED:20261006T060012Z LOCATION:Zoom or Duffield Lecture Theatre (host: TBC) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tianmu Gao (RSAA) "TBC (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150130T030000Z DTEND:20150130T030500Z DTSTAMP:20261011T152430Z UID:if9j5rqpki6e0bidsufoot42ig@google.com CREATED:20150119T080606Z DESCRIPTION:Phil Dooley will briefly introduce himself and answer any quest ions about using ANU media services. LAST-MODIFIED:20250925T231032Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Phil Dooley (ANU Communications Office) "ANU media services" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150210T000000Z DTEND:20150210T010000Z DTSTAMP:20261011T152429Z UID:ec892qkc2hfffibdvlpir00e9s@google.com CREATED:20150201T052106Z DESCRIPTION:Radiotherapy (X-Rays that destroy cancer cells) is essential to treat half of all cancers. Right now\, the world needs 10\,000 additional radiotherapy machines to meet demand. The two major hurdles to provision of these machines are the exorbitant capital and ongoing costs (up to eigh t million dollars per machine plus 10%-20% annual service) and the recruit ment and retention of a highly skilled workforce (10 on-site staff per mac hine) in rural\, regional centres and developing countries. I will describ e a novel new system we are building\, Nano-X\, that completely changes th e way we treat patients for radiotherapy by moving the complexity of the s ystem from hardware to software. The imaging and tracking (source finding) techniques being pioneered for Nano-X form part of an inter-disciplinary research program being developed through a CAASTRO collaboration currently involving Medical Physics and Astrophysics at Sydney and Curtin Universit ies\, together with the Nelune Comprehensive Cancer Centre at Prince of Wa les Hospital. I will use this seminar to introduce the project and encoura ge expressions of interest from graduate and postgraduates interested in b ecoming involved in a cross-disciplinary program between medical and astro nomy with the potential to have a major impact on patient health outcomes around the world. LAST-MODIFIED:20150206T022605Z LOCATION:CSO common room (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ilana Feain (U Sydney) "RadioAstronomy meets RadioTherapy: An inter -disciplinary approach enabling better outcomes for cancer patients around the world" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160708T040000Z DTEND:20160708T050000Z DTSTAMP:20261011T152429Z UID:0nokplmq6mr03pa4kkr37svk3s@google.com CREATED:20160704T075106Z DESCRIPTION:I will be presenting my dissertation work done in the past thre e years at the RSAA/ANU and the Institue for Astronomy/University of Hawai 'i. Gas flows are one of the fundamental processes driving galaxy evolutio n. This thesis explores gas flows in local galaxies by studying metallicit y gradients and galactic-scale outflows in normal star-forming galaxies. T his is made possible by new integral field spectroscopy data that provide simultaneously spatial and spectral information of galaxies. With the new 3D data\, I study metallicity gradients and galactic winds to understand i nflows and outflows in star-forming galaxies. I show that metallicity grad ients in isolated disk galaxies are remarkably simple and universal. Simpl e chemical evolution models reveal that these simple metallicity gradients are a direct result of the coevolution of gas and stellar disk while gala ctic disks build up their masses from inside-out. Tight constraints on the ir mass outflow rates and inflow rates can be placed. I also investigate g alactic winds in normal star-forming galaxies using data from the SAMI Gal axy Survey. I show that galactic winds are found to be very common even in normal star-forming galaxies that were not expected to host winds. By com paring galaxies with and without hosting winds\, I show that galaxies with high star formation rate surface densities and bursty star formation hist ories are more likely to develop large-scale galactic winds. LAST-MODIFIED:20160704T075106Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:I-Ting Ho (IfA Hawaii/RSAA) "Gas flows in star-forming galaxies in the era of 3D spectroscopy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170228T000000Z DTEND:20170228T010000Z DTSTAMP:20261011T152429Z UID:ekiq5sfjqfusmobor1t2ctjltg@google.com CREATED:20170110T011108Z DESCRIPTION:We investigate how accurately the total mass of neutrinos is co nstrained from the magnitude dispersion of SNe Ia due to the effects of gr avitational lensing. For this purpose\, we use the propagation equation of light bundles in a realistic inhomogeneous universe. With a fitting formu la for the nonlinear matter power spectrum taking account of the effects o f massive neutrinos\, we find that in our model it is possible to obtain t he upper imit ~1.0 eV for future optical imaging surveys with the Wide-Fie ld InfraRed Survey Telescope and Large Synoptic Survey Telescope. Furtherm ore\, we discuss how deep we need to observe SNe Ia and to what extent we have to reduce the magnitude error except for lensing in order to realize the current tightest limit _m_ < 0.2[eV]. LAST-MODIFIED:20170110T011108Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Toshi Futamase (Tohoku University) "Constraints on neutrino masses from the lensing dispersion of Type Ia supernovae" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200924T010000Z DTEND:20200924T013000Z DTSTAMP:20261011T152429Z UID:kifiuh6o1sms59ks567qvhgq7s@google.com CREATED:20200907T040611Z DESCRIPTION:TBD LAST-MODIFIED:20200907T040611Z LOCATION:ZOOM 997 8534 1005 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dávid Guszejnov (UT Austin (USA)) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170213T000000Z DTEND:20170213T010000Z DTSTAMP:20261011T152429Z UID:c1j5sbp1g9egqj9thj633fss3g@google.com CREATED:20160706T082118Z DESCRIPTION:Despite the critical role that Type Ia supernovae (SNe Ia) play in the chemical enrichment of the Universe and their great importance in measuring cosmological distances\, we still don't know for certain how the y arise. Most models can be broadly grouped into either "accretion" or "me rger" scenarios\, with the former typically implying a hot\, luminous phas e (0.1 -- 1 million K\, 10^38 erg/s) at some point prior to explosion. Pas t efforts to directly detect the progenitors of very recent\, nearby SNe I a in archival soft X-ray images have produced only upper limits\, and are only constraining assuming progenitors with very high temperatures immedia tely preceding the explosion. In this talk\, I will outline our new approa ch: given that such objects should be strong sources of ionizing radiation \, one may instead search the environment surrounding nearby SN Ia remnant s for interstellar matter ionized by the progenitor. Such ''relic'' nebula e should extend out to tens of parsecs and linger for roughly the recombin ation timescale in the ISM\, of order 10\,000 -- 100\,000 years. With this in mind\, I will introduce our new narrow-band survey for relic nebulae s urrounding young Magellanic SN Ia remnants and accreting white dwarfs\, al ready underway using the Magellan Baade telescope (PI: Alejandro Clocchiat ti). In a similar manner\, we have also placed deep upper limits on the te mperatures and luminosities of the progenitors of Tycho (SN 1572) and othe r Galactic SNe Ia from the study of their Balmer-dominated shocks. In addi tion to opening a new era of ''SN Ia archaeology''\, I will also discuss h ow these results can put new constraints on binary population synthesis mo dels. LAST-MODIFIED:20170210T000605Z LOCATION:Duffield Lecture Theatre (host: Bonnie Zhang) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tyrone Woods (Monash University) "Type Ia Supernova Archaeology: Se arching for the relics of progenitors past" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200611T233000Z DTEND:20200612T000000Z DTSTAMP:20261011T152429Z UID:8gduenv705lceacatvg9d1ns80@google.com CREATED:20200610T105104Z DESCRIPTION:Please see separate reminder email for zoom details. LAST-MODIFIED:20200611T022105Z LOCATION:ZOOM (host: Tucker) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Claire Yung (RSAA) "PhB talk: Reverberation Mapping of Active Galac tic Nuclei using the ANU 2.3m telescope" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240423T010000Z DTEND:20240423T023000Z DTSTAMP:20261011T152429Z UID:j8lkp8pnb2cr1oo5768aksjh2k@google.com CREATED:20231212T120227Z DESCRIPTION:The Milky Way's satellite dwarf galaxies are powerful probes of many important astrophysical processes. Their kinematics provide insights into galactic dynamics and the nature of dark matter\, while their chemic al compositions preserve a history of early galaxy formation and nucleosyn thesis. Recently\, all-sky astrometry from the Gaia satellite has enabled the discovery and characterization of dwarf galaxies at different stages o f tidal disruption. These new galaxies lie at the extremes of dwarf galaxy parameter space\, whether in their structural properties or their star fo rmation histories. In this talk\, I will show how spectroscopic observatio ns of the kinematics and chemistry of these newly discovered dwarf galaxie s can provide crucial insights into galactic dynamics and nucleosynthesis. I will show how kinematics of tidally disrupting diffuse dwarf galaxies p robe the interaction between the Milky Way and Large Magellanic Cloud\, an d highlight how the increased diversity of dwarf galaxy star formation his tories clearly shows the importance of neutron star mergers in dwarf galax y chemical evolution. LAST-MODIFIED:20240411T014612Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Sven Buder) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alex Ji (U. Chicago) "Dwarf Galaxy Archaeology in the Gaia Era" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220909T050000Z DTEND:20220909T053000Z DTSTAMP:20261011T152429Z UID:cgpbm3a9i8meltku59450gvrak@google.com CREATED:20220902T014108Z DESCRIPTION:Astronomy as a career has been\, for the majority of people inv olved\, an academic pursuit\, however there are increasingly wide-spread a pplications in other sectors. Today\, potential markets range from the alr eady bustling amateur astronomy scene to rapidly growing wide-scale indust rial applications. We at Tuparev AstroTech\, with partners Astrosysteme Au stria\, are involved in projects spanning this whole spectrum. On the one side\, the increasing amount of satellites in orbit and the rising amounts of space debris mean the space around the Earth could rapidly be rendered unusable. As part of this effort\, we are attempting to create a large\, worldwide network to monitor satellites and space junk\, covering regimes not included in the current generation of monitoring programmes. We are in volved in every step from manufacturing and setting up the telescopes\, to developing the pipeline for detecting and determining properties of such objects\, through to the expected petabyte database management. On the oth er side\, for amateur and professional astronomers\, we are developing a r ange of inter-connected\, modern astronomy tools and applications\, develo pment of affordable spectrographs\, renovation of old observatory faciliti es as well as location of potential sites for new observatories. In this t alk\, I will give an overview of some of the projects we are involved in a s well as some of the wider astronomy market out there. LAST-MODIFIED:20220902T014108Z LOCATION:DLT & ZOOM (host: Marcus Birch) \nZoom: https://anu.zoom.us/j/9978 5341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Thomas Jackson (Tuparev AstroTech) "Software\, Space Junk and (Robo tic) Observatories" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240625T010000Z DTEND:20240625T020000Z DTSTAMP:20261011T152429Z UID:getk7elohlm46sljacu0gf6mkg@google.com CREATED:20240415T040629Z DESCRIPTION:It is now known that a significant fraction of the Milky Way's ISM resides in a so-called 'dark' phase\, usually defined as a mixture of cold\, optically thick HI and diffuse molecular hydrogen with densities th at are insufficient to form and shield CO. I will present a brief overview of the so-called 'Dark ISM' — where it resides\, how much there is\, an d its characteristic properties. I will then focus on two aspects of struc ture in the dark gas: (1) AU-scale structures in the cold atomic medium an d their possible implications in measuring the fraction of cold/opaque HI\ , and (2) underlying structure in CO-dark molecular gas that can give rise to very broad\, very weak molecular spectral features in OH and HCO+. I w ill introduce two new observational experiments that may further constrain both of these phenomena. LAST-MODIFIED:20240617T233612Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hayden Park) \nZoom: https ://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jo Dawson (Macquarie U.) "Small-Scale Structure in the "Dark ISM"" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210921T010000Z DTEND:20210921T020000Z DTSTAMP:20261011T152429Z UID:h33udu9sqgns1272bkv50mhu00@google.com CREATED:20210907T065610Z DESCRIPTION:Previous work on refining orbital states and/or physical object characteristics has used either semi-empirical or statistical regression techniques. Semi-empirical techniques have been applied to objects whose o rbital states and/or physical object characteristics are already known to high degree and do provide academically interesting observations on object -specific perturbative phenomena. However\, semi-empirical techniques can not be extrapolated and applied to the wider orbital population\, whose or bital states and/or physical object characteristics are known to a lesser degree and may operate in orbital regimes substantially different from tho se studied. The refinement solutions provided by statistical regression te chniques are 'best-fit' rather than unique\, because they do not attempt t o narrow the solution space using fundamental physical principles such as the conservation of energy and momentum. s thesis aims to extend the work of orbital refinement by exploiting additional strategies and techniques\, including (1) the replacement of semi-empirical or statistical regression techniques with multivariate optimisation\; (2) the application of fundam ental physics\, particularly celestial mechanics\, as constraints to the s olution process\; and (3) the addition of a stochastic discrepancy functio n to represent natural or non-natural forces that are not represented in t he perturbative models employed. Multivariate optimisation creates the opp ortunity to correct all states\, physical object characteristics\, and nat ural and non-natural forces simultaneously. The application of celestial m echanics principles narrows the family of solutions returned to those that adhere to the laws of conservation of energy and momentum. Forces represe nted by a stochastic discrepancy function are designed to account for the inability to exploit the full accuracy of geophysical\, planetary and atmo spheric models due to the amount of high-performance computing capability available to this work. The method is tested against three of the accident al orbital conjunctions that have occurred to date. These test scenarios p rovide further determinism to the system of equations for development and evaluation purposes and offer new forensic details on the cases not seen i n previous literature. It is anticipated that subsequent works which expan d on the lessons learned from implementing these strategies will deliver a method capable of correcting the states\, physical characteristics and na tural or non-natural forces of objects considered individually. LAST-MODIFIED:20210909T070109Z LOCATION:ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Richard Samuel (RSAA) "End-of-Thesis Colloquium: Computational phys ics-based refinement of orbital states\, characteristics and behaviours us ing multivariate optimisation" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230713T010000Z DTEND:20230713T020000Z DTSTAMP:20261011T152429Z UID:43ofcsso9qkql6oq39vi2m51sc@google.com CREATED:20230703T010106Z DESCRIPTION:The diffuse\, ionized gas at the interface of the Milky Way's i nterstellar medium (ISM) and circumgalactic medium is a reservoir of futur e star-forming fuel and of metals generated by stars in the Galaxy. Metals in this gas are tracers of the feedback processes that drive the Galactic fountain. However\, accurate measurements of the metallicity in this regi on are challenging due to the uncertain ionization correction\, and blendi ng with the Milky Way ISM. In this talk\, I will present the metallicity m easurements of ionized gas clouds along the sight lines of 8 halo globular clusters (GCs) at galactic heights of z 10 kpc. We use the archival HST/ COS and HST/STIS spectra of the UV bright stars in the GCs\, and address t he blending by fitting Voigt profiles to all absorption components. The to tal hydrogen column is strictly constrained by pulsar dispersion measureme nt for the same GCs. I will discuss the Galactic Fountain mechanism as a p robable origin of infalling gas clouds based on the decreasing metallicity with decreasing infall time. Moreover\, a large scatter in metallicity is also found\, and I will discuss its potential impact on the metallicity d istribution of the ISM. LAST-MODIFIED:20230705T025605Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Trey) \nZoom: https://anu. zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Bo-Eun Choi (University of Washington) "The Metallicity Mapping of the Diffuse Gas at the Milky Way Disk-halo Interface" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190620T010000Z DTEND:20190620T020000Z DTSTAMP:20261011T152429Z UID:6mqp8lj4r2poskc5k3kjovggv0@google.com CREATED:20190509T030213Z DESCRIPTION:I will discuss the results of a search for extremely metal-poor stars based on SkyMapper data release DR1.1. The search process involves photometric selection and low-resolution spectroscopic follow-up at the 2. 3m that provides estimates of effective temperature\, surface gravity and metallicity ([Fe/H]) for the candidates. The selection process is very eff icient: for the 2618 candidates with 2.3m spectra that have photometric me tallicities <_ -2.0\, 41% have [Fe/H] <_ -2.75 and only ~7% have [Fe/H] > -2.0. The most metal-poor candidate has [Fe/H] < -4.75 and is notably C-ri ch. We find that the metallicity distribution function for the observed sa mple\, which is dominated by 'carbon-normal' stars\, has a power-law slope of Delta(log N)/Delta([Fe/H]) = 1.5 +/- 0.1 for -4.0 <_ [Fe/H] <_ -2.75\, but appears to drop abruptly at [Fe/H] ~ -4.2 in line with previous studi es. The small fraction of stars below this limit are all C-rich. LAST-MODIFIED:20190619T040104Z LOCATION:Duffield Lecture Theatre (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Gary Da Costa (RSAA) "Results from the SkyMapper DR1.1 Search for E xtremely Metal-Poor Stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161111T033000Z DTEND:20161111T035000Z DTSTAMP:20261011T152430Z UID:19rkjk9fd6n4fqb80eb3p7g744@google.com CREATED:20161109T002106Z DESCRIPTION:TBD LAST-MODIFIED:20161109T043106Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Martin Asplund (RSAA) "GMT update from the SAC perspective" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230207T000000Z DTEND:20230207T010000Z DTSTAMP:20261011T152429Z UID:umkt5kb88foth6k5sce5oi6q3g@google.com CREATED:20221107T220126Z DESCRIPTION:Nearly three decades ago\, two teams of astronomers used a samp le of just ~40 Type Ia supernovae (SNe Ia) to reveal a ground-breaking mys tery: the accelerating expansion of the Universe. The quest to understand the underlying force (dubbed dark energy) behind this expansion\, which cu rrently makes up ~70% of the mass-energy density in our Universe\, has cap tivated the field of modern cosmology ever since. My PhD takes an in-depth look at the SNe Ia modelling underlying all modern SN measurements of dar k energy. I apply key updates to existing models\, validate new models\, d evelop methods to quantify and reduce underlying systematics within the mo dels\, and explore the impact of previously unparameterised host-galaxy re lationships in the model framework. The results are presented in the conte xt of the Dark Energy Survey's 3-Year Supernova Analysis\, and directly co ntribute to the upcoming DES 5-Year SN analysis. LAST-MODIFIED:20230205T001606Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Takafumi Tsukui) \nZoom: h ttps://anu.zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Georgina Taylor (RSAA) "Light-Curve Models for the Next Generation of Supernova Cosmology (End of Thesis Talk)." TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160407T010000Z DTEND:20160407T020000Z DTSTAMP:20261011T152429Z UID:iet7dormaiae6k05h68jpquhm8@google.com CREATED:20160301T042613Z DESCRIPTION:During the last decade a third window for ground-based astronom y was opened and high energy astrophysics now enables studies up to photon energies of 100 TeV. A wide range of objects were discovered to emit sign ificant amounts of energy in the high-energy gamma-ray regime\, including star-forming regions\, pulsars\, supernova remnants\, massive binaries\, t he diffuse interstellar medium\, the Galactic Centre\, AGN\, etc. Observat ions in this energy domain enable measurements of cosmic star-formation\, intergalactic magnetic fields\, the cosmic non-thermal energy density\, so urces of neutrinos and cosmic rays\, and provide constraints on dark matte r and several extensions of the standard model of particle physics. The ta lk will introduce the techniques and current instruments\, discuss some re cent highlights\, including studies of the Galactic Centre\, the LMC\, and Supermassive Black Holes\, and will describe the future Very-High-Energy gamma-ray observatory CTA and the proposed Australian participation to thi s new facility. LAST-MODIFIED:20160403T075107Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Stefan Wagner (University of Heidelberg) "The New Frontier of High- Energy Gamma-ray Astrophysics" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190131T000000Z DTEND:20190131T010000Z DTSTAMP:20261011T152429Z UID:n928fb37mct6lfiphegnu82khk@google.com CREATED:20181105T043125Z DESCRIPTION:The birth of stars and the formation of galaxies are cornerston es of modern astrophysics. While much is known about how galaxies globally and their stars individually form and evolve\, one fundamental property t hat affects both remains elusive. This is problematic because this key pro perty\, the stellar initial mass function (IMF)\, is a key tracer of the p hysics of star formation that underpins almost all of the unknowns in gala xy and stellar evolution. It is perhaps the greatest source of systematic uncertainty in star and galaxy evolution. The past decade has seen a growi ng number and variety of methods for measuring or inferring the shape of t he IMF\, along with progressively more detailed simulations\, paralleled b y refinements in the way the concept of the IMF is applied or conceptualis ed on different physical scales. This range of approaches and evolving def initions of the quantity being measured has in turn led to conflicting con clusions regarding whether or not the IMF is universal. Here I summarise t he growing wealth of approaches to our understanding of this fundamental p roperty that defines so much of astrophysics\, and highlight the importanc e of considering potential IMF variations\, reinforcing the need for measu rements to quantify their scope and uncertainties carefully. I present a n ew framework to aid the discussion of the IMF and promote clarity in the f urther development of this fundamental field. LAST-MODIFIED:20190123T055107Z LOCATION:CSO Common Room (host: Battisti) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Andrew Hopkins (Macquarie University) "Measuring the stellar initia l mass function" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181211T000000Z DTEND:20181211T010000Z DTSTAMP:20261011T152430Z UID:ua08l08jiei744pifrum9t84oc@google.com CREATED:20180822T015210Z DESCRIPTION:Astronomy is now very much a big-data science. Gaia has had its second data release and is on track to measure the brightness\, position and kinematics of close to 109 stars. TESS and PLATO will observe pulsatio ns in > 105 targets. They will add to the approximately 2 x105 stars tha t have had their oscillations monitored by Kepler and CoRoT. To exploit su ch large data sets the tools of analysis devised must demonstrate speed\, accuracy and versatility. Speed and accuracy are required to process the s heer volume of data collected. Versatility is necessary because although t here will be overlap in the many surveys\, not all stars will have the sam e quantities measured. It is paramount that methods are designed to handle missing or inhomogeneous data sets -- we must maximize the information ex tracted from the available observations. I will discuss the Stellar Param eters in an Instant Pipeline (SPI) which is a machine learning algorithm t hat makes use of detailed asteroseismic observations to rapidly and robust ly determine stellar parameters. LAST-MODIFIED:20181202T104107Z LOCATION:CSO Common Room (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:George Angelou (MPIA) "Applications of Machine Learning in Stellar Astrophysics" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170427T010000Z DTEND:20170427T020000Z DTSTAMP:20261011T152429Z UID:67mb87vmdhm4hflub0jgc3d2vs@google.com CREATED:20170316T052609Z DESCRIPTION:Supermassive black holes that are rapidly accreting matter (and sometimes outshining their host galaxies) were the first sources discover ed at cosmological redshifts. Despite progress in the intervening half-cen tury\, key questions remain about how black holes affect the evolution of their host galaxies\, as well as how they self-regulate their own growth. I will discuss so-called "AGN feedback\," which is a topic of intense theo retical and observational interest. I will focus in particular on what we are learning from multiwavelength observational studies of the nearest and brightest active galactic nuclei. LAST-MODIFIED:20170316T052609Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:David Rupke (Rhodes College) "Do Supermassive Black Holes Help to R egulate Galaxy Evolution and" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220428T010000Z DTEND:20220428T020000Z DTSTAMP:20261011T152429Z UID:jv6mkv5fteqejftcd54vfcd6e4@google.com CREATED:20220407T062116Z DESCRIPTION:My research goal is to reverse engineer the formation and evolu tion of the Milky Way\, using the snapshot of information recorded in its stars. This is an endeavour across a huge range of temporal and spatial sc ales. Both individual stellar atmospheres and million star surveys are rev ealing the connection of present to past\, and ultimately allowing us to p lace the Milky Way in a cosmological context. A cornerstone of my work is in making measurements of stellar ages from stellar spectra. These ages ar e critical to learn the formation and evolutionary properties of the Galax y: where stars were born\, how they have moved\, and how individual abunda nces quantify the diversity of birth environments. This talk will present my past research\, which has set out to link the chemical to the structura l evolution of the Milky Way\, and lay out specific future directions in t he realm of signatures of formation\, GALAH and stellar gremlins. LAST-MODIFIED:20220427T234606Z LOCATION:DLT & ZOOM (host: Sven Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Melissa Ness (Columbia University) "Invited Colloquium: The Milky W ay Galaxy as a galaxy in the Universe" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180717T010000Z DTEND:20180717T020000Z DTSTAMP:20261011T152429Z UID:tvv7qbkt8h7j1q2lrfttugfuis@google.com CREATED:20180612T061609Z DESCRIPTION:Until about a decade ago\, star clusters were considered "simpl e" stellar populations: all stars in a cluster were thought to have simila r ages and the same metallicity. Only the individual stellar masses were t hought to vary\, in essence conforming to a "universal" initial mass funct ion. Over the past decade\, this situation has changed dramatically. I wil l discuss my group's recent progress in this context\, with particular emp hasis on the properties and the alleged presence of multiple populations i n Local Group star clusters across the full age range. Some of our recent results imply a reverse paradigm shift\, back to the old simple stellar po pulation picture for at least some intermediate- age (~2 Gyr-old) star clu sters\, which opens up exciting avenues for future research efforts. LAST-MODIFIED:20180713T050105Z LOCATION:Duffield Lecture Theatre (host: Zerjal) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Richard de Grijs (Macquarie University) "Not-so-simple stellar popu lations in nearby\, resolved massive star clusters" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260714T013000Z DTEND:20260714T023000Z DTSTAMP:20261011T152430Z UID:nuutc6gcvmbl40hl1p7k4sghs8@google.com CREATED:20260527T013429Z DESCRIPTION:Neutrinos and dark matter are the most abundant\, hardest to de tect\, and least understood constituents of the Universe. In this talk\, I will describe recent developments in both areas.\n \nNeutrino physics is entering an exciting new era. Massive new experiments\, now operating or u nder construction\, will deliver unprecedented quantities of data and tran sform the field into a precision science. I will focus on a novel approach to measuring CP violation in neutrino oscillations using atmospheric neut rinos\, which may surpass the sensitivity of accelerator-based experiments in parts of parameter space.\n \nThe identity of the cosmological dark ma tter remains one of the biggest open questions in science. I will outline the status of direct-detection searches and new strategies to probe dark m atter interactions in terrestrial experiments. I will also discuss complem entary probes based on the capture of dark matter in stars\, which can pro vide sensitivity to interactions that are difficult or impossible to obser ve on Earth. LAST-MODIFIED:20260615T230007Z LOCATION:Zoom or Duffield Lecture Theatre (host: Daniela Montes Doria) \nZo om: https://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Nicole Bell (U. Melbourne) "Neutrinos and Dark Matter: New Windows on the Invisible Universe" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220607T010000Z DTEND:20220607T020000Z DTSTAMP:20261011T152429Z UID:4575qhfaq18qmv1utbb8q3hrig@google.com CREATED:20220429T043114Z DESCRIPTION:Less than 1 billion years after the Big Bang the hydrogen in th e Universe transitioned from a neutral to ionized state. The details surro unding the Epoch of Reionization are among the biggest unknowns in modern astrophysics. Significant progress has been made in the last 5 years on wh en the reionization of cosmic hydrogen concluded\, however we are yet to d iscover exactly how much ionizing radiation escapes from galaxies through to the intergalactic medium. Determining the escape fraction (fesc) of ion izing radiation is key to modelling and understanding this era. I will sum marise our team's effort on three different fronts. 1) The direct detectio n and characterisation of Lyman-continuum emission from galaxies just afte r the reionization era\; 2) The lack of correlation between oxygen emissio n lines and Lyman continuum escape fraction\; 3) IGM transmission bias and methodology for recovering the posterior probability distribution of fesc . Our observations shows that a small fraction (or during a small fraction of time or viewing angle) of Lyman continuum emitters tend to be high fes c ('on')\, whereas most galaxies have fesc close to zero ('off'). The comp lementary theoretical work highlights the limitations of assuming an avera ge\, smooth IGM transmission. To finish\, in a look to the future\, I will introduce our plans to use a MAVIS to measure the escape fraction of ioni zing radiation from redshift 6 galaxies at the conclusion of the Epoch of Reionization. LAST-MODIFIED:20220602T042606Z LOCATION:DLT & ZOOM (host: Neco Kriel) \nZoom: https://anu.zoom.us/j/997853 41005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Emma Ryan-Weber (Swinburne University) "Invited Colloquium: The pho tons that ionized the Universe" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161216T030000Z DTEND:20161216T032000Z DTSTAMP:20261011T152429Z UID:937uueg44qni61v1kik7p932ho@google.com CREATED:20161214T034604Z DESCRIPTION:The filter system employed in the SkyMapper survey of the south ern sky incorporates a narrow 'v' filter centered on the Ca II K-line at 3 933Ang\, facilitating the identification of extremely metal-poor (EMP) sta rs in the photometric dataset. A initial survey carried out during telesc ope commissioning resulted in the discovery of the most iron-poor star kno wn (SMSS J0313-6708) and a further 41 stars with [Fe/H] < -3.0 dex. In th is contribution we present initial results from a new search for EMP stars based on the SkyMapper Early Data Release (EDR). The EDR covers ~1/3rd o f the southern sky. We will discuss the selection process\, possible bias es\, and initial outcomes from the on-going low resolution spectroscopic f ollow-up program with the ANU 2.3m telescope at Siding Spring Observatory that is used to define the best candidates for observation at high dispers ion. LAST-MODIFIED:20161214T034604Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Gary Da Costa (RSAA) "The SkyMapper Search for Extremely Metal Poor Stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240215T230000Z DTEND:20240216T050000Z DTSTAMP:20261011T152429Z UID:l05m8tinfg878984gf2m3amc3o@google.com CREATED:20231120T224123Z DESCRIPTION:TBC LAST-MODIFIED:20231120T224123Z LOCATION:Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.zoom.us/j /83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Christian Wolf (RSAA) "SkyMapper Fest" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220923T040000Z DTEND:20220923T043000Z DTSTAMP:20261011T152430Z UID:uobjiamtsmnjbbb4nh25ijmrj8@google.com CREATED:20220913T020111Z DESCRIPTION:Gregory would present information on the opportunities provided by the ADACS Merit Allocation Program for accessing software support. LAST-MODIFIED:20220913T020111Z LOCATION:DLT & ZOOM (host: TBD) \nZoom: https://anu.zoom.us/j/99785341005?p wd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Gregory Poole (Swinburne University) "ADACS Merit Allocation Progra m" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230922T040000Z DTEND:20230922T043000Z DTSTAMP:20261011T152430Z UID:nfoqp9a841ubrlf500rftn9vcc@google.com CREATED:20230823T045613Z DESCRIPTION:The visibility of female role models in science is vital for en gaging and retaining women in scientific fields. I will present results fr om our recently accepted paper (Ross et al. 2023\, AU Journal of Education \, in press)\, where we analyse four senior secondary science courses deli vered across the states and territories in Australia: Biology\, Chemistry\ , Environmental Science\, and Physics. We compared male and female represe ntation within the science courses by examining the mentions of male and f emale scientists along with the context of their inclusions in the syllabu ses. We find a clear gender bias with only one unique mention of a female scientist. This bias will contribute to the continuing low engagement of w omen in scientific fields. We outline possible solutions to address this i ssue\, including the accreditation of scientific discoveries to include fe male scientists and explicit discussion of structural barriers preventing the participation and progression of women in STEM. LAST-MODIFIED:20230823T045613Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark) \nZoom: https://anu. zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Andrew Battisti (RSAA) "Invisible women: Gender representation in h igh school science courses across Australia" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150618T010000Z DTEND:20150618T020000Z DTSTAMP:20261011T152429Z UID:qislmu258chlqdlu4a0uvao150@google.com CREATED:20150118T234615Z DESCRIPTION:Since the pioneering work of Henry Norris Russell 100 years ago \, the study of nearby stellar populations has served as a foundation for our quest to understand the nature of galaxies. Today\, studies of resolve d stellar populations constrain fundamental relations - such as the initia l mass function of stars\, the time scales of stellar evolution\, the timi ng of mass loss and amount of energetic feedback\, the color-magnitude rel ation and its dependency on age and metallicity - that represent key ingre dients in our prescription to interpret light from the Universe and to mea sure the physical state of galaxies. In this presentation\, I'll describe new\, high-precision measurements of some of the most important relations that provide this mapping between resolved and unresolved light\, and disc uss new opportunities for stellar population studies given an unprecedente d suite of astronomical tools that are now on our horizon - GAIA\, JWST\, LSST\, WFIRST\, 30-meter telescopes. LAST-MODIFIED:20150607T212107Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jason Kalirai (STScI) "Stellar Astrophysics: 100 Years after Russel l" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250411T040000Z DTEND:20250411T043000Z DTSTAMP:20261011T152429Z UID:n4jmtfi1mp2k3clhd5ns52hlu8@google.com CREATED:20250326T024611Z DESCRIPTION:An introduction to outreach activities and opportunities at MSO . LAST-MODIFIED:20250326T024611Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Brad Tucker) \nZoom: https ://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Brad Tucker (RSAA) "Outreach activities at Mount Stromlo" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150612T040000Z DTEND:20150612T042000Z DTSTAMP:20261011T152429Z UID:prc9cvkpvo5kecb97i6bo22ruk@google.com CREATED:20150603T084106Z DESCRIPTION:The Hubble constant is one of the most important parameters in the cosmological model\, setting both the size and age of the Universe. Pr esent uncertainties in the standard cosmological model such as the dark en ergy equation-of-state and the properties of neutrinos\, can be constraine d by measurements of the Hubble constant to a higher precision. The Mega-S H0ES project aims exactly this bye measuring the Hubble constant with perc ent-level uncertainty. I will give an overview of the Mega-SH0ES project a nd the techniques it is using\, including the Parallel Astrometric Spatial Scanning (PASS) on WFC3\, Infrared Cepheids\, and 17 New Type Ia Supernov a host galaxies. LAST-MODIFIED:20150609T082606Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Brad Tucker (RSAA) "Mega-SH0ES" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260609T050000Z DTEND:20260609T060000Z DTSTAMP:20261011T152430Z UID:ch1ha7h4f8lls09ocallgqe7es@google.com CREATED:20260503T113741Z DESCRIPTION:Our monthly skillshare sessions offer a practical\, hands-on sp ace for students and postdocs to exchange research skills\, professional d evelopment tools\, and effective workflows in an informal and supportive s etting. Skillshare is run on the second Tuesday of each month\, 3:00-4:30i sh pm in the CSO Common Room\, with ~15-30 minutes of introduction followe d by ~30-60 minutes of panel discussions or open-ended hands-on activities . LAST-MODIFIED:20260503T113741Z LOCATION:Zoom or CSO Common Room (host: Sven Buder) \nZoom: https://anu.zoo m.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Monthly Skillshare (RSAA) "Near-Peers Advice Panel" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210625T033000Z DTEND:20210625T043000Z DTSTAMP:20261011T152429Z UID:4lmcdul02d66l6ec734q82r7bg@google.com CREATED:20210624T020605Z DESCRIPTION:The coming decades will see stellar parameters like temperature \, radius\, and metallicity produced for many millions of new stars as par t of both current and upcoming massive stellar surveys. However\, for any new insights into stellar or Galactic physics to reach their full potentia l\, these parameters need to be calibrated by a library of benchmark stars whose properties are as fundamental and model independent as possible. Su ch a library allows separate surveys to be put on the same fundamental sca le\, and is particularly important for challenging regions of the paramete r space where models are more uncertain. In this talk I give an overview o f my PhD research to broaden our library of stellar benchmarks\, as well a s how I have used such benchmarks to calibrate a spectroscopic survey of l ow-mass stars and constrain exoplanet demographics. LAST-MODIFIED:20210624T020605Z LOCATION:ZOOM and Duffield Lecture Theatre (host: Harry Kenchington-Goldsmi th) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Adam Rains (RSAA) "End-of-Thesis Colloquium: Stellar Benchmarks and a Few Things to Do With Them" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210416T040000Z DTEND:20210416T043000Z DTSTAMP:20261011T152429Z UID:pi7fqmk49mk5de3msdlg6dcit4@google.com CREATED:20210302T051117Z DESCRIPTION:We start the weekend with our new open-mic talks. LAST-MODIFIED:20210415T235105Z LOCATION:ZOOM and Duffield Lecture Theatre (host: Lyla Jung) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Timothy Bateman and Chris Flynn (Swinburne) "The Molonglo Observato ry Synthesis (Radio) Telescope (MOST)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150410T040000Z DTEND:20150410T042000Z DTSTAMP:20261011T152429Z UID:gguinpp38v5vqgdtkogs31imo4@google.com CREATED:20150119T064122Z DESCRIPTION:The abundance of lithium in metal-poor\, near-main-sequence sta rs lies well below the value obtained from Standard Big Bang Nucleosynthes is constrained by the result of the Wilkinson Microwave Anisotropy Probe. Perhaps the most widely held opinion is that this is driven in large part by an incomplete understanding of the physics of the stars. Indeed\, over the past decade of so\, very different conclusions based of stellar observ ations have been put forward concerning the nature of the Spite Plateau in the (A(Li)\, Teff) and (A(Li)\, [Fe/H]) - planes. For example\, the Plate au has been described as: (i) ultrathin but postprimordial (Ryan et al. 19 99)\; broken (Melendez et al 2010)\; and (iii) undergoing meltdown (Bonifa cio et al 2010). We also know that both of the known dwarfs with [Fe/H] < -4.5 have lithium abundances well below the value on the Spite Plateau. I propose to present further Li abundances for extremely metal-poor dwarfs in the range -4.0 < [Fe/H] < -3.0\, and to discuss the tensions and curiou s differences that currently exist among the various observational results \, including those of the most Fe-poor star currently known\, SM0313-6708 ([Fe/H] < -7.3). LAST-MODIFIED:20150330T013107Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:John Norris (RSAA) "The Lithium Abundances of the Most Metal-poor S tars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150417T042000Z DTEND:20150417T044000Z DTSTAMP:20261011T152429Z UID:92n2vjjch9cto84blj10k29vr8@google.com CREATED:20150119T064124Z DESCRIPTION:The SAMI Galaxy Survey has now observed more than a thousand ga laxies from the nearby universe. I will give an overview of the SAMI Galax y Survey data and discuss some of the work being done by RSAA on the emiss ion line properties\, in particular the complexities associated with ident ifying shocks and some of the interesting galaxy features we've found to d ate. LAST-MODIFIED:20150413T040607Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anne Medling (RSAA) "Shocks in SAMI Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160812T040000Z DTEND:20160812T042000Z DTSTAMP:20261011T152429Z UID:hn2to672bq7fj03dhe2upsa2sc@google.com CREATED:20160525T032118Z DESCRIPTION:I briefly review recent developments in Galactic bulge science for non-bulge Astronomers. Recent years have seen a precision mapping of t he global parameters of the Galactic bulge such as the distance\, structur e\, extinction\, and metallicity-distribution function of the bulge. New a reas of investigation including chemical tagging\, chemodynamical families \, dark matter mapping\, and the search for the oldest stars in the Galaxy . In most of these areas\, and in Galactic bulge research as a whole\, ANU astronomers have played a leading role in defining\, redefining\, and lea ding bulge-related research. LAST-MODIFIED:20160808T115106Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:David Nataf (RSAA) "Galactic Bulge Review Talk for non-Bulge Astron omers" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240503T040000Z DTEND:20240503T050000Z DTSTAMP:20261011T152429Z UID:l0ro1ciei71oe235pll3rld3fk@google.com CREATED:20240428T031609Z DESCRIPTION:N/A LAST-MODIFIED:20240428T031609Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Christoph Federrath) \nZoo m: https://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Christoph Federrath (RSAA) "HDR school review town hall" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260414T050000Z DTEND:20260414T063000Z DTSTAMP:20261011T152430Z UID:mlffs78and8askcjc4qc1f3t00@google.com CREATED:20251125T233111Z DESCRIPTION:Our monthly skillshare sessions offer a practical\, hands-on sp ace for students and postdocs to exchange research skills\, professional d evelopment tools\, and effective workflows in an informal and supportive s etting. Skillshare is run on the second Tuesday of each month\, 3:00-4:30 ish pm in the CSO Common Room\, with ~15-30 minutes of introduction follow ed by ~30-60 minutes of panel discussions or open-ended hands-on activitie s. LAST-MODIFIED:20260210T225221Z LOCATION:CSO Common Room (in-person only) (host: Sven Buder) \nZoom: https: //anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Monthly Skillshare (RSAA) "Github basics and workflows using online presence as example" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150703T040000Z DTEND:20150703T042000Z DTSTAMP:20261011T152429Z UID:j1hvllpab9l9gjtntq7pjos7sk@google.com CREATED:20150514T203613Z DESCRIPTION:The CHARA array at Mt Wilson\, California\, is the world’s hi ghest angular resolution instrument\, able to image the surface of stars a nd measure angular diameters down to about 200 micro-arcseconds. With six simultaneous telescopes\, ~300 optical elements\, dozens of active servo l oops and ~500 actuators\, the system is already arguably the most complex optical or infrared telescope system in the world. It is capable of full r emote operation\, and runs with a staff of approximately 10 people and a p ublication rate of approximately 14 papers/year (including several in Scie nce and Nature). Despite the success of CHARA\, the future of the facility depends critically on improved sensitivity and precision. I will describe the adaptive optics upgrade currently underway\, which includes a feed fo rward component where the wavefront sensor is located 200m upstream of the deformable mirror in the optical train. I will conclude with the kinds of science that these upgrades will enable\, focusing on young stars and exo planets. LAST-MODIFIED:20150703T055106Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Michael Ireland (RSAA) "The Adaptive Optics Upgrade for the CHARA A rray" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201116T220000Z DTEND:20201116T230000Z DTSTAMP:20261011T152429Z UID:p013bm1uk3k9pvn2ad4885ggdk@google.com CREATED:20200916T021117Z DESCRIPTION:The Vera C. Rubin Observatory will capture images of the full s outhern sky every 3/4 nights. It will increase our knowledge of our deep a nd dynamic universe focusing on\; (i) dark energy and dark matter\, (ii) c ataloging the solar system\, (iii) Milky Way structure and formation and ( iv) exploring the transient sky. The Rubin Obs. survey goals — wide\, fa st\, deep — led to a very different observatory that required adaptation and optimization. The active optics for instance needed to be optimized t o achieve the best image quality possible (still seeing limited) over its 3.5 degrees field of view\, to enable such great research. In this present ation\, I will briefly go over the science goals of Rubin Obs. and will ta lk in more details about their implications on the observatory design. In particular\, I will focus on the strategy to obtain the image quality need ed for such goals. I will also give an update of the Rubin Obs. constructi on. LAST-MODIFIED:20201111T113609Z LOCATION:ZOOM 997 8534 1005 (host: Menon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sandrine Thomas (Rubin Observatory/LSST\, USA) "Invited Colloquium: The Vera C. Rubin Observatory: an Original System to Discover the Deep an d Dynamic Universe" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250313T000000Z DTEND:20250313T010000Z DTSTAMP:20261011T152429Z UID:aqcrs8v28qclgt3b85vo5lsdhs@google.com CREATED:20241121T045619Z DESCRIPTION:Neutral hydrogen (HI) absorption provides a window into the col d neutral gas of the interstellar medium (ISM). Using the ASKAP telescope\ , the Galactic ASKAP (GASKAP) project is surveying HI absorption across th e Galactic plane and the Magellanic clouds\, massively increasing our know ledge of cold HI. How do you scale up a boutique process previously used f or a few tens of spectra to something that can be run across hundreds of t housands of measurements that GASKAP will obtain though? And what is this unprecedented data set telling us about the ISM in our Galaxy and our near est neighbours? In this talk I will describe the data validation processes and absorption pipeline that go together to produce the GASKAP HI absorpt ion dataset\, and the cold gas properties of the Magellanic system. LAST-MODIFIED:20250309T224107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Naomi McClure-Griffiths) \ nZoom: https://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQ T09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:James Dempsey (RSAA) "HI Absorption with GASKAP (End-of-thesis talk )" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210601T010000Z DTEND:20210601T020000Z DTSTAMP:20261011T152430Z UID:5tj9iokttmomjggsrea089i59c@google.com CREATED:20210303T022122Z DESCRIPTION:TBD LAST-MODIFIED:20210528T033107Z LOCATION:ZOOM and DLT (host: Sven Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dorrit Jacob (ANU RSES) "Invited Colloquium: Biomineralization and diamond formation in the Earth's lithosphere" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150625T230000Z DTEND:20150626T050000Z DTSTAMP:20261011T152429Z UID:3fbn6e314v5stpgjpf3lnb7d8g@google.com CREATED:20150511T053111Z DESCRIPTION:Various student talks will be presented. LAST-MODIFIED:20150625T044106Z LOCATION:Duffield Lecture Theatre (host: David Yong) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Students (RSAA) "Annual student thesis talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210629T010000Z DTEND:20210629T020000Z DTSTAMP:20261011T152429Z UID:5ospc9725nrdmoovp5blg6h7qs@google.com CREATED:20210215T211126Z DESCRIPTION:High-redshift galaxies are the source of the ionizing radiation responsible for driving the Epoch of Reionization (EoR). Our knowledge o f high redshift (z>6) galaxy formation is constantly improving and will ta ke yet another important step forward with the imminent launch of JWST. I n tandem to this\, the upper limits on the 21cm power spectrum from neutra l hydrogen during the EoR are continually improving\, with a firm measurem ent being a certainty in coming years. In order to maximise what we can l earn from these two complimentary observational datasets\, we need to be a ble to model them together\, self-consistently. However\, this is a diffic ult task. In this talk I will give a brief overview of why this is\, befor e moving on to discuss semi-analytic models as a useful and powerful compl iment to other relevant simulation methods. I will then present some of th e recent and ongoing work being carried out at the University of Melbourne ASTRO 3D node using the Meraxes semi-analytic model to explore high redsh ift galaxy formation and the EoR. In particular\, I will focus on the effe cts of dust modelling assumptions on inferred galaxy formation parameters\ , constraining the escape fraction of ionising photons\, and extending the mass resolution of simulations to resolve the faintest ionising sources. To finish off\, I will switch gears and discuss Science and Technology Aus tralia's STEM Ambassador program and the importance of scientists actively advocating for evidence based policy and interacting with politicians. LAST-MODIFIED:20220618T125715Z LOCATION:ZOOM and DLT (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Simon Mutch (Uni Melbourne) "Invited Colloquium: Modelling the firs t galaxies and the Epoch of Reionization" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190404T000000Z DTEND:20190404T010000Z DTSTAMP:20261011T152429Z UID:j3uho1g319saq16cqvtsr3e4lg@google.com CREATED:20190317T232612Z DESCRIPTION:The cloud-scale physics of star formation and feedback represen t the main uncertainties in galaxy formation and evolution studies. In rec ent years\, it has become clear that the “star formation relation” bet ween the gas mass (surface density) and the star formation rate (surface d ensity) depends strongly on the spatial scale. We have shown that this mul ti-scale nature of the star formation relation is a direct probe of the cl oud-scale physics of star formation and feedback. By quantifying the detai ls of this scale dependence\, we can directly measure fundamental quantiti es describing star formation and feedback\, such as molecular cloud lifeti mes\, star formation efficiencies\, feedback timescales\, feedback outflow velocities\, feedback coupling efficiencies\, and coherence length scales . While these quantities were previously only accessible in the Local Grou p\, it is now possible to measure them across a representative part of the galaxy population\, from the nearby Universe out to high redshift (z > 2) . I will present the first systematic characterisation of the evolutionary timeline of molecular clouds and star-forming regions using the above met hod\, across a wide variety of galactic environments. I will show that sta r formation is regulated by efficient stellar feedback\, driving GMC dispe rsal on short timescales (1-5 Myr) due to radiation and stellar winds\, pr ior to supernova explosions. This feedback limits GMC lifetimes to about o ne dynamical timescale (10-30 Myr)\, with integrated star formation effici encies of only a few percent. Our findings reveal that galaxies consist of building blocks undergoing vigorous\, feedback-driven lifecycles\, that v ary with the galactic environment and collectively define how galaxies for m stars. These observations settle a long-standing question on the multi-s cale lifecycle of gas and stars in galaxies\, and open up the exciting pro spect of characterising cloud-scale star formation and feedback during gal axy formation and evolution. LAST-MODIFIED:20190327T113108Z LOCATION:CSO Common Room (host: Oh) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Melanie Chevance (Heidelberg University) "The Physics Driving the M olecular Cloud Lifecycle during Galaxy Formation and Evolution" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250506T010000Z DTEND:20250506T020000Z DTSTAMP:20261011T152429Z UID:aijm7bmp3sg60m9ovsrlg7bjv0@google.com CREATED:20250106T230128Z DESCRIPTION:Exoplanetary systems show an incredible diversity\, hosting pla nets with a vast range of masses\, radii\, and orbital separations. Howeve r\, it remains unclear whether this diversity stems from a distribution of initial conditions or is the result of multiple planet formation pathways . It is therefore fundamental to detect young\, embedded planets during th eir formation process. Recent observations of protoplanetary discs have re vealed rings and gaps\, spirals\, and asymmetries. These features have bee n interpreted as signatures of newborn protoplanets\, but their exact orig in remains unknown and\, until recently\, was poorly constrained by direct observation. In this talk\, I will show how high spatial and spectral res olution ALMA observations can be used to detect embedded planets within th eir discs. In particular\, I will present results from the exoALMA planet- hunting campaign\, which targeted 15 protoplanetary discs with deep\, high spatial and spectral resolution line observations. I will also discuss th e implications for planet formation pathways and share our new kinematic v iew of the physical processes at play during planet formation. LAST-MODIFIED:20250428T044108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Christophe Pinte (Monash U.) "Observing Planet Formation" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250904T010000Z DTEND:20250904T020000Z DTSTAMP:20261011T152429Z UID:jv0guafpro5ha5hb20qus805os@google.com CREATED:20250729T022110Z DESCRIPTION:Although the case against the existence of physical infinities has been made throughout history\, it is only in recent years that substan tial arguments against their existence have been formulated. This seminar will present these arguments and discuss the principal cosmological implic ations of the absence of physical infinities. LAST-MODIFIED:20250729T022110Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Peter Riggs (ANU Physics) "The Non-Existence of Physical Infinities and its Cosmological Implications" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240416T010000Z DTEND:20240416T023000Z DTSTAMP:20261011T152429Z UID:7or9svut9l5pdjtk51eae3sal4@google.com CREATED:20240321T034616Z DESCRIPTION:Understanding how galaxies form and evolve requires knowledge o f their cold gas component\, and how this depends on their structural and star formation properties\, as well as large-scale environment. Significan t effort has gone into large\, dedicated observing campaigns that have mea sured the atomic and molecular hydrogen content of sizeable samples of gal axies on global and local scales\, and placed these in the context of thei r optical and star-formation properties as well as environments. Despite t hese efforts\, much remains to be learned about the physical drivers of th ese relations and how the global cold gas properties of galaxies are linke d to the local process of star formation\, as well as how these relations evolve with cosmic time. In this talk I will discuss how ongoing surveys o f atomic and molecular gas content of galaxies -- from global to kpc scale s and from nearby to higher redshift systems -- are advancing this field a nd conclude with a forward outlook on Square Kilometer Array science in th is area. LAST-MODIFIED:20240326T223116Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hilay Shah) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Barbara Catinella (UWA) "The gas-star formation cycle in galaxies: a multi-scale and multi-phase challenge" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180710T010000Z DTEND:20180710T020000Z DTSTAMP:20261011T152429Z UID:npjeo84desghoqhn7geufmaijg@google.com CREATED:20180701T032206Z DESCRIPTION:The formation and evolution of spiral galaxies is a research to pic central to modern Astronomy. In this context\, the Milky Way offers a unique opportunity for astronomers to study a spiral galaxy in detail and thus informs many aspects of galaxy formation theory. The observational si gnatures of Galactic stellar components provide clues to its assembly hist ory. This thesis is focused on two main components of the Galaxy: the stel lar disk and bulge. In particular\, we examine the chemical properties of these components and their implications for Galactic evolution. LAST-MODIFIED:20180702T005106Z LOCATION:CSO common room (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ly Duong (RSAA) "Understanding the evolution of the Milky Way disk and bulge with the GALAH survey and HERMES spectrograph(End-of-thesis coll oquium)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240215T000000Z DTEND:20240215T010000Z DTSTAMP:20261011T152429Z UID:32bhml576bpjalcrgr76coglf4@google.com CREATED:20240207T050611Z DESCRIPTION:Industry or external engagement and career development for HDR candidates are inextricably related. With around half of our PhD graduates going on to careers outside academia\, we want to ensure they are in the best position to contribute their specialist skills\, knowledge and capabi lities. In this workshop I will discuss one of the major engagement pathwa ys for HDR candidates\, research internships\, explain the administrative process for it\, outline ANU supports and offer pointers on how HDR candid ates and supervisors can get started. At the end of the session we will al so have time for Q&A. LAST-MODIFIED:20240207T050611Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Christoph Federrath) \nZoo m: https://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ulrike Proske (ANU Office of the Dean (HDR)) "Industry engagement f or HDR candidates -- Research internship" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240521T010000Z DTEND:20240521T023000Z DTSTAMP:20261011T152429Z UID:gur3aigl4493iph0l2qs72vc9c@google.com CREATED:20231212T120231Z DESCRIPTION:The ASKAP First Large Absorption Survey in HI (FLASH) is a larg e-area search for neutral hydrogen in and around distant galaxies at redsh ift 0.4 < z < 1.0\, a cosmic epoch where our knowledge of the HI content o f galaxies remains patchy and incomplete. FLASH has two main science goals : to probe the redshift evolution of the neutral gas content of galaxies\, and to investigate gas accretion and feedback processes in active galacti c nuclei. Radio searches in the HI 21-cm line are unaffected by dust extin ction\, and FLASH provides one of the first genuine ‘HI-selected’ gala xy samples at intermediate redshift. I will give an update on the status o f the survey and present some new science results from papers recently sub mitted or in preparation. I will also outline the prospects for the full ( 24\,000 square degree) ASKAP FLASH survey which is due for completion in 2 028. LAST-MODIFIED:20240504T104112Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hiep Nguyen) \nZoom: https ://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Elaine Sadler (U. Sydney / CSIRO) "Neutral hydrogen in the distant Universe" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190704T010000Z DTEND:20190704T020000Z DTSTAMP:20261011T152429Z UID:e5juan26j4gumai1mstsu0ccr0@google.com CREATED:20190619T042104Z DESCRIPTION:Gas flows drive galaxy appearances\, from the largest scales wh ere they fuel galaxy formation and provide angular momentum\, to galaxy sc ales where density perturbations drive the appearance of spiral arms\, dow n to the smallest where the turbulent motions are key in determining how a nd where stars form. I will touch upon all these through three different s urveys I am involved in. I’ll describe how we can drive down to the phys ics of the links between galaxy evolution and gas flows using the statisti cs of the large galaxy surveys possible with the latest instruments like M USE\, ALMA and ASKAP. LAST-MODIFIED:20190624T021605Z LOCATION:Duffield Lecture Theatre (host: Battisti) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Brent Groves (RSAA) "The flows of gas: linking galaxy evolution and gas at multiple scales" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260721T050000Z DTEND:20260721T060000Z DTSTAMP:20261011T152430Z UID:hmn35c9b18nvo51t67c7jgebso@google.com CREATED:20260503T114411Z DESCRIPTION:Our monthly skillshare sessions offer a practical\, hands-on sp ace for students and postdocs to exchange research skills\, professional d evelopment tools\, and effective workflows in an informal and supportive s etting. Skillshare is run on the second Tuesday of each month\, 3:00-4:30i sh pm in the CSO Common Room\, with ~15-30 minutes of introduction followe d by ~30-60 minutes of panel discussions or open-ended hands-on activities . LAST-MODIFIED:20260713T000006Z LOCATION:CSO Common Room (host: Sven Buder) \n SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Monthly Skillshare (RSAA) "Technical Skill: MCMC uncertainty estima tion" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180326T000000Z DTEND:20180326T010000Z DTSTAMP:20261011T152429Z UID:7ds357igah85jr75f64q2pocvg@google.com CREATED:20180302T010106Z DESCRIPTION:The Hubble Space Telescope is operating at peak scientific capa bility even 28 years after its launch\, thanks to successful astronaut ser vicing missions and operations that keep the observatory in top condition. I will review the premiere scientific advancements achieved by Hubble\, including both those that were planned at launch (e.g. measuring the Hubbl e constant) and many that were never dreamed of at launch (e.g. finding ev idence for dark energy\; analyzing exoplanet atmospheres). Hubble observa tions are now helping prepare for JWST and other future missions\, and are contributing critical complementary observations for solar system probes like JUNO and New Horizons. I will discuss how Hubble can be used in its coming final years to provide the best science return\, complementing othe r space-based and ground-based observatories and setting the stage for fut ure flagship missions. LAST-MODIFIED:20180319T122608Z LOCATION:Duffield Lecture Theatre (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jennifer Wiseman (NASA Goddard) "The Hubble Space Telescope: 28 Yea rs of Cosmic Discovery" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260728T010000Z DTEND:20260728T020000Z DTSTAMP:20261011T152430Z UID:flpk6tbp4l9hode4ovdrdcinug@google.com CREATED:20260503T113729Z DESCRIPTION:My research connects stars\, dust\, and gas\, with the goal of building a unified multidimensional picture of the Milky Way and nearby ga laxies. I study the lifecycle of matter in galaxies: how gas and dust form molecular clouds\, how stars are born from these environments\, and how s tellar evolution and feedback return material back to the interstellar med ium. A central challenge is that galaxies and their internal structure\, i ncluding molecular clouds\, are complex\, hierarchical\, and only partiall y observed: we often infer intrinsically 3D processes from 2D projections\ , with incomplete distance and velocity information. To address this\, I d evelop data-driven machine learning methods that combine heterogeneous obs ervations into physically interpretable maps. These include Gaussian-proce ss based methods for 3D and 6D astrocartography\, which reconstruct the sp atial and kinematic structure of interstellar material\, and Gaussian mixt ure models with spatial Gaussian-process priors\, which allow us to infer structured stellar and dust populations while preserving spatial coherence .\n\nI will present my research built around these ideas\, from the discov ery and characterisation of the nearest molecular cloud to earth\, Eos\, t o 3D dust maps of Milky Way dust and molecular cloud structure\, and ongoi ng work on mapping the dust density in M33 using mixture models with GP pr iors. I will also discuss efforts to identify and characterise feedback-dr iven bubbles in both 2D observations and 3D data\, linking statistical str ucture to the physics of star formation and feedback. Looking ahead\, I wi ll outline how these tools can support future observational programs\, inc luding the NASA SMEX mission\, Eos. Together\, this work seeks to move fro m static snapshots of the Milky Way and nearby galaxies toward a unified\, multidimensional picture of how stars\, dust\, and gas interact across th e lifecycle of matter in galaxies and how they evolve. LAST-MODIFIED:20260716T040007Z LOCATION:Zoom or Duffield Lecture Theatre (host: Sven Buder) \nZoom: https: //anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:2 STATUS:CONFIRMED SUMMARY:Thavisha Dharmawardena (Monash U.) "Towards a Multidimensional View of the Milky Way and Nearby Galaxies: Tracing Stars\, Gas\, and Dust from the Nearest Molecular Cloud to Our Galactic Neighbours" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151002T040000Z DTEND:20151002T042000Z DTSTAMP:20261011T152429Z UID:5n19ij5nuam0kn59nndajugd8o@google.com CREATED:20150928T140106Z DESCRIPTION:Most applications for faculty positions request both a research and teaching statement. Having spent years honing one's research program\ , the former is relatively straight-forward. However\, most people have li ttle experience with developing a meaningful teaching philosophy even thou gh our primary job as faculty is to teach. What elevates a generic teachin g statement to an excellent one? In this informal discussion\, I provide s ome examples of proven learning methods such as peer instruction\, think/p air/share exercises\, in-class tutorials\, and undergraduate mentoring tha t can be incorporated into a personal teaching philosophy. LAST-MODIFIED:20150929T065106Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kim Vy-Tran (Texas A&M) "Tools for Developing a Teaching Philosophy " TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210325T000000Z DTEND:20210325T003000Z DTSTAMP:20261011T152429Z UID:updg66i1on8b1f1flc4od7mp4k@google.com CREATED:20210224T233114Z DESCRIPTION:Chemical tagging is a promising technique in galactic archaeolo gy to trace the evolutionary history of the Milky Way using elemental abun dances of stars along with galactic chemical evolution models to infer the ir birth location. However\, the precision with which elemental abundance s need to be measured and the precision that one can ascribe to formation locations is uncertain. Here\, I'll discuss my work on measuring the scal e of elemental abundance homogeneity in cosmological zoom-in simulations o f Milky Way-mass galaxies. I will show that 1-D galactic chemical evoluti on models are insufficient to capture the important azimuthal abundance st ructure that dominates galaxies at z > ~0.8. I will also show that 2-D ab undance patterns introduce more uncertainty in stellar birth sites than ty pical measurement uncertainties. This raises the important question\, how can we improve chemical evolution models to keep pace with higher resolut ion observations? LAST-MODIFIED:20210324T225606Z LOCATION:ZOOM (host: Sven Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Matthew Bellardini (UC Davis (USA)) "Constraining Chemical Tagging Using Simulated Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20211007T000000Z DTEND:20211007T003000Z DTSTAMP:20261011T152429Z UID:jo57n6a7dn8avc0bbdori0hpfo@google.com CREATED:20210908T004612Z DESCRIPTION:Massive stars contribute incredible amounts of energy to their surroundings across a variety of environments in the universe. Before the ir exciting deaths\, massive stars produce feedback through a number of me chanisms that are frequently used in subgrid physics models in galaxy simu lations to create realistic galaxies. Observations are a key to anchoring these simulations in reality\, but there has been limited work on this fro nt\, especially for the youngest\, embedded HII regions. I explore the eff ects of direct radiation pressure\, dust-processed radiation pressure\, ph otoionization heating and shock-heating from stellar winds in a sample of young HII regions (sources with radii < 0.5 pc) and determine which is the most important for very young stars. This analysis suggests radiative fee dback on dust drives the earliest stages of HII region expansion. Addition ally\, I study the effects of radiative feedback in an exciting population of extremely low-metallicity star-forming galaxies that have been discove red in the local universe which are analogues to Reionization Era galaxies . During the Epoch of Reionization radiative feedback played a significant role in shaping the universe\, and such analogues give us a detailed labo ratory to explore the effects from feedback. I present deep FUV and optica l spectra of two of these extreme emission line galaxies that have strong very-high-ionization optical and FUV emission lines (e.g.\, CIV\, HeII\, [ FeV]\, [ArIV]). I demonstrate that canonical photoionization models\, usi ng typical stellar population models\, catastrophically fail to reproduce the high-ionization emission lines. I constrain the stellar population pro perties using the FUV spectral features and explore the deficiencies of cu rrent stellar models. By simultaneously fitting the stellar and nebular em ission within these extremely high-ionization emission line galaxies\, I p rovide new observational benchmarks of radiative feedback for the next gen eration of stellar models at very low metallicity. By studying the effects of stellar feedback from single stars in the Milky Way to entire stellar populations in analogues to the first galaxies we can begin to build a coh erent picture of stellar feedback as it impacts the vast scales of the uni verse. LAST-MODIFIED:20210929T235607Z LOCATION:ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Grace Olivier (The Ohio State University\, USA) "Evolution of Stell ar Feedback from Reionization to The Milky Way: A Diverse Toolset of Imagi ng\, Spectroscopy\, and Modelling for Understanding the Impact of Massive Stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230131T000000Z DTEND:20230131T010000Z DTSTAMP:20261011T152430Z UID:cdtbo2fkosf7kvm9f01gkeskjo@google.com CREATED:20230123T033607Z DESCRIPTION:In recent years\, there has been an increasing interest in the role of cosmic rays (CRs) in galaxy evolution. Most galaxy simulations inc luding a relativistic CR fluid have shown that the latter can contribute t o the dynamics of the interstellar medium (ISM)\, aiding in the internal s upport against gravity and in the launching of galactic outflows. However\ , the extent to which CRs affect these phenomena is strongly sensitive to the way different CR transport mechanisms are treated in simulations. With the goal of understanding the details of CR transport on galactic scales\ , we compute the propagation of mildly-relativistic CRs in three different galactic environments typical of nearby disk galaxies reproduced by the T IGRESS simulations. We consider the realistic scenario in which resonant A lfven waves are responsible for CR scattering\, with a scattering coeffici ent that varies with the properties of the background gas. I will review t he main results of this analysis and discuss the potential impact of CRs o n the dynamical state of the ISM. LAST-MODIFIED:20230126T011606Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Aditi Vijayan) \nZoom: ht tps://anu.zoom.us/j/99785341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Lucia Armillotta (Princeton) "Cosmic-ray transport in star-forming galactic disks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240412T040000Z DTEND:20240412T050000Z DTSTAMP:20261011T152430Z UID:jseceep1i5gfojqanvo30fasjo@google.com CREATED:20240227T234128Z DESCRIPTION:TBC LAST-MODIFIED:20240227T234128Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Sven) \nZoom: https://anu. zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Nian (Jenny) Jiang (RSAA/AITC) "Alternative Career Pathways" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170210T030000Z DTEND:20170210T032000Z DTSTAMP:20261011T152430Z UID:1i27ps769eqvk60rrookkl9cd8@google.com CREATED:20170113T045606Z DESCRIPTION:Ultra-violet (UV) astronomy has long been neglected due to the UV opacity of the ozone layer\, and the cost involved to be a telescope sy stem that works. Typically UV telescopes are space-based\, with large comp lexities and costs\, however\, a balloon-based UV survey telescope\, GLUV \, offers a much cheaper and simpler alternative. Each GLUV is expected t o feature a primary mirror of 20-30cm\, observe at near-UV wavelengths (25 0-300nm)\, and observe up to 250 square degrees with a daily cadence for 6 month campaigns. The long term goal will be a constellation of 50 GLUVs a t one time. The unique wavelength range and cadence makes GLUV ideal for a variety of science cases\, primarily transient explosions and exoplanet t ransits. Specifically\, I will show how GLUV will be able to detect supern ova shock interactions\, measure of exoplanet atmospheres through transits \, and detect gravitational wave counterparts. LAST-MODIFIED:20170207T045104Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ryan Ridden-Harper (RSAA) "GLUV: A Balloon Based High Cadence UV Su rvey - Thesis proposal" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180920T010000Z DTEND:20180920T020000Z DTSTAMP:20261011T152429Z UID:4dg74he7pa8g1jqj5cvi4jg648@google.com CREATED:20180827T012106Z DESCRIPTION:The Panchromatic Hubble Andromeda Treasury is an HST multicycle program to image the north east quadrant of M31 to deep limits in the UV\ , optical\, and near-IR. The HST imaging has resolved the galaxy into over 150 million stars (comparable to ~1/2 the number of stars in SDSS)\, all with common distances and foreground extinctions. We have recently complet ed comparable imaging for the high-intensity star forming disk of M33. The se surveys add M31 and M33 to the Milky Way and Magellanic Clouds as funda mental calibrators of stellar evolution and star-formation processes. I wi ll briefly describe the survey strategy\, data reduction\, and key data pr oducts. I will then highlight work using the NIR stellar populations to co nstrain the large scale properties of the cold ISM\, with 25 pc resolution . These new maps offer the highest resolution available in M31\, and point to surprising challenges facing models of dust emission and new possibili ties for the study of pressure as a driver of star formation efficiency. LAST-MODIFIED:20180920T014606Z LOCATION:Duffield Lecture Theatre (host: Battisti) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Julianne Dalcanton (University of Washington) "Dissecting the Neare st Spiral Galaxies with the Hubble Space Telescope" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191025T030000Z DTEND:20191025T033000Z DTSTAMP:20261011T152429Z UID:ban19q6g74oa995mnu45om1v88@google.com CREATED:20191004T042611Z DESCRIPTION:Future wide Field of View high-order Adaptive Optics (AO) syste ms will be using multiple laser guide stars (LGSs) and deformable mirrors (DMs) conjugating at different altitudes (Multi-Conjugate AO\, MCAO). A to mographic reconstructor is required in such systems to compute the MCAO co rrections to be applied to DMs. While classical tomography algorithms like tSVD or MMSE are still used in existing AO systems\, Learn And Apply (LAA )\, a novel tomography approach first proposed in 2010 on Multi-Object AO systems\, has the potential of delivering better\, more uniform performanc e with the help of multiple fictive sensors. In this talk I will present m y PhD progress with respect to AO tomography algorithm simulations from ye ar 2018\, including atmosphere turbulence model\, tomography algorithms an d performance analysis. LAST-MODIFIED:20191023T002606Z LOCATION:Duffield Lecture Theatre (host: Zhang) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Hao Zhang (RSAA/AITC) "AITC Series - Laser Tomography in High-order Adaptive Optics" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160819T040000Z DTEND:20160819T042000Z DTSTAMP:20261011T152430Z UID:jakijki9u8m7ig32mnk3qos5os@google.com CREATED:20160808T115108Z DESCRIPTION:I discuss my fitness journey and motivations to recover my heal th after it reached a trough following two events in 2012\, the death of m y father and the completion of my PhD. I review the method I used first\, which worked inefficiently and at a snail’s pace\, as well as results fr om the literature of other methods that don’t work. I then discuss recen t developments that are transforming the field\, such as the evolving advi ce on nutritional supplements\, the importance of intensity in exercise\, the role of gut bacteria\, renewed interest in the benefits of fats and ch olesterols\, and the surprising benefits of fasting. References and recomm ended reading are provided. LAST-MODIFIED:20160808T115108Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:David Nataf (RSAA) "How I Lost 20 Kg: A Review of the Literature in Nutrition\, Exercise and Health Science" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141205T030000Z DTEND:20141205T032000Z DTSTAMP:20261011T152429Z UID:ns45us80dnd4i5iloq95ketfl4@google.com CREATED:20141124T012107Z DESCRIPTION:I will summarise the work I have done here at RSAA on transitin g exoplanets\, particularly with regard to the HATSouth discoveries. I wi ll then discuss some of the exoplanet projects I will be involved with in my new position at Geneva Observatory - primarily NGTS\, CHEOPS\, ESPRESSO \, TESS and PLATO. LAST-MODIFIED:20141128T092608Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Daniel Bayliss (RSAA) "Final Talk: Transiting Exoplanets" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241018T030000Z DTEND:20241018T040000Z DTSTAMP:20261011T152429Z UID:qqs4evgpu35ii47bv437d7fqvo@google.com CREATED:20241017T015106Z DESCRIPTION:Following last week’s Town Hall discussion where the Vice Cha ncellor outlined the financial challenges for ANU and the proposed College s restructure\, I wanted to provide an opportunity for local questions and discussion. I will briefly reoutline the two key messages of the ANU fina ncial position and a proposed academic realignment\, and attempt to clarif y questions about these and/or possible implications for RSAA. LAST-MODIFIED:20241017T015106Z LOCATION:Duffield Lecture Theatre (host: Stuart Wyithe) \nZoom: https://anu .zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Stuart Wyithe (RSAA) "Renew ANU RSAA discussion" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220621T010000Z DTEND:20220621T020000Z DTSTAMP:20261011T152429Z UID:c7bgo1mfg1j4brek7mtolbf7lk@google.com CREATED:20220317T231225Z DESCRIPTION:Radio astronomy\, in particular the measurement of polarised ra dio emission\, allows us to investigate a vitally important yet understudi ed aspect of astrophysics: magnetic fields. Magnetic fields in an astrophy sical context influence star formation and the evolution and dynamics of g alaxies\, acting on a range of size scales from the size of stars to inter acting galaxy systems. Soon\, the next generation of telescopes like the A ustralian Square Kilometre Array (SKA) Pathfinder (ASKAP) will be fully fu nctional for radio polarimetry observations and as such require test field s before they undertake all-sky surveys. This thesis acts as a bridge betw een early radio polarisation studies and the next steps in the study of as trophysical magnetic fields\, heading towards the epoch of ASKAP and the S KA. We document the most complete study of the Magellanic Clouds and a cla ssification of Faraday complexity\, which can be utilised in future studie s of low-mass galaxies and complex magnetic fields. LAST-MODIFIED:20220620T054107Z LOCATION:DLT & ZOOM (host: Neco Kriel) \nZoom: https://anu.zoom.us/j/997853 41005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jack Livingston (RSAA) "PhD Thesis Talk: Exploring the Magnetic Fie lds of the Milky Way and Magellanic System" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220930T040000Z DTEND:20220930T043000Z DTSTAMP:20261011T152429Z UID:veu8aok78t5orijv7pt2ichuvk@google.com CREATED:20220907T000614Z DESCRIPTION:I will share my experience of working in the Australian Public Service in Canberra during the 2021-22 Floods\, and lessons learnt as a sc ientist engaging with the Prime Minister's Office. LAST-MODIFIED:20220926T082606Z LOCATION:DLT & ZOOM (host: TBD) \nZoom: https://anu.zoom.us/j/99785341005?p wd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Aditya Chopra (APS) "Why the APS needs more Astronomers" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230912T010000Z DTEND:20230912T023000Z DTSTAMP:20261011T152429Z UID:mpuppsr6enp1plc35c9jc58ldc@google.com CREATED:20230806T233118Z DESCRIPTION:Large galaxies like the Milky Way form hierarchically\, with sm aller systems merging and accreting to form increasingly massive structure s. Evidence for this process can be found all around us: spatially in the form of stellar streams and tidally disrupting satellites in the Galactic halo\; dynamically as stellar overdensities in phase space within the Gala ctic disk\; and chemically\, in the form of abundance patterns distinct fr om those of typical stars which formed in situ within the Milky Way. I wil l briefly outline what we know - or at least\, think we know - about the M ilky Way's assembly history\, highlighting the work of two ongoing Austral ian-led spectroscopic surveys\, GALAH and S5\, in identifying and characte rising discrete accretion events. Recent studies with GALAH data clearly s how the importance of abundance patterns for detecting accreted structures within the Galaxy\, while S5 results I will discuss include evidence for the influence of the LMC on halo stream orbits\, an apparent orbital bias in the stellar streams observed\, and comparisons with FIRE simulation pre dictions for detectable streams. I will conclude with a look at the prospe cts of new facilities such as LSST for driving major advances in our under standing of how galaxies like the Milky Way grow. LAST-MODIFIED:20230907T113607Z LOCATION:TBD (host: Trey) \nZoom: https://anu.zoom.us/j/83410388355?pwd=Qm9 CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Daniel Zucker (Macquarie University) "From Little Things Big Things Grow: Tracing the Milky Way's Assembly History" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141121T030000Z DTEND:20141121T031500Z DTSTAMP:20261011T152430Z UID:btmm8e63mkmvhjqg9e3q6mh62o@google.com CREATED:20250925T231019Z DESCRIPTION:Sophisticated chemical evolution models have been successful in reproducing the current abundance gradient in our Milky Way and other nea rby galaxies\, but these models produce dramatically conflicting predictio ns for galaxies at intermediate distances and in the early universe. One m ajor problem with this work is that metallicity calibrations have been hin dered by large discrepancies\, particularly between diagnostics that use d ifferent sets of emission-lines\, and these discrepancies are not well und erstood. Fortunately\, large integral field spectroscopic surveys offer t he first large local datasets to resolve this issue and in this project\, 6 different metallicity calibrations were applied to a star-forming galax ies from the SAMI galaxy survey. LAST-MODIFIED:20250925T231019Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Diane Salim (RSAA) "Metallicity Calibrations and Gradients in SAMI Star-forming Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160315T000000Z DTEND:20160315T010000Z DTSTAMP:20261011T152429Z UID:cim7t02tp26naqkqsjvv8gok4k@google.com CREATED:20160224T231609Z DESCRIPTION:The heaviest elements in the periodic table are synthesized thr ough the r-process\, but the astrophysical site for r-process nucleosynthe sis is still unknown. The major current candidates are ordinary core-colla pse supernovae and neutron star merger. Ancient\, metal-poor ultra-faint d warf galaxies contain a simple fossil record of early chemical enrichment that provides the means to study clean signatures of nucleosynthesis event s\, and thus\, can yield unique information on the origin of these process es. Previously\, extremely low levels of neutron-capture elements were fou nd in the metal-poor stars in ultra-faint dwarf galaxies which supported s upernovae as the r-process site. Based on Magellan/MIKE high-resolution sp ectroscopy\, we have determined chemical abundances of nine stars in the r ecently discovered ultra-faint dwarf Reticulum II. Seven stars display ext remely enhanced r-process abundances\, comparable only to the most extreme r-process enhanced metal-poor stars found in the Milky Way's halo. The en hancement is also 2-3 orders of magnitude higher than that of stars in any of the other ultra-faint dwarfs. This implies the neutron-capture r-proce ss material in Reticulum II was synthesized in a single prolific event tha t is incompatible with r-process yields from ordinary core-collapse supern ovae but consistent with that of a neutron star merger. This would be the first signature of a neutron star merger in the early universe which holds the key to finally identifying the r-process production site. Furthermore \, such a single r-process event is a uniquely stringent constraint on the metal mixing and star formation history of this ultra-faint dwarf galaxy. (accepted for publication in Nature\, http://arxiv.org/abs/1512.01558) LAST-MODIFIED:20160309T002106Z LOCATION:Duffield Lecture Theatre (host: Helga Denes) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anna Frebel (MIT) "A single prolific r-process event preserved in a n ultra-faint dwarf galaxy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190827T010000Z DTEND:20190827T020000Z DTSTAMP:20261011T152429Z UID:sv89cn2h1ocmg3ss1qb5laujrc@google.com CREATED:20190731T062111Z DESCRIPTION:The gas-phase metallicity is one of the most fundamental proper ties of a galaxy. Measuring the gas-phase metallicity distribution allows us to gauge the age of the gas and hence how the galaxy has formed over ti me. By combining the gas-phase metallicity with galaxy evolution simulatio ns\, we can gain insight into dynamical processes which may have affected its formation process in the past. In my PhD\, we use spatially resolved s pectra from the SAMI galaxy survey and TYPHOON survey to explore the gas-p hase metallicity of galaxies as a function of stellar mass and environment . We also investigate the systematic errors and reliability of measuring g as-phase metallicity through popular strong emission line diagnostics. LAST-MODIFIED:20190823T034605Z LOCATION:Duffield Lecture Theatre (host: Oh) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Henry Poetrodjojo (RSAA) "Metallicity Gradients in Local Star-Formi ng Galaxies (End-of-Thesis Colloquium)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260917T010000Z DTEND:20260917T020000Z DTSTAMP:20261011T152430Z UID:4a1rg1tquuq1j6qlpl2bbjhsdk@google.com CREATED:20260915T050003Z DESCRIPTION:Since around 100 years it has been known that our Milky Way is not the only island of stars in the Universe. Many other galaxies have sin ce been found\, featuring an immense variety of properties. Diverse morpho logies\, kinematics\, and structures in their outskirts indicate that gala xies can have very different formation pathways. Over the years\, our gene ral understanding of galaxy evolution has improved through an increasing n umber of observations and simulations. But what about an individual galaxy ? What possibilities do we have to decipher the formation history of a sin gle galaxy from its observed present-day properties? Using a broad range o f observables in galaxies and comparing them between observations and simu lations\, I will present how these can be related to the formation histori es of galaxies and thus be used as indicators for an individual galaxy's p ast. For this\, I will show what information is encoded in the inner kinem atics of galaxies\, the low surface brightness structures found in their o utskirts\, and in the properties of so-called tracer populations: globular clusters and planetary nebulae. LAST-MODIFIED:20260915T050004Z LOCATION:Zoom or Duffield Lecture Theatre (host: N/A) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Lucas Valenzuela (RSAA) "What's Your Story? Deciphering galaxy form ation histories from present-day properties" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190502T033000Z DTEND:20190502T043000Z DTSTAMP:20261011T152429Z UID:p4eh2gr1h0ol5f91kjjkk08ols@google.com CREATED:20190325T095613Z DESCRIPTION:Strong gravitational lensing coupled with Integral field spectr ographic observations (IFS) and adaptive optics (AO) imaging techniques ha ve pioneered spatially resolved studies of high redshift galaxies (z>1). T he most magnificent cases of strong lensing are the giant arcs or multiple images around massive galaxy groups or clusters\, amplifying the total fl ux by a factor few times 10-100. With the recent advent of wide-field and multiple IFS (e.g.\, KCWI\, MUSE\, KMOS) on large telescopes\, we are no w entering an era of efficiently collecting spectra along the entire giant arcs. However\, there are a number of challenges in recovering the sourc e galaxy properties of such highly magnified arcs. The accuracy and precis ion of source-plane reconstruction of the most strongly lensed cases are f undamentally limited by 1. the lensing mass model and 2. the effect of the differential point-spread-function (PSF). While a huge effort has been ma de in the past decade to understand the systematics in lens modelling meth ods (e.g.\, Hubble Frontier Fields)\, relatively fewer work has been done on addressing the effect of the differential PSF. I aim to improve the sou rce reconstruction algorithms to achieve the highest resolution enabled by these lens models. Over the past 4 years of my PhD candidature\, we have developed an automated algorithm for forward source modelling of lensed ga laxies behind cluster-scale lenses that deconvolves the effects of PSF. Fu rthermore\, this algorithm fully exploits the natural resolution of lensin g and allows us to easily combine multiple images of the lensed galaxy to increase the signal to noise ratio in the source plane. Please join me in looking at high-redshift galaxies via nature's telescopes. LAST-MODIFIED:20190430T004605Z LOCATION:Duffield Lecture Theatre (host: Zerjal) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Soniya Sharma (RSAA) "High Resolution Source Reconstruction of Lens ed High Redshift Galaxies (End-of-Thesis Talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190724T040000Z DTEND:20190724T050000Z DTSTAMP:20261011T152429Z UID:oi4kpsbvcgki4mork7or2rjn8o@google.com CREATED:20190712T010606Z DESCRIPTION:[A colloquium by the shortlisted candidate for the new Centre f or Gravitational Astrophysics] The recent detections of gravitational wave s from merging black holes and neutron stars have established gravitationa l waves as a new cosmological messenger and opened remarkable opportunitie s for probing the nature of gravity and matter in unexplored regimes. Extr acting the rich science content of these gravitational-wave signals relies on cross-correlating the data with theoretical template models\, which mu st be highly accurate and efficient to generate. I will describe my recent work in developing such models using analytical methods and their connect ion to the nonlinear regimes accessible to numerical relativity simulation s. I will also discuss the importance of modeling for identifying the key characteristic parameters that link gravitational wave signatures to funda mental properties of the compact objects and for deriving new insights suc h as on nuclear physics from the observations\, and the greater impact fro m combining information in gravitational waves and electromagnetic counter parts. I will conclude with an outlook onto exciting prospects and urgent challenges as gravitational wave measurements transition from being isolat ed discoveries to precision physics in the next decade. LAST-MODIFIED:20190712T010606Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tanja Hinderer (University of Amsterdam) "Exploring new frontiers i n strong field gravity with gravitational waves" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200910T003000Z DTEND:20200910T013000Z DTSTAMP:20261011T152429Z UID:hfrhsmher35ttkli435au3shi0@google.com CREATED:20200831T060606Z DESCRIPTION:For those who haven't heard of us: Astronomy Data and Computing Services (ADACS) is an initiative of Astronomy Australia Ltd (AAL)\, deli vered in partnership with Swinburne University of Technology and Curtin Un iversity. We aim to provide astronomy-focused training\, support and profe ssional expertise to the Australian astronomy community to help it maximis e scientific returns on investments in data & computing infrastructure. O ne of the flagship programs of ADACS is its Merit Allocation Program. Thro ugh this program\, Australian astronomers can obtain access to the time of a group of dedicated professional software engineers (augmented with a su itable mix of computationally skilled astronomers) to start new software i nitiatives\; optimise established ones\; or to provide bespoke training wo rkshops. The allocation of resources is administered by an independent tim e allocation committee who evaluate proposals based on scientific merit an d impact. The call for expressions of interest for participation in the 2 021A semester (beginning Jan 1\, 2021) will open in early September\, with proposals due in early November\, 2020. In this talk I will provide a bri ef overview of ADACS and the ADACS Merit Allocation Program\, leaving time to answer questions regarding how to best engage this special program to grow or accelerate your research. If you have any additional questions or concerns - either after this talk or leading up to it - please don't hesit ate to contact me at gpoole@swin.edu.au. You can also visit https://adacs .org.au to learn more about ADACS and the services we provide. LAST-MODIFIED:20200907T041105Z LOCATION:ZOOM 997 8534 1005 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Gregory Poole (Swinburne University of Technology) "ADACS Merit All ocation Program - Overview and Q&A" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261110T040000Z DTEND:20261110T051500Z DTSTAMP:20261011T152430Z UID:3fqih1jf7ut22b0220b98ijg4c@google.com CREATED:20260503T114417Z DESCRIPTION:Our monthly Skillshare sessions provide an informal\, supportiv e\, and practical space for students and postdoctoral researchers to devel op and exchange research skills\, professional-development tools\, and eff ective workflows. The format is primarily focused on students. However\, e veryone is very warmly invited to join and contribute.\n\nSessions are hel d on selected Tuesdays from approximately 3:00-4:15ish pm in the CSO Commo n Room. Depending on the topic\, they may include short introductions\, de monstrations\, panel discussions\, interactive exercises\, or open-ended h ands-on activities. LAST-MODIFIED:20260803T020029Z LOCATION:Zoom or CSO Common Room (host: Sven Buder and Melanie Kaasinen) \n Zoom: https://anu.zoom.us/j/89544552112?pwd=Bdoo5fgMVS2Ls6e3Fs0NSNk9OMpaXn .1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA Skillshare (RSAA) "Mock Interviews" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151027T000000Z DTEND:20151027T010000Z DTSTAMP:20261011T152429Z UID:thfgpeearurodo1d4e579m0hh0@google.com CREATED:20150915T030111Z DESCRIPTION:The spectra of AGN host galaxies contain emission lines excited by radiation from both massive stars and the AGN accretion disk. Standard calibrations for the star formation rate\, AGN accretion rate and the phy sical conditions of the line-emitting gas are not applicable to such compo site spectra\, imposing significant limitations on studies of the physical processes driving the evolution of AGN host galaxies. In this talk I will explain how integral field spectroscopy can be combined with emission lin e ratio diagnostic diagrams to separate star formation\, AGN activity (and shock excitation!)\, both spatially and in their absolute contributions t o individual velocity components of individual emission lines. I will pres ent the first 2D maps of the star formation rates across AGN host galaxies without contamination from the AGN\, and the first maps of the narrow lin e region emission without contamination from star formation. The ability t o separate star formation and AGN activity will offer unprecedented insigh ts into the starburst-AGN connection\, both locally and at higher redshift s. LAST-MODIFIED:20151026T015605Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rebecca Davies (RSAA) "Dissecting Galaxies - Separating Emission Ex cited by Star Formation and AGN Activity" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190529T013000Z DTEND:20190529T020000Z DTSTAMP:20261011T152429Z UID:sijjon11e4s8fm2h7a4f089910@google.com CREATED:20190430T055612Z DESCRIPTION:The Australian Dark Energy Survey has conducted a 6-year Reverb eration Mapping program\, to measure the mass of the central supermassive black holes of almost 800 Active Galactic Nuclei at 0.13000 K-band sel ected galaxies at 0.6 < z < 1.0 with ultra-deep 20-hour long integration t imes on an 8 meter class telescope\, allowing both detailed stellar and ga s dynamical measurements. I will show for the first time that in the more massive galaxies\, the intrinsic gas velocity dispersion is not uniform as usually assumed\, but higher in their central regions. I will cross-check high redshift dynamical masses based on both stellar and ionised gas dyna mics and discuss the results in light of future observations with upcoming facilities\, which will probe the distant universe mainly through emissio n lines. LAST-MODIFIED:20190306T072608Z LOCATION:CSO Common Room (host: Cultinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Caroline Straatman (Ghent University) "Dynamical masses from stella r and gas kinematics and the LEGA-C survey at z ~ 1" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200911T040000Z DTEND:20200911T043000Z DTSTAMP:20261011T152429Z UID:l7eabf8hvfr712tc5i60chorro@google.com CREATED:20200824T044105Z DESCRIPTION:The new FoF format is like an Open Mic: Our speakers have 15 mi nutes each to talk about topics of their choice. The idea of the new FoF i s to get to know the many individuals that work under the same roof\, allo w newcomers to find friends easily\, and find new friends or colleagues wi th similar interests and hobbies. So feel free to talk about some of your most favourite adventures\, memorable Stromlo anecdotes\, your hobbies\, y our last COVID-DIY project\, your voluntary activities outside of Stromlo or whatever you are passionate about. Science talks (about a scientific to pic/question that you are interested in) are also welcome\, but be mindful of your audience (astronomers\, students\, engineers\, professional staff ). LAST-MODIFIED:20200909T205106Z LOCATION:ZOOM 997 8534 1005 (host: Martinez) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Katie Grasha and Lisa Kewley (RSAA) "FoF: Space Stamps and Gender D iversity at the ANU: 50:50 in 15 years" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181109T032000Z DTEND:20181109T034000Z DTSTAMP:20261011T152429Z UID:i3cblup6egspv15ef9an9rp8os@google.com CREATED:20181017T030106Z DESCRIPTION:Space debris poses a significant threat to the near-Earth space environment\, and has been a growing problem since the first satellite la unch in 1957. The Space Environment Research Centre (SERC) is building an Adaptive Optics Laser Guide Star Facility (LGSF) to improve debris trackin g abilities and eventually to enable laser pushing. In this talk I will pr esent my work on several of the LGSF subsystems including the beam transfe r optics and the beam centring loop. LAST-MODIFIED:20181031T003107Z LOCATION:Duffield Lecture Theatre (host: Zerjal) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Emily Rose Rees (AITC) "An Adaptive Optics Laser Guide Star Facilit y for Space Debris" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250722T010000Z DTEND:20250722T020000Z DTSTAMP:20261011T152429Z UID:3fr9o7lhhmbls266fvv505cumg@google.com CREATED:20250623T121107Z DESCRIPTION:In the current era of precision radial velocity instruments\, i t is the stellar behaviour that limits the detection of planets. Stellar m agnetic activity and surface phenomena can mask and mimic the signals of o rbiting planets\, even in quiet\, 'inactive' stars. This talk explores the current and emerging avenues for studying and mitigating stellar activity \, including the use of Gaussian Process (GP) regression to detect planets around stars of all activity levels\, and a new instrument for studying s tellar magnetic activity in the Southern hemisphere. LAST-MODIFIED:20250714T235707Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Tomasz Rozanski) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Belinda Nicolson (USQ) "One astronomer's noise is another's signal: Stars\, planets and magnetic fields" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251017T030000Z DTEND:20251017T033000Z DTSTAMP:20261011T152430Z UID:v11j8jd2remod0er97rjk7u3hk@google.com CREATED:20250917T113211Z DESCRIPTION:Turbulence is typically observed on large scales\, such as in a tmospheric flows or astrophysical gas clouds\, but the kinetic energy inje cted at these scales must eventually dissipate at comparatively smaller sc ales. In this talk I will explore where this kinetic energy goes\, in both the subsonic and supersonic regimes\, by using high resolution turbulence simulations. To characterise dissipative structures\, I will answer the f ollowing questions. How long does it take for large scale kinetic energy i njection to dissipate? And how is this dissipation correlated with key qua ntities such as the density and vorticity of the gas? On what scales is di ssipation strongest? What is the dimensionality of the turbulent structure s? LAST-MODIFIED:20251009T220607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Christoph Federrath) \nZoo m: https://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Edward Troccoli (RSAA) "On the dissipation of turbulence" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190219T030000Z DTEND:20190219T040000Z DTSTAMP:20261011T152429Z UID:ph66t0fl6uj56kpm3d7fhj2ejg@google.com CREATED:20190218T024604Z DESCRIPTION:We present a comprehensive suite of high-resolution (parsec-sca le)\, idealised (non-cosmological) galaxy merger simulations (24 runs\, st ellar mass ratio ~2.5:1) to investigate the connection between interaction -induced star formation and the evolution of the interstellar medium (ISM) in various temperature-density regimes. We use the GIZMO code and the sec ond version of the 'Feedback in Realistic Environments' model (FIRE-2)\, w hich captures the multi-phase structure of the ISM. Our simulations are de signed to represent galaxy mergers in the local Universe. In this work\, w e focus on the 'galaxy-pair period' between first and second pericentric p assage. We split the ISM into four regimes: hot\, warm\, cool and cold-den se\, motivated by the hot\, ionised\, atomic and molecular gas phases obse rved in real galaxies. We find that\, on average\, interactions enhance th e star formation rate of the pair (~30%\, merger-suite sample average) and elevate their cold-dense gas content (~18%). This is accompanied by a dec rease in warm gas (~11%)\, a negligible change in cool gas (~4% increase)\ , and a substantial increase in hot gas (~400%). The amount of cold-dense gas with densities above 1000 cm^3 (the cold ultra-dense regime) is elevat ed significantly (~240%)\, but only accounts for 0.15% (on average) of the cold-dense gas budget. LAST-MODIFIED:20190218T024604Z LOCATION:AITC1 Meeting Room (host: Battisti) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jorge Moreno (Pomona College) "Interacting galaxies on FIRE-2: The connection between enhanced star formation and interstellar gas content" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260324T003000Z DTEND:20260324T013000Z DTSTAMP:20261011T152430Z UID:p22cfletit5mi8fv1dj7b1dv2o@google.com CREATED:20260322T230605Z DESCRIPTION:The Parkes multi-beam system transformed single-dish radio astr onomy\, delivering the largest haul of new pulsars from any instrument\, d efinitive HI galaxy catalogues\, and the standard HI maps of the southern sky. These landmark surveys had to be conducted separately\, due to the co nflicting observation requirements between those of pulsars and HI. The el ectronic calibration (CAL) signal required for precise HI gain calibration contaminates pulsar power spectra and therefore must traditionally be swi tched off during pulsar searches. We invented the high-cadence CAL techniq ue\, in which the calibration signal is injected at the sampling rate and facilitate\, for the first time\, truly simultaneous pulsar and spectral-l ine surveys. Implemented on FAST with drift-scan mode\, the Commensal Radi o Astronomy FAST Survey (CRAFTS) has discovered more than 230 pulsars and 10 FRBs\, and released over 5\,000 square degrees of calibrated HI images. I will report several science highlights from CRAFTS\, including spatiall y resolved mapping of low-energy cosmic rays via HINSA\, origin of galacti c turbulence in M31\, and the origin of repeating fast radio bursts. LAST-MODIFIED:20260322T230606Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Maja Jablonska) \nZoom: ht tps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Di Li (Tsinghua U.) "The Commensal Radio Astronomy FAST Survey (CRA FTS) and a finding chart for SKA" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150417T040000Z DTEND:20150417T042000Z DTSTAMP:20261011T152429Z UID:n2u4qk1r1d3cis0t026f5a6hp0@google.com CREATED:20150119T064124Z DESCRIPTION:The recently discovered supernova 'SN Refsdal' and its lensed h ost galaxy is such a beautiful demonstration of the power of gravitational lensing. In this 15min talk\, I will tell you everything we know about this specific demonstration. LAST-MODIFIED:20150409T004109Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tiantian Yuan (RSAA) "The lensed host galaxy of the lensed supernov a 'SN Refsdal' at z = 1.49" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210305T030000Z DTEND:20210305T033000Z DTSTAMP:20261011T152429Z UID:rt8qh6h72pjknr8fq2qod10lpg@google.com CREATED:20210217T233111Z DESCRIPTION:We start the weekend with our new open-mic talks. LAST-MODIFIED:20210302T053106Z LOCATION:ZOOM and Duffield Lecture Theatre (host: Shyam Menon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Neco Kriel and TBD (RSAA) "Rubik's Cube through the lens of Group T heory" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260811T050000Z DTEND:20260811T061500Z DTSTAMP:20261011T152430Z UID:f06ro2lsb3hbp76p6t258kmjv0@google.com CREATED:20260803T010006Z DESCRIPTION:Our monthly Skillshare sessions provide an informal\, supportiv e\, and practical space for students and postdoctoral researchers to devel op and exchange research skills\, professional-development tools\, and eff ective workflows. The format is primarily focused on students\, in particu lar those enrolled in the ASTR8030 course Astronomy and Astrophysics Resea rch Skills. However\, everyone is very warmly invited to join and contribu te.\n\nSessions are held on selected Tuesdays from approximately 3:00-4:15 ish pm in the CSO Common Room. Depending on the topic\, they may include s hort introductions\, demonstrations\, panel discussions\, interactive exer cises\, or open-ended hands-on activities. LAST-MODIFIED:20260803T030007Z LOCATION:Zoom or CSO Common Room (host: Sven Buder and Melanie Kaasinen) \n Zoom: https://anu.zoom.us/j/89544552112?pwd=Bdoo5fgMVS2Ls6e3Fs0NSNk9OMpaXn .1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA Skillshare (RSAA) "Avoiding common writing pitfalls and buildi ng good habits" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180727T040000Z DTEND:20180727T042000Z DTSTAMP:20261011T152429Z UID:77vfv6bls862es84tgk7s6hfo0@google.com CREATED:20180501T043123Z DESCRIPTION:Science fiction has a rich variety of different stories. One co mmon trope is for characters to swap their minds or bodies and this is fre quently associated with a change of sex for the characters. I'll begin by examining some cases of this in different science fiction shows and discus sing why it isn't possible. Then I'll take a broader view of sex and gende r within science fiction\, considering symbiotic/parasitic aliens\, Time L ords and other examples of complex gender in alien species. Discussing how looking at these aspects give us a way to think about human sex and gende r. I'll finish off by talking about the only way that a body change may ac tually be possible that can be found in science fiction. LAST-MODIFIED:20180713T050110Z LOCATION:Duffield Lecture Theatre (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:J.J. Eldridge (The University of Auckland) "The Science of Sci-fi: body/mind swapping and gender diversity" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210622T010000Z DTEND:20210622T020000Z DTSTAMP:20261011T152429Z UID:nc4vec9so4hao4oep495cbuhts@google.com CREATED:20210211T053124Z DESCRIPTION:The Large and Small Magellanic Clouds (LMC/SMC)\, as two of the closest and most massive satellites of the Milky Way\, have significant e ffects on the local Universe\; including on the orbits of tidal streams\, and the distribution of ultra-faint satellites. However their masses\, and interaction history beyond the most recent LMC/SMC close passage\, remain poorly constrained. My thesis aims to understand the effects of past inte ractions between the Clouds by performing the first dedicated kinematic st udy of the Magellanic stellar outskirts. To do so\, I have developed and led the Magellanic Edges Survey (MagES)\, a spectroscopic study using 2dF+ AAOmega targeting ~8700 red clump and red giant branch stars across the hi ghly-substructured periphery of the Clouds. In combination with astrometri c measurements and high-precision photometry from the Gaia satellite\, the survey provides 3D kinematics and abundance information critical for unde rstanding the effects of dynamical perturbations on the Clouds. In this t alk\, I will present recent results from MagES on the kinematic and struct ural properties of the outer LMC\, including the origin of a large arm-lik e substructure to the north of the LMC found to be predominantly formed du ring a recent interaction with the Milky Way\; a sharp truncation in the w estern LMC disk likely due to an SMC crossing of the LMC disk plane ~400My r ago\; and complex southern substructures which are plausibly the result of multiple close interactions with the SMC over time. These are the first kinematic constraints on the dynamical history of the Clouds prior to the ir most recent close passage\, and will be critical for guiding future num erical models aiming to accurately describe the complex evolution of the M agellanic system. LAST-MODIFIED:20220618T125716Z LOCATION:ZOOM and Duffield Lecture Theatre (host: Lara Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Lara Cullinane (RSAA) "End-of-Thesis Colloquium: The Structure and Kinematics of the Magellanic Stellar Periphery" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160622T230000Z DTEND:20160623T000000Z DTSTAMP:20261011T152429Z UID:i96d2ravnau5qqkp6ue4nc0g5k@google.com CREATED:20160504T030115Z DESCRIPTION:TBD LAST-MODIFIED:20160504T030115Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Annual Student Talks (RSAA) "Various" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250925T010000Z DTEND:20250925T020000Z DTSTAMP:20261011T152430Z UID:caa9p63hr422pb7j1atlmcmn58@google.com CREATED:20250923T004106Z DESCRIPTION:Gravitational-wave observations by LIGO and Virgo have revealed a population of merging stellar-mass binary black holes. The recent GWTC- 4 data release has taken the number of confidently detected binary black h oles to over 150. While the broad connection between the inferred populati on and the physics that underlies black hole formation remains elusive\, t he new data is revealing new features in the population. In this talk\, I survey several of these interesting and sometimes perplexing features in t he population distribution. I will talk about what information about under lying formation channels and stellar astrophysics we can glean from them. I will also touch on the recent claims about evidence for pair instability transitions and put them in the context of what we understand about PISN stellar physics. LAST-MODIFIED:20250923T004106Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Lilli Sun) \nZoom: https:/ /anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sharan Banagiri (Monash U.) "The formation mechanisms of merging bi nary black holes: New insights from O4a" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181204T000000Z DTEND:20181204T010000Z DTSTAMP:20261011T152429Z UID:rcragnaa5mmf9ogbfm7h0d6l00@google.com CREATED:20180822T015210Z DESCRIPTION:Magnetic flux ropes - twisted bundles of magnetic field lines - are ubiquitous and fundamental structures in astrophysical and laborator y plasmas. Importantly\, they are reservoirs of free magnetic energy\, whi ch may be released in solar flares and in smaller flare-events associated with the heating of the solar corona. Magnetic reconnection allows restru cturing of the magnetic field and efficient dissipation of magnetic energy \, heating the plasma and generating non-thermal populations of electrons and ions. Reconnection also plays an important role in magnetically-confin ed fusion plasmas. The ideal kink instability in a twisted flux rope leads to the formation of current sheets and thus triggers magnetic reconnectio n\, in which the field relaxes to a lower energy state. First\, I will sh ow how instability in a single magnetic flux rope can lead to a confined s olar flare. Using a combination of 3D magnetohydrodynamic (MHD) simulation s and test-particles\, we predict observable signatures in both thermal an d non-thermal emission\, and thus propose a means for detection of twiste d magnetic fields in the solar corona. Then I will discuss interactions be tween multiple flux ropes\, showing how one unstable flux rope within an a rray of stable neighbours may trigger a heating avalanche. This has import ant implications for solar coronal heating. I will also describe MHD and t wo-fluid simulations of the merging of twisted magnetic tori during mergin g-compression formation of a spherical tokamak\, with application to the M AST device. Some ongoing studies of reconnection of magnetic filaments ass ociated with Edge Localised Modes in tokamaks will also be mentioned. LAST-MODIFIED:20181203T001104Z LOCATION:CSO Common Room (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Phillipa Browning (Jodrell Bank Centre for Astrophysics) "[RSAA/MSI colloquium] Plasma heating and particle acceleration in solar and tokamak twisted flux ropes" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171212T000000Z DTEND:20171212T010000Z DTSTAMP:20261011T152429Z UID:kjecb4eqhndoup99p7su5m4oco@google.com CREATED:20171204T041106Z DESCRIPTION:Galaxy clusters are the largest gravitationally bound objects i n the Universe and are excellent cosmological probes. Their power as cosmo logical probes\, however\, is currently limited by the systematics involve d in the measurement of their mass. In this talk\, I will discuss the meth od to estimate their masses using the weak-gravitational lensing of the Co smic Microwave Background (CMB). I will explain the systematics involved i n the measurements and the importance of using CMB polarisation data in th e future. Finally I will discuss the uncertainties in the mass estimates f or the current CMB experiments and provide realistic forecasts for the CMB -S3/S4 experiments. Reference: arXiv: 1705.00411 LAST-MODIFIED:20171204T041106Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Srinivasan Raghunathan (University of Melbourne) "Measuring masses of galaxy clusters using CMB-cluster lensing" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150205T000000Z DTEND:20150205T010000Z DTSTAMP:20261011T152429Z UID:i4j5d7u7f788un2op2mu6v25lk@google.com CREATED:20141207T231609Z DESCRIPTION:Clues to the formation and evolution of our Galaxy\, the Milky Way\, are hidden in the chemical abundances and kinematics of its stars. T he low-mass stars\, with ages comparable to the age of the Universe\, reta in the chemical composition of the gas cloud from which they formed. There fore\, spectroscopic studies of these 'stellar fossils' reveal clues about the history of our Galaxy. The discovery of the ongoing accretion of the Sagittarius dwarf galaxy confirmed that mergers with satellite dwarf galax ies have contributed to the formation of the Galactic halo. However\, star s that were accreted during the earliest times of the formation of the Gal actic halo have been elusive. This thesis aims to better understand how th e Galactic halo came to be. In particular\, I investigated the accretion o f dwarf galaxies by the Galaxy and the role of asymptotic giant branch (AG B) stars in the chemical evolution of these systems. Low- to intermediate- mass stars end their nuclear burning life on the AGB. It is during this ti me that rich nucleosynthesis occurs in the stellar interior. The newly syn thesised elements are then brought to the surface through mixing episodes before being ejected into the interstellar medium via strong mass loss. Th erefore\, AGB stars are important contributors to the build-up of elements in our Universe. I present stellar evolutionary tracks and nucleosyntheti c predictions for a grid of stellar models of low- and intermediate-mass A GB stars at Z = 0.001 ([Fe/H] = -1.2). The models cover an initial mass ra nge from 1 M_sol to 7 M_sol. Final surface abundances and stellar yields a re calculated for all elements from hydrogen to bismuth as well as isotope s up to the iron group. We present the first study of neutron-capture nucl eosynthesis in intermediate-mass AGB models\, including a super-AGB model\ , of [Fe/H] = -1.2. Neutron-capture elemental abundances have been measure d\, using high-resolution spectra obtained from Magellan\, for the sample of stars compiled by Nissen & Schuster (2010). The sample consists of a po pulation of stars theorised\, due to their abundances and kinematics\, to have been accreted from dwarf galaxies. The results provide further eviden ce that the Galactic halo contains a population of stars accreted from dwa rf galaxies and we find that AGB stars were able to contribute to the chem ical evolution of the earliest dwarf galaxies. LAST-MODIFIED:20150202T040604Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Cherie Fishlock (RSAA) "Final Thesis Talk: Why should we care about asymptotic giant branch stars?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250520T010000Z DTEND:20250520T020000Z DTSTAMP:20261011T152429Z UID:36mn83d5mrueelhiha7079isfo@google.com CREATED:20250106T230130Z DESCRIPTION:The Sun is a unique laboratory for understanding fundamental pr ocesses occurring in astrophysical plasmas. Energy transport from the sola r interior to the atmosphere results in multi-million degree coronal tempe ratures\, accelerating the solar wind out into the heliosphere. Moreover\, it drives dynamic atmospheric phenomena such as flares\, eruptions and je ts. I will give an overview of (selected) observations and MHD modelling e fforts. LAST-MODIFIED:20250516T023208Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Amit Seta) \nZoom: https:/ /anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:David Pontin (U. Newcastle) "Heating and dynamics of the Sun's atmo sphere" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150324T030000Z DTEND:20150324T040000Z DTSTAMP:20261011T152429Z UID:ikmq246tsjno27tgd80phj3r58@google.com CREATED:20150304T120114Z DESCRIPTION:The range of offshore 8m-class telescopes to which Australian a stronomers have access is about to undergo significant changes. I will out line the extensive suite of facilities on the Gemini\, Magellan\, and Keck telescopes to which all Australian astronomers will be able to apply for from now through to the end of 2017. The International Telescopes Support Office at the AAO is positioning itself to support users of these faciliti es in a range of ways that I shall discuss. LAST-MODIFIED:20150311T031611Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Stuart Ryder (International Telescopes Support Office\, AAO) "The c hanging landscape of Australian 8 metre telescope access" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240319T000000Z DTEND:20240319T013000Z DTSTAMP:20261011T152429Z UID:4kb6s235ovp5vvul8bd4nbhn7g@google.com CREATED:20240218T224115Z DESCRIPTION:Fast radio bursts (FRBs) are a genuine cosmic mystery: we've st udied them intensively for more than 15 years\, but we're still not sure w hat they are. Despite us still not having the whole picture\, huge strides have been made in the last few years\, thanks to the extraordinary yield of thousands of new FRBs discovered by the Canadian Hydrogen Intensity Map ping Experiment (CHIME). I wll present some of the recent work from CHIME\ , and will particularly highlight the unique ways in which FRBs are superb probes of gas\, magnetic fields\, and turbulence along the line of sight. LAST-MODIFIED:20240218T224115Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Trey Yang) \nZoom: https:/ /anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Bryan Gaensler (UC Santa Cruz) "Fast Radio Bursts and Their Foregro unds" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201015T000000Z DTEND:20201015T003000Z DTSTAMP:20261011T152429Z UID:9tkekm4actsipci316e51ta7co@google.com CREATED:20200929T070610Z DESCRIPTION:Asteroidal occultation observations have rapidly increased in n umber since they were first attempted in the late 20th century\, with more than 3\,000 observers participating over the last 30 years. The technique does not depend upon the asteroid being visible\, yet provides measuremen t of an asteroid's size and shape at the 1km level\, and astrometry of an asteroid in the order of milli-arcsecs for main belt asteroids\, and 10's of micro-arcsecs for trans-Neptunian objects\, TNOs. Peripheral results in clude the discovery of rings around Uranus\, Neptune\, and the asteroids C hiron\, Chariklo and Haumea\; the detection of the bilobal nature of Arrok oth before the New Horizons' flyby\; measurement of Pluto's atmospheric pr operties at high altitudes better than New Horizons\; and detection of dou ble stars with separations between 0.2 mas and 100 mas. Asteroidal occulta tion results are being used by The Minor Planet Center\, and JPL Horizons\ , to compute accurate asteroid orbits\; by the relevant Gaia team to verif y the Gaia measurements of asteroid positions\; and by the Japanese space agency for an accurate orbit and size of the Geminid meteor shower parent body (3200) Phaethon\, for the Destiny mission due to launch in 2024. A te am with time allocation on the JWST to record occultations by TNOs has ask ed for assistance with predictions. LAST-MODIFIED:20201008T051608Z LOCATION:ZOOM 997 8534 1005 (host: Wibking) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dave Herald (Murrumbateman) "Asteroidal occultations: Astrometry be tter than Gaia. Shape and size measurements at the 1km level" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170331T030000Z DTEND:20170331T032000Z DTSTAMP:20261011T152429Z UID:u0b9go33mplactpfv1e6sqlp6o@google.com CREATED:20170327T122105Z DESCRIPTION:Astronomy Data and Computing Services (ADACS) is a new initiati ve by Astronomy Australia Limited (AAL). It aims to provide astronomy-focu sed training\, support and expertise to allow astronomers to maximise the scientific return from data and computing infrastructure. It will be deliv ered jointly by Swinburne University of Technology\, Curtin University\, a nd Pawsey Supercomputing Centre. During 2017\, ADACS will: 1) Provide astr onomy-focused training in software development\, data management\, HPC and advanced data analysis to Australian astronomers\, to optimise the usage of\, and increase value from\, existing infrastructure. 2) Create/enhance astronomy data portals to facilitate the management\, sharing and reuse of data. 3) Collaborate/partner with national eResearch providers to help co ordinate and maximise the computing and storage resources available to ast ronomers. I will discuss in my talk these three service areas and how we plan to enhance the data and computing services delivered to the astronomy community. LAST-MODIFIED:20170327T122105Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Amr Hassan (Swinburne University of Technology) "Astronomy Data and Computing Services (ADACS)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251104T000000Z DTEND:20251104T010000Z DTSTAMP:20261011T152430Z UID:7loau3lidb2ggh6aeqvpehhacs@google.com CREATED:20250623T121118Z DESCRIPTION:Magnetars are a rare class of slow-spinning neutron stars that are thought to possess the strongest magnetic fields in the Universe. Firs t discovered over 45 years ago\, they have become an integral piece in our understanding of the transient sky\, with links to supernovae\, gamma-ray bursts\, fast radio bursts and potentially even gravitational waves. In t his talk I will present new results from the long-term monitoring of sever al ‘radio-loud’ magnetars with Murriyang\, the Parkes 64-m radio teles cope\, revealing bizarre post-outburst behaviours and clues to the origins of the fast radio burst phenomenon. I will also highlight a collaborative radio and X-ray polarimetry experiment that culminated in the first direc t detection quantum vacuum birefringence in nature. With high-frequency up grades to Murriyang and upcoming X-ray polarimetry missions\, magnetars ar e becoming not just astrophysical curiosities\, but important tools for co nducting precision tests of strong-field quantum physics. LAST-MODIFIED:20251010T131108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Tomasz Rozanski) \nZoom: h ttps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Marcus Lower (Swinburne U.) "Magnetars: The magnetic monsters of th e neutron star zoo" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150515T040000Z DTEND:20150515T042000Z DTSTAMP:20261011T152429Z UID:ipac3ck71vh05i9b64grncof64@google.com CREATED:20150319T060119Z DESCRIPTION:Type Ia supernovae are the thermonuclear explosion of a carbon- oxygen white dwarf. The explosion itself produces half a solar mass of rad ioactive nickel\, whose decay injects energy into the ejecta and powers th e bright (M_B ~ -19) optical light curve. We present a new technique for m easuring directly the amount of nickel created in the explosion by observi ng signatures of its daughter nucleus\, cobalt\, in very late time (t~200 days) spectra. Coupling this to recent work by Richard Scalzo\, we find th at SNe Ia from white dwarfs below the Chandrasekhar mass consistently prod uce a modest amount of nickel (~0.5 solar masses) while Chandrasekhar mass white dwarfs produce a broader range (0.4-1.2 solar masses) - this may co nsistute evidence for two distinct explosion mechanisms. This work makes h eavy use of RSAA resources\, including new data from the ANU 2.3m telescop e (WiFeS)\, RSAA Keck time (DEIMOS on Keck II)\, and collaborative work wi th RSAA Distinguished Visitor John Hillier (Pittsburgh). LAST-MODIFIED:20150514T203605Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Michael Childress (RSAA) "Measuring the power source for Type Ia su pernovae with late time spectra" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231205T000000Z DTEND:20231205T013000Z DTSTAMP:20261011T152429Z UID:aptcc48tnd90h5ohl6l17v04t4@google.com CREATED:20231019T131114Z DESCRIPTION:Stars are fossils that retain the history of their host galaxie s. Carbon and heavier elements are created inside stars and are ejected wh en they die. Elements heavier than iron (such as gold) are also produced b y neutron star mergers\, although the contribution is very uncertain. None theless\, it is possible to constrain star formation and chemical enrichme nt histories of the galaxies from the spatial distribution of elements in galaxies. This approach\, Galactic Archaeology\, has been popularly used f or our Milky Way Galaxy with a vast amount of data from Gaia and multi-obj ect spectrographs. This approach can also be applied to external galaxies thanks to integral field units. For comparing to these observations\, we h ave been running hydrodynamical simulations following detailed chemical en richment from cosmological initial conditions. Metallicity is higher in mo re massive galaxies\, and at the centre of galaxies. The mass--metallicity relations and radial metallicity gradients evolve at higher redshifts\, a nd current observations indicate somewhat strong stellar feedback. Element al abundances can put further constraints\; the fluorine-enhanced galaxy a t z=4.4 discovered by ALMA and the nitrogen emission of GN-z11 at z=10.6 t aken by JWST/NIRSpec suggest enrichment from Wolf-Rayet stars\, which beco mes dominant during intermittent star formation in the very early universe . LAST-MODIFIED:20231019T131114Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Emily Wisnioski) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Chiaki Kobayashi (U. Hertfordshire) "Cosmic Chemical Enrichment: fr om Stars to Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231123T000000Z DTEND:20231123T010000Z DTSTAMP:20261011T152429Z UID:v7d4a8falauoar2vr2t79rd13c@google.com CREATED:20231107T054610Z DESCRIPTION:The Large Magellanic Cloud (LMC) is one of the Milky Way's most prominent dwarf galaxy satellites. Positioned within the Milky Way's grav itational influence\, the LMC offers a unique opportunity to explore near- field cosmology in the context of stellar evolution\, star formation\, int erstellar medium behaviour\, and galaxy evolution. This thesis presents de tailed abundance measurements for various elements in stars within the LMC \, shedding light on their chemical composition and evolution. The first s tudy examines the presence of multiple populations in the 1.95 Gyr old LMC star cluster NGC 1846\, testing the 2 Gyr boundary for clusters showing c hemical abundance spread. Findings indicate no intrinsic star-to-star spre ad in Na and O\, but significant carbon spread suggests evolutionary mixin g in the red giant branch\, enhancing our understanding of the existence o f multiple populations in intermediate-age massive star clusters in galaxi es. The second study presents a search for extremely metal-poor (EMP) star s in the LMC\, crucial for unraveling the earliest stars and conditions du ring initial star formation in dwarf galaxies. Using SkyMapper DR3 and Gai a DR2 data\, seven stars with [Fe/H] <= -2.75\, including two with [Fe/H] <= -3\, were found. The third study then unveiled detailed abundance resul ts for these stars\, confirming them as the most metal-poor stars known in the Magellanic Clouds. While their abundance ratios resemble Milky Way ha lo stars\, only the more metal-rich stars display r-process element enhanc ements\, hinting at a 100 Myr timescale for substantial r-process enrichme nts. Together\, these studies contribute valuable insights into the chemic al composition\, evolutionary history\, and early star formation processes within the LMC\, advancing our understanding of stellar and galactic evol ution. LAST-MODIFIED:20231107T234610Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Sven Buder) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Wei Shen Oh (RSAA) "Investigating the chemistry of stars in the Lar ge Magellanic Cloud (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171113T000000Z DTEND:20171113T010000Z DTSTAMP:20261011T152429Z UID:8v70sftl8bc8rdsrb29et7jmcs@google.com CREATED:20171106T225610Z DESCRIPTION:New instruments and projects at ESO. LAST-MODIFIED:20171106T225610Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Luca Pasquini (ESO) "New instruments and projects at ESO" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250926T040000Z DTEND:20250926T043000Z DTSTAMP:20261011T152429Z UID:10shqecsrjuof7c38b554c8chk@google.com CREATED:20250901T003111Z DESCRIPTION:Our team launcher team has been developing over several semeste rs a VR application aimed at replicating the experience of visiting the GM T and Siding Spring Observatories. We would like you to join us and experi ence the application and give us feedback to expand and improve it. LAST-MODIFIED:20250922T023107Z LOCATION:CSO Common Room (NOTE CHANGE OF LOCATION) (host: TBD) \nZoom: http s://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tony Travouillon (RSAA) "Come experience Siding Spring and GMT in V R!" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240823T040000Z DTEND:20240823T050000Z DTSTAMP:20261011T152429Z UID:gon6744b5vue2esf002hps6hek@google.com CREATED:20240807T021613Z DESCRIPTION:The entirety of the dynamic infrared sky has only just begun to be explored. The field of multi-messenger time-domain astronomy has grown significantly over the past years with astronomical transient and variabl e events such as supernovae and gravitational waves. Whilst there are a si gnificant number of all-sky optical surveys that are observing these event s\, there are a substantially less number in the near-infrared even though it is known that extinction due to dust and dust formation events means t hat a proportion of these events cannot be seen in the optical regime. Her e\, two wide-field fully robotic near-infrared surveys are discussed\, Pal omar Gattini-IR and the Dynamic REd All-sky Monitoring Survey (DREAMS). Pa lomar Gattini-IR is a 0.3m telescope located at Palomar Observatory in Cal ifornia\, United States of America and DREAMS is a 0.5m telescope that wil l be located at Siding Spring Observatory. LAST-MODIFIED:20240819T000609Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jamie Soon (RSAA) "Observing The Dynamic Infrared Sky" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190823T040000Z DTEND:20190823T050000Z DTSTAMP:20261011T152429Z UID:qjuf4e3ag4qqn3b1m8eit3t6ik@google.com CREATED:20190806T035110Z DESCRIPTION:Bars are believed to be major drivers of secular evolution and radial mixing in spiral galaxies through its dynamical interaction with th e disc and the halo. Bars are present in around 70% of dic galaxies and th ey are thought to be key to the rearrangement of material and angular mome ntum as well as in the building up of the central bulge. I will review our current understanding of how bars affect their hosting galaxies throughou t time\, placing in this context the Milky Way bar. I will present recent observational results based on integral field spectroscopy of 2D and radia l distribution of the stellar and the ionised gas properties of a large sa mple of galaxies. I will also show some recent observational results on th e issues of bar formation and evolution to conclude on the importance of b ars in the galaxy makeover. LAST-MODIFIED:20190823T033607Z LOCATION:Duffield Lecture Theatre (host: Zerjal) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Isabel Perez (University of Granada) "Are galactic bars efficient a t stirring and mixing their discs?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230810T010000Z DTEND:20230810T020000Z DTSTAMP:20261011T152429Z UID:7hrfr27dc8s0otcrhs0p0rg7so@google.com CREATED:20230809T065606Z DESCRIPTION:Integrated field unit (IFU) spectroscopy provides a unique wind ow to explore gas-phase metallicity in the interstellar medium (ISM) of ga laxies in the local Universe. Two-point correlations are one of the next-g eneration methodologies proposed to extract new information on ISM diffusi on from metal fields inside galaxies. I will present two-point correlation analyses using CALIFA and MUSE that show this approach is robust across l ocal different datasets and can be a powerful tool to investigate the prop erties of the ISM of nearby galaxies when combined with an analytic model. The derived characteristic ISM diffusion length scales indicate that meta llicity correlations in galaxies are influenced by the competition between turbulent diffusion and galactic outflows. Two-point correlation methods are also applied to the high-resolution Auriga simulations obtaining consi stent results. The simulations reveal the interplay between internal and e xternal processes on setting the instantaneous mixing scale and how it evo lves with time. This new work provides new opportunities for next-generati on facilities (e.g.\, VLT/ERIS\, ELT/HARMONI\, GMT/GMTIFS) to push this te chnique beyond local Universe where the ISM is expected to be more turbule nt and galaxies are expected to host ubiquitous outflows. LAST-MODIFIED:20230809T065606Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark) \nZoom: https://anu. zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Zefeng Li (RSAA) "Metallicity correlations in galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260115T000000Z DTEND:20260115T010000Z DTSTAMP:20261011T152430Z UID:6n1ihbi9qdp05gh447epv78vh4@google.com CREATED:20251102T061614Z DESCRIPTION:Observations of neutral hydrogen (HI) within galaxies are an im portant tracer to probe the evolution of complex physical processes that o ccur within the interstellar medium (ISM). With its close proximity\, the gas of the Milky Way provides us the ideal laboratory to investigate these processes and the eventual formation of molecular clouds at scales beyond the sub-grid resolution of most numerical ISM simulations. Observations o f this calibre are vital to test our current theoretical understanding of the turbulent cascade and transition from warm neutral hydrogen to its coo ler phase counterpart. The SKA precursor\, ASKAP\, has observed the Milky Way foreground towards the Magellanic System in unprecedented detail\, wit h its current spatial resolution and unbiased detection manner cataloguing hundreds of Milky Way HI absorption sources within a relatively small fie ld of view\, rivalling the combined catalogue of previous detections acros s the entire sky. During my PhD\, I have worked alongside the GASKAP-HI Co llaboration in using these latest advancements in source density made by t he GASKAP-HI survey. I have used absorption measurements to reveal the det ailed variation of cold neutral medium properties across the plane of sky within a localised region containing filamentary structures\, providing an unbiased analysis of cold gas without the limitations of optically thin H I emission. Through the increased sensitivity compared to previous surveys \, we also reveal the prospects for using ASKAP and eventually the SKA to detect higher temperature phases in absorption\, as well as how resolution affects the phase separation of HI emission using current tools and techn iques. LAST-MODIFIED:20260115T020106Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Naomi McClure-Griffiths) \ nZoom: https://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOnt d.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Callum Lynn (RSAA) "The Structure and Spatial Properties of the Mil ky Way's Cold Neutral Medium with ASKAP (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231219T000000Z DTEND:20231219T013000Z DTSTAMP:20261011T152429Z UID:r35u6cfn4pslbt39uq7r9c5ud8@google.com CREATED:20231212T115608Z DESCRIPTION:I will report on the work done at ESO with collaborating instit utes and industry\, towards an LGS-AO facility for testing novel schemes a nd devices related to visible LGS-AO systems for astronomy and for satelli te communications. This is the CaNaPy (ESO) – ALASCA (ESA) project\, whi ch is installed and being commissioned at the ESA OGS 1m telescope in Tene rife. I will review the main requirements\, the system configuration\, the elements of novelty\, and how we have addressed them. I will show results of end-to-end simulations for the system. LAST-MODIFIED:20231212T115608Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Noelia Martinez Rey) \nZoo m: https://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Domenico Bonaccini Calia (ESO) "Pushing LGS-AO technologies towards Space awareness and SatComm" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160621T010000Z DTEND:20160621T020000Z DTSTAMP:20261011T152429Z UID:4itvdltegdv14033j5jjr6bnns@google.com CREATED:20160429T045113Z DESCRIPTION:TBD LAST-MODIFIED:20160517T002613Z LOCATION:Duffield Lecture Theatre (host: Michael Ireland) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Aaron Rizzuto (University of Texas) "Calibrating Star Formation and Stellar Evolution with Young Stellar Associations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230328T000000Z DTEND:20230328T010000Z DTSTAMP:20261011T152429Z UID:2uj3gthftfq1q4a77v2ir98t7k@google.com CREATED:20230321T002111Z DESCRIPTION:Fast radio bursts (FRBs) have a story which has been told and r etold many times over the past few years as they have sparked excitement a nd controversy since the pioneering discovery in 2007. The FRB class encom passes a number of microsecond to millisecond duration pulses occurring at Galactic to cosmological distances with energies spanning several orders of magnitude. Many radio telescopes around the world are currently underta king wide area surveys and targeted searches to discover and localise FRBs \, as their true potential can only be realised up host galaxy identificat ion and association. Significant effort is being put into localising FRBs to sub-arcsecond precision by radio interferometers around the globe. The MeerTRAP project at the MeerKAT telescope in South Africa has been operati onal since 2019 and has discovered ~35 FRBs and localised a handful of the m to host galaxies\, including an FRB localised to sub-arcsecond precision at z~1. In this talk\, I will present the recent discoveries from the Mee rTRAP project\, their multi-wavelength follow-up efforts and the possibili ty of ultra-long period magnetars being FRB progenitors. LAST-MODIFIED:20230321T002111Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hiep) \nZoom: https://anu. zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Manisha Caleb (Sydney Institute for Astronomy) "Exploring the trans ient landscape with MeerKAT: from FRBs to ultra-long period neutron stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251125T000000Z DTEND:20251125T010000Z DTSTAMP:20261011T152430Z UID:etr4k582ndmb3vp1q1c0qfr25g@google.com CREATED:20250623T121120Z DESCRIPTION:Cosmological galaxy formation simulations are essential tools f or interpreting observations\, designing surveys\, and exploring uncharted regions of galaxy parameter space. Yet\, these models face long-standing challenges\, such as reproducing galaxy emission consistently from the UV to the FIR\, as well as new ones\, including explaining the presence of ma ssive quenched galaxies in the early Universe revealed by recent observati ons. In this talk\, I will present how we are addressing these challenges with Shark\, a highly flexible\, open-source semi-analytic model of galaxy formation. I will highlight recent advances in Shark's physical modelling \, including the implementation of more realistic dust attenuation curves and improved treatments of AGN and environmental feedback\, which together enable a more accurate and predictive framework for galaxy evolution acro ss cosmic time. LAST-MODIFIED:20251103T021111Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Tim Gao) \nZoom: https://a nu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Claudia Lagos (UWA) "Feeding\, Feedback and Fading: A Shark's View of Galaxy Evolution" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230926T010000Z DTEND:20230926T023000Z DTSTAMP:20261011T152429Z UID:j0t3icfhl5oks6o64le5c14e58@google.com CREATED:20230806T233121Z DESCRIPTION:Type Ia supernovae are quite important in different fields of a strophysics\; for example as distance indicators in Cosmology\, as nucleos ynthesis sources for Chemical Evolution\, or as Tevatrons for cosmic-rays. Many questions surrounding their progenitors and their explosion mechanis ms however remain unanswered. In my talk\, I will first summarise a modell ing workflow (the "pipeline") that connects rapid binary evolution progeni tor models to supernova observables\, via supernova explosion and nucleosy nthesis simulations. I will then sketch how we can use model-specific nucl eosynthetic signatures of different explosion models to make inferences ab out what kind of white dwarfs explode as Type Ia supernovae. This includes population arguments based on the galactic chemical evolution of iron gro up elements such as manganese\, as well as inferences on individual supern ovae from the signatures long-lived radioactive isotopes leave in their la te-time light curves. I will conclude with some recent updates on the disc overy of the optical emission of the shocked ejecta in young Type Ia super nova remnants. LAST-MODIFIED:20230917T132610Z LOCATION:TBD (host: Sven) \nZoom: https://anu.zoom.us/j/83410388355?pwd=Qm9 CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ivo Seitenzahl (UNSW Canberra) "Type Ia supernovae: from explosion models to observations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250613T040000Z DTEND:20250613T043000Z DTSTAMP:20261011T152429Z UID:efq27arpamt7314lbsvahfbn30@google.com CREATED:20250520T122212Z DESCRIPTION:Turbulence is typically observed on large scales\, such as in a tmospheric flows or astrophysical gas clouds\, but the kinetic energy inje cted at these scales must eventually dissipate at much smaller scales. In this talk I will explore where this kinetic energy goes\, in both the subs onic and supersonic regimes\, by simulating turbulent flows of an interste llar gas cloud. Should it be expected that subsonic and supersonic turbule nce can be characterised by vortices or shocks? How long does it take for large scale kinetic energy injection to dissipate? And how is this dissipa tion correlated with key quantities such as the density and vorticity of t he gas? LAST-MODIFIED:20250610T215708Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Christoph Federrath) \nZoo m: https://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Edward Troccoli (RSAA) "The statistics and structure of dissipation in subsonic and supersonic turbulence" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161201T220000Z DTEND:20161202T060000Z DTSTAMP:20261011T152429Z UID:tjpvd9pi4am87ccrdo4e7ccms4@google.com CREATED:20161130T031605Z DESCRIPTION:This is the annual christmas seminars at Mount Stromlo. Student s from RSAA and elsewhere flok to the mountain to share their research wit h others. Invited talks from members of RSAA will also feature. LAST-MODIFIED:20161130T031605Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Student Christmas seminars (RSAA) "student Christmas seminars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180810T040000Z DTEND:20180810T050000Z DTSTAMP:20261011T152429Z UID:sf0mubt75jbp39qqu03rarp8b0@google.com CREATED:20180725T014109Z DESCRIPTION:Astronomy Australia Ltd (AAL) Member Update LAST-MODIFIED:20180727T020608Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mita Brierley (AAL) "Astronomy Australia Ltd Update" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150206T030000Z DTEND:20150206T032000Z DTSTAMP:20261011T152429Z UID:e19lpce4vfpbucerbgvjjobino@google.com CREATED:20150129T031108Z DESCRIPTION:Our understanding of star formation in galaxies is facilitated by observations\, at multiple wavelengths\, of emission which traces stell ar populations. Radio emission could provide an important extinction indep endent tracer\, however the relationship radio emission (at 1.4 GHz) and s tar formation rate (SFR) is not well understood. Using optical integral fi eld spectroscopy\, my work aims to better understand the local SFR calibra tions\, which use H-alpha and radio continuum emission\, when applied to d ifferent regions of a galaxy\, as well as to galaxies as a whole. In our s tudy of 13 radio-selected star-forming galaxies in the SAMI galaxy survey\ , we find that the radio continuum and H-alpha SFRs are consistent within galaxies which are not effected by shocks. We find that the ratio of SFR 1 .4GHz /SFR H-alpha may be increased (by up to an order of magnitude) in th e presence of shock excitation. Shocks from stellar winds and supernovae r emnants may re-accelerate populations of cosmic rays\, increasing the non- thermal radio emission and the SFR estimates. LAST-MODIFIED:20150622T074452Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sarah Leslie (RSAA) "A Radio-Optical Study of Resolved Star-Formati on in Galaxies from the SAMI Galaxy Survey" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180501T010000Z DTEND:20180501T020000Z DTSTAMP:20261011T152429Z UID:0ejbqap86lha40emnpv7c00uj4@google.com CREATED:20180207T022614Z DESCRIPTION:It is now well established that the star-formation activity of our Universe increased from the very early epochs\, peaked around z=2\, an d then decreased by an order of magnitude until present age. However\, the exact contribution of different galaxy populations to the total SFR budge t is not yet well-defined. Further progress in this area requires both a b etter understanding (or calibration) of SFR tracers used as well as deep o bservations of such tracers. The international panchromatic Cosmic Evoluti on Survey (COSMOS)\, is the only single survey large enough to study the c oupled evolution of the large-scale structure of the Universe\, galaxies\, star formation\, and active galactic nuclei across cosmic time. The 2 sq deg area of sky covered by COSMOS has the most extensive set of multi-wave length observations of any deep field sufficient to probe the high mass en d of galaxy populations out to high redshift\, spanning the entire electro magnetic spectrum from X-ray\, UV\, optical\, infrared to the radio. In th is talk I will cover two topics from my PhD work: 1) the evolution of gala xy opacity and dust distributions since z~1 and 2) the evolution of specif ic star formation since z~5 using radio continuum as a star formation rate tracer. LAST-MODIFIED:20180502T001106Z LOCATION:Duffield Lecture Theatre (host: Battisti) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sarah Leslie (MPIA) "Evolution of star formation and dust propertie s of galaxies over cosmic time" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250530T043000Z DTEND:20250530T050000Z DTSTAMP:20261011T152429Z UID:k3icdb2p4n8isivi0gfp09fh4k@google.com CREATED:20250523T032606Z DESCRIPTION:Deformable mirrors are a keystone of adaptive optics\, and flat tening them is required to ensure a proper baseline for optical observatio ns. This talk will go over developing a possible new algorithm to flatten the DM in a more efficient manner. In particular\, the algorithm will atte mpt to use a database of control matrices and learned pre-determined phase screens to determine the best matrix for flattening multiple actuators si multaneously\, as opposed to current methods of flattening each actuator o ne-by-one. I will discuss using a Python simulation of a 4f optical system with a DM and spatial light modulator (SLM)\, combined with reinforcement learning to form a DM-flattening algorithm\, and testing that in a labora tory set-up. LAST-MODIFIED:20250523T032607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Israel Vaughn) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Yuri Sheinker (RSAA/AITC) "Developing a flattening algorithm for a deformable mirror" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241015T000000Z DTEND:20241015T010000Z DTSTAMP:20261011T152429Z UID:o51cs25aaogpkmbg5pjqahs2gg@google.com CREATED:20240815T065135Z DESCRIPTION:Deep observational studies reveal that galaxies are surrounded by a faint\, diffuse stellar component: the intra-halo light (IHL). The IH L is typically referred to as the stellar halo in galaxies and the intra-c luster light in galaxy clusters. Regardless of mass scale\, the IHL is bel ieved to form primarily from the remnants of accreted galaxies\, providing a valuable probe into a galaxy's assembly history. In this talk\, we expl ore the formation of the IHL using a sample of galaxies drawn from the EAG LE suite of hydrodynamical simulations. First\, we introduce the dynamical decomposition technique used to isolate the discs\, bulges\, and IHL of g alaxies whose masses range from that of the Milky Way up to that of massiv e galaxy clusters. After characterising the present-day properties of the IHL for these galaxies\, we study the formation and assembly histories of their in situ and ex situ components. Although the IHL of most galaxies is dominated by ex situ stellar mass\, a significant in situ contribution al so exists\, with the formation mechanisms of the in situ IHL varying depen ding on the host halo mass. To conclude\, we examine the role of mergers i n shaping the present-day IHL of Milky Way-mass galaxies. Specifically\, w e show that while many Milky Way-mass disc galaxies with low-mass IHL exhi bit quiescent merger histories\, others have experienced significant merge rs since z=1. We discuss the origin of this result and potential implicati ons for studies aiming to reconstruct the assembly histories of galaxies f rom observations of their IHL content alone. LAST-MODIFIED:20240926T060120Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hilay Shah) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Katy Proctor (UWA) "The intra-halo light as a probe of galaxy assem bly" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260818T050000Z DTEND:20260818T061500Z DTSTAMP:20261011T152430Z UID:r1d3a1n84jobluro7jhdpfv1tk@google.com CREATED:20260503T114414Z DESCRIPTION:Our monthly Skillshare sessions provide an informal\, supportiv e\, and practical space for students and postdoctoral researchers to devel op and exchange research skills\, professional-development tools\, and eff ective workflows. The format is primarily focused on students\, in particu lar those enrolled in the ASTR8030 course Astronomy and Astrophysics Resea rch Skills. However\, everyone is very warmly invited to join and contribu te.\n\nSessions are held on selected Tuesdays from approximately 3:00-4:15 ish pm in the CSO Common Room. Depending on the topic\, they may include s hort introductions\, demonstrations\, panel discussions\, interactive exer cises\, or open-ended hands-on activities. LAST-MODIFIED:20260803T020011Z LOCATION:Zoom or CSO Common Room (host: Sven Buder and Melanie Kaasinen) \n Zoom: https://anu.zoom.us/j/89544552112?pwd=Bdoo5fgMVS2Ls6e3Fs0NSNk9OMpaXn .1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:RSAA Skillshare (RSAA) "How to make memorable plots" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230210T020000Z DTEND:20230210T030000Z DTSTAMP:20261011T152429Z UID:f1v0ls0jl697ltsadjdsdkh0ns@google.com CREATED:20230203T052809Z DESCRIPTION:The lecture presented by Airbus experts will address the variou s aspects linked to the radiation tolerance which is required for a space system. This will cover a description of the constraint - the space radiat ion environment - the failure mechanisms that such a constraint may trigge r on electronics\, materials and humans and finally the way Airbus Defence and Space engineering teams predict and mitigate the potential deleteriou s effects induced by radiation on such a non-repairable system LAST-MODIFIED:20230207T001109Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Aditi) \nZoom: https://anu .zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Indranil Chatterjee and Renaud Mangeret (Airbus) "Radiation toleran ce for a space system" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180823T010000Z DTEND:20180823T020000Z DTSTAMP:20261011T152429Z UID:u4u9otj8ld3ntrql6ag594fddk@google.com CREATED:20180822T015205Z DESCRIPTION:Galaxies form and evolve via physical processes that operate ov er a large dynamic range of spatial scales\, from the tens of kpc scales o f galactic disks down to the sub-pc scales in which stars form within GMCs . Optical integral-field spectroscopy\, especially when combined with IR\, sub-mm\, and radio datasets\, offers a powerful tool to study the physics of star formation\, feedback injection\, chemical enrichment\, and galact ic dynamics within galaxies\, but comprehensive surveys of nearby galaxies have been limited by their ~500 pc -1 kpc spatial resolution. At such coa rse resolution individual sites of star formation\, metal production and f eedback injection cannot be resolved. In this talk I will present early re sults from the "Physics at High Angular Resolution in Nearby Galaxies" (PH ANGS) survey\, a combination of two ESO and ALMA Large Programs aimed at m apping the ionized and molecular ISM and stellar content of all massive st ar forming galaxies in the Local Volume (D<17 Mpc) at <100 pc resolution. I will also discuss the Local Volume Mapper (LVM) project\, one of the pro grams to be executed as part of the Sloan Digital Sky Survey V (SDSS-V). T he LVM will start operating in 2020\, and will produce optical IFU data-cu bes of the bulk of the Milky Way disk\, the Magellanic Clouds\, M31\, and M33\, and dozens of Local Group dwarfs\, with spatial resolutions ranging from 0.1 pc to 20 pc\, resolving the scales in which stars form and feedba ck and metals are injected into the ISM. LAST-MODIFIED:20180822T015205Z LOCATION:Duffield Lecture Theatre (host: Moller) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Guillermo Blanc (Observatories of the Carnegie Institution for Scie nce) "Next Generation 3D Surveys of Nearby Galaxies: Resolving the Physics that Drive Galaxy Evolution" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190329T030000Z DTEND:20190329T033000Z DTSTAMP:20261011T152429Z UID:9f6bbsg0s0os5r8a1c66evqfno@google.com CREATED:20190228T072120Z DESCRIPTION:TBD LAST-MODIFIED:20190322T000108Z LOCATION:CSO Common Room (host: Zhang) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:James Gardner (RSAA) "Quantifying the velocity structure in turbule nt rotating molecular clouds" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201119T000000Z DTEND:20201119T010000Z DTSTAMP:20261011T152429Z UID:nvag8jtf83l4do1r5kdunj9kds@google.com CREATED:20201113T054108Z DESCRIPTION:The field of Galactic archaeology is currently undergoing a rev olution largely thanks to a new generation of ambitious stellar surveys as APOGEE\, GALAH\, SkyMapper and Gaia\, producing copious amounts of high q uality\, complementary data. Galactic chemical evolution plays an importan t role in the interpretation and understanding of this expanding body of d ata\, with the ultimate goal of probing the mechanisms of galaxy formation . I will present an overview of my work involving age determination using a full Bayesian framework of isochrones fitting\, accounting for initial m etallicity rather than present-day surface metallicity. Using this method with Gaia parallaxes\, I derive ages for the second data release of the GA LAH survey. I will present the reconstructed temporal evolution of element s such as Na\,Mg\,Al\,Si\,K\,Ca\,Sc\,Ti\,Cr\,Fe\,Ni\,Cu\,Ba and many more\ , and the implication of these trends in the context of chemical evolution and Galactic formation. I have further adapted this framework into derivi ng photometric stellar parameters for the SkyMapper Survey\, with the aim of tracing past merger events in the Galactic halo and unfolding the assem bly history of the Milky Way. LAST-MODIFIED:20201113T055610Z LOCATION:DLT and ZOOM 997 8534 1005 (host: Menon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jinying (Jane) Lin (RSAA) "End-of-Thesis Colloquium: Galactic Archa eology: The Milky Way in the context of large scale surveys" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230901T040000Z DTEND:20230901T043000Z DTSTAMP:20261011T152429Z UID:qs7kuls2rqpjdt9jre51ue0vhg@google.com CREATED:20230828T014609Z DESCRIPTION:TBD LAST-MODIFIED:20230831T001607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Francois Rigaut (RSAA) "My 2000km bike journey in Central Europe: a unique experience" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150813T010000Z DTEND:20150813T020000Z DTSTAMP:20261011T152429Z UID:3lhvmqrec56g8ckjj3d6mjjoig@google.com CREATED:20150802T234607Z DESCRIPTION:One of the most important questions in astronomy today is the s ource of the ionising photons that caused a predominantly neutral Early Un iverse to evolve into the ionised one we see today. I have investigated th is Epoch of Reionisation with a new suite of high resolution hydrodynamica l simulations\, created within the DRAGONS group. These simulations show t hat the galaxies observed at early times represent merely the tip of an ic eberg\; with a hidden population of faint galaxies that can Reionise the U niverse with ease. Although the global star formation history of the early universe is strongly constrained by current observations\, we actually kn ow little about the nature of star formation at this time (as given by the specific star formation rate). I will demonstrate that we can understand these objects but need to push our observations deeper\, a goal that will likely have to await the James Webb Space Telescope. LAST-MODIFIED:20150807T035105Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alan Duffy (Swinburne) "First Galaxies and DRAGONS" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150305T000000Z DTEND:20150305T010000Z DTSTAMP:20261011T152429Z UID:a6j60vm73ih7mrq7tsm6ba8sd0@google.com CREATED:20150108T012607Z DESCRIPTION:The first natural guide star (NGS) and laser guide star (LGS) a daptive optics (AO) systems on 8 to 10 m class telescopes were implemented on the Keck II telescope in 1999 and 2004\, respectively. Both Keck teles copes are now equipped with LGS AO systems and 558 refereed science papers have been published using data from these systems through 2014. The speak er will provide a brief overview of the Keck telescopes and instrumentatio n\, and then focus on the current and planned AO capabilities and the resu ltant science. LAST-MODIFIED:20150227T053106Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Peter Wizinowich (Keck) "Adaptive Optics at W. M. Keck Observatory" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150917T010000Z DTEND:20150917T020000Z DTSTAMP:20261011T152429Z UID:436nvlor0ugnlk9pspqcnnho70@google.com CREATED:20150810T020110Z DESCRIPTION:Planet formation is a subject being revolutionised by the stunn ing first long-baseline images from the ALMA telescope in Chile. The first of these\, of the HL Tau protoplanetary disc\, revealed a striking series of concentric rings but oddly\, no spirals\, as one might expect if the g aps in the disc are being carved by newborn planets. In this talk I'll sho w how the rings in HL Tau can be beautifully and convincingly explained as being caused by protoplanets\, but only when the interaction between gas and dust in the disc is accounted for. If there's time I'll speculate on w hat the future holds\, what we're likely to learn in the next 5-10 years f rom direct imaging of discs with ALMA\, HiCIAO and other telescopes\, why supporting theoretical work is urgently required\, and why we are well pla ced to plug that gap. LAST-MODIFIED:20150908T064105Z LOCATION:Duffield Lecture Theatre (host: Christoph Federrath) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Daniel Price (Monash) "Rings and no spirals - planet formation in a ction?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250807T010000Z DTEND:20250807T020000Z DTSTAMP:20261011T152429Z UID:qanmkoj62h3032cb2d90qhbbag@google.com CREATED:20250728T231606Z DESCRIPTION:In collaboration with GMTO and OHB Digital Connect\, Ingersoll Machine Tools has initiated construction of the largest telescope mount ev er built in the U.S. This 39 m‑tall\, 2\,100‑ton precision structure will support GMT's seven segmented primary mirrors\, advanced adaptive op tics\, and a suite of first-generation science instruments capable of deli vering diffraction‑limited spectroscopy and imaging across the visible a nd near‑infrared. Built in a newly expanded 40\,000 sq ft facility i n Rockford\, Illinois – equipped with the nation’s largest gantry mill – the mount will glide on a 50-micron film of oil via hydrostatic beari ngs\, ensuring friction-free movement and sub-arcsecond pointing stability essential for high-contrast\, high-stability observations. Over the cours e of this presentation\, Ingersoll’s Chief Engineer Giovanni Bonomi\, jo ined by VP of Sales Jason Melcher\, will introduce the company’s strengt hs in advanced precision engineering\, outline its journey in building the GMT mount\, and reflect on the broader impact of this milestone in astron omical infrastructure and scientific advancement. LAST-MODIFIED:20250807T034605Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Jenny Jiang) \nZoom: https ://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Giovanni Bonomi (Ingersoll Machine Tools) "Building the Giant Magel lan Telescope Mount at Ingersoll: Precision Engineering at Scale" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260901T050000Z DTEND:20260901T061500Z DTSTAMP:20261011T152430Z UID:0bc2kco1lbf1sgv37479dkura4@google.com CREATED:20260803T010014Z DESCRIPTION:Our monthly Skillshare sessions provide an informal\, supportiv e\, and practical space for students and postdoctoral researchers to devel op and exchange research skills\, professional-development tools\, and eff ective workflows. The format is primarily focused on students\, in particu lar those enrolled in the ASTR8030 course Astronomy and Astrophysics Resea rch Skills. However\, everyone is very warmly invited to join and contribu te.\n\nSessions are held on selected Tuesdays from approximately 3:00-4:15 ish pm in the CSO Common Room. Depending on the topic\, they may include s hort introductions\, demonstrations\, panel discussions\, interactive exer cises\, or open-ended hands-on activities. LAST-MODIFIED:20260803T020016Z LOCATION:Zoom or CSO Common Room (host: Sven Buder and Melanie Kaasinen) \n Zoom: https://anu.zoom.us/j/89544552112?pwd=Bdoo5fgMVS2Ls6e3Fs0NSNk9OMpaXn .1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA Skillshare (RSAA) "The ethical grey zone" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180809T010000Z DTEND:20180809T020000Z DTSTAMP:20261011T152430Z UID:crh4lns6atl1omhes8aeudvghc@google.com CREATED:20180625T111610Z DESCRIPTION:The measurements of the Hubble constant reveal a tension betwee n high-redshift (CMB) and low-redshift (distance ladder) constraints. If t his tension cannot be explained in terms of observational systematics then it will point towards new physics and explanations beyond the Standard Co smological Model. In my talk I will present a brief history of the measure ments of the Hubble constant and discuss the difference between high- and low-redshift constraints. I will investigate what types of observations co uld be used to resolve the problem from the observational side (i.e. point towards observational systematics)\, as well as\, I will discuss theoreti cal properties of models that could explain this tension away in terms of new physics. LAST-MODIFIED:20180730T235607Z LOCATION:Duffield Lecture Theatre (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Krzysztof Bolejko (University of Sydney) "The Hubble Trouble: obser vational systematics or a real anomaly pointing towards new physics?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161103T000000Z DTEND:20161103T010000Z DTSTAMP:20261011T152429Z UID:ul7dak4sgemlvjc9fn08h7nlg4@google.com CREATED:20160728T060621Z DESCRIPTION:This presentation recalls the principles and history of sodium guide star laser systems used in astronomy and space situational awareness adaptive optics. The first generation of sodium lasers used dye laser tec hnology to create the first sodium laser guide stars in Hawaii\, Californi a\, and Spain in the late 1980s and 1990s. These experimental systems were turned into the first laser guide star facilities to equip medium- to-lar ge diameter adaptive optics telescopes\, opening a new era of Laser Guide Star Adaptive Optics (LGS AO)- enabled diffraction-limited imaging from th e ground. Although they produced exciting scientific results\, these laser guide star facilities were large\, power-hungry and messy. In the USA\, a second-generation of sodium lasers was developed in the 2000s that used c leaner\, yet still large and complex\, solid-state laser technology. These are the systems in routine operation at the 8 to 10m-class astronomical t elescopes and 4m-class satellite imaging facilities today. Meanwhile in Eu rope\, a third generation of sodium lasers was being developed using inher ently compact and efficient fiber laser technology\, and resulting in the only commercially available sodium guide star laser system to date. Fiber- based sodium lasers are being or will soon be deployed at three astronomic al telescopes and two space surveillance stations. These highly promising systems are still relatively large to install on telescopes and they remai n significantly expensive to procure and maintain. We are thus proposing t o develop a fourth generation of sodium lasers: based on semiconductor tec hnology\, these lasers could provide a definitive solution to the problem of sodium LGS AO laser sources for all astronomy and space situational awa reness applications. LAST-MODIFIED:20161031T233105Z LOCATION:Duffield Lecture Theatre (host: Francis Bennet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Celine d'Orgeville (RSAA) "Four Generations of Sodium Guide Star La sers for Adaptive Optics in Astronomy and Space Situational Awareness" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180124T030000Z DTEND:20180124T032000Z DTSTAMP:20261011T152429Z UID:7ms09sgensmv88c5t3t0e5v5ns@google.com CREATED:20180119T064606Z DESCRIPTION:Many aspects of our daily life\, from communication and navigat ion\, to economic and social stability\, are dependent on communication wi th satellites in Earth orbit. These satellites are under threat from space debris which can prematurely degrade or destroy them. The Murchison Widef ield Array (MWA) has detected terrestrial radio reflected off space debris \, providing a new method with which to monitor this threat. In this talk I'll introduce the MWA and discuss how we can use it to detect and monitor space debris in order to strengthen our space situational awareness. LAST-MODIFIED:20180124T035605Z LOCATION:Duffield Lecture Theatre (host: Battisti) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Paul Hancock (Curtin University) "Detecting satellites and space de bris with the Murchison Widefield Array" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231104T030000Z DTEND:20231104T031500Z DTSTAMP:20261011T152429Z UID:qm6fnk2a82hq0fn691008fojjg@google.com CREATED:20231101T230607Z DESCRIPTION:he Space Careers Wayfinder education program is an ANU and CSIR O collaboration featuring diverse space professionals across Australia to encourage high schoolers and other space enthusiasts to consider a career in space. The program features a dozen of short (5-6mn) videos presenting a wide variety of careers in the space sector. Engaging supporting materia l is included for high school teachers\, career advisors\, and students to use in the classroom to explore concepts and ideas relevant to the Austra lian Year 9 and 10 curriculum. I will explain how this program came to be\ , the complexities associated with selecting a diverse group of people to feature in the videos and later interview them in the midst of nation-wide COVID restrictions\, what the programs aims to achieve and how you can he lp to share the word with your networks (schools\, family\, friends and co lleagues). The videos feature two of our own space enthusiasts at the ANU AITC: Noelia Martinez Rey and Joice Mathew! LAST-MODIFIED:20231101T230607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Celine d'Orgeville (RSAA) "The Space Careers Wayfinder education pr ogram" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210216T000000Z DTEND:20210216T010000Z DTSTAMP:20261011T152429Z UID:rrjra6s4ufkh684pr7dri17kb8@google.com CREATED:20210122T022610Z DESCRIPTION:Galactic archaeology is the use of the velocities and abundance s of stars to learn about the history of galaxy formation and nucleosynthe sis. I will tell three stories of galactic archaeology with three differe nt groups of elements: alpha elements\, the iron peak\, and the r-process. First\, I will present detailed abundances of individual stars in the dwa rf satellites\, stellar streams\, and smooth halo of M31. The evolution o f [alpha/Fe] in these stars supports the hierarchical assembly paradigm of galaxy formation. Second\, I will present abundances of manganese and nic kel in dwarf satellite galaxies of the Milky Way. These abundances are be st explained by a strong contribution of sub-Chandrasekhar-mass Type Ia su pernovae. Third\, I will present measurements of barium abundances in the globular cluster M15. The constancy of barium from the main sequence to t he red giant branch indicates that the stars in M15 were born with their u nusually large dispersion of r-process elements rather than acquiring it f rom an external source. LAST-MODIFIED:20210214T235206Z LOCATION:ZOOM (host: Sven Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Evan Kirby (Caltech) "Invited Colloquium: Galactic Archaeology - Ga laxy Formation and Nucleosynthesis" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191122T030000Z DTEND:20191122T033000Z DTSTAMP:20261011T152429Z UID:vo4mcpkj5p4dmfdtdvrk9bgc78@google.com CREATED:20191023T051110Z DESCRIPTION:We're all familiar with geostationary satellite antennas – th e Foxtel dishes atop many rooftops that point to a fixed location in space . The AITC has a number of programs\, however\, that rely on our ability to interact with satellites that freely zip across the sky under the influ ence of a plethora of perturbing forces. Understanding these forces is th e first step to being able to predict where any of the 20\,000+ catalogued orbital objects are at any particular instant so we know where – and wh en – to point our telescopes at them. In this talk I’ll outline how s atellites move\, how we find them and the challenges and opportunities the y afford to our communications and space environment research programs. LAST-MODIFIED:20191023T051110Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:James Webb (RSAA/AITC) "AITC Series – Space is big\, satellites a re (comparatively) small… the joys of finding\, tracking\, and using th em!" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151202T220000Z DTEND:20151203T060000Z DTSTAMP:20261011T152429Z UID:gcuho1ejchbommeo8s8lamumkg@google.com CREATED:20151002T050616Z DESCRIPTION:A number of student talks will be presented. LAST-MODIFIED:20151002T050616Z LOCATION:Duffield Lecture Theatre (host: Sarah Leslie) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Students (various affiliations) "Mt Stromlo Student Christmas Semin ars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180316T030000Z DTEND:20180316T040000Z DTSTAMP:20261011T152430Z UID:0gvhg2r4rtb7n3r0rdj79i9r4k@google.com CREATED:20180315T032105Z DESCRIPTION:Stars and star clusters form by gravitational collapse in regio ns of high density in the dynamically evolving multi-phase interstellar me dium. The process of stellar birth is controlled by the intricate interpla y between the self-gravity of the star-forming gas and various opposing ag ents\, such as supersonic turbulence\, magnetic fields\, radiative feedbac k\, cosmic rays\, and gas pressure. It is modified by the thermodynamic re sponse of the gas\, which is determined by the balance between various hea ting and cooling processes\, which in turn depend on the chemical composit ion of the material. I will discuss examples of recent progress and contro versy\, specifically\, I will focus about current attempts to bring numeri cal simulations and theoretical models closer to the observational domain. LAST-MODIFIED:20180315T050106Z LOCATION:Duffield Lecture Theatre (host: Federrath) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ralf Klessen (Heidelberg University) "Star Formation and ISM Dynami cs" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220527T010000Z DTEND:20220527T020000Z DTSTAMP:20261011T152429Z UID:n4uoh0qq2eqero45ki5n5u08to@google.com CREATED:20220524T000807Z DESCRIPTION:The measurement of distances via standard candles is a critical component of testing predictions of our standard cosmological model\, Lam bda-CDM\, in the local or late-time Universe. I have contributed meaningfu lly to two fields: (i) our understanding of dwarf galaxies as the smallest observable dark matter structures and (ii) the measurement of the Hubble constant via the calibration of Type Ia Supernovae. The former project bei ng the Exploration of Local VolumE Satellites (ELVES) relying on surface-b rightness fluctuations (SBF) and the latter being the Carnegie-Chicago Hub ble Program relying on the tip of the red giant branch (TRGB) -- both of w hich utilize properties of low-mass\, evolved stars that typify targets in the Apache Point Galactic Evolution Experiment (APOGEE). In this talk\, I will describe these from my lens of engineering techniques that can be ap plied en masse to future wide-area datasets or in a targeted fashion to fu ture deep datasets. I will particularly focus on the challenges for the wi de application of these techniques and my role in precisely and accurately addressing them by integrating archival and new observations on a variety of facilities. Thus\, in this talk\, I will connect my past\, current\, a nd future research contributions toward the goal of measuring precise and accurate distances in homogeneously collected data over a huge dynamic ran ge by using old stellar populations. LAST-MODIFIED:20220526T235106Z LOCATION:DLT & ZOOM (Talk delivered via zoom) (host: Shyam Menon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rachael Beaton (Princeton University) "Invited Colloquium: Large-Sc ale Survey Sized Distance Measurement" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201112T000000Z DTEND:20201112T003000Z DTSTAMP:20261011T152429Z UID:5ts7in0lh4dhvib90dhbbck9e8@google.com CREATED:20201001T054115Z DESCRIPTION:Context. The neutral hydrogen gas (HI) in the interstellar medi um (ISM) can be broadly categorised into three phases: the bistable a cold and warm neutral medium (CNM and WNM respectively) and the thermally unst able lukewarm neutral medium (LNM). The distribution of these phases can b e recovered by decomposing the 21-cm spectra into Gaussian components. Aim s. We used various Gaussian decomposition algorithms with the aim of ascer taining if different algorithms lead to different properties recovered abo ut the ISM. Methods. We generated synthetic datasets to compare Gausspy an d Gausspy+ across several different types of spectral profiles. The best a lgorithm was then used to decompose the whole-sky HI4PI results into Gauss ian components. We finally compared our decomposition results with those o btained by a previous investigation. Results. We first found that Gausspy+ performed better in recovering components especially in more complex spec tral profiles. However\, the results we obtained in the latter half were s ignificantly influenced by a poor fitting of Gaussian components to the sp ectra. Conclusions. The differences we observed in the synthetic tests wer e a promising lead that the results recovered by algorithms do indeed diff er. However\, the distributions we obtained for the HI4PI observations wer e not convincingly indicative of a relation between choice of algorithm an d the derived properties of the ISM. Further study into such an interdepen dence is needed. LAST-MODIFIED:20201111T004107Z LOCATION:ZOOM 997 8534 1005 (host: Seta) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Joshua Dai (RSAA) "ASC project: Quantifying the effect of Gaussian decomposition methods on the derived properties of the ISM" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201116T000000Z DTEND:20201116T034500Z DTSTAMP:20261011T152429Z UID:hv1fkbfn5m9u04amkhk3rvn594@google.com CREATED:20201112T074607Z DESCRIPTION:Finishing Honours and Master students will present their end-of -thesis talks. All welcome to attend. Honours section: 11:00 Kelly Kong: Using HI Fibres to Measure the Magnetic Field Tomography in the GALFA-HI Survey 11:30 Marcus Birch: Near-infrared imaging with InGaAs for DREAMS MAA section: 13:30 Zipeng Hu: Reconstructing 3D densities from 2D obse rvations of molecular gas 14:10 Donghee Nam: Testing the Turbulent Origi n of the Stellar Initial Mass Function LAST-MODIFIED:20201116T112606Z LOCATION:DLT and ZOOM 997 8534 1005 (host: Wolf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Honours and Masters Thesis Talks (RSAA) "Honours and Masters Thesis Talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200206T000000Z DTEND:20200206T010000Z DTSTAMP:20261011T152429Z UID:m1n5kv3ek3hbkpm3i752c4978k@google.com CREATED:20191202T224109Z DESCRIPTION:This talk presents a general picture of star cluster population s\, from their formation in the clumpy ISM to their eventual dissolution i n the smooth stellar field. The picture is general or unified in the sens e that it encompasses all the traditional categories of star clusters: ass ociations\, open clusters\, populous clusters\, globular clusters\, etc. The key element of this picture is the mass function of clusters (spectrum of cluster masses) and its time (age) dependence\, or equivalently\, the joint distribution of masses and ages. HST observations have revealed som e remarkable similarities in the mass-age distribution of clusters in diff erent galaxies\, analogous to similarities in the stellar mass function (I MF). This talk presents an overview of the observations and physical mech anisms underlying this picture of star cluster populations. LAST-MODIFIED:20200129T231606Z LOCATION:Duffield Lecture Theatre (host: Jin) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Michael Fall (STScI) "Star Cluster Populations: The Link Between S tar Formation and Galaxy Formation" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150212T000000Z DTEND:20150212T010000Z DTSTAMP:20261011T152429Z UID:h62niloo5liug7v6ainrfvt544@google.com CREATED:20141203T103112Z DESCRIPTION:The probability density function (PDF) is a simple analytical t ool for determining the hierarchical spatial structure of molecular clouds . It has been used frequently in recent years with dust continuum emission \, such as that from the Herschel space telescope and ALMA. These dust col umn density PDFs universally show a log-normal distribution in low column density gas\, characteristic of unbound turbulent gas\, and a power-law ta il at high column densities\, indicating the presence of gravitationally b ound gas. We have recently conducted a PDF analysis of the molecular gas i n the G333 and Vela C giant molecular cloud complexes\, using transitions of CO\, HCN\, HNC\, HCO+ and N2H+. The results show that CO and its isotop ologues trace mostly the log-normal part of the PDF\, while HCN and HCO+ t race both a log-normal part and a power law part to the distribution. On t he other hand\, HNC and N2H+ mostly trace only the power law tail. The dif ference between the PDFs of HCN and HNC is surprising\, as is the similari ty between HNC and the N2H+ PDFs. The most likely explanation for the simi lar distributions of HNC and N2H+ is that N2H+ is known to be enhanced in cool gas below 20K\, where CO is depleted\, while the reaction that forms HNC or HCN favours the former at similar low temperatures. The lack of evi dence for a power law tail in 13CO and C18O\, in conjunction for the resul ts for the N2H+ PDF suggest that depletion of CO in the dense cores of the se molecular clouds is significant. In conclusion\, the PDF has proved to be a surprisingly useful tool for investigating not only the spatial distr ibution of molecular gas\, but also the wide scale chemistry of molecular clouds. LAST-MODIFIED:20150622T074455Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Maria Cunningham (UNSW) "The probability density function in molecu lar gas in the G333 and Vela C molecular clouds" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150820T040000Z DTEND:20150820T050000Z DTSTAMP:20261011T152429Z UID:d3uds9ivilf2bp2j39osjte6sg@google.com CREATED:20150816T065605Z DESCRIPTION:We will give a brief overview our new proposed project\, Google -LUV (Loon Ultra-Violet). Last week\, we reached a verbal agreement with G oogle Project X\, to build a network of ultra-violet telescopes to survey both the dynamic and dark Universe. The telescopes will be flown on Google Loon\, which are long-duration\, high-altitude balloons. Providing access to high cadence near-UV photometry. Google will provide the first balloon platform for a launch at the end of 2016/early 2017\, and as they increas e their balloon flights\, they will give us a share\, on the order of 20 f or every 1000 balloons (per week) they launch. We will retrofit our balloo ns with small (20 - 30cm) telescopes operating in the near-UV (200 - 300nm ). We will use the balloons to perform a wide-field\, high-cadence UV surv ey. We are looking to develop the scientific goals and cases and are looki ng for people to participate. There will be plenty of time for discussion about ideas and what you'd like to do. LAST-MODIFIED:20150817T042105Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Brad Tucker & Rob Sharp (RSAA) "Google - LUV (Loon Ultra-Violet)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220303T000000Z DTEND:20220303T003000Z DTSTAMP:20261011T152430Z UID:5cmhq85gdiagau1udtourlojg4@google.com CREATED:20220117T041607Z DESCRIPTION:Using data obtained with the Dark Energy Camera on the Blanco 4 -metre telescope in Chile between 2013 and 2019\, the Dark Energy Survey ( DES) has observed hundreds of millions of galaxies and obtained light curv es for tens of thousands of extragalactic transients. DES is using these d ata to constrain the properties of dark energy. In this talk\, I will pres ent results obtained from data that were taken during the first three year s of the survey\, and will then summarise work that is being done now to a nalyse the full dataset. LAST-MODIFIED:20220301T002606Z LOCATION:DLT & ZOOM (host: Neco Kriel) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Chris Lidman (RSAA) "The Dark Energy Survey - Recent results and fu ture prospects" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191115T030000Z DTEND:20191115T032000Z DTSTAMP:20261011T152430Z UID:40s1307kqu3nvp26qv9dm04qns@google.com CREATED:20191106T112108Z DESCRIPTION:The evolution of molecular clouds and star formation is fundame ntally affected by turbulence. However\, methods for accurately measuring the turbulence of clouds\, particularly molecular clouds which include sy stematic motion\, are not well defined. Motivated by this\, we aim to deve lop a method to recover the 3-dimensional turbulence of clouds from observ able data. We simulate a rotating molecular cloud of radius 1 parsec and i nvestigate its true turbulence and the turbulence which can be measured fr om observational data. We investigate the spatial mean of the second momen t map and find it to be an overestimate of the true turbulence\, to decrea se at a faster rate than the 3-dimensional turbulence over time\, and to h ave a non-constant correction factor when compared to the 3-dimensional tu rbulence. We also investigate the standard deviation of the gradient subtr acted first moment map and find it to be an underestimate of the true turb ulence\, to increase at a faster rate than the 3-dimensional turbulence ov er time\, and to have a non-constant correction factor when compared to th e 3-dimensional turbulence. We then consider recovering the turbulence by combining the information encoded in the second moment map and the gradien t subtracted first moment map. We take the average of the two statistics a nd find it to be a more appropriate turbulence quantifier\, but suggest th at further investigation be done. LAST-MODIFIED:20191111T090105Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Madeleine Stewart (RSAA) "Methods for recovering the 3-dimensional turbulence of a rotating molecular cloud using data which can be obtained from observational data" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240725T010000Z DTEND:20240725T020000Z DTSTAMP:20261011T152429Z UID:sprqkg2kjo0ktagq227u8323fc@google.com CREATED:20240716T012609Z DESCRIPTION:We study the SDSS-IV MaNGA database consisted of spatially reso lved spectra of ~10\,000 galaxies to understand the emission properties of the associated ionizing sources. With the help of the BPT diagrams’ cla ssification scheme\, we train Spender (Melchoir et al 2021) to distinguish the dominant ionizing mechanism with information from the spectra outside of the strong emission lines usually used for classification. We find tha t a large fraction of LINER-like emission spectra can be distinguished by stellar absorption features associated with an old\, metal-rich stellar co mponent. This is consistent with previous work finding that LINER emission could be driven by a stellar population of old low-mass evolved stars. LAST-MODIFIED:20240716T012609Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Vanhiep Nguyen) \nZoom: ht tps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ahmad Nemer (NYU) "A deeper dive into the BPT diagrams and the orig in of LINER emission with machine learning" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150306T032000Z DTEND:20150306T034000Z DTSTAMP:20261011T152429Z UID:6jpajr1dd1cmv54t7lv4lpf0ps@google.com CREATED:20150119T064115Z DESCRIPTION:The next large instrument on a Gemini telescope\, GHOST\, is be ing built by a collaboration including AAO\, ANU and NRC-Herzberg. It aims to be a high efficiency fiber fed Echelle spectrograph with a wide wavele ngth range. I will describe the design’s background\, including lenslet- based image slicing that reduces slit losses while maintaining high resolu tion\, and why despite cost constraints\, the spectrograph has several mod es\, including a precision radial velocity mode and a two object mode. I w ill show simulated data from the unusual spectral format\, and describe th e work from here in the critical/final design phase. LAST-MODIFIED:20150302T231106Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Michael Ireland (RSAA) "Progress on the Gemini High-resolution Opti cal SpecTrograph (GHOST)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181113T000000Z DTEND:20181113T010000Z DTSTAMP:20261011T152429Z UID:paffbkqkc5ort3dcri6otv0o4o@google.com CREATED:20180929T054111Z DESCRIPTION:I investigate factors that influence the lifetime of protoplane tary discs in binary stars with the broad understanding that the longer th e lifetime of a disc (in a single or binary star) the higher the likelihoo d of producing planets. I present theoretical work done using the AMR MHD code FLASH on the formation of binary stars and the evolution of their dis cs in these systems. I simulated the collapse of molecular cores until the formation of protostars and followed the early evolution of these systems . I investigated the influence that binarity has on the global evolution o f a young stellar system\, including looking at mechanisms such as accreti on of material\, jets and outflows\, and dynamical interactions. I also pr esent observational work done to determine the typical survivability of di scs in binary star systems. This work was carried by using the Australian National University 2.3m telescope to search for radial velocity variation in disc-bearing members of the $11$ and $17$~Myr regions Upper Scorpius a nd Upper Centaurus-Lupus. I find the binary fraction of disc-bearing stars in these regions do not differ significantly from the field star binary f raction. This may suggest the typical lifetime of discs in single and bina ry stars is comparable. Overall I find that while in some scenarios binary stars may produce hostile environments for planet formation via the destr uction of circumstellar discs\, the formation of large circumbinary discs is possible. This can lead to the formation of planets about binary stars to be just as likely as the their formation around single stars. LAST-MODIFIED:20181108T043608Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rajika Kuruwita (RSAA) "The formation and evolution of discs around young binary stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151119T000000Z DTEND:20151119T010000Z DTSTAMP:20261011T152429Z UID:blbphtb0skdvpjvuh8iqrkfk4k@google.com CREATED:20150903T015611Z DESCRIPTION:The main obstacle to understanding the formation and evolution of galaxies is our limited knowledge of the role played by gas. In particu lar\, we still lack measurements of the cold hydrogen gas\, which is the r eservoir for future star formation\, for large and unbiased samples for wh ich ancillary data on stellar and star formation properties are also avail able. Fortunately\, the Square Kilometre Array (SKA) and its precursor tel escopes promise to fill this gap\, ushering a golden era for studies of ga s in galaxies. In this talk\, I will show how pre-SKA facilities are alrea dy allowing us to make significant progress in this field. By taking advan tage of atomic hydrogen (HI) observations obtained as part of the GALEX Ar ecibo SDSS and ALFALFA surveys\, I will demonstrate that the combination o f deep\, targeted observations and spectral stacking of blind\, large-area shallow surveys is critical in order to characterize how the gas content of galaxies depends on their structure\, star formation activity and envir onment. I will also discuss the properties of the highest-redshift HI dete ctions to date\, and point out the relevance of all these findings for the next-generation HI surveys. LAST-MODIFIED:20151110T031606Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Barbara Catinella (ICRAR/UWA) "Gas and star formation properties of massive galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151120T032000Z DTEND:20151120T034000Z DTSTAMP:20261011T152430Z UID:g07i12piqaqjnfl5hnq8no2hnk@google.com CREATED:20151102T114611Z DESCRIPTION:I will introduce the work I will be doing for my Masters Thesis . I will first give background on protoplanetary disks and their structure s and features and then discuss which disks I will be studying and give an overview of the methods I will use to do this. LAST-MODIFIED:20151118T041607Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Eloise Birchall (RSAA) "Masters Thesis Proposal: Signs of Planet Fo rmation in Disks Around Young High-Intermediate Mass Stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240524T040000Z DTEND:20240524T050000Z DTSTAMP:20261011T152429Z UID:njsc2pgo5i7u7rhdt2sb2b8uu0@google.com CREATED:20240521T214107Z DESCRIPTION:The adaptive optics (AO) system requires natural guide stars to differentiate the focus error generated by the vertical shift in the sodi um centroid altitude together with atmospheric turbulence. This dependency on NGS restricts achieving usable sky coverage and AO operation during da wn. One of the proposed approaches to distinguishing these two focus error s is to continuously monitor the region of the sodium layer where the lase r guide star (LGS) is generated. The classical approaches used for this ta sk\, direct imaging and LIDAR technology\, have limitations on spatial res olution and equipment requirements. The technique of continuously amplitud e modulating the guidestar laser (GSL) according to the pseudo-random bina ry sequence (PRBS) has the potential to overcome the limitations of classi cal approaches and reduce the dependency of the AO system on the NGS. Howe ver\, for this technique to be implemented in AO systems\, it must be vali dated at different modulation strengths and modulation frequencies that sa tisfy the system requirements. Therefore\, I conducted a study to experime ntally verify the PRBS modulation technique for LGS applications. The stud y began with numerical simulations considering the parameters of two poten tial test sites in Australia: the 1.8-m EOS telescope at Mount Stromlo in Canberra and the 2.3-m ANU telescope at Siding Spring Observatory in Coona barabran. The numerical simulation study was extended to large and extreme ly large telescopes. Based on the system design and the on-sky requirement to validate the technique with two potential test sites in Australia\, ha rdware components were chosen\, procured\, and characterized in the labora tory. An experiment was conducted to validate the technique in the laborat ory with the chosen hardware. The study validated that the PRBS technique has the potential to overcome the monitoring of the sodium layer with clas sical approaches with high-power lasers. LAST-MODIFIED:20240521T214107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sowmya Krishna (RSAA) "Monitoring Mesospheric Sodium Layer for Lase r Guide Star Adaptive Optics by Continuous Laser Modulation Technique (End -of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170216T000000Z DTEND:20170216T010000Z DTSTAMP:20261011T152429Z UID:ps3j1uq8tv00e205u79je8o9qs@google.com CREATED:20170131T232108Z DESCRIPTION:In this talk\, I will describe ongoing work to study galaxy for mation and evolution in a cosmological framework with numerical simulation s. The simulations are performed using a moving-mesh approach that inherit s advantages of traditional particle- and grid-based methods by combining continuous spatial and temporal adaptivity with accurate solutions to the fluid equations of motion. Physically motivated models are included in th e simulations to account for feedback from stellar evolution and black hol e growth\, processes thought to be essential to galaxy assembly. Some app lications of the simulations will be presented\, including galaxy morpholo gies and fine structure\; tracking galaxies in time\; stellar halos and th eir age and metallicity gradients\; and the merger rate of galaxies. Shor tcomings of the simulations will be discussed along with efforts to refine the modelling to give better agreement with certain observables. LAST-MODIFIED:20170212T224105Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Lars Hernquist (Harvard) "Galaxy Assembly and Evolution" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180807T010000Z DTEND:20180807T020000Z DTSTAMP:20261011T152429Z UID:e05j04ml7uf49v8rk07rflmmak@google.com CREATED:20180801T072607Z DESCRIPTION:Binary stars are common\, and exert an outsize impact on many a reas of astrophysics. They are the source of a wide range of phenomena fro m type Ia supernovae to gravitational wave sources. Despite their importan ce\, the formation mechanism for the progenitors of interacting binaries a re still poorly understood. In this talk I will describe our understanding of binary formation in general\, and recent progress on the origin of clo se binaries. I will show how the evolution of the observed binary occurren ce rates as a function of stellar mass\, period\, and metallicity can plac e tight constraints on formation models. LAST-MODIFIED:20180802T051106Z LOCATION:Duffield Lecture Theatre (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kaitlin Kratter (University of Arizona) "The origin of close binary stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180105T030000Z DTEND:20180105T032000Z DTSTAMP:20261011T152429Z UID:7g69ermcj48asf4sob9ig50b9c@google.com CREATED:20171120T233611Z DESCRIPTION:Star formation driven outflows are believed to play an importan t role in regulating the conversion of gas to stars\, particularly in low mass galaxies. However\, the relationship between the presence of outflows and the rate and concentration of star formation within galaxies is a top ic of ongoing debate. I will present results from our adaptive optics inte gral field study of star formation driven outflows at z~2.3\, and discuss the kiloparsec scale properties of star formation in regions with and with out outflows. LAST-MODIFIED:20180103T045605Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rebecca Davies (MPE) "Kiloparsec Scale Properties of Star Formation Driven Outflows at z~2.3 with the SINS-AO Survey" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170421T043000Z DTEND:20170421T045000Z DTSTAMP:20261011T152429Z UID:l57qnjo60uhk6nd4av2be9qtag@google.com CREATED:20170419T013604Z DESCRIPTION:Luminous and ultraluminous infrared galaxies [(U)LIRGs] are som e of the most extreme objects in the universe with their elevated star for mation rates and/or presence of a powerful AGN\, playing a central role in the evolution of galaxies throughout cosmic history. The 201 local (U)LI RGs (z<0.088) comprising the Great Observatories All-Sky LIRG Survey (GOAL S) provide an unmatched opportunity to characterize their diverse properti es in a large\, statistically significant sample\, in addition to comparis ons with their high redshift counterparts. In this talk I will first pres ent the Herschel PACS and SPIRE far infrared image atlas of the entire GOA LS sample (encompassing the 70-500 micron wavelength range)\, and demonstr ate the excellent data quality as described in Chu et al. (2017). The Her schel GOALS images presented here are the highest resolution\, most sensit ive and comprehensive far-infrared imaging survey of the nearest (U)LIRGs to date. This allows us for the first time to directly probe the critical far infrared and submillimeter wavelength regime of these systems\, enabl ing us to accurately determine their bolometric luminosities\, infrared su rface brightnesses\, star formation rates\, and dust masses and temperatur es on spatial scales of 2-5 kpc. In addition\, the superb resolution of H erschel means we can resolve many of the galaxy pairs and systems within t he GOALS sample\, allowing us to measure far infrared fluxes of component galaxies. Finally\, using the Herschel photometry in conjunction with Spi tzer\, WISE\, and IRAS data\, I will show our first results on the global properties of (U)LIRGs such as their average 3-500 micron infrared SEDs an d far infrared colors\, and compare them to lower infrared luminosity obje cts. We also compare and contrast their infrared SED shapes with previous ly published SED templates from the literature which will be presented in an upcoming paper. Finally as a treat\, I will show some of my favorite p hotographs and a time lapse video from Maunakea\, one of the best astronom ical observing sites in Hawai`i. LAST-MODIFIED:20170419T032605Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jason Chu (University of Hawaii) "Understanding Local Luminous Infr ared Galaxies in the Herschel Era" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230718T010000Z DTEND:20230718T020000Z DTSTAMP:20261011T152429Z UID:hfhljjl9k8po3js9c3rq2bfbvc@google.com CREATED:20230626T021607Z DESCRIPTION:TBA LAST-MODIFIED:20230626T021607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBA) \nZoom: https://anu.z oom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Zefeng Li (RSAA) "TBA (End of Thesis Talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181120T032000Z DTEND:20181120T034000Z DTSTAMP:20261011T152430Z UID:arvvjvu0286c5t2lpb609igua0@google.com CREATED:20181101T233111Z DESCRIPTION:Performing experiments in near-space environments can be prohib itively expensive. The Yerraloon project aims to provide a solution to thi s in the form of a high-altitude balloon mounted platform. Two teams of en gineering students from ANU have worked on realising this goal throughout 2018\, creating a prototype which has seen a successful flight. This prese ntation will showcase the progress made by the two ANU teams on the projec t thus far. LAST-MODIFIED:20181117T102106Z LOCATION:CSO Common Room (host: Zerjal) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:YerraLoon Techlauncher Team (AITC) "A High-Altitude Balloon Platfor m for Near Space Experimentation" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170112T220000Z DTEND:20170113T060000Z DTSTAMP:20261011T152429Z UID:3gbhi4o7le67nrk3nr9k9c69l0@google.com CREATED:20161209T040609Z DESCRIPTION:The RSSA Summer Research Students will give end of project pres entations. LAST-MODIFIED:20161209T040609Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Summer Students (various affiliations) "Summer Student Seminar" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241029T000000Z DTEND:20241029T010000Z DTSTAMP:20261011T152429Z UID:oduo673q05mnorl7ssbir1ou10@google.com CREATED:20240815T065140Z DESCRIPTION:Studying the formation and evolution of galaxies\, from the epo ch of reionization (EoR) to the present day\, unveils a captivating narrat ive of cosmic history. Hydrogen Lyman-alpha (Lyα) emission is a critical probe for understanding the high-redshift Universe and a powerful tool to shed light on star-formation activities. Emergent Lyα spectra (single\, d ouble peak) provide useful hints on circumgalactic medium (CGM) gas kinema tics and interstellar medium (ISM) structure. Further\, the precise timing of reionization and sources capable of emitting sufficient ionizing photo ns (Lyman-continuum or LyC photons) remain subjects of active debate till date. Direct observation of LyC photons is almost impossible at z > 4 due to strong intergalactic medium (IGM) attenuation. Lyα emission\, however\ , serves as a reliable indirect tracer of LyC leakage. Using VLT/MUSE data \, we have been studying Lyα emitting galaxies\, known as Lyα emitters ( LAEs) up to the edge of cosmic reionization. Particularly\, by simulating observed double-peaked profiles of Lyα emission using radiative transfer model\, we have been investigating complex gas kinematics (inflows and out flows)\, ISM properties and conditions that lead to escape of both Lyα an d LyC photons. We have also been investigating the survival of Lyα photon s from luminous LAEs showing broad line profiles during the reionization e ra. Our findings suggest that high-luminosity LAEs at z > 6 tend to reside in more highly ionized regions compared to lower luminosity LAEs\, self-s hielding them from IGM scattering. This study advances our understanding o f the cosmic reionization process in the Universe. LAST-MODIFIED:20241002T233618Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Vanhiep Nguyen) \nZoom: ht tps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tamal Mukherjee (Macquarie) "Probing galaxy kinematics and the epoc h of reionization using Lyman-alpha emission (ECR Colloquium)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230831T010000Z DTEND:20230831T023000Z DTSTAMP:20261011T152429Z UID:omnah6nvr5usiqg25sguqh7mas@google.com CREATED:20230818T042113Z DESCRIPTION:Cosmological simulations are power houses to understand the for mation of structures through cosmic time\, from the largest collapsed stru ctures of galaxy clusters to individual galaxies\, from early redshifts as high as z=10 to present day. However\, comparisons to observations at dif ferent times are needed to test the accuracy of the implemented models\, a nd to connect the observables at varying redshifts to the evolution pathwa ys of structures. Using one of the largest state-of-the-art hydrodynamical cosmological simulation suites\, Magneticum Pathfinder\, we analyze how s tructure formation is imprinted in present-day properties. Starting with t he evolution of the earliest quenched galaxies and protoclusters\, we show that they evolve into a large range of halos at present day\, and only ra rely into the most massive clusters observed at low redshifts. Using prese nt-day properties as a lens into the past\, we demonstrate that some of th e best tracers of formation pathways are the substructures\, the presence of shells\, streams\, and satellite planes around galaxies\, and the centr al kinematics of galaxies. The latter can even be used to infer the fracti ons of accreted stars\, which we find to be much more difficult when emplo ying radial stellar density distributions. We will take you on a journey t o explore galaxy formation from the highest to lowest redshifts\, connecti ng to observations from JWST\, MAGPIE\, and SAMI. LAST-MODIFIED:20230828T012108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Emily) \nZoom: https://anu .zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rhea-Silvia Remus (Universitats-Sternwarte Munchen) "From Cosmic Da wn to Present-day: Connecting Large Scale Structure and Galaxy Properties" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191010T000000Z DTEND:20191010T010000Z DTSTAMP:20261011T152429Z UID:ou92rrg37hkvvqscprj03dv8lg@google.com CREATED:20191001T061603Z DESCRIPTION:The short time domain (< 1 day) is the frontier of transient as tronomy. In this frontier\, new phenomena are waiting to be discovered tha t may hold the answers to crucial questions\, particularly for progenitors of extreme events e.g.\, supernovae\, gravitational waves/kilonovae\, and GRBs. I will present the work from my thesis to develop GLUV\, a high cad ence UV survey telescope system\, and a systematic search of Kepler/K2 dat a through the Background Survey for undiscovered transients. From the Back ground Survey I have detected numerous unknown transients serendipitously observed by Kepler. The First confirmed discovery is a WZ Sge type dwarf n ova called KSN:BS-C11a\, with a broken rise that indicates new physics in dwarf nova. The detection of a broken rise in KSN:BS-C11a was only possibl e with high cadence observations\, and is indicative of future discoveries that will be made in the short time domain as we explore it with Kepler\, TESS and GLUV. LAST-MODIFIED:20191002T035605Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ryan Ridden (RSAA) "The Fronteir of Cosmic Cataclysms (End-of-Thesi s Colloquium)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171116T043000Z DTEND:20171116T045000Z DTSTAMP:20261011T152429Z UID:c4e6qo6u75jdfi2sr00qbm4l14@google.com CREATED:20171115T223106Z DESCRIPTION:Planet 9 is a predicted new planet on the edge of the Solar Sys tem. A large effort has been made to identify where or where not it may e xist. The SkyMapper Southern Sky Survey has catalogued vast areas of the parameter space of Planet 9. In order to search through the images\, we w orked with BBC Stargazing Live to conduct a citizen science search. Here we will update the progress of that search including processing the data f rom the citizen science search and the analysis of potential candidates. LAST-MODIFIED:20171115T224106Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jonah Hansen and Gianni Gagliardo (ANU) "Process the Planet 9 Citiz en Science Search Data" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151211T030000Z DTEND:20151211T033000Z DTSTAMP:20261011T152429Z UID:fpf51vs7b6f7ugb2c6ougg2reg@google.com CREATED:20151130T050108Z DESCRIPTION:I review some of what I’ve recently learned about the portray al by and of women in Hollywood productions. I first discuss how women are under-represented in roles as writers\, directors\, cinematographers\, et c\, some of the discussion around the issue\, and in contrast how many men manage to make it to the top of the queue fairly quickly. I then continue with a few case studies such as Starship Troopers\, Frozen\, and Jurassic World\, each provides an invaluable\, distinct lesson in how women are an d can be portrayed by Hollywood\, and what the forces for that portrayal a re. LAST-MODIFIED:20151203T000108Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:David Nataf (RSAA) "Portrayal of and by Women in Hollywood" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190725T233000Z DTEND:20190726T003000Z DTSTAMP:20261011T152429Z UID:mo6ri1g1o109men4r1d43qs450@google.com CREATED:20190712T010608Z DESCRIPTION:[A colloquium by the shortlisted candidate for the new Centre f or Gravitational Astrophysics] Neutron stars host the densest stable matte r in the universe. Accurately modeling their multi-messenger astrophysics relies on a detailed description of the equation of state above nuclear de nsity\, and astronomical observations ranging from x-ray timing to gravita tional waves are in turn being used to constrain the properties of this de nse matter. The first gravitational-wave signal from a neutron star coales cence was observed in August 2017. I will describe how LIGO and Virgo have used this signal to constrain the equation of state of dense matter in ne utron stars. The gravitational-wave transient was almost immediately assoc iated with a short gamma-ray burst\, and three- dimensional localization o f the source using LIGO and Virgo data enabled a electromagnetic follow-up campaign that identified an associated kilonova in the galaxy NGC 4993. A dditional information about dense matter emerges from such observations of light in concert with the gravitational waves. A new observing run began in April 2019\, and LIGO and Virgo have already sent public alerts for a c ouple of neutronstar merger candidates. I will outline prospects for learn ing about matter with gravitational waves in the current Advanced-detector era\, and discuss how precision measurements with future ground-based obs ervatories can map the phase diagram of dense neutron-rich matter. LAST-MODIFIED:20190712T010608Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jocelyn Read (California State University Fullerton) "Neutron star matter and gravitational waves" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221013T003000Z DTEND:20221013T010000Z DTSTAMP:20261011T152429Z UID:0p9nltupvj1ovrolfn47ssbd8s@google.com CREATED:20221007T095608Z DESCRIPTION:Outflows are likely to play a key role in shaping the early ass embly of galaxies. Tidal interactions trigger star formation and black hol e growth which subsequently drive outflows\, ejecting gas and metals into the surrounding environment. Detecting and characterizing outflows at z > 3.5 is challenging\, but ground-breaking new observational datasets are no w providing the first key insights into their properties. I will present e xciting new results from the ESO large program XQR-30\, focusing on the pr operties of CIV absorbers at z=4-6 which probe the early enrichment of the circumgalactic medium by star-formation-driven outflows. I will also brie fly introduce two new surveys that will use ALMA and JWST to directly cons train the prevalence and properties of outflows in the early Universe. LAST-MODIFIED:20221012T045106Z LOCATION:DLT & ZOOM (host: Neco Kriel) \nZoom: https://anu.zoom.us/j/997853 41005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rebecca Davies (Swinburne University) "Outflows in the era of galax y assembly" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170721T040000Z DTEND:20170721T042000Z DTSTAMP:20261011T152429Z UID:ae4uuipcsq1jqnhr585k9uj3nk@google.com CREATED:20170710T014106Z DESCRIPTION:I have recently been shown that it may be possible to use activ e galactic nuclei as standardisable candles\, which would allow us to prob e cosmological parameters at higher redshifts than possible with type Ia s upernovae. In my annual review I talk about the progress I have made towar ds using DES and OzDES observation to make this a reality. LAST-MODIFIED:20170719T231106Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Natalia Sommer (RSAA) "Annual review: Reverberation Mapping — Stu dying the Universe by Studying Active Galactic Nuclei" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210701T010000Z DTEND:20210701T013000Z DTSTAMP:20261011T152429Z UID:3vi63hrn1hnruijes98gs3phc0@google.com CREATED:20210603T040113Z DESCRIPTION:The first detection of gravitational waves (GWs) from the coale scence of two stellar mass black holes in 2015 opened a long-sought window into our universe. Since then\, nearly 100 such compact binary coalescenc es (CBCs) have been detected by the LIGO and Virgo interferometers. In 201 9\, the LIGO-Virgo collaboration (LVC) provided public alerts of GW events in close to real time\, a service made possible by the LVC's five low-lat ency data analysis pipelines which continuously analyse data collected by the interferometer network. The SPIIR pipeline\, developed at the Universi ty of Western Australia\, is the fastest of the five pipelines\, performin g a coherence search for cosmic GW signals. In this talk I will give an ov erview of the novel SPIIR method and its application in GW detection\, res ults from the third observing run\, and the prospects for real-time and 'e arly warning' detection of GWs in the upcoming fourth LIGO-Virgo-KAGRA obs erving run. LAST-MODIFIED:20210617T023113Z LOCATION:ZOOM and DLT (host: Lyla Jung) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Fiona Panther (UWA) "Low-latency detection of gravitational waves: The SPIIR pipeline" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250403T000000Z DTEND:20250403T010000Z DTSTAMP:20261011T152429Z UID:phb36s4ic1beefgnag6rvdptlo@google.com CREATED:20250317T025610Z DESCRIPTION:We employ natural language processing algorithms with attention \, repurposed to receive QSO spectra to predict unseen spectra\, broad lin es\, and super massive black hole masses. We find that the trained algorit hm is able to reproduce with high significance masked broad lines and/or c ontinua in QSO spectra\, highlighting an ability to learn from and leverag e physical information imprinted amongst the entire spectrum. A key implic ation is that this information may help to refine physical properties such as single-epoch black hole masses. We tested the algorithm's ability to d irectly predict black hole masses\, with no spectral fitting or decomposit ion\, finding reasonable success to reproduce single-epoch prescriptions. Finally\, the algorithm is able to reconstruct broad UV lines such as C IV and Ly-alpha in the presence of broad absorption lines\, outflows or inte rvening IGM. We will discuss the attention mechanism\, which allows us to peek inside and probe what information is being used to make the above pre dictions and several broad future applications that we envision. LAST-MODIFIED:20250331T225607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Chris Wolf) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Benedict Rouse (Pontificia Universidad Catolica de Chile) "Decoding AGN Spectra: Predicting and Reconstructing Broad Lines" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190801T010000Z DTEND:20190801T020000Z DTSTAMP:20261011T152429Z UID:5vhu9122lof08qbqnpompevsp8@google.com CREATED:20190702T003109Z DESCRIPTION:TBD LAST-MODIFIED:20190702T003109Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Troels Haugbølle "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170519T043000Z DTEND:20170519T045000Z DTSTAMP:20261011T152429Z UID:bs6ojmu32813i8p002rr7atb5k@google.com CREATED:20170313T232108Z DESCRIPTION:I will talk about recent work studying gas and star-formation i n samples of galaxies. In particular\, using the new xGASS survey\, we hav e found unusually gas-rich and star-forming central galaxies in small grou ps\, which we interpret as evidence of feeding from the cosmic web. At the other extreme\, the ALFALFA HI survey is finding gas-rich galaxies with a lmost invisible stellar populations. These (almost) dark galaxies are exce ptionally inefficient at forming stars and may be related to the recently re-discovered class of "ultra-diffuse" galaxies. LAST-MODIFIED:20170314T045110Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Steven Janowiecki (The University of Western Australia) "Gas and st ar formation in galaxies: the role of environment and (almost) dark galaxi es" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191122T030000Z DTEND:20191122T033000Z DTSTAMP:20261011T152429Z UID:n27cq27r6stujghjbg8dij7lkg@google.com CREATED:20191023T050511Z DESCRIPTION:We're all familiar with geostationary satellite antennas – th e Foxtel dishes atop many rooftops that point to a fixed location in space . The AITC has a number of programs\, however\, that rely on our ability to interact with satellites that freely zip across the sky under the influ ence of a plethora of perturbing forces. Understanding these forces is th e first step to being able to predict where any of the 20\,000+ catalogued orbital objects are at any particular instant so we know where – and wh en – to point our telescopes at them. In this talk I’ll outline how s atellites move\, how we find them and the challenges and opportunities the y afford to our communications and space environment research programs. LAST-MODIFIED:20191023T050511Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:James Webb (RSAA/AITC) "AITC Series – Space is big\, satellites a re (comparatively) small… the joys of finding\, tracking\, and using th em!" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170824T010000Z DTEND:20170824T020000Z DTSTAMP:20261011T152430Z UID:7p45cvl9t5jua9dfg9953urnfk@google.com CREATED:20170509T042114Z DESCRIPTION:The Milky Way hosts the annihilation of a few *10^43 positrons every second. Radionuclides capable of supplying such positrons are synthe sised in stars\, stellar remnants\, and supernovae. For decades\, however\ , there has been no positive identification of a main stellar positron sou rce. This has led to suggestions that many positrons originate from exotic sources like the Galaxy's central super-massive black hole or dark matter annihilation\, but such sources would not explain the recently-detected p ositron signal from the extended Galactic disk. We show that a single type of transient source\, deriving from stellar populations of age 3-6 Gyr an d yielding ∼ 0.03 MSun of the positron emitter 44Ti\, can simultaneously explain the absolute positron luminosity of the Galaxy and the morphology of the annihilation signal. Our binary population synthesis modelling dem onstrates that this transient is likely the merger of two low-mass white d warfs\, likely observed in external galaxies as a particular sub-luminous\ , thermonuclear supernova\, known as SN1991bg-like. LAST-MODIFIED:20170814T014108Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Roland Crocker (ANU) "An origin for most Galactic antimatter in low luminosity thermonuclear supernovae" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240313T030000Z DTEND:20240313T040000Z DTSTAMP:20261011T152429Z UID:k079j5df00t42lc4amlcrshh20@google.com CREATED:20240225T225617Z DESCRIPTION:During the first million years of evolution\, nascent planetary systems are embedded in dense disk-shaped clouds of gas. These circumstel lar disks are home to a myriad of hydrodynamical processes\, which bring a bout turbulence and the emergence of viscous-like behavior\, enabling accr etion of gas onto the protostar. Meanwhile\, micron-sized dust grains embe dded in the disk are growing through coagulation onto pebbles and rocks. L osing angular momentum to gas drag\, the pebbles drift toward the star in a process that turns out to be hydrodynamically unstable. This "streaming instability" has a positive feedback effect on the small solids\, concentr ating them strongly enough to achieve gravitational collapse into km-sized bodies\, forming the first planetesimals\, that subsequently grow through accretion of the remaining pebbles. Giant storm systems in the disk\, sim ilar to Jupiter's Great Red Spot\, may exist in quiescent zones of the dis k. These are even more prone to collecting solid material\, producing the first terrestrial planets and cores of giant planets. In this talk\, I wil l discuss the state of the art and recent advances in the field of planet formation\, as well as pressing problems such as how to find evidence for streaming instability in the Kuiper belt objects\, the structures observed in high resolution ALMA and VLA images of circumstellar disks\, and how t o interpret them. LAST-MODIFIED:20240225T225617Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Christoph Federrath) \nZoo m: https://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Wladimir Lyra (New Mexico State University) "Evolution of Circumste llar Disks and Planet Formation" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170810T010000Z DTEND:20170810T020000Z DTSTAMP:20261011T152429Z UID:agoolj6beee2lk8puvqli0ljck@google.com CREATED:20170710T014109Z DESCRIPTION:Hubble has revolutionized the discovery and study of very dista nt galaxies through its deep imaging surveys. Together the HST WFC3/IR and ACS cameras have opened up the exploration of the universe in the first b illion years after the Big Bang. I will discuss what we have learned abou t the earliest galaxies during the reionization epoch at z>6 from the rema rkable HST and Spitzer imaging surveys (e.g.\, HUDF/XDF\, GOODS\, HUDF09/1 2 and CANDELS)\, as well as surveys of galaxy clusters like the Frontier F ields (HFF). Lensing clusters provide extraordinary opportunities for char acterizing the faintest earliest galaxies\, but also present extraordinary challenges. Together these surveys have reliably established the volume d ensity of galaxies in the first billion years down to extremely faint leve ls around -14.5 mag. The results from deep UV luminosity functions from Hu bble\, combined with the recent results from Planck\, indicate that galaxi es dominate the UV ionizing flux that reionized the universe. Some of the greatest surprises have come from the discovery of very luminous galaxies at z~8-11\, around 400-650 million years after the Big Bang. Spectroscopic followup of these very rare\, bright galaxies has confirmed redshifts fro m z~7 to z~11\, and revealed\, surprisingly\, strong Lyman alpha emission near the peak of reionization when the HI fraction in the IGM is high. The small sizes of galaxies at high redshifts\, from analysis of the HFF clus ter samples\, reveal objects that\, remarkably\, are as small as globular clusters and dwarf galaxies. The recent confirmation of a z=11.1 galaxy\, just 400 million years after the Big Bang\, by a combination of Hubble and Spitzer data\, pushed Hubble into JWST territory\, far beyond what we eve r expected Hubble could do. Twenty years of astonishing progress with Hub ble and Spitzer leave me looking to JWST to provide even more remarkable e xploration of the realm of the first galaxies at "Cosmic Sunrise". The la test results on the sizes of distant galaxies\, on the star formation rate density at z~10 and from Planck indicating that reionization began around z~10 together have significant implications for the detectability of the "first galaxies" with JWST. LAST-MODIFIED:20170717T064110Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Garth Illingworth (University of California\, Santa Cruz) "Galaxies at Cosmic Dawn: Exploring the First Billion Years with Hubble and Spitzer - Implications for JWST" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170503T013000Z DTEND:20170503T015000Z DTSTAMP:20261011T152429Z UID:oo6mlo44mqqbl90p11a4994dus@google.com CREATED:20170502T051103Z DESCRIPTION:There is a growing interest in the development of ground statio n technology for catalogue maintenance or ad-hoc measurements of orbital o bjects like space debris or satellites for initial orbit prediction. Optic al methods are providing efficient solutions for space situational surveil lance in order to support catalogue maintenance. The Institute of Technica l Physics already operates a laser ranging station with a fiber-based lase r transmitter and another transportable one built in a 20 ft ISO container which is in progress. The setup of both stations will be briefly presente d. Furthermore the exploitation of the ranging data which can contain not only the slant range but also information about the dimension and rotation of an orbital object is discussed in this work. LAST-MODIFIED:20170502T051103Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Leif Humbert (German Aerospace Center\, Institute of Technical Phys ics\, Stuttgart) "INNOVATIVE TECHNOLOGIES FOR OPTICAL GROUND STATIONS" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240209T030000Z DTEND:20240209T040000Z DTSTAMP:20261011T152429Z UID:et6jqh3k15sb3634jrjeb2h7jg@google.com CREATED:20240204T232609Z DESCRIPTION:Supernova explosions are some of the most energetic and luminou s events in the universe\, and understanding them is crucial for many area s of astrophysics. One way to gain insight into the physical processes inv olved in these explosions is through supernova tomography\, which involves reconstructing a spatially resolved explosion model using a spectral time series. However\, this requires a radiative transfer model and is computa tionally intractable with traditional means\, requiring millions of MCMC s amples. A new solution to this problem is the use of surrogate models or e mulators\, which employ machine learning techniques to accelerate simulati ons. In this talk\, we present a new emulator for the radiative transfer c ode TARDIS that outperforms existing emulators and provides uncertainties in its prediction. This offers the foundation for a future active-learning -based machinery that will be able to emulate very high dimensional spaces of hundreds of parameters crucial for unraveling urgent questions in supe rnovae and related fields. Our work provides a promising avenue for unders tanding the physical processes involved in supernova explosions and their progenitors\, with implications for a wide range of astrophysical phenomen a. In this talk\, I will elaborate on the technique and describe various s cience cases explored by my group and the TARDIS collaboration. LAST-MODIFIED:20240207T050608Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Chris Wolf) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Wolfgang Kerzendorf (Michigan State University) "Reconstructing the physics of transients using machine learning" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240620T010000Z DTEND:20240620T020000Z DTSTAMP:20261011T152430Z UID:javi1qv4719trumaejcs5smsck@google.com CREATED:20240415T040127Z DESCRIPTION:In recent decades\, simulations of galaxy formation and evoluti on have become invaluable tools for understanding our Universe. The curren t simulation landscape encompasses a wide range\, from modeling individual galaxies to the large-scale structure of the cosmos\, while simultaneousl y incorporating the physics of stellar feedback\, AGN feedback\, chemical enrichment\, gas accretion\, outflows\, and more. However\, each simulatio n employs slightly different assumptions\, leading to diverse predictions for galaxy properties. Understanding the specific choices made in calibrat ing these models is essential for distinguishing between different impleme ntations. This talk will investigate the implications of these choices on galaxies\, with a particular emphasis on the evolution of metallicity. The metal content of galaxies can trace the gas flows within them\, serving a s a direct indicator of the underlying physical processes driving galaxy e volution. Our findings suggest that metallicity is a critical area for exp loration that may help constrain future simulation models and provide deep er insights into the physics driving galaxy evolution. LAST-MODIFIED:20240614T015110Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Katie Grasha) \nZoom: http s://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alex Garcia (U. Virginia) "Using the Metal Content of Simulated Gal axies to Understand Galaxy Evolution" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250617T010000Z DTEND:20250617T020000Z DTSTAMP:20261011T152429Z UID:ghi8oa0caekrrptko6qech9v24@google.com CREATED:20250520T123613Z DESCRIPTION:Selecting a plasma simulation tool is an exercise in compromise . Naïve application of the many tools available will in the best-case res ult in computationally expensive results. In the worst case\, it will give gibberish results. In the first part of this talk I will give a high-leve l overview of the hierarchy of models and explain when they might be used. I’ll then share results from continuum plasma simulations of the Richtm yer-Meshkov instability to show how different the results might be for the same problem. In the second part of the talk\, I will discuss the applica tion of magnetohydrodynamics to the simulation of solar flares and coronal mass ejections. The goal of this work is the prediction of space-weather\ , the combined phenomena driven by solar eruptions that can damage space a nd terrestrial infrastructure as well as driving the beautiful auroras. LAST-MODIFIED:20250622T062708Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Christoph Federrath) \nZoo m: https://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kyriakos Tapinou (U Sydney) "What do you want from your plasma simu lation?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150521T010000Z DTEND:20150521T020000Z DTSTAMP:20261011T152429Z UID:b5nt66snold8po6gsjecnpvals@google.com CREATED:20141218T102613Z DESCRIPTION:Observations of the cosmos provide a valuable tool to study the fundamental laws of nature. The future generation of astronomical surveys will provide data for a sizeable fraction of the observable sky. These ri ch data set should provide the means to answer fundamental questions: what are the laws of physics at high energies in the Early Universe? what is t he nature of neutrinos? what is the dark matter? what is the dark energy? why are there baryons at all? In this talk I will review the current statu s\, provide a roadmap for future prospects and discuss in detail how we mi ght approach the task of extracting information from the sky to answer the above questions. LAST-MODIFIED:20150518T073604Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Raul Jimenez (University of Barcelona) "Fundamental physics and obs ervations of the Universe" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250902T010000Z DTEND:20250902T020000Z DTSTAMP:20261011T152429Z UID:634d39ojch8kqolgd6q0usisqk@google.com CREATED:20250520T123619Z DESCRIPTION:The historic detection of gravitational waves from the electrom agnetically bright binary neutron star merger GW170817 enabled the first s tandard siren measurement of Hubble's constant (H0). The accuracy and pre cision of this measurement depends crucially on how well the merger inclin ation angle is constrained\, given its strong covariance with luminosity d istance. Modeling the light curve of the jet's afterglow provides constrai nts on inclination\, but is highly dependent on the similarly uncertain je t opening angle. Past studies have improved on this by invoking high-resol ution radio observations\, obtained through very long baseline interferome try\, to constrain the viewing angle. In this talk\, I will present our Ba yesian visibility-plane model-fitting framework that provides a more infor med and robust measurement of the viewing geometry of GW170817\, by includ ing all relevant data\, robustly handling systematic uncertainties\, rigor ously sampling model parameter space and using new hydrodynamical jet mode ls. We extend our framework to fit for H0 directly\, and consider various plausible peculiar velocity corrections to present a new and improved sta ndard siren measurement of H0. Strikingly\, we find our result to be in be tter agreement with one of the two precise and independent H0 measurements that are famously in tension. LAST-MODIFIED:20250814T070107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Ashley Tan) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kelly Gourdji (CSIRO) "Revisiting GW170817 at milliarcsecond scale: high-precision constraints on jet geometry and Hubble's constant" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170317T033000Z DTEND:20170317T035000Z DTSTAMP:20261011T152429Z UID:18dt8cq6kek49nul5g57udd1lo@google.com CREATED:20170301T104610Z DESCRIPTION:The stellar halo hosts only a small fraction of the baryonic co mponent of the Galaxy (< 1%)\, however the study of its structural propert ies is fundamental both to understand the formation and evolution of the M ilky Way and to study the Galactic dynamics. The easiest way to infer the spatial distribution of objects in the halo is counting the stars that are tracers of the halo population as for example RRLyrae (RRL). Results of past works are only in roughly agreement and are limited in the volume sam pling of the halo by the footprint of the used survey. In this context\, t he advent of GAIA offers a dramatic improvement. Although the final catal ogue of variable stars will be released only by the end of the mission (ab out 2020)\, I present a method to select a sample of RRLs by using only time integrated quantities from the first Gaia data release. I analysed the sample to retrieve the properties of the the inner halo (Rg<28 kpc): its shape is well reproduced by a oblate ellipsoid flattened along the z-a xis (axes ratio about 0.55). while the density follows a single power-law with index about -2.7. There is no evidence of a change of slope of the de nsity\, but for the first time we are able to show directly on the data a change of halo flattening at large radii (Rg>20-25 kpc). Finally\, I discu ss the possible extensions and improvement of this work that can be obtai ned with the future GAIA data releases. LAST-MODIFIED:20170307T215606Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Giuliano Iorio (University of Bologna) "A First Gaia look at the in ner halo" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151203T220000Z DTEND:20151204T060000Z DTSTAMP:20261011T152429Z UID:l2a6f4qr5n0339kg0e7kv2pmuo@google.com CREATED:20151002T050616Z DESCRIPTION:A number of student talks will be presented. LAST-MODIFIED:20151002T050616Z LOCATION:Duffield Lecture Theatre (host: Sarah Leslie) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Students (various affiliations) "Mt Stromlo Student Christmas Semin ars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260716T013000Z DTEND:20260716T023000Z DTSTAMP:20261011T152430Z UID:0b6if79mdlgh2upcvqgj5dnr9s@google.com CREATED:20260503T114412Z DESCRIPTION:Metal-poor stars are among the oldest observable objects we can study in the Milky Way today. Formed over 10 billion years ago\, their at mospheres retain the pristine chemical imprint of their birth environments . By analysing these chemical abundance patterns\, we can directly probe t he early history of our Galaxy. In this end-of-thesis talk\, I combine che mical and kinematic data from these ancient stars to explore the early evo lution of the Galactic disk\, shedding light on the processes that shaped it into the structure we observe today. LAST-MODIFIED:20260715T020005Z LOCATION:Zoom or Duffield Lecture Theatre (host: TBC) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ben Lowe (RSAA) "Tracing the Chemical Evolution of the Early Milky Way with Metal-Poor Stars (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250227T000000Z DTEND:20250227T010000Z DTSTAMP:20261011T152429Z UID:ln4kfc4acpsej5a89cb09bt9h8@google.com CREATED:20241108T053125Z DESCRIPTION:Spiral structures are commonly found in the local Universe\, ye t their origins and influence on gas and stars remain debated. A powerful approach to probing these mysteries is mapping the interstellar medium and stellar age across spiral arms. During my PhD\, I studied spiral galaxies at z~0.3 and z~0 using IFU data from the MAGPI (MUSE) and TYPHOON surveys . I find azimuthal variations in star formation rate and gas-phase metalli city\, supporting density wave theory at both redshifts. However\, some ga laxies also align with dynamic spiral theory\, and one nearby spiral exhib its an azimuthal offset opposite to density wave predictions\, possibly du e to an ongoing merger. This suggests that no single theory explains all s piral structures at low redshifts. Since observations capture only snapsho ts over cosmic time\, I use Auriga simulations to trace the azimuthal dist ribution of stellar age over 5 Gyr. I find a younger leading edge in most snapshots\, consistent with density wave theory\, while gas-rich interacti ons can erase these azimuthal variations\, recovering within 600 Myr. Futu re studies\, such as high-redshift observations and higher time-resolution simulations\, will better constrain the long-term evolution of spiral gal axies. LAST-MODIFIED:20250120T025119Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Katie Grasha) \nZoom: http s://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Qianhui Chen (RSAA) "Constraining the evolution of spiral galaxies over cosmic time with observations and simulations (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210406T010000Z DTEND:20210406T020000Z DTSTAMP:20261011T152429Z UID:fmt8alpkjqfveh9svgr2uj609s@google.com CREATED:20210114T070111Z DESCRIPTION:TBD LAST-MODIFIED:20210317T215612Z LOCATION:ZOOM (host: Shyam Menon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Olivia Byrd (US AFRL) "Invited Colloquium" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240312T000000Z DTEND:20240312T013000Z DTSTAMP:20261011T152429Z UID:j24g4455o7hu3trgkutb4ji1o8@google.com CREATED:20231212T120224Z DESCRIPTION:The Universe started without the heavy elements that make the c omplexity of our surrounding world (e.g. carbon\, oxygen). In this talk\, I will showcase ground-breaking advances in the numerical modelling of how these chemical elements are produced in stars\, how they are dispersed ar ound young galaxies by energetic events\, and how they get ionized to powe r the emission and absorption lines we observe in the spectra of distant o bjects. Leveraging these new prediction capabilities will take us from int erpreting the highest-redshift emission lines observable by JWST to the mo st local chemical abundances of Galactic stars\, shedding a new light on h ow metal-poor stars enriched the Universe in the process. LAST-MODIFIED:20240219T113614Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Trey Yang) \nZoom: https:/ /anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Martin Rey (Oxford U.) "Live fast\, die young: how the Universe got its first chemical elements from early stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180816T010000Z DTEND:20180816T020000Z DTSTAMP:20261011T152430Z UID:nu6pg45nunhqt076v73eikt5tc@google.com CREATED:20180725T083111Z DESCRIPTION:For several years the Director General of the European Space Ag ency\, Johann-Dietrich Wörner\, has been advocating the creation of a hum an-robotic ‘Moon Village’ as the next major step in international spac e exploration. In this talk I will examine the scientific case for such a facility on the lunar surface. An analogy may be the way in which human ou tposts in Antarctica facilitate research activities across multiple scient ific disciplines on that continent. Scientific fields expected to benefit from a Moon Village will include: planetary science\, astronomy\, astrobio logy\, life sciences\, and fundamental physics. From an astronomical point of view\, a particularly important aspect may be accessing lunar geologic al records of the early evolution of the Sun and of the Solar System's cha nging location in the Galaxy. In addition\, the farside of the Moon may be the best location anywhere in the Solar System from which to conduct low- frequency radio astronomy. Last\, but perhaps not least\, establishing a M oon Village may help develop the use of lunar resources which may make fut ure space science activities more affordable. LAST-MODIFIED:20180815T175106Z LOCATION:Duffield Lecture Theatre (host: Birchall) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ian Crawford (Birkbeck College London) "Why we should build a Moon Village: The scientific case for returning to the Moon" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180321T000000Z DTEND:20180321T010000Z DTSTAMP:20261011T152430Z UID:hqqjj3l2ahmf8l1rvcgdd51dc8@google.com CREATED:20180319T121607Z DESCRIPTION:TBD LAST-MODIFIED:20180320T060606Z LOCATION:AITC meeting room 1 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Roger Smith (Caltech Optical Observatories) "The Zwiki Transient Fa ctory (ZTF)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201009T030000Z DTEND:20201009T033000Z DTSTAMP:20261011T152429Z UID:it410ma5itv8l3afo6bfef4cog@google.com CREATED:20200826T024113Z DESCRIPTION:The new FoF format is like an Open Mic: Our speakers have 15 mi nutes each to talk about topics of their choice. The idea of the new FoF i s to get to know the many individuals that work under the same roof\, allo w newcomers to find friends easily\, and find new friends or colleagues wi th similar interests and hobbies. So feel free to talk about some of your most favourite adventures\, memorable Stromlo anecdotes\, your hobbies\, y our last COVID-DIY project\, your voluntary activities outside of Stromlo or whatever you are passionate about. Science talks (about a scientific to pic/question that you are interested in) are also welcome\, but be mindful of your audience (astronomers\, students\, engineers\, professional staff ). LAST-MODIFIED:20201008T051605Z LOCATION:ZOOM 997 8534 1005 (host: Martinez) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Marusa Zerjal and Arthur Puls (RSAA) "Slovenia and Brasil" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250729T010000Z DTEND:20250729T020000Z DTSTAMP:20261011T152429Z UID:34a5gbpnnpbrsg4scrl0t6hcrc@google.com CREATED:20250520T123616Z DESCRIPTION:As we pursue explanations to the details of galaxy evolution th rough statistics and large galaxy surveys\, both at low and high redshift\ , there is an ever growing demand for sophisticated SED fitting techniques . Not just the estimators for stellar mass and SFR they were originally de signed to be\, these techniques are today relied upon to extract the histo ry of star formation. Doing this means implementing more physically motiva ted models. Beyond expanding the detail we derive\, these more physical mo dels ensure greater accuracy of the fundamental parameters like stellar ma ss. In this talk I will outline the developments made through the code Pro Spect in terms of the underlying models\, and present a characterisation o f the biases introduced through various common assumptions. I will finally present the first results from a new technique that combines SED fitting with simultaneous structural analysis. LAST-MODIFIED:20250703T020108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hajime Ogane) \nZoom: http s://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sabine Bellstedt (UWA) "In pursuit of realistic star formation hist ories from SED fitting" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201211T030000Z DTEND:20201211T033000Z DTSTAMP:20261011T152429Z UID:gvlo7jsdn9gpojdai50td194ks@google.com CREATED:20201210T040107Z DESCRIPTION:The new FoF format is like an Open Mic: Our speakers have 15 mi nutes each to talk about topics of their choice. The idea of the new FoF i s to get to know the many individuals that work under the same roof\, allo w newcomers to find friends easily\, and find new friends or colleagues wi th similar interests and hobbies. So feel free to talk about some of your most favourite adventures\, memorable Stromlo anecdotes\, your hobbies\, y our last COVID-DIY project\, your voluntary activities outside of Stromlo or whatever you are passionate about. Science talks (about a scientific to pic/question that you are interested in) are also welcome\, but be mindful of your audience (astronomers\, students\, engineers\, professional staff ). LAST-MODIFIED:20201210T040107Z LOCATION:ZOOM 997 8534 1005 (host: Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ken Freeman\,Geoff McNamara (RSAA\,MSATT) "Intuition in Research an d Mentoring MSATT kids in 2021" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261022T000000Z DTEND:20261022T010000Z DTSTAMP:20261011T152430Z UID:184peik50fq5qhr05ldbrklbik@google.com CREATED:20260904T010014Z DESCRIPTION:I will discuss the chemical evolution of the Milky Way in the l ight of detailed Galactic chemical evolution models. Indeed\, we are in a golden era for Galactic archaeology thanks to the advent of large spectros copic surveys\, that can provide detailed stellar abundances of stars in t he Galaxy. Stellar ages can then provide further fundamental constraints t o reconstruct the Galactic history. Then\, by means of detailed chemical e volution models\, it is possible to predict the chemical abundances expect ed in the stars of the different Galactic components. From the comparison between data and model predictions\, it is possible to constrain the histo ry of star formation occurred in each component\, and thus the history of the entire Galaxy. In particular\, I will focus on the chemical bimodality between the Galactic thick and thin discs. I will start by discussing the dichotomy in the [α/Fe] vs. [Fe/H] diagram where we can clearly see two distinct sequences corresponding to the thick and thin discs\, and then I will discuss the bimodality in other abundance patterns\, from light to he avy elements. LAST-MODIFIED:20260923T130011Z LOCATION:Zoom or Duffield Lecture Theatre (host: Giada Casali) \nZoom: http s://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Valeria Grisoni (INAF) "Galactic archaeology with chemical evolutio n models" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241206T000000Z DTEND:20241206T010000Z DTSTAMP:20261011T152430Z UID:o86t2p3sq659sj1ef01p728r6g@google.com CREATED:20241202T024606Z DESCRIPTION:Deciphering the physical processes occurring in the inner regio ns of protoplanetary disks is key to understanding the environmental condi tions of planet formation and evolution. This requires the development of cutting-edge instruments with high-angular resolution capabilities\, in wh ich we are actively involved at the University of Cologne. I will first pr esent the GRAVITY enterprise that has enabled high-sensitivity long-baseli ne interferometry at the ESO Very Large Telescope Interferometer and show new results that have been obtained in the framework of the GRAVITY YSO su rvey on the characterization of the innermost regions of protoplanetary di sks. I will point at new opportunities offered by the GRAVITY(+) upgrade a nd the NOTT high-contrast visitor instrument. I will finally introduce the ESO Extremely Large Telescope program for first-light instruments\, more specifically our on-going effort in the construction of the METIS instrume nt – the mid-infrared imager and spectrograph for the ELT – and the an ticipated science in the study of planet-forming disks. NOTE: THIS SEMINAR IS PART OF THE AAO ASTRALIS SERIES\, AND SO WILL NOT BE BROADCAST ON THE STANDARD ANU ZOOM LINK. INSTEAD\, IT WILL BE AT https://aao.zoom.us/j/8464 1803247?pwd=cdnmO1qNb6vwKavKEA0KbUjgBaoCfm.1. LAST-MODIFIED:20241202T024606Z LOCATION:ZOOM\, https://aao.zoom.us/j/84641803247?pwd=cdnmO1qNb6vwKavKEA0Kb UjgBaoCfm.1 (host: N/A) \nZoom: https://anu.zoom.us/j/83410388355?pwd=Qm9C MWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Lucas Labadie (University of Cologne) "VLTI/ELT synergies for the s tudy of protoplanetary disks and planet formation" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230905T010000Z DTEND:20230905T023000Z DTSTAMP:20261011T152429Z UID:4c51b9725jlubqhksgh53vn7is@google.com CREATED:20230806T233117Z DESCRIPTION:Hydrogen deficient carbon (HdC) stars are a rare class of super giant variable star with less than 1% hydrogen by mass. They exhibit a wea lth of exotic characteristics such as production of dust\, carbon-rich atm ospheres\, anomalous isotopic ratios\, and very low metallicities. The mos t likely explanation for their formation is via a low-mass white dwarf mer ger\, namely a CO-WD + He-WD merger. In this talk I will present the evide nce that we see for this exotic formation mechanism\, such as the oxygen i sotopic ratio\, our efforts in stellar modelling\, and population synthesi s modelling. I will also provide an overview of their unique characteristi cs and pathways for current work on them\, especially regarding dust produ ction\, variability\, and our current understanding of their kinematics us ing Gaia data. LAST-MODIFIED:20230906T005106Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Francois) \nZoom: https:// anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Courtney Crawford (University of Sydney) "Hydrogen Deficient Carbon Stars - What happens after a white dwarf merger?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161013T000000Z DTEND:20161013T010000Z DTSTAMP:20261011T152429Z UID:a3l3v8oa71r9aeudks1jq9v9ks@google.com CREATED:20160801T041118Z DESCRIPTION:The study of gas kinematics is a fundamental tool to derive the dynamical properties of disk galaxies. In this context\, spectroscopic ob servations of gas emission-lines have been widely used. The derivation of rotation velocity and gas velocity dispersion is however challenging becau se these two quantities become degenerate as the spatial resolution of obs ervations decreases (beam smearing). I will present a new approach to deri ve the kinematics of disk galaxies from emission-line observations. Our me thod works on 3D datacubes rather than on velocity fields\, thus it takes advantage of the full information available in the data and is particularl y powerful in disentangling rotation from velocity dispersion. I will comp are our 3D technique to traditional 2D/1D methods and show some results on disk galaxies both in the local and in the high-z Universe. LAST-MODIFIED:20161003T224607Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Enrico di Teodoro (RSAA) "Kinematics of local and high-z galaxies t hrough 3D modelling of emission-line data-cubes" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170804T040000Z DTEND:20170804T042000Z DTSTAMP:20261011T152430Z UID:3grcvqimakp4shc0898gaoqhvk@google.com CREATED:20170725T000606Z DESCRIPTION:Magnetic fields are known to play a crucial role in the interst ellar medium (ISM) of the Galaxy. Radio polarimetry provides an excellent method of measuring magnetic fields in the ISM. Galactic supershells are s ome of the largest structures in the Galactic ISM\, and should perturb the structure of Galactic magnetic fields. I will present my work determining the structure and strength of magnetic fields associated with a Galactic supershell. This was achieved by modelling the effect of the magnetic fiel ds on polarised radio continuum emission\, and fitted using maximum likeli hood techniques. I will also discuss my recent visit to the Dominion Radio Astrophysical Observatory in Canada\, and present some preliminary result s from the Southern low-frequency Galactic Magneto-Ionic Medium Survey. LAST-MODIFIED:20170725T000606Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alec Thomson (RSAA) "Thesis annual review: Magnetic fields of a Gal actic Supershell" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261110T000000Z DTEND:20261110T010000Z DTSTAMP:20261011T152430Z UID:2tc1g2bjppras5gltmmdl0m3lo@google.com CREATED:20260615T020028Z DESCRIPTION:TBC LAST-MODIFIED:20260716T070024Z LOCATION:Zoom or Duffield Lecture Theatre (host: TBC) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Angel Lopez-Sanchez (Macquarie U.) "TBC" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180814T010000Z DTEND:20180814T020000Z DTSTAMP:20261011T152429Z UID:9oad4d00hlttgdmvsa1ualm2as@google.com CREATED:20180720T014111Z DESCRIPTION:The magnetic universe can be unveiled by measurements of Rotati on Measure (RM) of polarised extragalactic sources in radio wavelengths. S uch RM-grid experiments have allowed studies of magnetic fields in a wide range of astrophysical objects such as Galactic HII regions\, the Milky Wa y\, nearby galaxies like the Magellanic Clouds and M31\, and distant galax ies. As the largest RM catalogue to date with measurements towards 37\,543 sightlines\, the Taylor RM catalogue is a powerful dataset for cosmic mag netism studies. Their RM values were derived from polarisation measurement s at two frequencies only\, hence susceptible to npi-ambiguity. Despite ef forts to minimise this effect\, some sources in the catalogue could still have their RM values deviate from the true values by +- 652.9 rad m-2. In this talk\, I will present our work using new broadband spectro-polarimetr ic observations of 23 npi-ambiguity candidates in the Taylor catalogue wit h the Jansky VLA at L-band (1-2 GHz). We revealed 9 sources suffering from npi-ambiguity. From this\, we estimated the number of sources in the enti re catalogue which may suffer from the same RM ambiguity. Our study furthe r revealed that off-axis polarisation leakage affects the Taylor catalogue \, leading to unpolarised sources mistakenly listed as polarised\, as well as deviations of their RM values from ours even after correcting for the npi-ambiguity. We also exploited the broadband capability of the Jansky VL A to investigate Faraday complexities of our sample\, including preliminar y study of broadband polarisation time variabilities. LAST-MODIFIED:20180730T021109Z LOCATION:Duffield Lecture Theatre (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Yik Ki (Jackie) Ma (MPIfR) "Breaking the Ambiguity -- The Taylor RM Catalogue and the Magnetic Universe" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251112T030000Z DTEND:20251112T040000Z DTSTAMP:20261011T152430Z UID:m67vuhfoteqmqm2kjg3ho2tha8@google.com CREATED:20251109T213106Z DESCRIPTION:We investigate whether a deep learning\, residual neural networ k (Res-Net 2\, developed by Nishizaki et al. (2020)) can accurately predic t the layout of a deformable mirror based on an input PSF. We simulate a 4 f-system\, a deformable mirror and PSF propagation and find that Res-Net 2 is unable to predict the DM to a high standard (despite its passing the i nitial checkerboard test). We predict that this may be attributed to a com bination of not enough information being provided to the algorithm and the similarities between the PSFs being greater than the differences. We find that exaggerating the differences through taking the log of the PSF array increases the prediction accuracy\, potentially opening a new avenue in D M calibration. LAST-MODIFIED:20251109T213106Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Israel Vaughn) \nZoom: htt ps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Yuri Sheinker (RSAA/AITC) "Testing a machine learning algorithm's p recision in predicting DM layout" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160818T010000Z DTEND:20160818T020000Z DTSTAMP:20261011T152429Z UID:2jj53cqum74uf00jhg05s5upjk@google.com CREATED:20160712T030711Z DESCRIPTION:The introduction of visible integral field spectrographs in the last decade led to major developments in the kinematic classification of galaxies. From two-dimensional stellar kinematic measurements\, the SAURON and ATLAS-3D survey suggested that galaxies can be classified as fast and slow rotators. The very different dynamical properties of these groups su ggest that there is more than one formation path for creating early type g alaxies. Recent cosmological hydrodynamical simulations suggest\, however\ , that in order to better understand the assembly and merger history of ga laxies\, the deviations from a Gaussian line of sight velocity distributio n have to be studied. In particular the high order kinematic moments h3 (s kewness) and h4 (kurtosis) of the lines can be used to decode a galaxy's c osmological assembly history. In this talk\, I will assess these result by using stellar kinematic measurements from the SAMI Galaxy Survey. From th e high order moments\, we have developed a new method for kinematically cl assifying galaxies. I will compare our new kinematic classes to other glob al galaxy properties\, and show that this method has real potential for li nking the high order moments to the type of mergers galaxies experienced i n their past. LAST-MODIFIED:20160810T011607Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jesse van de Sande (University of Sydney) "Revisiting galaxy classi fication with SAMI through high-order stellar kinematics" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181106T000000Z DTEND:20181106T002000Z DTSTAMP:20261011T152429Z UID:0q4qv0tahulqb0ui5reacuu4p8@google.com CREATED:20181104T222605Z DESCRIPTION:Star and planet formation are intimately entwined\, and it is d ifficult to consider one without its implications for the other. Here I wi ll discuss the progress of my simulations of the formation of a protostell ar disc and its associated chemical and physical evolution to investigate the implications this has for the earliest stages of planet formation. I u se the magneto-hydrodynamic adaptive mesh refinement code FLASH to simulat e the collapse of a cloud into a star and disc\, and follow the path of ga s throughout the disc using tracer particles to probe the disc environment . The information from the tracer particles can then be compared with what is observed and found in meteoritic data to understand the links between the earliest stages of star and planet formation. LAST-MODIFIED:20181104T222605Z LOCATION:Duffield Lecture Theatre (host: Oh) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Eloise Birchall (RSAA) "PhD Annual Review: Early Evolution in Proto stellar Discs" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240228T000000Z DTEND:20240228T013000Z DTSTAMP:20261011T152429Z UID:o7aaf9s2bm4tv4pusr4g5eink4@google.com CREATED:20240220T233610Z DESCRIPTION:Massive stars within young star clusters underpin galaxy evolut ion physics. Massive stars shape their environments through mechanical fee dback\, ionisation\, and heavy element enrichment of the interstellar medi um (ISM). Yet\, our understanding of these stars' chemical composition\, e specially at low metallicity\, remains uncertain. This limits our ability to quantify how they interact with the ISM and the resulting emission line observables. By quantifying chemical abundance ratios over cosmic time an d integrating them into stellar and photoionisation models self-consistent ly\, we are starting to accurately predict galaxy properties across epochs . In this presentation\, we will merge stellar models with observations of star forming regions\, linking the formation of stars to the global galac tic environment. We will explore significant knowledge gaps\, paving the w ay to quantify energy\, metal\, and matter flows on 10 parsec scales. Addi tionally\, we highlight how JWST observations are addressing the disparity between local and high-redshift realms. We'll end by demonstrating how th is work establishes a foundational framework for future investigations wit h MAVIS\, which will enable detailed characterisations of resolved stellar populations beyond our cosmic neighbourhood. LAST-MODIFIED:20240227T012108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Stu Wyithe) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Katie Grasha (TBC) "Bridging the universe with young star clusters" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200917T010000Z DTEND:20200917T013000Z DTSTAMP:20261011T152429Z UID:gjfer91iubh51jn8olfi1f6dik@google.com CREATED:20200901T052608Z DESCRIPTION:Galactic archaeology is the study of the formation history of t he Milky Way through the motions\, ages\, and chemical composition of star s. The study of Galactic archaeology requires accurately estimating spectr oscopic stellar parameters and abundances (collectively known as labels)\, which is currently limited due to the incompleteness and limited accuracy of atomic line parameters and the spectroscopic analysis methods being sl ow and/or inaccurate. During my PhD\, I will develop tools for advanced sp ectrum synthesis and analysis methods that are both fast and accurate\, an d will furthermore quantify systematic errors. I will apply these tools to two large spectroscopic surveys. In project 1\, I aim to compute syntheti c profiles of the Ca infrared triplet that include chromospheric effects\, which will provide more accurate metallicities\, Ca abundances\, and radi al velocities. In project 2\, I will create a rapid but accurate pipeline that measures stellar labels whilst propagating systematic and observation al errors for the GALAH spectroscopic survey. In project 3\, I will push t he limits on extracting information from spectra with limited resolution a nd wavelength range in the context of the Gaia Radial Velocity Spectrograp h\, which will yield radial velocity estimates for 150 million stars. Comb ined these projects will provide catalogues which will show an unprecedent ed new picture of the chemical evolution of the Milky Way. LAST-MODIFIED:20200907T232608Z LOCATION:ZOOM 997 8534 1005 (host: Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Xi (Ella) Wang (RSAA) "Galactic archaeology through advanced statis tical methods and 3D non-local thermodynamic equilibrium radiative transfe r (thesis proposal talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230419T010000Z DTEND:20230419T020000Z DTSTAMP:20261011T152429Z UID:fki272lfenupo0k3pi3s19ubuo@google.com CREATED:20230417T060606Z DESCRIPTION:With the help of multi-aperture scintillation sensor (MASS) tec hnology applied on small telescopes\, a profile monitoring instrument for atmospheric optical turbulence intensity is developed. It will be deployed at Saishiteng Mountain in China for optical turbulence parameters measure ment in 2022\, where can be candidate site for the Chinese 12-meter Large Optical-infrared Telescope (LOT). The instrument is configured to sample t he turbulence with elevations above 500m with a low-resolution. It is diff erent from the classic MASS developed by Cerro Tololo Inter-American Obser vatory(CTIO)\, we use EMCCD as the spatial filter and the detector instead of concentric annular apertures and photomultipliers. We provide technolo gical particulars of the archetype and describe a parallel comparison test of two MASS systems conducted at Xuyi Observatory in Novermber\, 2021\, s howing the combined observation accuracy of the detection allowed by the M ASS instruments is better than $0.02"$ and the intensity $C_n^2(h)dh$ of a single turbulence layer is better than $10^{-14}m^{1/3}$. In addition\, t he Differential Image Motion Monitor (DIMM) as well as two Lunar Scintilla tion (LuSci) systems were also conducted in this comparison test. The comb ination of DIMM and MASS permits to investigate integral turbulence intens ity in ground layer\, and we offer instances of the measurement results an d compared it to LuSci. LAST-MODIFIED:20230418T075607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBA) \nZoom: https://anu.z oom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Chong Pei (Niaot\, CAS) "Development and comparison experiment of M ASS optical turbulence profiler used for Saishiteng Mountain site testing" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230124T000000Z DTEND:20230124T010000Z DTSTAMP:20261011T152429Z UID:k6rmobvl7ge8ke6budp4c35l0s@google.com CREATED:20230111T001606Z DESCRIPTION:TBD LAST-MODIFIED:20230124T034107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Maddie Mckenzie) \nZoom: h ttps://anu.zoom.us/j/99785341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ethan Crosby (RSAA) "Near-Field Cosmology and the Satellite Galaxy Systems of Nearby L_star Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150728T010000Z DTEND:20150728T020000Z DTSTAMP:20261011T152429Z UID:3b1os55utb4nf79rotcnqt5j7g@google.com CREATED:20150719T122105Z DESCRIPTION:The magnetic history of the Universe is uncharted. Measurements of magnetic fields on scales larger than galaxy clusters are needed to di stinguish between fields generated in the primordial Universe and those ge nerated at later epochs\, with implications for particle physics\, cosmolo gy\, and astrophysics. Yet such measurements remain elusive. In this talk I will review mechanisms for generating magnetic fields across cosmic time \, implications for post-recombination physics\, and current observational constraints on intergalactic magnetic fields. I will describe my efforts to develop a novel statistical probe of the magnetic field power spectrum in cosmic web filaments using Faraday rotation measures. I will introduce CHILES Con Pol\, a forthcoming ultra-deep 1.4 GHz radio survey with the Ka rl G. Jansky Very Large Array. CHILES Con Pol will reach an unprecedented SKA-era rms sensitivity of 400 nJy\, entering new parameter space for stud ies of galaxy evolution and enabling the first robust constraints on the i ntergalactic magnetic field power spectrum. LAST-MODIFIED:20150719T122105Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Christopher Hales (NRAO) "Magnetic Fields in Large Scale Structure" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200707T000000Z DTEND:20200707T010000Z DTSTAMP:20261011T152429Z UID:j0iha1h83242b0tm3im6m25uqo@google.com CREATED:20200706T031105Z DESCRIPTION:Outflows of matter and radiation from galaxies play an importan t role in their evolution\, and that of the circumgalactic environment. Co smic rays and magnetic fields\, as major components of the interstellar me dium\, can strongly influence that interaction - in the right circumstance s. I will describe the plasma physics basis for cosmic ray driven galactic outflows\, some its remarkable consequences and challenges\, and future prospects. LAST-MODIFIED:20200706T031105Z LOCATION:ZOOM 997 8534 1005 (host: Seta) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ellen Zweibel (University of Wisconsin\, Madison) "The Role of Cosm ic Rays in Multiphase Galactic Outflows" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150127T000000Z DTEND:20150127T010000Z DTSTAMP:20261011T152430Z UID:ef6fdv4v2imm9r4ne1pbp3ocag@google.com CREATED:20150115T010104Z DESCRIPTION:An important research area of modern astronomy is to understand the physics of jets from Active Galactic Nuclei (AGN) and their interacti on with the interstellar medium (ISM) or intracluster medium (ICM). My the sis aims to understand the energetics and composition of the jet near its origin\, and its interaction with the ICM\, focusing on detailed models of the inner structure of a spectacular radio source Hydra A. The key featur es of my modelling are that 1) I identify the four bright knots in the no rthern jet of Hydra A as biconical reconfinement shocks\, which result whe n an over-pressured jet starts to come into equilibrium whit the galactic atmosphere 2) The curved morphology of the source and the turbulent transi tion of the jet to a plume are produced by the dynamical interaction of a precessing jet with the ICM. In my thesis\, I provided an innovative theor etical approach to estimate the jet velocity from the information of the i nner jet knots and the oscillation of the jet boundary. I also explored th e complex morphology of the source and the heating of the ambient medium v ia the forward shock using a three dimensional precessing jet-ICM interact ion model. With the 3D models I successfully reproduced key features of th e source\, for example\, i) Four bright knots along the jet trajectory at approximately correct locations\, 2) The curvature of the jet within 10 kp c\, 3) The turbulent transition of the jet to a plume\, and 4) A misaligne d bright knot in the turbulent flaring zone. From my model I determined th at the heating of the atmosphere by the jet would be gentle\, which is con sistent with the assessment of the physics of cooling flow. LAST-MODIFIED:20250925T231030Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mohammad Nawaz (RSAA) "Interaction of Hydra A jets with the Intracl uster medium" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230609T040000Z DTEND:20230609T050000Z DTSTAMP:20261011T152429Z UID:97paio31gthos82u6u2t51km2k@google.com CREATED:20230606T225608Z DESCRIPTION:For Sitian\, which is time-domain survey with the cadence of 30 min and it composed of 17 groups X 3 (u\,g\,i-bands) 1-meter telescopes. Most telescopes will be built in west of China\, the Lenghu site\, and may be some ones will be built in the southern hemisphere\, e.g.\, Chile\, Aus tralia or South African. Thus the telescopes will be a network for the who le sky. Another project EAST is an 8-m telescope proposed by Peking Univer sity. For the telescope\, the mature technology of LAMOST will be applied and the cost is relatively low for the similar aperture telescope. It also will be built in west of China\, the lenghu site\, and it will be the onl y 8-10m telescope in the EAST hemisphere. LAST-MODIFIED:20230606T225608Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hiep) \nZoom: https://anu. zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Zhou Fan (NAOC) "New chances of astronomy in China: the Sitian and EAST projects" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221110T000000Z DTEND:20221110T010000Z DTSTAMP:20261011T152429Z UID:abg7q121g3qbbb5ns69plsbgo0@google.com CREATED:20221026T223110Z DESCRIPTION:Our understanding of dwarf galaxies has evolved from a time—n ot all that long ago—when these systems were thought of as interesting\, but rare and unusual objects of little relevance to larger-scale processe s associated with galaxy formation\, to the modern picture where dwarf gal axies are now viewed as building blocks of significant components of lumin ous modern-day galaxies and as windows to the earliest phases of star and galaxy formation and perhaps keys to helping uncover the nature of dark ma tter. I will provide a very brief survey of this transformation\, focusin g on some of the key characteristics of dwarf galaxies that have brought t hem to the forefront of galactic archeological studies along with stellar streams and high-redshift galaxies. I will outline recent results that my collaborators and I have produced and the instrumentation we have develope d to carry out these studies. And I will describe where we hope to go in t he near future\, suggesting some ambitious longer-term goals for dwarf-gal axy studies. LAST-MODIFIED:20221107T224606Z LOCATION:DLT & ZOOM (host: Neco Kriel) \nZoom: https://anu.zoom.us/j/997853 41005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mario Mateo (University of Michigan) "Dwarf Galaxies over Cosmic (a nd Human) Time" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220908T010000Z DTEND:20220908T020000Z DTSTAMP:20261011T152429Z UID:86do7o7d9qdkrsoie9a8k6oja0@google.com CREATED:20220906T002608Z DESCRIPTION:Over the last decade\, ALMA has opened up our view of the fuel for star formation in distant galaxies\, by probing the emission from cold \, molecular gas and dust. Multiple surveys of dust and CO emission have provided a view of how the total gas content evolves from z~4 to today\, a nd how this relates to the build up of stellar mass in galaxies. However\, zooming in to individual galaxies remains a challenge. How is star-formin g gas distributed relative to the existing stars? And\, what are the physi cal conditions within the gas? In this seminar\, I will provide a short ov erview of the current highest-resolution view of cold gas in galaxies at C osmic Noon and what indicates about the structures of these early galaxies compared to local galaxies. I will also highlight how we are probing the turbulence\, temperature and density of this cold gas\, from galaxies at C osmic Noon to the EoR\, and how some of these conditions may be changing. Throughout the talk\, I will highlight the current challenges and give som e perspective for the next decade of studies of star-forming gas in distan t galaxies. LAST-MODIFIED:20220906T002608Z LOCATION:DLT & ZOOM (host: Neco) \nZoom: https://anu.zoom.us/j/99785341005? pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Melanie Kaasinen (ESO Garching) "Cold Gas in Distant Galaxies\, fro m Cosmic Noon to the EoR" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160218T000000Z DTEND:20160218T010000Z DTSTAMP:20261011T152429Z UID:9sqn36fdnfl0rbp1prbatvvf6c@google.com CREATED:20151018T222616Z DESCRIPTION:The SAMI instrument on the AAT is currently taking integral fie ld spectroscopy of ~3000 nearby galaxies as part of the SAMI Galaxy Survey . This is the largest sample ever across a broad range in both stellar mas s and environment (from field galaxies to groups to clusters). Based on io nised gas and stellar kinematics in the SAMI galaxies\, I will discuss the relationship between dynamical misalignments and the influence of environ ment\, morphology and timescales on the origin of gas in galaxies. The l arge size of SAMI is ideal to test previous findings (e.g. from ATLAS 3D) on a larger sample. The future however lies in much larger samples and Aus tralia will again lead the world with a 100\,000 nearby galaxy survey with Hector. Hector will be the new massively-multiplexed IFU spectrograph on a new 3 degree field top end for the Anglo-Australian Observatory and the next main dark-time instrument for the observatory. I will describe the sc ience and instrument design for Hector and the current status of the proje ct. LAST-MODIFIED:20160210T005108Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Julia Bryant (CAASTRO\, U Syd) "IFU galaxy studies now and then" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150327T032000Z DTEND:20150327T034000Z DTSTAMP:20261011T152430Z UID:56t2jtaekrnos4iip25djddnd4@google.com CREATED:20150119T064120Z DESCRIPTION:There is now strong evidence for stars that have been born with initial helium mass fractions as high as Y=0.40\, such as in the globular cluster Omega Centauri. However\, the evolution\, chemical yields\, and f inal fates of helium-rich stars are poorly understood. In this talk\, I wi ll present results for the evolution and nucleosynthesis of asymptotic gia nt branch models with masses of 3 to 6 Msun at a metallicity of [Fe/H] ~= -1.4 with He-normal and He-rich compositions. I will also discuss the impl ications for chemical evolution and white dwarf remnant formation. LAST-MODIFIED:20150323T062607Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Luke Shingles (RSAA) "Helium-rich stellar and chemical evolution" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150717T040000Z DTEND:20150717T042000Z DTSTAMP:20261011T152429Z UID:j23vklsl3ui561knllonnj3cjk@google.com CREATED:20150623T071610Z DESCRIPTION:TBD LAST-MODIFIED:20150709T092606Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Christopher Owen (RSAA) "Annual Thesis Talk" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240906T040000Z DTEND:20240906T043000Z DTSTAMP:20261011T152429Z UID:eu9mn5ehepaut9dvqm5ckk3534@google.com CREATED:20240801T171118Z DESCRIPTION:Since its establishment\, Mt Stromlo has had policies around bo th the environment and lighting to allow us to do our work and keep the sk ies as relatively dark as possible. While the necessity of this may have s topped or been reduced with the 2003 fires\, in the past 5 years\, Omexom\ , which manages and operates the lighting infrastructure in Canberra\, as well as the ACT Government\, have been aiming to reduce light spill and th e carbon footprint of the city. The ACT lighting network has been slowly u pgraded to both better and more efficient lights (LEDs) as well as power p oles that can be individually controlled and have a custom power/wattage o utput. In a first of its kind experiment\, for the past few months\, we h ave been trialing reducing the overall lighting of Canberra at various lev els\, and measuring the impacts on sky glow\, sky brightness\, as well as the energy and subsequent CO2 emission savings - which add up to Gigawatts worth of energy. We will present the system\, experiment\, and results fr om this as well as where to next - both in Canberra and as a model for oth er cities across the world. Talks from Brad Tucker (RSAA)\, Pete Swanton ( RSAA)\, Danny Bettay (Cybernetics / Omexom)\, Michael Rosetta (Omexom)\, D avid Hua (ACT Government) LAST-MODIFIED:20240801T171118Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Brad Tucker (RSAA) "Lighting Reduction for Canberra - Reducing Ligh t Pollution\, Lower CO2 Emissions\, and Saving Money" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260331T003000Z DTEND:20260331T013000Z DTSTAMP:20261011T152430Z UID:g5avp4cl1vchfb5ptb6maat1eo@google.com CREATED:20260322T230606Z DESCRIPTION:Despite observing more than 6000 planets around other stars\, w e still struggle to understand exactly how planets are formed and why they have the properties they have. The answer lies in protoplanetary discs: t he dusty\, swirling gas discs where planets are born. It is most common to assume that protoplanetary discs have a flat geometry much like a dinner plate. However\, observations over the last few years have revealed that m ore than a third of planet forming discs show warped geometries\, where th e orientation of the disc changes with distance from the central star. IN some spectacular cases these discs may also be torn or broken from the gra vitational interaction with the central stars. In this talk I will explore the origin of warped discs and their consequences for planet formation. I will also introduce our new numerical method\, adaptive particle refineme nt\, a new tool to tackle these very problems. LAST-MODIFIED:20260322T230606Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Arunima) \nZoom: https://a nu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rebecca Nealon (Monash U.) "Planet formation in warped discs" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141111T000000Z DTEND:20141111T010000Z DTSTAMP:20261011T152430Z UID:h4ufqbc2hit7b8q92a41t76k5k@google.com CREATED:20141117T132840Z DESCRIPTION:I will review my biography of Jacobus Cornelius Kapteyn that is about to appear. I started some early work on this while visiting Stromlo four years ago\, after Ken and I completed an Annual Reviews chapter. I w ill focus on Kapteyn's organizational and astronomical work. name=Federico Lelli name=Michele Trenti name=Elisabete da Cunha name=Sajay Mathew LAST-MODIFIED:20250925T231016Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Piet van der Kruit (University of Groningen) "The born investigator of the heavens" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250429T010000Z DTEND:20250429T020000Z DTSTAMP:20261011T152430Z UID:cocab400ba1nll6b9ckjmdsn9c@google.com CREATED:20250106T230127Z DESCRIPTION:Direct imaging of exoplanets and protoplanetary disks at solar- system scales promises unprecedented insights into exoplanet science\, inc luding high-resolution characterization of exoplanet surfaces\, atmosphere s\, and biosignatures. This potential is particularly exciting in light of the upcoming generation of Extremely Large Telescopes (ELTs). However\, a chieving the extraordinary angular resolutions and contrasts necessary for such observations surpasses the limits of conventional technologies. Astr ophotonics -- an emerging field focused on the manipulation and processing of light within integrated circuits and optical fibres -- is poised to re volutionize direct imaging of habitable-zone\, Earth-like exoplanets. This technology offers precise control of light\, enhanced stability\, and cri tically\, the capability to measure previously inaccessible properties of incoming starlight. For instance\, on-chip nulling interferometers enable milli-arcsecond imaging scales by utilizing destructive interference to ef fectively suppress contaminating starlight\, thus readily accessing the ha bitable zones around nearby stars. Additionally\, photonic lanterns (a cen tral focus of this talk) facilitate comprehensive wavefront measurement\, distinguishing genuine planetary signals from atmospheric seeing and speck le noise. By simultaneously capturing amplitude\, phase\, spatial coherenc e\, and spectral information\, these devices integrate adaptive optics wit h advanced image reconstruction techniques\, enabling the recovery of supe r-diffraction-limited images and spectra. In this presentation\, I will di scuss these cutting-edge astrophotonic technologies and instruments\, high light recent advancements\, and explore future developments that will ulti mately allow detailed imaging and high-resolution spectroscopy of habitabl e-zone exoplanets in reflected light. LAST-MODIFIED:20250426T021705Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hajime Ogane) \nZoom: http s://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Barnaby Norris (U. Sydney) "Astrophotonics and a new era of exoplan et imaging" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260528T013000Z DTEND:20260528T023000Z DTSTAMP:20261011T152430Z UID:vbic87gk6r2cq96vah49cf5r9g@google.com CREATED:20260503T114409Z DESCRIPTION:The intergalactic medium (IGM) represents the dominant reservoi r of baryons at high redshift\, traces the architecture of the cosmic web dominated by dark matter\, and fuels on-going galaxy evolution. The IGM ha s been studied using Quasi-Stellar Objects (QSO) absorption lines includin g the Lyman alpha forest (LAF). But because of the low surface brightness and extended\, diffuse distribution\, direct detection of an emission equi valent to the absorption LAF has been challenging. Using KCWI\, we have de tected an emission Lyman α forest (ELAF). The emission forest is highly e xtended\, shows filamentary morphology with filaments connecting galaxies\ , exhibits statistics like the absorption Lyman α forest\, displays spect ra resembling the absorption forest\, and is correlated with galaxy-traced over-densities consistent with bias like dark matter. We conclude that th e ELAF may provide a new tool for tracing a significant fraction of the co smic web of baryons and dark matter. We have also discovered a virial scal ing in the Circum-Galactic Medium of nearby galaxies\, demonstrating a cle ar transition in CGM properties moving from lower mass\, star forming gala xies\, to higher mass galaxies that may be beginning to quench. I will pre sent status of the Stratospheric Cosmic Web Imager (SCWI) program\, a Brin son Exploration Hub balloon experiment\, focused on emission from the Circ um-QSO\, the Circum-Galactic Medium\, and the cosmic web. SCWI offers the opportunity to image the cosmic web in the local universe for the first ti me and compare its properties to those at high redshift. Finally\, I will review the current capabilities and upgrade plans for the W. M. Keck Obser vatory. LAST-MODIFIED:20260527T013421Z LOCATION:Zoom or Duffield Lecture Theatre (host: Mike Ireland) \nZoom: http s://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Chris Martin (Caltech) "Imaging the Cosmic Web with the Keck Cosmic Web Imager" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210909T004500Z DTEND:20210909T013000Z DTSTAMP:20261011T152429Z UID:28q4ns4pqlsktf6cdc986e96mc@google.com CREATED:20210906T054607Z DESCRIPTION:The cosmic star formation rate density is known to have decline d by a factor of ~10 to present day after reaching its peak at z ~ 2. Ther e were drastic differences in the star-forming conditions between z ~ 0 an d z ~ 2\, such that galaxies in the past were more star-forming\, gas-rich \, and had more turbulent interstellar media. Given the complexity of the star formation histories of galaxies\, it is not trivial to pinpoint the e xact physical mechanisms responsible for the decline of the star formation activity from z ~ 2 to z ~ 0. This motivates a further investigation with the Middle Ages Galaxy Properties with Integral Field Spectroscopy (MAGPI ) survey\, to study the spatially resolved star formation activity of gala xies at intermediate redshifts (z ~ 0.3). For this PhD thesis project\, I propose to constrain the physical mechanisms responsible for the quenching of star formation activity at intermediate redshifts with the MAGPI surve y. I will also be looking into connecting the low- and high-z universes wi th MAGPI\, to better understand the full picture of star formation quenchi ng. Moreover\, I will be tying MAGPI observations with cosmological simula tions to not only interpret the results\, but also constrain the theory be hind simulations. LAST-MODIFIED:20210908T221607Z LOCATION:ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jae Yoen (Marcie) Mun (RSAA) "Thesis Proposal Talk: Spatially resol ving the star formation activity of galaxies at 3 - 4 Gyrs of lookback tim e" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261208T040000Z DTEND:20261208T051500Z DTSTAMP:20261011T152430Z UID:kpqat0mbvafml30o7673hlkfc4@google.com CREATED:20260503T114416Z DESCRIPTION:Our monthly Skillshare sessions provide an informal\, supportiv e\, and practical space for students and postdoctoral researchers to devel op and exchange research skills\, professional-development tools\, and eff ective workflows. The format is primarily focused on students. However\, e veryone is very warmly invited to join and contribute.\n\nSessions are hel d on selected Tuesdays from approximately 3:00-4:15ish pm in the CSO Commo n Room. Depending on the topic\, they may include short introductions\, de monstrations\, panel discussions\, interactive exercises\, or open-ended h ands-on activities. LAST-MODIFIED:20260803T020032Z LOCATION:Zoom or CSO Common Room (host: Sven Buder and Melanie Kaasinen) \n Zoom: https://anu.zoom.us/j/89544552112?pwd=Bdoo5fgMVS2Ls6e3Fs0NSNk9OMpaXn .1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:RSAA Skillshare (RSAA) "Research Statements and 1st Fellowship Page s" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181122T000000Z DTEND:20181122T010000Z DTSTAMP:20261011T152429Z UID:6j60usuj21a2t91pk9cjr5uph4@google.com CREATED:20181101T043611Z DESCRIPTION:A fire preparedness information on evacuation procedures\, emer gency contacts\, safe havens etc. All staff are encouraged to attend. LAST-MODIFIED:20181117T102107Z LOCATION:CSO Common Room (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:ANU (ANU) "A fire preparedness talk" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241001T010000Z DTEND:20241001T020000Z DTSTAMP:20261011T152429Z UID:p7u1bphqbc8ccep72vbo65tv38@google.com CREATED:20240415T235646Z DESCRIPTION:The current structure formation model of Lambda Cold Dark Matte r has been successful in explaining many observational results mainly from galaxy redshift surveys. However\, there are still some remaining issues including the missing satellite problem and H_0 tension. I will first disc uss dark galaxies\, composed mostly of dark matter with little or no stars \, which can be important tools for understanding the missing satellite pr oblem. I will then discuss a new redshift survey\, the All-sky Spectroscop ic Survey (A-SPEC)\, which helps to understand the H_0 tension. I emphasis e the power of combining observations from different wavelengths with cosm ological simulations. LAST-MODIFIED:20240915T234113Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hayden Park) \nZoom: https ://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ho Seong Hwang (Seoul National U.) "Dark galaxies and A-SPEC: Missi ng satellite problem and H_0 tension" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171207T000000Z DTEND:20171207T010000Z DTSTAMP:20261011T152429Z UID:h93vtlef2bv29r7vjmf0v08foo@google.com CREATED:20171016T121615Z DESCRIPTION:The presence of dust in galaxies significantly alters their obs erved spectral energy distributions. If not properly accounted for\, this will lead to incorrect estimates for many derived quantities\, such as the star formation rate\, stellar mass\, and photometric redshift. Virtually all studies of star forming galaxies\, both local and distant\, make use t he attenuation curve derived from a small sample of local starburst galaxi es to correct for the effects of dust. However\, it is not clear how reaso nable the general application of this curve is for typical galaxies or as a function of redshift. I will present results from utilizing ~10\,000 loc al (z<0.1) star forming galaxies to derive average dust attenuation curves and to identify the extent to which attenuation curves vary as a function of various galactic properties. LAST-MODIFIED:20171124T091609Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Andrew Battisti (RSAA) "Characterizing Dust Attenuation in Local St ar Forming Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210528T040000Z DTEND:20210528T043000Z DTSTAMP:20261011T152429Z UID:mksbfjp69r2l4rfh6687h0ou3g@google.com CREATED:20210502T230109Z DESCRIPTION:I will discuss my research fellowship at the Museum of Applied Arts & Sciences (MAAS) that explores the role of women in the production o f the Astrographic Catalogue. This practice-based research translates hand -written logbooks of astronomy data into virtual space to create an augmen ted reality artwork where the women's signatures appear in a virtual star chart of the sky they mapped. LAST-MODIFIED:20210519T235107Z LOCATION:DLT and ZOOM (host: Sven Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anna Raupach (ANU\, School of Art and Design) "Light Echoes: digiti sing hand-drawn traces left by women who mapped the Southern Hemisphere fo r the Astrographic Catalogue" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251020T023000Z DTEND:20251020T033000Z DTSTAMP:20261011T152430Z UID:dsqletgq5esn3ctl83lr3m479o@google.com CREATED:20251013T062107Z DESCRIPTION:When does situational or occupational stress become detrimental ? What is the difference between Burnout and Depression? Basics of Burnout is a 1-hour seminar and facilitated discussion that defines the core comp onents of Burnout\, presents evidence-based strategies to treat the sympto ms\, and discusses how to prevent work-related stress. In this seminar\, w e cover the prevalence and impact of burnout in academic and employee popu lations. We provide an overview of the burnout cycle and how to break it\, and we emphasize which factors contribute to burnout and how we can addre ss them in an academic environment. We will provide some tips on how to de al with burnout in oneself and in colleagues. About Sarah: Dr. Sarah Bidd le is a Dragonfly Ambassador and STEM Postdoctoral Fellow at the Center fo r Astrophysics | Harvard & Smithsonian. Sarah is an expert in galaxy evolu tion as well as a passionate mental health speaker and advocate\, presenti ng numerous workshops for early career astronomers. LAST-MODIFIED:20251013T062107Z LOCATION:Duffield Lecture Theatre and ZOOM (host: Melanie Kaasinen) \nZoom: https://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sarah Biddle (Harvard CfA) "Basics of Burnout: Causes and Remedies in a Research Environment" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251209T000000Z DTEND:20251209T010000Z DTSTAMP:20261011T152430Z UID:u820inda23ehpt6jeim81s2ms8@google.com CREATED:20250708T064124Z DESCRIPTION:Spectroscopy is information-rich\, but systematics-dominated. T hat means there's a lot more information to extract if we are careful abou t what we assume. I will demonstrate this with two classes of examples. Th e first example is integral field spectroscopy\, where we typically ignore spatial correlations between sky-adjacent spectra\, which limits what we can measure. Instead\, I will show that joint spectro-spatial fits can rec over true signals that are undetectable in any single spectrum. The second example is in stellar spectroscopy\, where knowingly imperfect models dri ve biases in inferred parameters\, and those models won't substantially im prove in our lifetime. I will describe methods to account for these system atics (including Gaussian Processes) and tractably marginalize over them\, leading to more accurate and precise inferences. LAST-MODIFIED:20251205T034107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Tomasz Rozanski) \nZoom: h ttps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Andrew Casey (Monash) "Flexible forward models for spectroscopy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180622T040000Z DTEND:20180622T050000Z DTSTAMP:20261011T152429Z UID:99qh4622gtj4rdvu7ocodhatb8@google.com CREATED:20180601T023112Z DESCRIPTION:The University is committed to providing a workplace that is he althy\, safe and without risk to the environment. During a recent Universi ty WHS Committee meeting\, a discussion was held surrounding mountain bike riding at Mt Stromlo Forest Park. Whilst participation in recreational ac tivities has shown to lead to many health benefits\, some activities also present a number of hazards to riders health and safety. Even though this activity generally takes place during non-work hours (i.e. during travel t o or from work) all RSAA staff\, students and visitors are invited to part icipate in a collaborative discussion toward the development of a hazard m anagement plan. LAST-MODIFIED:20180601T023113Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Laura Burton (WHS) "Recreational mountain bike riding at Mt Stromlo Forest Park" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230324T030000Z DTEND:20230324T031500Z DTSTAMP:20261011T152430Z UID:n42dr83ij6e2kvoq0j891rnv6s@google.com CREATED:20230217T231110Z DESCRIPTION:ChatGPT\, an AI language model developed by OpenAI\, is capable of writing reports\, abstracts\, code\, and much more. In this presentati on\, I will showcase how ChatGPT can assist you in your daily workflow\, s aving you time and effort - it already saved me the effort of writing this title and abstract. LAST-MODIFIED:20230317T025609Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hiep) \nZoom: https://anu. zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Patrick Armstrong (RSAA) "Streamlining Astronomy Research with Chat GPT" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150508T042000Z DTEND:20150508T044000Z DTSTAMP:20261011T152429Z UID:cga0k29psai87ht65qiflpa84k@google.com CREATED:20150504T025106Z DESCRIPTION:Naomi McClure-Griffiths and Mike Ireland\, visited NAOC and KIA A (part of PKU) in Beijing in April\, as part of an ANU delegation to try and explore collaboration opportunities. The long-term goal of the trip wa s to find ways to attract more joint PhD students. We will provide a brief report on our visit\, and will describe how targeted increased collaborat ion with China has the potential to improve the research competitiveness o f RSAA. LAST-MODIFIED:20150622T074530Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Michael Ireland & Naomi McClure-Griffiths (RSAA) "Report on China v isit" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240227T000000Z DTEND:20240227T013000Z DTSTAMP:20261011T152429Z UID:h84inknao7l0ea13v8plvt72co@google.com CREATED:20231212T003617Z DESCRIPTION:Multiple stellar populations are found in the inner Milky Way\, including some of the most ancient. In this talk I will give an update on the Milky Way's bar\, which dominates the gravitational potential in the Galaxy's central 5 kpc\, and discuss recent work on the structural and dyn amical properties of stellar populations in this region and the constraint s these place on their evolutionary history and origin. LAST-MODIFIED:20240213T082113Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Vanhiep Nguyen) \nZoom: ht tps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ortwin Gerhard (MPE) "Structure and Dynamics of Stellar Populations in the Inner Galaxy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170224T030000Z DTEND:20170224T032000Z DTSTAMP:20261011T152430Z UID:324jh1mc6qjb7no764pofiivuc@google.com CREATED:20170208T232708Z DESCRIPTION:I will present news from the recent Keck Science Steering Commi ttee meeting\, which was held last week in Hawaii. This will include updat es on present and upcoming instrumentation\, repairs to the mirror segment s\, and other miscellaneous items. LAST-MODIFIED:20170222T004106Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dougal Mackey (RSAA) "- Keck Observatory Update -" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250321T030000Z DTEND:20250321T033000Z DTSTAMP:20261011T152429Z UID:dt8a9inh6qd5g4dqtgpdf9b8fk@google.com CREATED:20250312T005108Z DESCRIPTION:Antarctica remains one of the more difficult and fascinating pl aces to visit in the world. It is a unique place with amazing marine anima ls and birdlife. The presentation will consist of images collected durin g the voyage as well as interesting facts that were learned along the way. Photographs of landscapes\, penguins\, seals\, and whales are provided w ith various facts to be feasted upon. LAST-MODIFIED:20250312T005108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Brian Taylor (RSAA) "Antarctica Trip Report with Facts and Photos" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190215T030000Z DTEND:20190215T040000Z DTSTAMP:20261011T152429Z UID:90suoj456b52farvim044e6qvk@google.com CREATED:20190110T003114Z DESCRIPTION:The interstellar medium (ISM) is the heart of the cosmic evolut ion\, where the cosmic baryonic cycle ends with gravitational collapse to form stars and begins again by stellar feedback. Since the two competing p rocesses are tightly coupled with the (thermo)dynamical state of the ISM\, numerical simulations of a complex\, heterogeneous ISM play a key role to advance our understanding in this subject. In this talk\, I will describe recent achievements in modeling the star-forming ISM using a novel numeri cal framework\, called TIGRESS (Three-phase ISM in Galaxies Resolving Evol ution with Star formation and Supernova feedback). In the TIGRESS framewor k\, a part of galactic disks is self-consistently simulated by solving MHD equations with self-gravity and supernova/FUV radiation feedback from mas sive young stars. With the help of realistic simulations\, I will present how we build (1) effective theories for star formation/ISM/feedback and (2 ) synthetic observations to interpret detailed and diverse observations. I will primarily focus on theories for self-regulation of star formation ra tes and multiphase galactic outflows to provide a physical understanding o f observed correlations between star formation rates\, outflow properties\ , and galactic conditions. I will then close by introducing our ongoing pr ojects on multiwavelength synthetic observations\, with a case study for d ust polarization maps. LAST-MODIFIED:20190205T012608Z LOCATION:CSO Common Room (host: Zhang) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Chang-Goo Kim (Princeton) "Introducing TIGRESS: where gravity and f eedback meet the real ISM" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141120T000000Z DTEND:20141120T010000Z DTSTAMP:20261011T152430Z UID:2a0no4mqo1l4phnsdkrjbd1mps@google.com CREATED:20141117T060335Z DESCRIPTION:I will present a new model for seeding black holes in cosmologi cal simulations\, in which gas properties determine where they form. Using this model\, I will show how AGN feedback affects the evolution of massiv e galaxies\, causing them to become less massive\, smaller\, and redder. I n addition\, several observed relationships\, including cosmic star format ion rate density\, galaxy luminosity function\, and [alpha/Fe]-mass\, can only begin to be reproduced when it is included. Finally\, I will show ho w the enrichment history of massive galaxies and the IGM may be influenced by AGN feedback. LAST-MODIFIED:20250925T231019Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Philip Taylor (University of Hertfordshire) "AGN Feedback in Cosmol ogical Simulations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150219T000000Z DTEND:20150219T010000Z DTSTAMP:20261011T152429Z UID:7p3lv1ndqj4fmq2lobngtamtl0@google.com CREATED:20141117T060344Z DESCRIPTION:After being first recognised as a distinct category of Gamma-Ra y Bursts (GRBs)\, the progenitors of short GRBs have remained highly elusi ve although we have long suspected that they are compact binary mergers. E lectromagnetic counterparts of Short GRBs are typically faint and rapidly fade below detection thresholds\, making them notoriously difficult to stu dy. In 2013\, the first "smoking gun" detection was made\, providing stron g evidence that the net is finally closing in on the progenitors of short GRBs. In the coming years\, if there is a joint detection of a short GRB a nd a gravitational wave burst by Advanced LIGO\, this progenitor theory wi ll be confirmed. The compact binary merger progenitor is typically thought to produce a black hole central engine. However\, we have now identified prolonged energy injection in short GRB lightcurves that is inconsistent w ith the expected black hole central engine. In this talk\, I will summaris e the observational constraints on the progenitors of short GRBs and descr ibe an alternative central engine model\, a millisecond magnetar\, that is capable of explaining the prolonged energy injection that we observe. LAST-MODIFIED:20150128T225115Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Antonia Rowlinson (CSIRO) "Constraining the progenitor and central engine of short GRBs" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151209T000000Z DTEND:20151209T010000Z DTSTAMP:20261011T152429Z UID:r5lgddlg8cbv5v43csjq1bha9c@google.com CREATED:20151109T055617Z DESCRIPTION:Recent molecular observations indicate supersonic cloud-cloud c ollision is one of the important modes of O star formation. The O star for mation regions studied so far include super star clusters (Westerlund2\, N GC3603\, RCW38 etc.)\, mini-starbursts (NGC6334\, NGC6357 etc.)\, HII regi ons (M42/43\, M20 etc.)\, and Spitzer bubbles (RCW120 etc.). In this talk I will present some of the recent discoveries of CCC and discuss physics o f the collision-induced turbulent layer. Since the collision time scale is short ~10^5 yrs\, O star formation is a rapid process with a mass accreti on rate higher than 10^-4Mo/yr. LAST-MODIFIED:20151206T234605Z LOCATION:Duffield Lecture Theatre (host: Helga Denes) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Yasuo Fukui (Nagoya University) "O star formation triggered by clou d-cloud collision (CCC)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210316T003000Z DTEND:20210316T010000Z DTSTAMP:20261011T152430Z UID:4huc5urn74dkpj1cvbnc9sb4us@google.com CREATED:20210226T011608Z DESCRIPTION:The Galactic Archaeology with HERMES (GALAH) survey is a large high-resolution spectroscopic survey of the Galaxy\, aiming to unravel the formation and evolution of the Galaxy over time. The abundance of iron\, [Fe/H]\, is an essential stellar parameter for estimating the age the star s. In the third data release of the GALAH survey\, we observe a systematic trend of underestimated [Fe/H] with increasing (true) [Fe/H] for metal-ri ch giant stars. We highly suspect that it is wrong microturbulence velocit ies (Vmic) causing the low [Fe/H]. In this talk\, I will give the details of how we test this hypothesis and discuss how wrong Vmic decreases [Fe/H] in GALAH DR3. LAST-MODIFIED:20210309T071106Z LOCATION:Duffield and ZOOM (host: Sven Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anne Xie (RSAA) "ASC Project: How Wrong Microturbulence Velocity (V mic) Decreases Iron Abundance ([Fe/H]) of Metal Rich Giants in GALAH DR3" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231130T000000Z DTEND:20231130T010000Z DTSTAMP:20261011T152429Z UID:l58sivmkq8u7lqg3v0la4a8if8@google.com CREATED:20231112T225712Z DESCRIPTION:High-resolution near-infrared spectroscopy is one of the key to ols to access the physics of the cool universe. In particular\, the charac terization of exoplanet atmospheres and their molecular constituents has i n recent years demanded the highest fidelity instruments with exquisite se nsitivity in this wavelength regime at high spectral resolution. At the VL T\, CRIRES+ has been long awaited to occupy this parameter range (R=10^5\; 1-5um)\, and has proven to be in highest demand since its first-light alm ost two years ago. CRIRES+ has transformed the CRyogenic InfraRed Echelle Spectrograph into a virtually new instrument with a 10-fold simultaneous s pectral bandwidth\, introducing cross-dispersion and large-area state of t he art Hawaii-2RG mosaics as detector focal plane. The instrument features new capabilities such as spectropolarimetry\, a refurbished SCAO system\, a new and enhanced calibration suite including precision RV references an d Fabry-Perot etalon\, and a metrology system to deliver an exquisite inst rumental stability. n this talk\, I will present the instrument and its ke y performance on sky\, touch on the challenges of its development and inte gration\, describe what it took to deliver it to the telescope and to the community\, and highlight some of the scientific results of its first two years of operation at UT3. LAST-MODIFIED:20231113T131715Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Vanhiep Nguyen) \nZoom: ht tps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ulf Seeman (ESO) "From the lab to the sky: good vibrations with CRI RES+ at the VLT" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160419T010000Z DTEND:20160419T020000Z DTSTAMP:20261011T152430Z UID:pl1i16fhknfveqrjuscqbe0gic@google.com CREATED:20160417T122604Z DESCRIPTION:Recently a powerful paradigm has emerged to understand the natu re of star-forming galaxies. Their star formation rate\, metallicity\, and gas mass are set by a balance between star formation and outflows\, and a ccretion. This model provides a convenient framework to understand galaxy scaling relations and their intrinsic scatter. However\, because of the hi ghly unconstrained strength of galactic winds in low-mass galaxies and the incredibly long depletion times common in dwarfs\, it is unclear if dwarf galaxies also obey this equilibrium\, or if dwarfs are fundamentally diff erent from more massive star-forming galaxies. I will present high-resolut ion simulations of dwarf galaxies with resolved supernovae\, which will re veal why dwarfs have long depletion times in the first place and whether t hey can launch strong enough outflows to be in equilibrium. LAST-MODIFIED:20160418T000605Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:John Forbes (University of California\, Santa Cruz) "Dwarf galaxies : in balance or off-kilter?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260312T000000Z DTEND:20260312T010000Z DTSTAMP:20261011T152430Z UID:gvk3gs2fu9dijahturboupkb78@google.com CREATED:20260210T105614Z DESCRIPTION:The accretion of material onto compact objects powers some of t he most luminous objects in the Universe\, and as a physical process is of ten accompanied by energetic outflows in the form of winds and jets. These outflows represent a vital step in our understanding of cosmic history as they can sculpt the evolution of entire galaxies. Fundamental questions r egarding the physical conditions under which outflows are launched from ac cretion flows\, and their subsequent evolution through a galaxy\, remain u nanswered\, hampered by the long evolutionary timescales of individual act ive galactic nuclei. In the last decade a powerful new method of detecting and studying accretion onto previously quiescent supermassive black holes (SMBHs) has emerged\, through the discovery and follow-up of objects know n as tidal disruption events (TDEs). A TDE is initiated by the destruction of a star scattered close to the central SMBH by tidal forces. In the pro cess of being accreted\, this stellar debris temporarily increases the lum inosity of the SMBH to super-Eddington rates\, which then fades over years -to-decades\, providing the unique opportunity to witness the real-time ev olution of an accretion flow around an SMBH. Accompanying this accretion a re outflows launched at speeds approaching a significant fraction of the s peed of light\, which then produce synchrotron emission observable at radi o frequencies from shocks between these outflows and the ambient gas surro unding the SMBH. In this talk\, I will present an overview of research pro gress to date in the field of TDEs\, discuss the long-standing fundamental questions which TDE observations are addressing\, and look forward to fut ure progress which we can expect as the field matures from the study of si ngle events to large statistically significant samples in the era of the L SST and SKA. I will provide an overview of my work on elucidating the orig ins of radio emission in TDEs\, including contributions to our understandi ng of the scale invariance of accretion-outflow coupling\, the fundamental mechanisms that launch outflows in TDEs\, and how we can use observations of TDE outflows to measure the sub-parsec gas density profiles in quiesce nt galaxies. LAST-MODIFIED:20260308T232108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Adelle Goodwin (Curtin U.) "Tidal disruption events as unique probe s of supermassive black holes\, disk winds\, jets\, and circumnuclear envi ronments (Stromlo Radio Fellow candidate talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221208T000000Z DTEND:20221208T010000Z DTSTAMP:20261011T152429Z UID:4rp5a4n5hhvb7j90svm9220k2g@google.com CREATED:20220926T020220Z DESCRIPTION:Early stars and galaxies emitted sufficient ionizing photons to ionize all of the gas between galaxies. This epoch of reionization establ ished the conditions from which modern-day galaxies emerged\, but very lit tle has been observed about the sources of ionizing photons or how the Uni verse became reionized. Here\, I present recent results that tie together both local galaxies and galaxies within the epoch of reionization to revea l new constraints on the sources of reionization. I will focus on recent d irect observations of galaxies squarely within this time period with the J ames Webb Space Telescope. However\, JWST observations cannot directly con strain the sources of ionizing photons. A large sample of local galaxies k nown to emit ionizing photons\, called the Low-Redshift Lyman Continuum Su rvey\, provides the template to constrain how ionizing photons escape dist ant galaxies. I will present some recent results from this survey that are directly applicable to the high-redshift universe and look forward to upc oming JWST observations that will constrain the sources of cosmic reioniza tion. LAST-MODIFIED:20221205T230307Z LOCATION:DLT & ZOOM (host: Hiep Nguyen) \nZoom: https://anu.zoom.us/j/99785 341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:John Chisholm (UT Austin) "The sources of reionization: new insight s from nearby and far away" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180726T010000Z DTEND:20180726T020000Z DTSTAMP:20261011T152429Z UID:jf4sraej693s0gecqffkqjg9k4@google.com CREATED:20180501T043123Z DESCRIPTION:Most stellar evolution models used today in many aspects of ast ronomy assume those stars are single. This is at odds with our growing und erstanding that most stars are in binary systems close enough the two star s can interact and experience very different evolution to that of single s tars. I will discuss how the Binary Population and Spectral Synthesis (BPA SS) code provides a tool to be able to include these different evolutionar y pathways when studying stellar systems. I will show the importance of ac counting for binary interactions by discussing a few examples. These will include stellar populations in HII regions\, open clusters and globular cl usters as well as the variety of both electromagnetic and gravitational tr ansients. LAST-MODIFIED:20180713T050109Z LOCATION:Duffield Lecture Theatre (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:J.J. Eldridge (The University of Auckland) "Do we really need to wo rry about binary stars?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160721T040000Z DTEND:20160721T050000Z DTSTAMP:20261011T152429Z UID:drjonln5sg2mkg9oniehpk88ss@google.com CREATED:20160718T021605Z DESCRIPTION:A new method for measuring the cosmological parameters governin g the expansion history of the universe is introduced. The method uses the Alcock-Paczynski (AP) test applied to the shape of the galaxy two-point c orrelation function along and across the line-of-sight. The redshift-space distortion (RSD) effects have been the major obstacle for the AP test. We find that the RSD effects on the correlation function are large at a give n redshift but do not vary much as redshift increases\, and that the shape of the correlation function is nearly conserved. If a wrong cosmology is adopted\, the conversion from the observed galaxy redshift to comoving dis tance results in distortion of the shape of the correlation function that varies systematically in redshift. We applied to this method to simulated data and also to the recent SDSS DR12 galaxy survey data to obtain an impr essive constraint on the dark energy equation of state w and matter densit y parameter omega_m. LAST-MODIFIED:20160720T033104Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Changbom Park (Korea Institute for Advanced Study) "Cosmological Co nstraints from the Redshift Dependence of Galaxy Clustering Anisotropy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240328T000000Z DTEND:20240328T010000Z DTSTAMP:20261011T152429Z UID:757hmtkvuc8355f995bh1a5b3c@google.com CREATED:20240325T040608Z DESCRIPTION:The exoplanetary system around beta Pictoris is one of the most iconic and well-studied circumstellar environments to date. It comprises of the first ever directly imaged (debris) disk and two directly imaged su per-Jovian gas giant planets orbiting the host star at ~3 and ~10 au\, com parable to the orbital separations of the gas giants in our own Solar Syst em. Here\, we present the first JWST NIRCam and MIRI observations of the p rominent debris disk\, as well as direct images of the outer exoplanet bet a Pictoris b between 2 and 5 micron. The former reveal hints of a recent c ollision through the presence of an extended secondary disk in thermal emi ssion never seen before. The most conspicuous feature is a trail of materi al\, a "cat's tail" that bends away from the disk. The connection of this new feature with the main disk is co-located with the previously reported CO clump\, which further reinforces the collisional scenario. We present a model of this secondary disk\, sporadically producing dust that broadly r eproduces the morphology\, flux\, and color of the cat's tail and suggests that the secondary disk is comprised largely of porous\, organic\, and re fractory dust grains. The new images of the planet beta Pictoris b provide a view on its atmosphere at wavelengths inaccessible from the ground and agree well with predictions from models assuming a thick and cloudy atmosp here. JWST high-contrast imaging heralds a new era for studying the therma l emission of circumstellar disks and for the characterization of clouds a nd disequilibrium chemistry on fainter planets\, which cannot be detected from the ground at 3-5 micron. In addition to results from JWST\, I was a postdoc at Space Telescope Science Institute during JWST launch\, I’ll a lso describe the process of commissioning the telescope and the key challe nges of instrumentation for such a complex project. LAST-MODIFIED:20240325T040608Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mike Ireland) \nZoom: http s://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jens Kammerer (ESO) "JWST high-contrast imaging of the emblematic b eta Pictoris system: a cat's tail in the disk and clouds in the planet atm osphere" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230209T000000Z DTEND:20230209T010000Z DTSTAMP:20261011T152429Z UID:8doq84fkftqlcdcjlu0egs9pfg@google.com CREATED:20230201T233611Z DESCRIPTION:X-ray binary jets are candidates for cosmic-ray particle accele rators above 10^15 eV. Since shock waves formed inside the jets are consid ered to be the main acceleration region\, the identification of structures associated with shock waves is important to elucidate the physical proper ties of particle acceleration by X-ray binary jets. The microquasar SS433 is one of the most active jets in the system and has attracted attention a s a source of cosmic-ray particle acceleration\, as gamma rays have been d etected on the jet. The presence of a filamentary structure extending in a north-south direction at the terminal region of the SS433 eastern jet is a subject of interest as a cosmic ray particle acceleration source. We per formed spectral and polarimetric analysis using 114-8\,000 MHz data observ ed by VLA and LOFAR\, and verified that the filamentary structure at the j et terminal region may be related to the shock wave. The maximum energy of cosmic rays that can be accelerated by the jet terminal shock was also es timated. These results will be presented in this talk. LAST-MODIFIED:20230205T001608Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Lindsey Oberhelman) \nZoom : https://anu.zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Haruka Sakemi (Kagoshima University) "Cosmic-ray particle accelerat ion at microquasar jet terminal region" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150130T030500Z DTEND:20150130T032500Z DTSTAMP:20261011T152429Z UID:9b5oej9t5cm65g0fu8pnvpkr9c@google.com CREATED:20150119T071206Z DESCRIPTION:I will briefly summarise the methods to estimate the magnetic f ield strengths of different types of neutron stars and the caveats associa ted with them. In this context I will present some recent results we have obtained in finding the limits to the field strengths of accreting millise cond X-ray pulsars from the interaction between the accretion disk and neu tron star magnetosphere. LAST-MODIFIED:20150126T234609Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dipanjan Mukherjee (RSAA) "Measuring magnetic field strengths of ne utron stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150806T010000Z DTEND:20150806T020000Z DTSTAMP:20261011T152429Z UID:jg327niica0cr3ln467j5q8vr0@google.com CREATED:20150625T073614Z DESCRIPTION:The Large Area Telescope (LAT) on board the Fermi gamma-ray spa ce telescope (launched in 2008) has revolutionized the field of gamma-ray astronomy\, producing a plethora of scientific results over a broad range of areas\, from Galactic (e.g. pulsars\, SNRs) to extra-Galactic (e.g. GRB s\, AGN) astronomy. The number of (> 100 MeV) gamma-ray sources has increa sed by over an order of magnitude\, to over 3\,000\, in just the first fou r years of the LAT mission. The origin of >1000 of these sources\, however \, remains a mystery\; these are the so-called unassociated gamma-ray sour ces\, with no known astrophysical counterpart at any other wavelength. Whi le many LAT unassociated sources likely belong to known classes of objects (e.g. pulsars)\, a more exotic origin for some of these sources is also p ossible (e.g. dark matter annihilation). Using the properties of known gam ma-ray sources\, one can train a computer\, via machine learning algorithm s\, to automatically rank and classify unassociated sources\, according to their most likely class. I will present our efforts to apply a number of popular algorithms (e.g. logistic regression\, random forests) to the sour ces in the most recent LAT catalog (3FGL). These results will aid further studies and follow-up observations of LAT unassociated sources. By priorit izing the most promising candidates in certain categories (e.g. pulsars)\, we will optimize the search strategy and reduce the amount of time and ef fort required to identify the nature of these sources. LAST-MODIFIED:20150731T123606Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Pablo Saz Parkinson (University of Hong Kong & UCSC) "Automatic Cla ssification of Fermi Large Area Telescope Gamma-ray Sources using Machine Learning Techniques" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170622T010000Z DTEND:20170622T020000Z DTSTAMP:20261011T152429Z UID:9ti2ionkt2qh820313dtstqfok@google.com CREATED:20170618T235104Z DESCRIPTION:One of the most common features of disk galaxies in the local u niverse is the presence of prominent spiral arms. Despite major developmen ts in the 1960s and decades of studies\, we still don’t know what the ne cessary and sufficient conditions are for spiral arm formation. Current ef forts on the theory of spiral arm formation primarily focus on testing var iations of density wave or swing amplifications on nearby galaxies. Progre ss in this field is slow. Breakthroughs can come from observations of high -redshift galaxies when spiral arms are in the early stage of formation. I n this talk\, I will present some of my first results on integral field sp ectroscopic observations of the most ancient spiral galaxies at z>2\, incl uding gravitationally lensed galaxies. The high-spatial resolution kinemat ic fields imply a population of rare spiral galaxies living in dynamically cold environments at high redshift. I will discuss how ongoing follow-up IFS observations on a larger sample of spiral galaxies at z>2 can help to constrain the earliest onset mechanisms for spiral arms. LAST-MODIFIED:20170618T235104Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tiantian Yuan (RSAA) "Spiral Arm Formation at High Redshift" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260526T013000Z DTEND:20260526T023000Z DTSTAMP:20261011T152430Z UID:dfd32vmg1sqp0vs3atgi35gp10@google.com CREATED:20260503T113616Z DESCRIPTION:Despite considerable progress in global seismology\, mineral ph ysics\, geodynamics\, paleomagnetism\, computational methods and mathemati cal geophysics\, Earth’s core remains enigmatic. Progress in understandi ng the structure and evolution of the Earth's inner core – a metallic ba ll about the size of Pluto – has been impeded by the lack of geometric c overage of seismic body waves due to an uneven global distribution of eart hquakes and receivers. For example\, only recently have we confirmed that its innermost part contains distinct seismic anisotropy. In seeking ways f orward\, we started experimenting with earthquake coda correlation by comp aring digital waveforms recorded at different locations many hours after t he onset of large earthquakes.\n\nApplying the coda correlation principles proved the inner core’s solidity by unambiguously detecting shear waves spreading through it. Furthermore\, we showed the existence of a low-velo city equatorial torus in the outermost outer core. We also showed that a s ingle seismograph and global-scale waveform cross-correlations between sei smic events (inter-source correlation) could be used to scan planetary cor es. Using a growing number of global seismic stations\, we observed up-to- fivefold reverberating waves from selected earthquakes along the Earth’s diameter\, confirming a distinct anisotropy in the innermost inner core. I will review my group’s most important results and ambitions to date\, with brief stops at the Earth’s centre and its various shells\, the Outb ack\, the Southern Ocean bottom\, Antarctica\, the Moon and Mars. As I hop e to demonstrate\, the coda-correlation and similar innovative methods co mbined with further development and the proliferation of seismic sensors w ill play a central role in global and planetary seismology in the coming d ecades. LAST-MODIFIED:20260527T013909Z LOCATION:Zoom or DLT (host: TBD) \nZoom: https://anu.zoom.us/j/82974980739? pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Hrvoje Tkalcic (ANU RSES) "Looking Deep Inside the Earth and Planet s with Coda Correlation Wavefield" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170303T033000Z DTEND:20170303T035000Z DTSTAMP:20261011T152429Z UID:su5sa1kd8tcs4n7u4d6qtkgfr0@google.com CREATED:20170303T032104Z DESCRIPTION:The cosmic dust plays a crucial role in the formation of stella r populations. Extinction curve fitting is a standard method to reveal inf ormation about dust grain sizes and compositions. An analysis is performed over ultra-violet to infrared data of quasars and gamma-ray bursts rangin g from 0.71 6 have been discovered in deepest imaging campaigns with HST\, the redshift and intrinsic faintness of these objects present a challenge for spectroscopy. As such\, relatively little is known about the physical conditions in galaxies at the earliest cosmic times and the limited obser vations we do have pose challenges to current stellar population models. W hile still difficult\, these issues can be circumvented by studying 'extre me' galaxies at lower redshifts (1 < z < 6). I will highlight our recent w ork in this direction from cutting edge facilities such as MUSE on the VLT as well as ultra-deep HST imaging and spectroscopy. In one particular reg ion\, the Hubble Ultra Deep Field\, we have performed the deepest integral field spectroscopic survey with MUSE. With data of up to 30-hour depth\, we have uncovered an abundant population of galaxies with physical propert ies similar to those at the highest redshifts\, including a hitherto invis ible population that represent the faintest and lowest-mass galaxies we ha ve ever discovered at cosmological distances. Detailed studies of these po pulations will shed light onto the galaxy formation process and give us a preview of science in the JWST era. LAST-MODIFIED:20190712T010604Z LOCATION:Duffield Lecture Theatre (host: Oh) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Michael Maseda (Leiden University) "Spectroscopy of Galaxies in the Early Universe: A JWST Sneak Peek" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171103T033000Z DTEND:20171103T035000Z DTSTAMP:20261011T152429Z UID:kkhhop8htfdqirh5jctjclccjs@google.com CREATED:20171011T230108Z DESCRIPTION:1E0102.2-7219 (E0102 for short) is one of the handful of known oxygen-dominated\, young supernova remnants. These systems\, caught only a few 1000 years after the SN explosion of a massive star\, display fast mo ving (a few 1000 km/s)\, oxygen-bright\, hydrogen-poor filaments visible a t optical wavelengths: the outer-layers of the progenitor star\, expelled during the SN explosion\, and (still) expanding ballistically. In this tal k\, I will present recent observations of E0102 with the MUSE optical inte gral field spectrograph at the VLT. I will describe both the original moti vation for these observations — namely the first detection of Sulfur lin es from the fast ejecta with the WiFeS integral field spectrograph - as we ll as the exciting and unanticipated discoveries that were found lurking i n the MUSE datacube. LAST-MODIFIED:20171101T231109Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Frederic Vogt (ESO) "What lies in the shadows … no more! The MUSE view of SNR E0102 in the SMC" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170131T000000Z DTEND:20170131T010000Z DTSTAMP:20261011T152429Z UID:mat4b0j5cn7o2428qot4e621c8@google.com CREATED:20170122T234105Z DESCRIPTION:Star formation is inherently a 'multiscale' process. In this ta lk\, I will present an overview of my thesis research in molecular cloud a nd star formation. In particular\, I will focus on the MHD\, gravitational \, and shock dynamical processes related to structure formation in the ISM \, from clouds to cores. To model each of these processes\, I have used th e numerical code\, AstroBEAR. AstroBEAR is a powerful multiphysics\, adapt ive mesh refinement tool developed at the University of Rochester. It is p ublicly available\, free to download\, and suitable for a wide-range of as trophysical contexts. LAST-MODIFIED:20170128T064105Z LOCATION:Duffield Lecture Theatre (host: Christoph Federrath) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Erica Fogerty (University of Rochester) "From Clouds to Cores: Mode ling Star Formation with AstroBEAR2.0" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161021T030000Z DTEND:20161021T032000Z DTSTAMP:20261011T152430Z UID:oadg0jo98kol3suth6npql0hto@google.com CREATED:20161012T025605Z DESCRIPTION:CSIRO Astronomy and Space Science operates the Australia Telesc ope National Facility (ATNF)\, comprising the 64-m Parkes radio te lescope\, the Australia Telescope Compact Array (ATCA) and the Australian Square Kilometre Array Pathfinder (ASKAP) and\, with the addition of other telescopes\, operates the Long Baseline Array (LBA). CASS also manages astronomy use of NASA's Canberra Deep Space Communication Complex 70-m a nd 34-m antennas at Tidbinbilla. In this talk we will give an update on th e ATNF and discuss its transition into the SKA era. It is clear that we do not have the funding to maintain the full ATNF capabilities across all ou r telescopes. That means we need to look for new funding or roles for the telescopes and make some choices about the available capabilities. We ar e seeking your input into how the ATNF might best serve the community over the coming decade. LAST-MODIFIED:20161019T235104Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Baerbel Koribalski (CSIRO) "Australia Telescope National Facility - Update and Future" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260804T050000Z DTEND:20260804T061500Z DTSTAMP:20261011T152430Z UID:2mmcqbth97p9v0017949k9scpg@google.com CREATED:20260803T010005Z DESCRIPTION:Our monthly Skillshare sessions provide an informal\, supportiv e\, and practical space for students and postdoctoral researchers to devel op and exchange research skills\, professional-development tools\, and eff ective workflows. The format is primarily focused on students\, in particu lar those enrolled in the ASTR8030 course Astronomy and Astrophysics Resea rch Skills. However\, everyone is very warmly invited to join and contribu te.\n\nSessions are held on selected Tuesdays from approximately 3:00-4:30 ish pm in the CSO Common Room. Depending on the topic\, they may include s hort introductions\, demonstrations\, panel discussions\, interactive exer cises\, or open-ended hands-on activities. LAST-MODIFIED:20260803T020005Z LOCATION:Zoom or CSO Common Room (host: Sven Buder and Melanie Kaasinen) \n Zoom: https://anu.zoom.us/j/89544552112?pwd=Bdoo5fgMVS2Ls6e3Fs0NSNk9OMpaXn .1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA Skillshare (RSAA) "The science of scientific writing" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231208T030000Z DTEND:20231208T031500Z DTSTAMP:20261011T152429Z UID:p1voj06sdsimtrsetc6iiitgis@google.com CREATED:20231120T011116Z DESCRIPTION:Last year I gave a FoF talking about methods of celestial navig ation (finding your location on Earth\, especially at sea\, using the sky) . People then asked me if I was going to try it out for real\, so I though t I would -- I bought a nautical sextant and set myself the goal of workin g out the MSO's latitude and longitude using measurements of the Sun. How does it work? How accurately did I locate the observatory? I'll talk about that\, and -- weather permitting -- we can have a live hands-on demonstra tion afterwards. If anyone wants to try it out for themselves afterwards\, you're welcome to drop by my office (CSO 1.32) on sunny days. LAST-MODIFIED:20231120T011116Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBC) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Cameron Van Eck (RSAA) "Finding Myself: a Celestial Navigation Prac tical Exercise" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260731T040000Z DTEND:20260731T043000Z DTSTAMP:20261011T152430Z UID:d474nn119e1e4ndtfnj1fp07q4@google.com CREATED:20260527T013426Z DESCRIPTION:The past decade has seen a number of large surveys of AGB stars in the Solar Neighbourhood\, facilitated by development of new\, faster o bservatories. This has encouraged rapid progress in understanding the phys ics and chemistry of AGB-star outflows. Unlike other surveys\, the Nearby Evolved Stars Survey focuses on obtaining a large\, volume-limited dataset of CO mass-loss rates and sub-mm continuum observations\, to characterise the statistics of AGB stars in the Solar Neighbourhood\, with the ultimat e goal of measuring the total dust and gas return. I will present our obje ctives\, along with a selection of recent results from the survey\, includ ing the statistical relationships between gas- and dust-mass-loss rates\, outflow velocities and stellar variability. Our data show extended envelop es on arcminute scales in both gas and dust for nearby AGB stars\, reveali ng the evolution of mass-loss and dust properties over time. I will put th ese results into perspective\, highlighting their potential to shed light on a range of open questions. NESS is committed to open science and open-s ource analysis of the evolved stellar population in the Solar Neighbourhoo d\, providing both data and code for use by the broader community.\n\nPete r also just recently moved into industry and will also spend a few minutes talking about his experience in transitioning from astronomy to data scie nce in Australia. LAST-MODIFIED:20260729T070007Z LOCATION:Zoom or Duffield Lecture Theatre (host: Melissa Ness) \nZoom: http s://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:2 STATUS:CONFIRMED SUMMARY:Peter Scicluna (U. Hertfordshire) "The Nearby Evolved Stars Survey - a statistical view of local evolved stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141201T030000Z DTEND:20141201T040000Z DTSTAMP:20261011T152430Z UID:qejld1ahn612o2de9b4r8mfkgo@google.com CREATED:20141118T074448Z DESCRIPTION:Stellar models are one of the backbones of modern astronomy. Re cent advances in observational astronomy - through asteroseismology\, prec ision photometry\, high-resolution spectroscopy\, and large-scale surveys - are placing stellar models under greater quantitative scrutiny than ever . The model limitations are being exposed and the next generation of stell ar models is needed as soon as possible. Here we review the evolution and importance of core helium burning stars and then discuss a range of method s\, both theoretical and observational\, that we are using to advance the models. Known observationally as SdB\, red clump\, horizontal branch\, and second clump stars\, core helium burning stars are numerous and relativel y luminous and therefore contribute disproportionately to distant/extragal actic emission. Our best models of these stars are very uncertain\, and po orly constrained by observations. These uncertainties propagate to the lat er phases of stellar evolution\, undermining the accuracy of models of sup ernova explosions and red giants - both vital to the chemical evolution of the Universe. LAST-MODIFIED:20250925T231023Z LOCATION:Duffield Lecture Theatre (host: David Nataf) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Simon Campbell (Monash University) "Towards 21st century stellar mo dels: Star Clusters\, Supercomputing\, and Asteroseismology" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160310T000000Z DTEND:20160310T010000Z DTSTAMP:20261011T152430Z UID:jsrvm44tq5oapf7vcojcbbnee0@google.com CREATED:20160204T045614Z DESCRIPTION:The deferred photometric pipeline of SNLS uses only photometry to detect and classify type Ia supernovae (SNe Ia). The advantages of a ph otometric sample include larger number of events classified as type Ia\, l arger redshift coverage and no need for spectroscopic observations. In thi s seminar I will present improvements on the detection of transient events for this pipeline and SNe classification using photometric redshifts obta ined directly from light curves. First\, a subtracted image stack treatmen t was developed to reduce the number of non SN-like events using morpholog ical component analysis. This technique exploits the morphological diversi ty of objects to be detected to extract the signal of interest. With this method spurious detections were reduced and coordinate resolution was impr oved for the SNLS 3 year sample. Second\, a new classification using photo metric SN redshifts is introduced. This algorithm provides redshifts for a ll events with a better average precision and lower catastrophic errors th an the host galaxy photometric redshift catalogue used in the previous ana lysis. The classification was optimised by machine learning algorithms whi ch provide a sample of SN Ia with estimated high purity. LAST-MODIFIED:20160204T045614Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anais Moller (RSAA) "Detecting and classifying type Ia SNe using on ly photometry" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160719T010000Z DTEND:20160719T020000Z DTSTAMP:20261011T152429Z UID:q4hbtpga0br9d28pu1sp9jgc9g@google.com CREATED:20160516T014116Z DESCRIPTION:In 1990s\, coeval\, co-moving\, and gravitationally unbound ste llar groups were discovered. Classified as “moving groups”\, they hav e contributed on many important studies such as evolution of planetary sys tems and low-mass stars. In spite of their importance\, currently identif ied moving groups have ambiguity which can cause problems in membership an d the related researches. The objective and unbiased analysis of young ne arby stars is required to solve this problem. We will perform 7-dimension al machine-learning based analysis using a large data-set of young nearby stars. Here\, I present a preliminary result. LAST-MODIFIED:20160712T030707Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jinhee Lee (University of Georgia) "Analysis of young nearby moving groups: a preliminary result using machine-learning based method" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210507T040000Z DTEND:20210507T043000Z DTSTAMP:20261011T152430Z UID:s5htnrqt1qbuaao4e33qrgplgk@google.com CREATED:20210422T034607Z DESCRIPTION:We start the weekend with our new open-mic talks. LAST-MODIFIED:20210422T034607Z LOCATION:ZOOM and Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ben Wibking and David Brodrick (RSAA) "Reproducible Research in Ast ronomy and Fun And Games With Radio - Part II" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191106T000000Z DTEND:20191106T010000Z DTSTAMP:20261011T152429Z UID:nbcei7r8g79itlauumas3um84c@google.com CREATED:20190913T023611Z DESCRIPTION:The dynamic infrared sky is hitherto largely unexplored. The in frared is key to understand elusive stellar fates that are opaque\, cold o r dusty. The infrared unveiled the otherwise opaque heavy element nucleosy nthesis in neutron star mergers. I will describe multiple projects to char t the time-domain in the infrared. I will begin with the SPitzer InfraRed Intensive Transients Survey (SPIRITS) --- a systematic search of 194 nearb y galaxies within 30 Mpc\, on timescales ranging between a week to a year\ , to a depth of 20 mag with Spitzer's IRAC camera. SPIRITS has already unc overed over 131 explosive transients and over 2536 strong variables. Of th ese\, 64 infrared transients are especially interesting as they have no op tical counterparts whatsoever even with deep limits from Keck and HST. Int erpretation of these new discoveries may include (i) deeply enshrouded sup ernovae\, (ii) stellar mergers with dusty winds\, (iii) 8--10 solar mass s tars experiencing e-capture induced collapse in their cores\, (iv) the bir th of massive binaries that drive shocks in their molecular cloud\, or (v) formation of stellar mass black holes. Motivated by the treasure trove of SPIRITS discoveries\, we just commissioned Palomar Gattini-IR - a new 25 sq deg J-band camera to robotically chart the dynamic infrared sky. We hav e also begun building WINTER - a new 1 sq deg yJH-band camera on a new 1m telescope at Palomar Observatory. We have proposed DREAMS - a new wide-fie ld infrared telescope at Siding Springs Observatory. LAST-MODIFIED:20191105T083604Z LOCATION:CSO Common Room (host: Travouillon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mansi Kasliwal (Caltech) "The Dynamic Infrared Sky" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190222T030000Z DTEND:20190222T032000Z DTSTAMP:20261011T152430Z UID:6u43i5cbd3rbj0hob5db2pmri8@google.com CREATED:20181203T012614Z DESCRIPTION:Magnetars are young neutron stars with high surface magnetic fi elds\, exceeding around 10 TeraGauss. Pulsed non-thermal quiescent X-ray e mission extending between 10 keV to >150 keV has been observed in about 10 magnetars by RXTE\, INTEGRAL\, Suzaku\, NuSTAR and Fermi-GBM. This talk b riefly describes a model for such hard X-ray signals\, wherein the emissio n is produced by resonant Compton upscattering of soft thermal photons fro m the neutron star surface. Key pulsation and spectral signatures can be u sed to constrain the viewing geometry and the angle between the magnetic a nd spin axes of magnetars. Polarization probes by future Compton telescope s may enable the discernement of whether or not attenuation by magnetic ph oton splitting is active. LAST-MODIFIED:20190211T044607Z LOCATION:CSO Common Room (host: Zerjal) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Matthew Baring (Rice University) "Discerning the Magnetic Inclinati on of Spinning Magnetars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150306T030000Z DTEND:20150306T032000Z DTSTAMP:20261011T152430Z UID:em9u9dbpptqhrkv6amq7c1osrc@google.com CREATED:20150226T121608Z DESCRIPTION:I will present here some of the work that I\, my group and coll aborators have done on understanding the heating and cooling of the neares t L* galaxy to our own\, Andromeda. Its proximity means that we gain a hig h resolution picture of a typical galaxy unobtainable anywhere else except for the Milky Way\, but being external\, we can see the integrated pictur e at the same time\, making comparisons with more distant surveys much eas ier. With observations from the X-ray to radio\, including Hubble and Hers chel observations\, we have a picture of a galaxy not seen anywhere else. LAST-MODIFIED:20150227T053107Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Brent Groves (RSAA) "Heating and Cooling in our Galactic Neighbour\ , Andromeda" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241011T033000Z DTEND:20241011T040000Z DTSTAMP:20261011T152430Z UID:d2iji6vo4vs7trmajv191aiclk@google.com CREATED:20240930T015614Z DESCRIPTION:First in a series of student-led workshop. I'll be providing an overview of the Julia language\, and some hands-on examples on where Juli a is great for astronomical computing\, and where it's overkill. If you wi sh to attend\, please fill out this form: https://forms.gle/VyyUUsBZdtzQuW oP8. To get the most out of this workshop\, you should have a working inst allation of Julia on your device of choice! LAST-MODIFIED:20241002T233612Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Patrick Armstrong (RSAA) "Pat's Julia Workshop - Why I use Julia (a nd why you might not want to)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151009T030000Z DTEND:20151009T034000Z DTSTAMP:20261011T152429Z UID:f9lns0d6alvnbdrs9cdji8v0cc@google.com CREATED:20150929T023607Z DESCRIPTION:I review recent developments in the study of interstellar extin ction\, specifically findings on the wavelength-dependence of the extincti on curve both within the Milky Way and toward nearby galaxies\; And how th ese affect distance determinations to the Galactic centre\, and in the con text of Hubble’s constant\, and toward Type Ia supernovae. Most importan tly\, the mean ratio of extinction in I-band to V-band is ~15% lower than previously believed - this in turn leads to a ~6% increase in the distance modulus toward M101 (the Pinwheel galaxy). For a sample of ~1\,800 Galact ic bulge sightlines\, we find at least two degrees of freedom in the shape of the extinction curve\, rather than one (e.g. R_{V})\, which we confirm with a principal component analysis. We measure a mean ratio of A_{V}/A_{ Ks}~ 13.50\, and find a ~100% systematic offset with additional ~40% scatt er in the reddening estimates from the Planck dust maps. LAST-MODIFIED:20150929T023607Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:David Nataf (RSAA) "Recent Developments in the Study of Interstella r Extinction" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221014T030000Z DTEND:20221014T033000Z DTSTAMP:20261011T152429Z UID:ipjc4oena98uhtq48j0h6pring@google.com CREATED:20220907T001117Z DESCRIPTION:Noelia and David will talk to us about Laser Beam Shaping and T he Geology of Mount Stromlo in this week's fun and interesting Feast-of-Fa cts. LAST-MODIFIED:20221005T052911Z LOCATION:DLT & ZOOM (host: TBD) \nZoom: https://anu.zoom.us/j/99785341005?p wd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Noelia Martinez Rey and David Brodrick (RSAA) "Laser Beam Shaping: the ring everyone wants and The Geology of Mount Stromlo" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240614T023000Z DTEND:20240614T033000Z DTSTAMP:20261011T152429Z UID:naca465jhtjb75soqf02kd0m7s@google.com CREATED:20240521T021618Z DESCRIPTION:In a number of conversations this year with our student and pos tdoc communities we have identified scientific discourse within RSAA\, and sharing our research in an informal environment as missing parts of our s cientific culture. With the aim of addressing this opportunity we are intr oducing a regular Stromlo Science Lunch. The Stromlo Science Lunch will be BYO\, and held in the CSO common room on Fridays at 12.30pm during weeks alternate to the fortnightly BBQ. The format will include brief\, informa l presentations of several recently submitted papers led from RSAA. The id ea is for the informal presentation to be led by the RSAA author followed by questions. There should be no need for additional preparation. In the w eek leading up to the Stromlo Science Lunch I will solicit papers for pres entation. Please feel welcome to volunteer if you have a new result to des cribe. LAST-MODIFIED:20240521T021618Z LOCATION:CSO Common Room (host: Stuart Wyithe) \nZoom: https://anu.zoom.us/ j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Stuart Wyithe (RSAA) "Stromlo Science Lunch" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191031T000000Z DTEND:20191031T010000Z DTSTAMP:20261011T152429Z UID:i60nenpc7g84ku63o7k7ked71c@google.com CREATED:20190806T020617Z DESCRIPTION:The well-known time dilation effect from the Special Theory of Relativity is where the time interval between two events is shorter for a 'moving' observer than for a 'stationary' observer. One explanation of ti me dilation is that there is a physical flow of time which occurs at diffe rent rates for each observer. This explanation is quite common in non-tec hnical accounts of time dilation despite the flow of time not being experi mentally established. In this seminar\, it will be shown how Special Rela tivity provides an interesting result concerning whether this common expla nation can be consistently maintained. LAST-MODIFIED:20191029T091605Z LOCATION:Duffield Lecture Theatre (host: Zhang) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Peter Riggs (RSPE) "Time Dilation and Rates of Flow of Time" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210420T010000Z DTEND:20210420T020000Z DTSTAMP:20261011T152429Z UID:slsdfu50b45bd2dmvvelq30q08@google.com CREATED:20210211T052616Z DESCRIPTION:Abstract: Over the past 10 years\, I have been working on many projects at AAO. This talk will only cover some major works that I have been doing. Firstly\, I will talk about my research activities as an inst rument scientist which covers from the fluid atmospheric dispersion correc tor\, miniature fiber wavefront sensor\, and scatter light analysis etc. Then\, I will discuss some optical design and engineering activities relat ed to multi-object spectrograph and fiber positioning development. LAST-MODIFIED:20210415T073107Z LOCATION:ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jessica Zheng (AAO-Macquarie) "Invited Colloquium: 10+ years at AAO " TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240409T010000Z DTEND:20240409T023000Z DTSTAMP:20261011T152429Z UID:f5g3l8o3t6jr37oelbro4s6p34@google.com CREATED:20231212T120226Z DESCRIPTION:In this talk\, I will review the methods currently investigated to determine the nature of dark matter from cosmological and astrophysica l observations. LAST-MODIFIED:20240404T224608Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Vanhiep Nguyen) \nZoom: ht tps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Celine Boehm (U. Sydney) "How cosmology and astrophysics can help d etermine the dark matter microphysics" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240927T040000Z DTEND:20240927T043000Z DTSTAMP:20261011T152429Z UID:0cirml7dr95scrgfs49mbue1gk@google.com CREATED:20240925T040109Z DESCRIPTION:I'll talk about some of the surprising challenges I've encounte red when teaching undergraduates\, and innovative methods to overcome them . These will include the surprising persistence of misconceptions\, the ba ttle against "plug-and-chug" approaches\, flipped classrooms and AI. LAST-MODIFIED:20240925T040109Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Sven Buder) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Paul Francis (RSAA) "Challenges in teaching undergraduate science" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250224T020000Z DTEND:20250224T030000Z DTSTAMP:20261011T152429Z UID:tud5sllglofv4fv0048tpl6d00@google.com CREATED:20250218T105107Z DESCRIPTION:Nulling interferometry adds high-contrast capability to the hig h-angular resolution of astronomical interferometry. This is critical for studying planet formation at Solar-system scales and habitable zones arou nd nearby\, mature stars at thermal-infrared wavelengths. The Large Binoc ular Telescope Interferometer (LBTI) is so far the most successful and sci entifically productive astronomical nulling interferometer. I will introd uce the study of exozodiacal dust (dust in or near the habitable zone of a star) as a key science application of nulling interferometry. I will the n describe the LBTI’s design and performance and summarize the results o f the HOSTS survey for exozodiacal dust. I will also describe a new nulli ng instrument (NOTT\, PI: D. Defrere) we are developing for the Very Large Telescope Interferometer that will be used to study exozodiacal dust and forming giant planets near the water ice lines of protoplanetary disks. F inally\, I will pivot towards Fizeau (imaging) interferometry and it’s g rowing application with the LBT(I). With this technique we are working to continue LBT’s legacy as a crucial science and instrumentation pathfind er for the future 30-m-class telescopes and\, in fact\, to firmly establis h LBT's status as the first one of them. I will also describe opportuniti es for Australian researchers to get involved in LBT\, either on an indivi dual basis or as a community. LAST-MODIFIED:20250218T105107Z LOCATION:ZOOM only (host: N/A) \nZoom: https://anu.zoom.us/j/83410388355?pw d=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Steve Ertel (U. Arizona) "Studying habitable zones with precision i nterferometry" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260319T000000Z DTEND:20260319T010000Z DTSTAMP:20261011T152430Z UID:ks59gafpmjm3esnpqivt6f711s@google.com CREATED:20260122T000212Z DESCRIPTION:Quasars\, as the most luminous active galactic nuclei\, are cru cial for studying supermassive black holes\, galaxy evolution and cosmolog y. In last two decades\, we carried out three major spectroscopic quasar s urveys in China. The LAMOST quasar survey identified 67\,521 quasars\, and 29\,513 of them are new discoveries. The bright high-redshift survey foun d over 100 quasars at z > 5\, offering a key database for studying the evo lution after the cosmic reionization. The discovery of a quasar with 12-bi llion-solar-mass black hole at z = 6.3\, later confirmed by JWST\, challen ging the theory of black hole growth in the early Universe. We also carrie d out a survey of quasars behind the Galactic Plane\, a rarely explored re gion due to severe Galactic extinction. We selected more than 160\,000 qua sar candidates and identified about 1\,500 quasars behind the Galactic Pla ne. We measured the emission-line properties and black hole masses of all these quasars. In the future\, we will continue the quasar survey with the Chinese Space Station Telescope (CSST)\, expected to be launched in 2027\ , and look forward to further collaborations with Australian astronomers. LAST-MODIFIED:20260308T083110Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Ashley Tan) \nZoom: https: //anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Xue-Bing Wu (KIAA / PKU) "Quasar Surveys in China" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260203T000000Z DTEND:20260203T010000Z DTSTAMP:20261011T152430Z UID:bgr5vlrd224ivomk3ar49qnr4k@google.com CREATED:20251203T021609Z DESCRIPTION:About half the light ever emitted by stars over the history of the universe was absorbed by interstellar dust and re-radiated at long wav elengths. Dust-rich galaxies are the sites of intense starbursts that can rapidly assemble and then cut short the growth of the earliest generations of massive galaxies. I will discuss the ways that two synergistic telesco pes - ALMA in the submillimeter and JWST in the infrared - are changing ou r view of where and how dust is produced in early massive galaxies\, and w hat happens to it after they become quiescent. I will present some recent results that cover different stages of the life cycle of dust in the early universe\, including its production and growth in dust-rich starbursts\, its connection to the ISM in more typical massive galaxies\, and its appar ently rapid destruction as galaxies transition to quiescence. LAST-MODIFIED:20260115T020107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Justin Spilker (Texas A&M) "Cleaning up the dusty universe with JWS T and ALMA" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200123T000000Z DTEND:20200123T010000Z DTSTAMP:20261011T152429Z UID:2jhj7k1jja4u0diai2vhvsfuac@google.com CREATED:20191119T105610Z DESCRIPTION:The James Webb Space Telescope (JWST) will provide a great oppo rtunity to explore high redshift galaxies\, and understand the role of gal axies in the reionization of the Universe. I will present our observationa l plans for the Guaranteed Time Observations of the NIRSpec Instrument Sci ence Team\, including those co-ordinated with the NIRCam Team as part of t he JADES survey. Determining the UV luminosity function to faint magnitude s\, coupled with more accurate determinations of the escape fraction (from observations of the Balmer lines and UV continuum)\, will address the ion izing photon budget from galaxies. The census of the fraction of high reds hift star-forming galaxies with Lyman alpha in emission will constrain the neutral fraction of the IGM at z>6\, and the size of the ionized bubbles\ , and the study of rest-UV absorption lines and nebular emission will shed light on the outflows and the role of the circum-galactic medium. Working at between 1 and 5 microns\, NIRSpec on JWST has the capability to explor e the star formation rates\, metallicities and IGM surroundings of galaxie s within the epoch of reionization. LAST-MODIFIED:20200113T004105Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Andy Bunker (University of Oxford) "Exploring the high redshift Uni verse with the James Webb Space Telescope" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190531T040000Z DTEND:20190531T050000Z DTSTAMP:20261011T152429Z UID:m556a26nuhuaq5a5lbsjlf8eig@google.com CREATED:20190523T064608Z DESCRIPTION:AITC recently received ACT funding to build a new Planewave 0.7 m telescope on mount Stromlo to develop a laser communication system using adaptive optics. Some of the telescope time will be available for other s cientific projects. This presentation is a request for interest to the RSA A astronomy community before finalising the telescope design. If you have any scientific project that may benefit from access to such facility\, com e and join the discussion. LAST-MODIFIED:20190528T022654Z LOCATION:Duffield Lecture Theatre (host: Zhang) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Francis Bennett\, Tony Travouillon and James Webb (AITC) "A new 0.7 m telescope on Mount Stromlo" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171117T030000Z DTEND:20171117T032000Z DTSTAMP:20261011T152429Z UID:impvu3r1hshckgrt7cg4l7nfoc@google.com CREATED:20171106T052610Z DESCRIPTION:Stars form in dense gas. The molecular emission line HCN(1-0) i s thought to be a tracer of dense gas\, with strong emissivity typically o bserved in regions of active star formation. For the past dozen years\, wo rk by the likes of Gao & Solomon (2004)\, Wu et al. (2005\,2010)\, Usero e t al. (2015)\, Bigiel et al. (2015\,2016) and more have gone a long way to wards defining how star formation rates and HCN emission luminosities rela te. The observed correlation offers strong constraints on the efficiency o f star formation in dense gas\, but to make this precise we need to calibr ate the mapping between HCN emission and gas mass and density. In this tal k I will discuss my research with Christoph and Mark on calibrating such a correlation through post-processing of high-resolution simulations of sta r formation in dense gas clouds. Our work confirms existing correlations b etween HCN luminosities and dense gas\; and we present a new empirical rel ationship between HCN emission and star formation rates that calibrates th e observed values to yield physical star formation rates per freefall time . LAST-MODIFIED:20171115T053106Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Adam Onus (ANU) "Calibrating the Relation Between HCN Luminosity an d Star Formation Rate in Molecular Clouds" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151210T000000Z DTEND:20151210T010000Z DTSTAMP:20261011T152429Z UID:31ki9uammor59hsdi8cna69cug@google.com CREATED:20151109T020115Z DESCRIPTION:The most fundamental unsolved problems in galaxy formation revo lve around "feedback" from massive stars and black holes. I'll present new simulations which combine new numerical methods and physics in an attempt to realistically model the diverse physics of the interstellar medium\, s tar formation\, and feedback from stellar radiation pressure\, supernovae\ , stellar winds\, and photo-ionization. These mechanisms lead to 'self-reg ulated' galaxy and star formation\, in which global correlations such as t he Schmidt-Kennicutt law and the global inefficiency of star formation -- the stellar mass function -- emerge naturally. Within galaxies\, feedback regulates the structure of the interstellar medium\, and many observed pro perties of the ISM\, star formation\, and galaxies can be understood as a fundamental consequence of super-sonic turbulence in a rapidly cooling\, s elf-gravitating medium. But feedback also produces galactic super-winds th at can dramatically alter the cosmological evolution of galaxies\, change the nature of dark matter cores and ‘cusps’\, and re-structure the cir cum-galactic and inter-galactic medium. These winds depend non-linearly on multiple feedback mechanisms in a way that explains why they have been so difficult to model in previous "sub-grid" approaches. This resolves long- standing problems in understanding even apparently "simple" galaxy propert ies like the mass-metallicity relation. Finally\, I'll discuss where stell ar feedback fails\, and additional feedback\, perhaps from AGN\, is really needed to explain observations. LAST-MODIFIED:20151206T224605Z LOCATION:Duffield Lecture Theatre (host: Christoph Federrath) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Phil Hopkins (Caltech) "The Diverse Implications of Stellar Feedbac k for Galaxy Formation" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250805T010000Z DTEND:20250805T020000Z DTSTAMP:20261011T152429Z UID:88eaf1e87hfq5jeauneup7dtbg@google.com CREATED:20250520T123617Z DESCRIPTION:Radio supernovae span over 3 orders of magnitude in evolutionar y timescale and 10 orders of magnitude in peak luminosity. This immense pa rameter space reflects the diversity in massive star evolution and the mys terious microphysics of relativistic particle acceleration. The highest lu minosity explosions point to jets launched by powerful central engines and /or extreme mass loss in a star’s final centuries\, while the lowest lum inosity events indicate tenuous winds\, low explosion energies\, and/or th e limits of particle acceleration. In this talk\, I will highlight the lum inosity extremes from both an observational and theoretical point of view. For high-luminosity events\, I will show how we are data mining modern sk y surveys to find statistical samples of luminous\, long-duration explosio ns\, and will discuss the evidence for binary-driven mass loss as their po wer source. For low-luminosity events\, I'll go on a deep dive into SN 118 1\, the least radio-luminous supernova ever observed\, discussing how it a nd similar remnants can help test theories of particle acceleration. I'll conclude with some prospects for next-generation radio facilities\, and so me thoughts on how the diversity in radio supernovae might lead us toward a more nuanced understanding of stars\, shocks\, and their feedback on the surrounding ISM. LAST-MODIFIED:20250725T120606Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Tomasz Rozanski) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dillon Dong (NRAO Socorro) "What can we learn from the vast diversi ty in radio supernovae?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170616T040000Z DTEND:20170616T042000Z DTSTAMP:20261011T152429Z UID:62p78k6oub1qc070c7gds42ifs@google.com CREATED:20170519T061109Z DESCRIPTION:The brightest gamma ray line associated with our Galaxy is prod uced by the annihilation of ~5*10^43 antimatter positrons each second. Nea rly 50 years on from the discovery of this gamma ray line\, the origin of the antimatter responsible for producing it has remained mysterious\, with a variety of astrophysical phenomena - from supernovae to our Galaxy's SM BH - implicated. Any explanation for the origin of this Galactic antimatte r must not only explain the total rate of positron production in the Galax y\, but must also explain the morphology of the gamma ray line and the ove rall positron annihilation spectrum. In this talk I will discuss my work o n positron propagation in Galactic outflows\, and on understanding the ste llar populations that host SN1991bg-like supernovae\, recently shown to be a compelling source of a large fraction of the diffuse antimatter in our Galaxy. I will also introduce PosMC\, a state of the art positron microphy sics simulation\, and the new python package delilah\, designed to streaml ine the study of supernova host galaxies with IFU data. Finally\, I provid e a brief summary of my future work with the Dark Energy Survey\, using ma chine learning techniques to identify peculiar sub-luminous supernovae usi ng only photometric data. LAST-MODIFIED:20170614T012604Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Fiona Panther (RSAA) "Annual Review 2017: Hunting down the origin o f Galactic antimatter" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260217T000000Z DTEND:20260217T010000Z DTSTAMP:20261011T152430Z UID:26s186lerv9acst8jes6jids0g@google.com CREATED:20251203T021612Z DESCRIPTION:The high angular resolution and infrared sensitivity of JWST ar e enabling the detection and investigation of the early stages of star for mation in extragalactic regions. I will review recent results obtained in nearby galaxies by the JWST-FEAST project in terms of tracking the most re cent sites of star formation\, measuring their timescales for feedback\, c onnecting these sites to the underlying molecular reservoirs\, and linking the low-redshift results to the high-redshift findings that are starting to pour in. LAST-MODIFIED:20260206T102108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Katie Grasha) \nZoom: http s://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Daniela Calzetti (U. Massachussetts - Amherst) "The JWST View of St ar Formation\, Feedback and Timescales" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160519T010000Z DTEND:20160519T020000Z DTSTAMP:20261011T152429Z UID:94utm9gqnb3eca2ftgjtrnpbog@google.com CREATED:20151125T042615Z DESCRIPTION:The Milky Way is the galaxy which in principle can be observed the best as it can be resolved into individual stars of which we can measu re their 6D phase space coordinates as well as their chemical abundances. This allows us to disentangle the convoluted formation history of the Gala xy in terms of chemical as well as kinematical evolution. Practical studie s have however been hindered by the fact that the Sun is sitting inside of the Milky Way\; a complete census thus requires all sky surveys. In the p ast decade\, several massive spectroscopic wide-area observing campaigns s uch as the RAVE\, SEGUE\, GALAH and APOGEE surveys have been initiated (an d some of them even completed) providing us for a first time a systematic census of the stellar content of our Galaxy. I will present some of the re sults of these campaigns on the chemo-dynamical evolution of the Milky Way and conclusions we can draw on the formation of galaxies in general. I wi ll provide an outlook on what the Gaia astrometric campaign will be able t o achieve\, in particular when combined with the next generation of spectr oscopic surveys such as WEAVE and 4MOST. LAST-MODIFIED:20160517T002605Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Matthias Steinmetz (Leibniz Institute for Astrophysics Potsdam (AIP )) "Structure and formation of the Milky Way as seen by large spectroscopi c surveys" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170811T040000Z DTEND:20170811T042000Z DTSTAMP:20261011T152430Z UID:7dj1gi451ov2nprqnfkdtlrmpo@google.com CREATED:20170809T061104Z DESCRIPTION:JWST is one of the largest and most challenging science project s ever undertaken. It is approaching launch in late 2018 from French Guian a on an Ariane 5 rocket. The optical telescope assembly with the science i nstruments (OTIS) is currently in a very large vacuum chamber at Johnson S pace Center undergoing cryogenic vacuum testing\, while the spacecraft and the huge sunshield are being tested at Northrop Grumman in Los Angeles. T his Integration and Testing (I&T) phase will dominate activities for the n ext year. I will talk about where we are in the program\, and give some p ersonal insights into what it takes to do such a remarkable mission. This will be informal and I look forward to questions and discussion. LAST-MODIFIED:20170809T075605Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Garth Illingworth (University of California\, Santa Cruz) "A status update on JWST: Bringing one of the most challenging science" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160211T000000Z DTEND:20160211T010000Z DTSTAMP:20261011T152429Z UID:obgs60en8ig15t4dar8v8io7vc@google.com CREATED:20151127T063113Z DESCRIPTION:We addressed strictly line-by-line differential abundance analy sis using high resolution\, high signal-to-noise ratio spectra on field st ars (e.g.\, stellar binaries\, terrestrial planet hosts etc.) and open clu ster stars (e.g.\, the Hyades stars) in order to seek for and test the pos sible chemical signatures of planet formation. Our researches can help to answer a few fundamental questions: how planet formation affect the chemic al compositions of the host stars and whether stellar birth environment af fect the formation of planet. This thesis also has ramifications for Galac tic archeology since we measured the accurate abundance variations in a be nch mark open cluster and arise a crucial challenge to the current view of Galactic archeology. LAST-MODIFIED:20160201T234108Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Fan Liu (RSAA) "Final Thesis Talk - Chemical signatures of planet f ormation in field and open cluster stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150710T040000Z DTEND:20150710T044000Z DTSTAMP:20261011T152429Z UID:0tsdu4ufc009vs5atnmp9m0um0@google.com CREATED:20150706T061104Z DESCRIPTION:The SkyMapper Southern Survey has been underway in earnest sinc e March 2014. This week an initial 'Test Data Release' of nearly 70 sq deg of images and photometric catalogues was announced at the Annual Meeting of the ASA by RSAA’s Chris Onken. These data are freely available to the Australian community in preparation for the release of DR1 later this yea r. In this brief talk Chris W will walk us through the progress of the sur vey and details of the Test Data Release\, while Simon will present a live demonstration of the website and data access methods. If you’ve been wa iting patiently for actual SkyMapper data\, this is the talk for you! LAST-MODIFIED:20150709T092605Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Simon Murphy & Christian Wolf (RSAA) "The SkyMapper Test Data Relea se" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241210T000000Z DTEND:20241210T010000Z DTSTAMP:20261011T152429Z UID:1v4jbtcr1ic0utlald40sqlo0g@google.com CREATED:20241127T224107Z DESCRIPTION:Over the first few million years of their life\, the evolution of young stars is governed by the interaction with their surrounding proto planetary disks. This interaction regulates the exchange of mass and angul ar momentum between the star and the disk\, with a direct influence on the formation and migration dynamics of close-in planets. While observing fac ilities like ALMA have revealed the complex geometries of the outer disk r egions in exquisite detail\, the spatial scales relevant to star-disk inte raction are often too small to be resolved with the same techniques. Howev er\, detailed physical reconstructions of the inner disk dynamics can be a chieved by mapping the characteristic variability signatures of young star -disk systems across the wavelength spectrum. In this talk\, I will provid e an overview of the manifold time domain behaviors that pre-main sequence stars of different mass may exhibit over timescales of hours to years\, a s seen through the eyes of high-precision\, space-borne observatories like Kepler/K2. I will then discuss what these observations can reveal regardi ng the physics of young stars and the interplay between the star\, the dis k\, and any nascent planets. I will also present the Early eVolution Explo rer (EVE)\, a new NASA Small Explorer mission concept that is being develo ped by an international team of researchers between the USA\, Europe\, and Australia to investigate the earliest stages in the co-evolution of young stars and planets. LAST-MODIFIED:20241128T005608Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Laura Venuti (SETI Institute / UNSW) "A time domain view of young s tars and their planet-forming disks on the early pre-main sequence" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241119T000000Z DTEND:20241119T010000Z DTSTAMP:20261011T152429Z UID:rflmp2v2ds19mgi0fmst03v3dk@google.com CREATED:20240815T063638Z DESCRIPTION:Stars between 0.8 to 8Msun are the most common evolved stars in galaxies. In their evolved phases these stars contribute significant gas and dust to galaxies\, and contribute to galactic chemical evolution. The richest nucleosynthesis occurs when the stars are on the AGB\, where eleme nts such as C\, F and elements heavier than iron are produced in their cor es\, and mixed to the stellar surface by convection. Intense mass-loss the n expels this material into the interstellar medium\, leaving the white dw arf remnant. The integrated contribution of low and intermediate-mass star s is usually determined by calculating theoretical stellar models of an en tire population but these calculations are subject to a number of uncertai nties. In particular in recent years it has become apparent that many AGB stars and planetary nebulae are shaped by interaction with a companion. Se cond\, the minimum mass of stars that produce C and heavy elements is stil l very uncertain. This uncertainty is important for chemical evolution sin ce the lowest mass is usually the most numerous. In this talk I discuss re cent efforts to improve our understanding of how low and intermediate-mass stars contribute to galaxies. This includes examining the role of a compa nion on populations of stars\, and using observations to better constrain mass loss\, rotation and convective mixing. LAST-MODIFIED:20240815T063638Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hayden Park) \nZoom: https ://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Amanda Karakas (Monash U.) "Improving stellar models and yields of low and intermediate-mass stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160503T010000Z DTEND:20160503T020000Z DTSTAMP:20261011T152429Z UID:i8bksg4bqq115sn9eseg02s7gg@google.com CREATED:20160210T230618Z DESCRIPTION:Star clusters form in a tumultuous process of gas accretion\, turbulent collapse\, and dispersal\, in which their initial properties\, l ike structure\, density\, and boundedness\, are forged. Into this mix\, n ewborn stars emit energy and momentum in several forms. How does energet ic stellar feedback interfere with the ongoing arrival of new matter? W hat ultimately ends a cluster's formation\, and how does it then impact th e wider interstellar medium? I will approach these questions with physica l arguments and make connections to recent observations of young and adole scent clusters. LAST-MODIFIED:20160503T003104Z LOCATION:Duffield Lecture Theatre (host: Christoph Federrath) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Christopher Matzner (University of Toronto) "Birth tantrums of star clusters" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150227T032000Z DTEND:20150227T033000Z DTSTAMP:20261011T152429Z UID:2tnuo0kdsb2p63jov5nt8q4t3k@google.com CREATED:20150223T003106Z DESCRIPTION:The NGS2 instrument is prototyped in cardboard along with GeMS to determine spatial interactions and aid mechanical design and integratio n planning. LAST-MODIFIED:20150223T005607Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Laila Salam Sezin (AITC Intern) "Cardboard Prototype of an Optical Instrument designed for Gemini Telescope" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180724T010000Z DTEND:20180724T020000Z DTSTAMP:20261011T152429Z UID:k6nbvdf1gjb6m1hq8ebr42jaa0@google.com CREATED:20180701T024607Z DESCRIPTION:Dwarf galaxies are low mass\, low luminosity galaxies that are the building blocks of all galaxies observed today. According to this cosm ological framework\, these systems may have played a crucial role in re-io nizing the universe. However\, star formation is an inefficient process in dwarf galaxies due to their large gas fractions\, low metal content and s hallow potential wells. Studies suggest that dwarfs are systematically def icient in ionizing photons\, a deficit that may be linked to the underprod uction of massive stars and massive star clusters. In my talk\, I will dis cuss my recent work using Hubble Space Telescope observations of clustered sites of star formation in two nearby starburst dwarf galaxies\, NGC 2366 and IC 2574. This work aims to study the H-alpha emission from young (< 1 0 Myrs) star clusters that host short-lived massive stars capable of produ cing ionizing radiation. Further understanding recent massive star formati on in these low star-formation-rate dwarf galaxies will shed light on the universality of the initial mass function (IMF)\, or the initial distribut ion of stellar masses at birth\, across a range of galactic environments. Though the IMF is observed to be largely non-variant throughout local star forming regions\, its invariance at all size scales and environments is w idely debated. Examining the IMF in the low density dwarf galaxy environme nt is worthwhile to investigate how efficiently these galaxies are produci ng massive stars and clusters compared with their more massive spiral coun terparts. LAST-MODIFIED:20180719T133609Z LOCATION:Duffield Lecture Theatre (host: Battisti) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alyssa Sokol (UMASS) "H-alpha Luminous Star Clusters in Nearby Dwar f Galaxies NGC 2366 and IC 2574: Investigating the Universality of the Ste llar Initial Mass Function using SLUG" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170505T040000Z DTEND:20170505T042000Z DTSTAMP:20261011T152430Z UID:klntsuqoh8rfmj7eu5isk3ohgo@google.com CREATED:20170501T063605Z DESCRIPTION:The statistical properties of the Tully-Fisher relation provide important constraints for semi-analytical models and numerical simulation s of galaxy formation and evolution. Over the past decades\, the scatter i n the Tully-Fisher relation has been decreased significantly by accurate p hotometric measures in the NIR bands. However\, the small measurement erro rs on total luminosity can no longer explain the observed scatter. Therefo re\, we abandon the classical concept of the Tully-Fisher relation as a co rrelation using the width of global HI profile and consider instead the in ternal kinematics of gas in galaxies. We implement an improved kinematic m easure by deriving high quality rotation curves\, taking into account warp s and streaming motions in the disk due to spiral arms or a bar. As a resu lt\, our studies show that besides the wavelength dependence\, statistical properties of the Tully-Fisher relation are highly sensitive to the inter nal kinematics of gas. LAST-MODIFIED:20170501T063605Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anastasia Ponomareva (ANU) "How important are resolved rotation cur ves for the Tully-Fisher relation study?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231114T000000Z DTEND:20231114T010000Z DTSTAMP:20261011T152429Z UID:84b0tr1fbvtva3t0q48v96cak4@google.com CREATED:20231031T113109Z DESCRIPTION:The 21-cm signal from neutral hydrogen in the early Universe wi ll provide unprecedented information about the first stars and galaxies. E xtracting this information\, however\, requires accounting for various ast rophysical processes. Semi-analytical models (SAM) are well-suited for thi s purpose. In this talk\, I will give an introduction to the physics of th e Epoch of Reionisation (z ~ 10 - 5) and also the Meraxes SAM. I will then turn to my contributions to Meraxes during my Ph.D. I will conclude with Fisher forecasts on the constraints on the astrophysics (X-ray luminosity\ , UV escape fraction\, star formation rate\, and supernova feedback) of th e nascent population of galaxies that detection of the 21-cm power spectra will enable. LAST-MODIFIED:20231031T113109Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Vanhiep Nguyen) \nZoom: ht tps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Balu Sreedhar (U. Melbourne) "Hydrogen in the first billion years: Simulating the epoch of reionisation" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190813T010000Z DTEND:20190813T020000Z DTSTAMP:20261011T152430Z UID:ljm3jg52bvmagvrhqvfa0uul68@google.com CREATED:20190718T030613Z DESCRIPTION:The nature of the relationship between the ionising processes o f star formation and AGN accretion remains a mystery. In recent years\, in tegral field spectroscopy (IFS) has greatly improved the study of star for mation-AGN mixing within individual galaxies. Initial work in my PhD focus ed on improving upon the recent star formation-AGN mixing methods by intro ducing a theoretical method using photoionisation model grids. We show tha t the systematic effects associated with different models of the ionising stellar spectrum parameters in the model grids are small\, and hence many choices of parameter model is sufficient to use in an H II region model gr id. We demonstrate a new theoretical calculation of the AGN fraction in in tegral field unit (IFU) spaxels using data from the TYPHOON/PrISM survey\, and also show the dependence of the AGN fraction calculation on the spati al resolution of the observations. Finally\, we demonstrate a new three-di mensional diagnostic diagram\, capable of separating the emission from the three ionising sources of star formation\, shocks\, and AGN simultaneousl y. We include comparisons to external data sets to strengthen our results. LAST-MODIFIED:20190805T042106Z LOCATION:Duffield Lecture Theatre (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Joshua D'Agostino (RSAA) "Separation of Line Emission from Star For mation\, Shocks\, and AGN Ionisation in Galaxies (End-of-Thesis Colloquium )" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240510T040000Z DTEND:20240510T050000Z DTSTAMP:20261011T152429Z UID:dira49um7op2ip7oaik5ih0i9o@google.com CREATED:20240505T063608Z DESCRIPTION:N/A LAST-MODIFIED:20240505T063608Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Michael Ireland) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mike Ireland (RSAA) "Coursework school review town hall" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201002T040000Z DTEND:20201002T043000Z DTSTAMP:20261011T152429Z UID:qsm5q80778ucpf5iceek1i6uh8@google.com CREATED:20200826T024112Z DESCRIPTION:The new FoF format is like an Open Mic: Our speakers have 15 mi nutes each to talk about topics of their choice. The idea of the new FoF i s to get to know the many individuals that work under the same roof\, allo w newcomers to find friends easily\, and find new friends or colleagues wi th similar interests and hobbies. So feel free to talk about some of your most favourite adventures\, memorable Stromlo anecdotes\, your hobbies\, y our last COVID-DIY project\, your voluntary activities outside of Stromlo or whatever you are passionate about. Science talks (about a scientific to pic/question that you are interested in) are also welcome\, but be mindful of your audience (astronomers\, students\, engineers\, professional staff ). LAST-MODIFIED:20200928T032108Z LOCATION:ZOOM 997 8534 1005 (host: Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Patrick Armstrong and TBD (RSAA) "The Julia Language - The lovechil d of Python and C" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230811T040000Z DTEND:20230811T044500Z DTSTAMP:20261011T152429Z UID:ttb5uqkklob9s6o67ill3u9c6k@google.com CREATED:20230726T062113Z DESCRIPTION:TBA LAST-MODIFIED:20230726T062113Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBA) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:James Beattie (RSAA) "Unveiling the hidden curriculum: my experienc e and some advice for applying to US postdocs" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241022T000000Z DTEND:20241022T010000Z DTSTAMP:20261011T152429Z UID:utdbrj6mvetkf445mma46ullkg@google.com CREATED:20240815T065137Z DESCRIPTION:I will first present some of the observational and theoretical evidence for the morphological and dynamical transformation of galaxies th rough cosmic time. This transformation is thought to result from the compl ex interplay between the hierarchical merging of dark matter halos and bar yonic processes. I will first show that measuring and contrasting the dyna mical state of galaxies using gas and stars in and beyond the local Univer se is an important test of our understanding of structure formation. I wil l discuss barriers to the accurate measurement of dynamical evolution in g alaxies and suggest possible solutions. In particular\, strategies for mit igating the 'progenitor bias' in observational surveys will be outlined. I will discuss some recent results from the Middle-Ages Galaxy Properties w ith Integral field spectroscopy (MAGPI) Survey\, a VLT/MUSE large programm e designed to replicate the depth and spatial resolution of local integral field spectroscopy surveys at intermediate redshift (z~0.3). MAGPI provid es a 3D snapshot of the dynamical state of both the ionised gas and stars in galaxies at the highest feasible lookback time. LAST-MODIFIED:20240926T235120Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Maya Jablonska) \nZoom: ht tps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Caroline Foster (UNSW) "The dynamical and morphological transformat ion of galaxies through cosmic time" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150814T040000Z DTEND:20150814T042000Z DTSTAMP:20261011T152429Z UID:m95tos7o2ufan8r5656ks4b908@google.com CREATED:20150710T141611Z DESCRIPTION:In my final Feast of Facts at RSAA\, I will summarise the outco mes of our ~3-year program to observe supernovae\, which I have dubbed the ANU+WiFeS SuperNovA Program (AWSNAP). In ~80 nights of observing\, we hav e collected 440 spectra of 232 unique targets\, and have classified 67 sup ernovae. With the aid of a new observing database and database-driven inte rface to the PyWiFeS reduction package\, we have reprocessed the last thre e years of data and will release our spectra publicly later this year. I' ll discuss some science highlights so far\, and try to convince you that s pectroscopy will be a critical element for the now-begun SkyMapper Superno va Survey. LAST-MODIFIED:20150810T020105Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Michael Childress (RSAA) "AWSNAP: The ANU+WiFeS SuperNovA Program" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191122T030000Z DTEND:20191122T033000Z DTSTAMP:20261011T152429Z UID:vglvbs6hvfsral9sso6tdbf50o@google.com CREATED:20191023T002612Z DESCRIPTION:We're all familiar with geostationary satellite antennas – th e Foxtel dishes atop many rooftops that point to a fixed location in space . The AITC has a number of programs\, however\, that rely on our ability to interact with satellites that freely zip across the sky under the influ ence of a plethora of perturbing forces. Understanding these forces is th e first step to being able to predict where any of the 20\,000+ catalogued orbital objects are at any particular instant so we know where – and wh en – to point our telescopes at them. In this talk I’ll outline how s atellites move\, how we find them and the challenges and opportunities the y afford to our communications and space environment research programs. LAST-MODIFIED:20191023T002612Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:James Webb (RSAA/AITC) "AITC Series – Space is big\, satellites a re (comparatively) small… the joys of finding\, tracking\, and using th em!" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170913T010000Z DTEND:20170913T020000Z DTSTAMP:20261011T152429Z UID:i9tsq5c4f91k06o2bq7mj8em4s@google.com CREATED:20170904T102607Z DESCRIPTION:We use a large\, statistically very well characterized X-ray fl ux-limited sample of galaxy clusters to study the large-scale structure of the Universe out to redshifts of ~ 0.4. From the cluster mass function we obtain tight constraints on the matter density and amplitude parameter of the density fluctuation power spectrum. We find some tension in the resul ting amplitude parameter with the prediction from the PLANCK results in th e frame of the standard Lambda-CDM cosmological model. The tension implies a less pronounced fluctuation amplitude of nearby large-scale structure a s compared to the predictions based on Planck and a pure LCDM model. The r esults can be reconciled\, however\, by for example introducing massive ne utrinos. We also use the cluster sample to study the matter distribution i n the local Universe. One of the findings of this study is a locally under dense region in the Southern Galactic Cap\, with interesting consequences for local measurements of cosmological parameters\, like the Hubble consta nt. LAST-MODIFIED:20170912T213606Z LOCATION:Duffield Lecture Theatre (host: Zhang) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Hans Boehringer (MPE) "Cosmology and Cosmography with X-ray Galaxy Clusters" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221209T030000Z DTEND:20221209T033000Z DTSTAMP:20261011T152429Z UID:2t2mf202sa70am8pl5nc8qc8js@google.com CREATED:20221005T053326Z DESCRIPTION:While enormous progresses have been made towards understanding of the cosmic production of low-Z (Z<30) elements\, much less is known abo ut the detailed Galactic evolution and formation sites of elements beyond Fe (Z>30)\, which are formed by captures of neutrons on seed nuclei. This situation is rapidly changing thanks to the recent advent of many massive stellar spectroscopic surveys that are mapping large sample of stars in th e Galaxy with high-quality spectra that allow robust measurement of abunda nces of neutron-capture elements. In this talk\, I will introduce our rece nt work in which we use observed abundances in Galactic populations from G aia-ESO survey to constrain the formation and origins of neutron-capture e lements and their Galactic production cites. LAST-MODIFIED:20221205T230309Z LOCATION:DLT & ZOOM (host: Lindsey Oberhelman) \nZoom: https://anu.zoom.us/ j/99785341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jianhui Lian (MPIA) "Origin and enrichment of neutron-capture eleme nts probed by Gaia-ESO survey" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260210T040000Z DTEND:20260210T053000Z DTSTAMP:20261011T152430Z UID:0466cevq6chllm519ndhro1qmk@google.com CREATED:20251125T233109Z DESCRIPTION:Our monthly skillshare sessions offer a practical\, hands-on sp ace for students and postdocs to exchange research skills\, professional d evelopment tools\, and effective workflows in an informal and supportive s etting. Skillshare is run on the second Tuesday of each month\, 3:00-4:30 ish pm in the CSO Common Room\, with ~15-30 minutes of introduction follow ed by ~30-60 minutes of panel discussions or open-ended hands-on activitie s. LAST-MODIFIED:20260210T225207Z LOCATION:CSO Common Room (in-person only) (host: Sven Buder) \nZoom: https: //anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Monthly Skillshare (RSAA) "Finding Research Questions and Superviso rs" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250701T010000Z DTEND:20250701T020000Z DTSTAMP:20261011T152429Z UID:p6pvckkiptkou6q4l4iec5q0v0@google.com CREATED:20250610T215710Z DESCRIPTION:In this talk\, I present the first set of 3D magnetohydrodynami c (MHD) simulations performed with the Riemann-Geomesh code. We study the dynamics of the magnetically channeled winds of magnetic massive stars in full 3D using a code that is uniquely suited to spherical problems. Specif ically\, we perform isothermal simulations of a smooth wind on a rotating star with a tilted\, initially dipolar field. We compare the mass-loss\, a ngular momentum loss\, and magnetospheric dynamics of a template star (wit h the properties that are reminiscent of the O4 supergiant zeta-Pup) over a range of rotation rates\, magnetic field strengths\, and magnetic tilt a ngles. The simulations are run up to a quasi-steady state\, showing the ep isodic centrifugal breakout events of the mass outflow\, confined by the m agnetic field loops that form the closed magnetosphere of the star. The ca talogued results provide perspective on how angular momentum varies for di fferent configurations of rotation rate\, magnetic field strength and larg e magnetic tilt angles. In agreement with previous 2D MHD studies\, we fin d that high magnetic confinement reduces the overall mass-loss rate\, and higher rotation increases the mass-loss rate. In addition\, we estimate th e angular-momentum evolution\, spin-down time\, and mass-loss evolution of magnetic massive stars for different values of magnetic field strength\, rotation rate\, and dipole tilt. LAST-MODIFIED:20250610T215710Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dinshaw Balsara (University of Notre Dame) "Geodesic Mesh MHD - Mod eling Magnetic Massive Stars in 3D\; Simulations of a Magnetic O Star" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240514T010000Z DTEND:20240514T023000Z DTSTAMP:20261011T152429Z UID:8f46irdg26rpr5id3tp6vovkbs@google.com CREATED:20231212T120230Z DESCRIPTION:The faint\, diffuse\, low surface brightness universe has to-da te generally only been observed in specialised surveys. These surveys have revealed the wealth of information about galaxy evolution available from such low surface brightness observations. Tidal features around galaxies ( faint shells\, tidal tails\, halos and stellar streams) call tell us about their recent merging history and intracluster light (diffuse\, extended s tellar light observed to spread across the centre of galaxy clusters) prov ides a holistic trace of the emerging history in the galaxy cluster enviro nment. The 8.4m Vera C. Rubin Observatory's Legacy Survey of Space and Tim e (LSST) will revolutionise low surface brightness astronomy when it start s in 2025. The deep\, multi-band\, optical observations over the whole sou thern sky will transform our understanding of galaxy evolution\, particula rly by opening up the low surface brightness universe with enormous sample s. I will present my group's research using Hyper-Suprime Cam Subaru Strat egic Project imaging and cosmological hydrodynamical observations to prepa re for tidal feature and intracluster light research into galaxy evolution with LSST. LAST-MODIFIED:20240411T014619Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Maya Jablonska) \nZoom: ht tps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sarah Brough (UNSW) "Galaxy Evolution in a Low Surface Brightness U niverse" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180719T010000Z DTEND:20180719T020000Z DTSTAMP:20261011T152429Z UID:n47bdcdts17mmp98nhcovar28g@google.com CREATED:20180701T023108Z DESCRIPTION:The standard model of cosmology\, the LambdaCDM (LCDM) model\, is based on a shortcut rather than a full application of the Einstein equa tion to the observed Universe. Several cosmologists working towards more r ealistic cosmological models\, within the context of standard general rela tivity (the Einstein equation)\, find that the emergence of negative avera ge spatial curvature over the past 5 to 10 billion years\, as a result of the main epoch of formation of the cosmic web of filaments of galaxies\, c lusters of galaxies\, and voids\, provides a numerically and observational ly realistic dark-energy-free model of the Universe. Separating the LCDM m odel from relativistic-structure-formation models of the Universe will be one of the challenges for 4MOST and other upcoming deep wide galaxy survey s. LAST-MODIFIED:20180701T023108Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Boud Roukema (Torun Centre for Astronomy\, Nicolaus Copernicus Univ ersity) "Hypothesis: dark energy is recent negative average spatial curvat ure" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220407T010000Z DTEND:20220407T020000Z DTSTAMP:20261011T152429Z UID:cecqjacu55a8v3m0hh95lbeit0@google.com CREATED:20220314T000115Z DESCRIPTION:One of the main goals of the Dark Energy Spectroscopic Instrume nt (DESI) is to test Einsteins general theory of relativity by measuring t he growth of structure with redshift-space distortions. Including direct m easurements of galaxy peculiar velocities offer a unique perspective on ma ss and motions in the low redshift Universe\, enabling precision tests of different gravitational models. Using only spare fibres over the lifetime of the DESI survey\, we aim to produce the largest catalogue of peculiar v elocities ever assembled (30 times larger than the 6dFGSv and 2MTF surveys ). This sample will augment constraints on the growth rate of structure fr om the DESI BGS\, reducing the uncertainty by a factor of ~ 2.5 at z < 0.1 compared to the BGS alone. This sample will also enable exquisite tests o f the scale-dependence of the growth rate of structure\, which cannot be a chieved with the BGS alone but is a potential smoking-gun for General Rela tivity\, and provide a legacy sample for correcting the peculiar motions o f transients such as those observed by LIGO. The final phase of Survey Val idation\, the DESI "1%" Survey\, was completed on 13/05/2021. During this phase\, DESI observed 25\,198 galaxies from our FP sample and 4097 galaxie s from our TF sample. This is already 3 times the current largest FP sampl e (6dFGSv) and 2 times the current largest homogeneous TF sample (2MTF). LAST-MODIFIED:20220324T221214Z LOCATION:DLT & ZOOM (host: Stefania) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Khaled Said Soliman (University of Queensland) "The DESI Peculiar V elocity survey" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220315T000000Z DTEND:20220315T010000Z DTSTAMP:20261011T152429Z UID:pnihsp0c581cl8kuhgsqeutr3o@google.com CREATED:20220215T224609Z DESCRIPTION:For most of the subfield's history\, exoplanets have been studi ed without regard to their Galactic context. Gaia has now overturned this state of affairs and enabled for the first time precision studies of exop lanet host stars in the Galactic context. I'll describe how Galactic kine matics can provide precise model-independent relative ages for exoplanet h ost stars and highlight the impacts those relative ages have had on our un derstanding of the origin and fate of short-period planets. LAST-MODIFIED:20220308T131708Z LOCATION:DLT & ZOOM (host: Neco Kriel) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kevin Schlaufman (Johns Hopkins University\, USA) "Invited Colloqui um: Planet Formation and Evolution Revealed by Exoplanet Host Stars in the Galactic Context" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230310T030000Z DTEND:20230310T040000Z DTSTAMP:20261011T152429Z UID:jsr6tedf15hhiuvfdl6t79n75c@google.com CREATED:20230305T084207Z DESCRIPTION:The throne of RSAA Trivia Champ currently lies vacant. In this session of Feast of Facts\, we take direct steps to address this lacunae i n our community by hosting the RSAA Trivia Championship\, All are welcome to put on their thinking caps and push the nerdiest-knee forward. Winners to receive the Ultimate Prize- "the Judgment Free Bragging Rights". LAST-MODIFIED:20230305T084207Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Aditi) \nZoom: https://anu .zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Aditi Vijayan (RSAA) "RSAA Trivia Championship" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240613T010000Z DTEND:20240613T023000Z DTSTAMP:20261011T152429Z UID:9tm4e6mso7msbofns2q6slqt7c@google.com CREATED:20231212T120641Z DESCRIPTION:This talk presents the scientific motivation of the James Webb Space Telescope (JWST)\, technical challenges and solutions\, space orbit\ , observing cadence\, and the infrared focal plane arrays that are the "ey es" of the observatory. Technical performance and scientific images will b e presented. LAST-MODIFIED:20240423T232626Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Tony Travouillon) \nZoom: https://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:James Beletic (Teledyne Imaging Sensor) "The James Webb Space Teles cope: Humanknd's greatest space science facility" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171011T000000Z DTEND:20171011T010000Z DTSTAMP:20261011T152430Z UID:us7653n7vt5k8ak0437o3c8vlo@google.com CREATED:20171010T212104Z DESCRIPTION:Our knowledge of planets other than the eight "classical" Solar System bodies is in its infancy. We are discovering thousands of planets orbiting stars other than our own\, and yet we know little or nothing abo ut their chemistry\, formation and evolution. Planetary science therefore stands at the threshold of a revolution in our knowledge and understandin g of our place in the Universe: just how special are the Earth and our So lar System? It is only by undertaking a comprehensive chemical survey of the exoplanet population that we can hope to answer these critical questio ns. With the arrival of improved or dedicated instruments in the coming de cade\, planetary science will expand beyond the narrow boundaries of our S olar System to encompass our whole Galaxy. LAST-MODIFIED:20171010T212104Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Giovanna Tinetti (UCL) "A chemical survey of exoplanets" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260505T013000Z DTEND:20260505T023000Z DTSTAMP:20261011T152430Z UID:na7m9nra2685h0iumdmrmpqpfk@google.com CREATED:20260503T015257Z DESCRIPTION:Avoided crossings are an ubiquitous physical phenomenon in the dynamics of few-body systems. I illustrate how they emerge in asteroseismo logy --- the analysis and interpretation of normal modes in stars --- and specifically in variable stars possessing stochastically-excited oscillati ons. I describe a one-to-one correspondence between these standing waves a nd hybridised molecular orbitals. Operational predictions for the frequenc ies\, lifetimes\, and visibilities of normal modes emerge from this corres pondence\, and are now increasingly exploited to yield observational disco veries of stellar rotation\, magnetism\, and star-planet interactions. Whe reas stars are usually assumed to be spherically\, or at least azimuthally \, symmetric\, this approach enables us to relax this constraint in the ra dial direction. In particular I report recent uses of it to discover a new class of variable stars: those with insides and outsides that rotate arou nd different axes. I will conclude with some outlines of ongoing investiga tions into differentially oblique pulsations under azimuthally asymmetric magnetic configurations. LAST-MODIFIED:20260505T005005Z LOCATION:Zoom or DLT (host: Maja Jablonska) \nZoom: https://anu.zoom.us/j/8 2974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Joel Ong Jia Mian (U. Sydney) "Asteroseismic Adventures Around Azim uthal Asymmetry" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161129T000000Z DTEND:20161129T010000Z DTSTAMP:20261011T152429Z UID:hu3hep5g9sbq9ff774nm2jm1ig@google.com CREATED:20161121T001106Z DESCRIPTION:In June 2003\, Japanese two universities\, University of Tokyo and Tokyo Institute of Technology successfully launched the world first Cu beSats "XI-IV" and "CUTE-1" using Russian rocket together with 4 other uni versities' CubeSat. That was the icebreaking event as to micro/nano/pico- satellite development activities in Japan and the world. Triggered by the success of XI-IV and CUTE-1\, many universities in Japan started their ow n satellite projects\, mostly for educational objectives\, and 37 Japanese university satellites have been launched till now. University of Tokyo al ready developed 8 satellites\, and 7 of them were launched and operated su ccessfully in orbit. Two CubeSat "XI-IV(2003)" and "XI-V (2005)" were pri marily for space engineering education\, but from the third satellite "PRI SM" we have been challenging towards more practical applications. PRISM a ims to obtain about 30 m resolution Earth remote sensing images\, which wa s actually achieved in 2009. Our fourth satellite "Nano-JASMINE\," which is now waiting for launch\, has "Astrometry" mission to obtain very precis e 3D map of large number of stars in space. From 2010\, I organized natio nwide micro-satellite project named "Hodoyoshi Project\," through which\, three Earth remote sensing satellites "Hodoyoshi-1\,3\,4" were launched in 2014 by Russian Dnepr\, which showed excellent performance of taking Eart h pictures of 6m\, 40m and 240m ground resolutions\, with which we are now seeking practical applications for agriculture\, forestry\, fishery\, dis aster monitoring\, etc. Based on the bus technologies developed in Hodoyo shi Project\, in December 2014\, we launched world first 50kg- class deep space probe "PROCYON\," which escaped from Earth gravitational field and v arious observation and experiment were conducted successfully in deep spac e. Based on the obtained technologies\, we just started development of 6U CubeSat "EQUULEUS" targeting towards Earth Lunar Lagrange Point 2 to be l aunched by NASA's SLS rocket in 2018. In this way\, University of Tokyo ha s been stepping up from education to practical applications of micro/nano/ pico-satellites\, and plans to extend their applications to wider areas. In my talk\, I will show this history\, some technical details and discus s future possibilities of micro/nano/pico-satellites. LAST-MODIFIED:20161123T051105Z LOCATION:Duffield Lecture Theatre (host: Francis Bennet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Shinichi Nakasuka (University of Tokyo) "University Micro/nano/pico -satellites Challenge towards Innovative Space Utilizations and Space Scie nce/Explorations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221207T000000Z DTEND:20221207T010000Z DTSTAMP:20261011T152429Z UID:ust9f51ir6s09999pobplo65bs@google.com CREATED:20220926T020219Z DESCRIPTION:Rest-frame far-ultraviolet (FUV) spectra are fundamental to our understanding of star-forming galaxies\, providing a unique window on mas sive stellar populations\, chemical evolution\, feedback processes\, and r eionization. JWST will soon usher in a new era\, pushing the FUV spectrosc opic frontier beyond z=10. The success of such future endeavors hinges on a comprehensive understanding of the massive star populations and interste llar medium (ISM) gas conditions that power the observed FUV spectral feat ures. I will present the COS Legacy Archive Spectroscopic SurveY (CLASSY) Treasury as a powerful and promising solution. The CLASSY atlas is the fir st high-quality\, high-resolution FUV spectral catalog of star-forming gal axies at z~0. The spectra contain a suite of emission and absorption lines that simultaneously characterize the massive stellar populations that pop ulate metal-poor galaxies\, the physical properties of large-scale outflow s that regulate star formation\, and the chemical abundance patterns of th e gas and stars. The CLASSY sample is consistent with the z∼0 mass-meta llicity relationship\, but is offset to higher star-formation rates by rou ghly 2 dex\, similar to z~2 galaxies. This unique set of properties makes the CLASSY atlas the benchmark training set for studies of star-forming ga laxies across cosmic time. LAST-MODIFIED:20221206T000606Z LOCATION:DLT & ZOOM (host: Aditi Vijayan) \nZoom: https://anu.zoom.us/j/997 85341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Danielle Berg (UT Austin) "Bridging Galaxy Evolution Across Cosmic Time With the CLASSY Survey" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231128T000000Z DTEND:20231128T013000Z DTSTAMP:20261011T152429Z UID:2r1biajh7tjkm0i3mpo7pqhj48@google.com CREATED:20231013T030614Z DESCRIPTION:NASA's Kepler\, TESS\, and Roman missions are providing high pr ecision time-series photometry of millions of stars in the search for tran siting planets. While wildly successful at revolutionising our understandi ng of planetary systems\, these data also provide a unique opportunity to study the evolution of magnetic activity across stellar lifetimes. From st ellar flares to rotation and brightness variations on years-long timescale s\, these missions have transformed our understanding of stellar activity and how it varies with stellar mass\, age\, and composition. In this talk\ , I will present an overview of how these exoplanet-focussed missions have enabled a lagniappe of science results\, improving our understanding of s tellar surfaces\, and some of the opportunities to extend this understandi ng further in the coming years. LAST-MODIFIED:20231113T131713Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ben Montet (UNSW) "What can exoplanet search missions teach us abou t stellar physics?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230314T000000Z DTEND:20230314T010000Z DTSTAMP:20261011T152429Z UID:av7qovsdtdtv0h7g68h72v54t4@google.com CREATED:20230307T230609Z DESCRIPTION:Radio recombination lines (RRLs) are an unobscured tracer of io nized gas in both the diffuse interstellar medium (ISM) as well as high-ma ss star forming regions. The HII Region Discovery Surveys (HRDS) have near ly tripled the number of known high-mass star forming regions in the Milky Way by detecting RRL emission toward infrared-identified HII region candi dates. HII regions are the classic tracer of structure in galaxies\, and t heir physical conditions (e.g.\, metallicity\, internal kinematics) inform models of high-mass star formation and Galactic chemodynamical evolution. I will give a brief overview of our latest Australia Telescope Compact Ar ray HRDS project\, the Southern HII Region Discovery Survey\, highlight tw o serendipitous RRL discoveries and their implications\, and preview some preliminary results with the first Galaxy-wide flux-limited HII region sam ple. In particular\, I will describe two novel techniques -- enabled by ou r now-complete HII region sample -- to constrain the morphological structu re of the Milky Way disk. LAST-MODIFIED:20230307T230609Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hiep) \nZoom: https://anu. zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Trey Wenger (University of Wisconsin-Madison) "Galactic HII Regions and Structure in the Milky Way" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240507T010000Z DTEND:20240507T023000Z DTSTAMP:20261011T152430Z UID:6v97pak7bvdvniqbvjabmt6bao@google.com CREATED:20231212T120229Z DESCRIPTION:One of the most uncertain aspects related to our understanding of the end points of stellar evolution is the link between the progenitor star and the nature of the supernova explosion that the progenitor will un dergo. Even though hundreds of supernovae are discovered each year by opti cal surveys\, these sources are usually too distant to resolve the ejecta and immediate surrounding of the exploded star. However\, due to their lon g lifetimes and close proximity\, supernova remnants which are the long li ved structures that result from the supernova explosion of either a white dwarf or a massive star\, provide us with a unique opportunity to study su pernova explosion and dynamics up close and in detail. In this talk\, I wi ll highlight some recent advances that have been made in the understanding of supernovae and their progenitors using multi-wavelength studies of sup ernovae and their remnants. LAST-MODIFIED:20240421T234611Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Trey Yang) \nZoom: https:/ /anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Katie Auchettl (U. Melbourne) "The imprint of their explosions: Usi ng supernova and their remnants to understand stellar death" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200403T030000Z DTEND:20200403T040000Z DTSTAMP:20261011T152430Z UID:v2b6m2gfk7uu62fv930ivf49b8@google.com CREATED:20200325T042605Z DESCRIPTION:Climate change is\, quite rightly\, becoming a key concern for many people. However\, reducing greenhouse gas emissions is only one aspec t of sustainable living. An area where we have almost complete control is what we do with our rubbish. In this talk I will introduce the many proble ms associated with our attitude towards waste\, explain why recycling isn' t all it's cracked up to be (but you should still do it)\, and present a p lethora of tips for reducing the amount of waste you send to landfill. LAST-MODIFIED:20200331T001605Z LOCATION:ZOOM (details below) (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Phil Taylor (ANU) "Towards A Zero Waste Life" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260219T000000Z DTEND:20260219T010000Z DTSTAMP:20261011T152430Z UID:3i61mgqlvngpf02rhr595abpi4@google.com CREATED:20260113T011108Z DESCRIPTION:Present-day disk galaxies\, including the Milky Way\, consist o f an older thick disk and a younger thin disk. How those structures formed and evolved over cosmic time has remained an open question\, but signific ant advances recently came from JWST\, ALMA observations\, and numerical s imulations. Thanks to JWST's sharp vision and IR sensitivity\, we identify thin and thick disk structures out to 10 Gyr ago and find a tight mass-si ze-height relation. By observing galaxies directly at earlier epochs\, we find that galaxies first host thick disks by 10 Gyr ago\, and later form t hin disks within the thick disks. This structural transition proceeds in a downsizing manner: more massive galaxies form thin disks earlier. The for mation time of the Milky Way thin disk aligns with the transition epoch ob served in its progenitors. We show that the turbulence-regulated disk form ation naturally explains the delayed formation of thin disks in low-mass g alaxies. By extending our observations to earlier times with larger sample s up to 12 Gyr\, we find that today's thick disk formed from initially a t hin\, dynamically hot disk\, which subsequently thickened adiabatically du e to internal dynamics with enhanced gas fraction or external perturbation s. ALMA observations and simulations indicate that gas physics play a cent ral role in this process. I will further discuss the MW galaxy formation i n the broader context of galaxy formation. LAST-MODIFIED:20260219T010607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hiep Nguyen) \nZoom: https ://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Takafumi Tsukui (Kavli IPMU / U. Tokyo) "ALMA and JWST insights int o the thin- and thick- disk formation" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190411T010000Z DTEND:20190411T020000Z DTSTAMP:20261011T152430Z UID:kpmf5bjon5ngfjb8dgv1nefe8o@google.com CREATED:20190110T233622Z DESCRIPTION:Most galaxies consist of a dispersion-dominated bulge region an d a regularly rotating disk. These components have built up their mass sep arately through different processes\, yet are evolving together. It has be come commonplace to separate the light from bulge and disk regions to bett er understand their formation and contribution to their host galaxy. The s ame techniques can also be applied to IFS data of other galaxy components\ , such as bars and spiral arms. I will detail some of the latest results f rom the MaNGA galaxy survey\, including efforts to study stellar populatio ns in lenticular galaxies within bulge and disk regions\, and an investiga tion into the influence of bars on the secular evolution of disk galaxies. LAST-MODIFIED:20190401T234107Z LOCATION:CSO Common Room (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Amelia Fraser-McKelvie (University of Nottingham) "The complicated lives of disk galaxies: lessons from IFS" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180413T040000Z DTEND:20180413T042000Z DTSTAMP:20261011T152429Z UID:u3fpmv9nl9po8sqrfvelr5s9p4@google.com CREATED:20180324T121108Z DESCRIPTION:For my PhD\, I propose a project on the formation and evolution of young giant exoplanets. By directly imaging gas giants as they form\, we want to learn more about the formation mechanism itself as well as how young planets interact with the circumstellar disk. Using novel detection techniques such as kernel-phase or sparse aperture masking behind an integ ral field unit on the world's largest telescopes\, we want to explore regi ons closer to the PSF than ever before. Our observations aim on solar syst em scales (5 - 20 au) in the nearest star forming regions where young anal ogues of our own gas giant planets like Jupiter and Saturn should reside. LAST-MODIFIED:20180413T004110Z LOCATION:Duffield Lecture Theatre (host: Panther) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jens Kammerer (RSAA) "Fourier Plane Imaging of Young Giant Exoplane ts (Thesis Proposal)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221104T030000Z DTEND:20221104T033000Z DTSTAMP:20261011T152429Z UID:eomth233uvk6mbg59nrbaa5v90@google.com CREATED:20221103T025107Z DESCRIPTION:Small-scale fluctuating magnetic fields of order nG to muG are observed in supernova shocks and galaxy clusters\, where amplifications of the field are likely caused by the Biermann battery mechanism induced thr ough curved shock vorticity. However\, these fields cannot be amplified fu rther without the presence of the turbulent dynamo mechanism\, which gener ates large-scale magnetic energy through the stretching and compression of magnetic flux lines. Thus\,  we present here novel three-dimensional mag netohydrodynamic (MHD) simulations of a laser-driven shock propagating int o a stratified\, multiphase medium\, with a small-scale seed magnetic fiel d\, to investigate the post-shock turbulent magnetic field amplification v ia the fluctuating dynamo. The test configuration used here is currently b eing tested in the shock tunnel facility at the National Ignition Facility (NIF). In order to probe the statistical properties of the post-shock tur bulent region\, we use tracer trajectories to track its evolution through the Lagrangian framework\, thus providing a high-fidelity analysis of the shocked medium. Our simulations indicate that the growth of the magnetic f ield\, which accompanies the near-Saffman power-law kinetic energy decay i n the absence of turbulence driving\, exhibits fundamentally different cha racteristics as compared to periodic box simulations. Seemingly no distinc t phases exist in its evolution.  Yet\, the growth rates are still consis tent with those expected for compressive driving in subsonic\, compressibl e turbulence. Phenomenological understanding of the dynamics of the magnet ic and velocity fields are also elucidated via second-order Lagrangian fre quency spectrums\, which yield the expected inertial range scalings in the Lagrangian bridge relations. LAST-MODIFIED:20221103T025107Z LOCATION:DLT & ZOOM (host: Neco Kriel) \nZoom: https://anu.zoom.us/j/997853 41005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Justin Kin Jun Hew (RSAA) "Lagrangian statistics of a shock-driven turbulent dynamo in decaying turbulence" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190430T010000Z DTEND:20190430T020000Z DTSTAMP:20261011T152429Z UID:kteqc8h17ni3t660v3m4cfl8u4@google.com CREATED:20190311T232617Z DESCRIPTION:The University of Tokyo Atacama Observatory (TAO) Project is to construct and operate a 6.5m infrared telescope at the summit of Co. Chaj nantor (altitude 5640m) in northern Chile by UTokyo. Thanks to the dry cli mate and the high altitude\, excellent observation condition in the NIR to MIR wavelengths is verified with a pathfinder 1-m telescope miniTAO. The 6.5m telescope has two Nasmyth foci where two facility instruments\, SWIMS for the near-infrared and MIMIZUKU for the mid- infrared\, will be instal led and two folded- Cassegrain foci for carry-in instruments. I will give project overview and the curren status of TAO project\, as well as key sci ence topics. LAST-MODIFIED:20190426T030105Z LOCATION:Duffield Lecture Theatre (host: Zerjal) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mamoru Doi (University of Tokyo) "The University of Tokyo Atacama O bservatory" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240418T010000Z DTEND:20240418T020000Z DTSTAMP:20261011T152429Z UID:bt9r2gc6g7a882gv5d0no0bo2k@google.com CREATED:20240415T053107Z DESCRIPTION:Low-dimensional representations of high-dimensional data can re veal underlying structures and patterns that are not apparent in the origi nal space. By projecting the data to a low-dimensional space\, we construc t a more compact and informative representation\, making it easier to visu alize and interpret the data. There are many ways to obtain low-dimensiona l representations\, ranging from calculating simple summary statistics to constructing latent representations using sophisticated dimensionality red uction methods. In this talk\, I will demonstrate the power of low-dimensi onal representations in the analysis of close binary light curves\, focusi ng on a) the detection of the Darwin instability in the light curves of co ntact binary stars\, and b) the separability of the light curves of contac t binary stars\, semidetached binary stars\, and dark companion binary sys tems\, which host electromagnetically silent black holes or neutron stars. LAST-MODIFIED:20240415T053107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Yuan-Sen Ting) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Milan Pesta (Charles University) "Utilizing Low-Dimensional Represe ntations in the Analysis of Close Binary Light Curves" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170816T010000Z DTEND:20170816T020000Z DTSTAMP:20261011T152429Z UID:jt17qee2ijkdrknbvk2i7fnupo@google.com CREATED:20170810T041105Z DESCRIPTION:The race to be the first ELT on the sky is on. Alone in the Nor th\, the Thirty Meter Telescope is pushing through its design and construc tion effort with components being built in all of its 5 member countries. We will review the progresses made for all of its major components: Optics \, Structure\, Controls\, AO\, Instrumentation and take some bets on its e ventual site: Mauna Kea or La Palma. LAST-MODIFIED:20170810T041105Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tony Travouillon (TMT) "An update on the construction of the Thirty Meter Telescope" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180522T010000Z DTEND:20180522T020000Z DTSTAMP:20261011T152429Z UID:87ej0fagsoksqq35rgahhmukn0@google.com CREATED:20180322T061118Z DESCRIPTION:The physical conditions in the narrow-line regions (NLRs) of ac tive galactic nuclei (AGN) may be constrained by comparing spectroscopic o bservations with photoionisation models. The key parameters are the gas-ph ase abundances\, the ionisation parameter\, the gas pressure\, and the sha pe of the ionising spectrum. The first part of this thesis presents a mode l of the ionising continuum radiation in Seyfert AGN. This model OXAF pres erves the physically-motivated shapes of existing theoretical models while simplifying them to a three-parameter form designed for photoionisation m odelling. The second part of the thesis is the presentation of the full da ta release of the Siding Spring Southern Seyfert Spectroscopic Snapshot Su rvey (S7). Three-dimensional data cubes\, two-dimensional emission-line fi ts\, and other products are provided to the astronomical community\, along with a large number of maps of gas kinematics across the S7 sample. In th e third part of the thesis\, a Bayesian code is presented that compares ph otoionisation model grids with observed emission line fluxes. This code Ne bulaBayes is agnostic to model parameters\, dimensionality\, and the chose n emission lines. Grids of MAPPINGS photoionisation models are calculated and used with NebulaBayes to infer physical parameters in two dimensions a cross four 'pure Seyfert' galaxies selected from the S7 sample. The result s are the first robust two-dimensional measurements of gas-phase metallici ty in Seyfert NLRs\, and show steep metallicity gradients into extraplanar ionisation cones in the case of edge-on galaxy NGC 2992\, and an inverse metallicity gradient in the galaxy ESO 138-G01. The near-constant ionisati on parameters suggest that radiation pressure regulates the density struct ure of NLRs on multi-kiloparsec scales. The ionising radiation is measured to be harder in ionisation cones than elsewhere\, but the results are sen sitive to spectral contamination. The fourth part of this thesis addresses mixing of NLR emission with emission from HII-regions in star-forming gal axies. A 'mixing' grid (combining HII and NLR model grids) is coupled with a statistically powerful sample from the Sloan Digital Sky Survey (SDSS) to constrain the HII-AGN 'mixing fractions' using NebulaBayes. It is found that for the majority of Seyfert-classified SDSS spectra\, the majority o f the Balmer emission arises in HII regions as opposed to NLRs. The final results presented in the thesis are the first systematic and robust measur ements of the gas-phase metallicities of active galaxies in the SDSS. The metallicities associated with Seyfert-classified emission are shown to be consistently high and the SDSS AGN follow the upper locus of the SDSS stel lar mass-metallicity relation. LAST-MODIFIED:20180520T024607Z LOCATION:Duffield Lecture Theatre (host: Panther) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Adam Thomas (RSAA) "End-of-thesis talk: The ionising radiation and gas-phase metallicity in the narrow-line regions of Seyfert galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260316T000000Z DTEND:20260316T010000Z DTSTAMP:20261011T152430Z UID:4nqssedunopnauv60k0i3k5bms@google.com CREATED:20260313T041606Z DESCRIPTION:Magnetised plasma permeates dark matter halos across the Univer se\, from the circumgalactic medium of individual galaxies to galaxy group s\, clusters\, and the surrounding cosmic web. Yet despite its ubiquity\, we lack a coherent observational framework for how magnetic fields shape a nd regulate baryon transport -- governing how gas accretes\, mixes\, redis tributes\, and survives transit across the hierarchy of structure. Recent advances in broadband radio polarimetry and dense rotation measure (RM) gr ids now enable a transition from isolated detections to statistical plasma diagnostics across halo mass and environment. In this talk\, I will focus on the galaxy group regime -- the scale at which cosmic web accretion\, h alo gas redistribution\, and feedback processes intersect most consequenti ally -- and present three complementary radio polarisation experiments tha t probe: (i) magnetised mixing at radio lobe-halo interfaces\, (ii) magnet ised structure beyond thermodynamic detection limits in group and cluster outskirts\, and (iii) the statistical emergence of trans-virial magnetised structure across group populations. Together\, these results illustrate h ow magnetised plasma can be used as a tracer of baryon transport across sc ales and establish the foundations of a coordinated program to map the geo metry\, scaling laws\, and dynamical influence of magnetised baryons acros s the full halo mass spectrum. I will highlight the first results from thi s program and outline how this framework can be realised and expanded at R SAA through survey-scale analysis\, theoretical integration\, and targeted follow-up -- positioning RSAA to lead into the SKA era of magnetised plas ma astrophysics. LAST-MODIFIED:20260315T233607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Stu Wyithe) \nZoom: https: //anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Craig Anderson (RSAA) "Tracing the Magnetised Baryon Cascade Across Halo Mass (Stromlo Radio Fellow candidate talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251106T220000Z DTEND:20251107T013000Z DTSTAMP:20261011T152430Z UID:vi79u5e0t87t9qepq1r33eudo8@google.com CREATED:20250924T003115Z DESCRIPTION:Honours and masters end-of-thesis talks LAST-MODIFIED:20250924T003115Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Chris Wolf) \nZoom: https: //anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Honours and masters students (RSAA) "Honours and masters end-of-the sis talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180207T000000Z DTEND:20180207T010000Z DTSTAMP:20261011T152429Z UID:gq0p9jqt78qh3mf69c5qhldqj4@google.com CREATED:20180128T111609Z DESCRIPTION:The polarized synchrotron emission of the Milky Way cosmic ray electrons propagates to us through a magneto-ionic medium that causes Fara day rotation. The emission process has been understood since the 1950s\, b ut the astrophysics of the propagation of the polarized radiation has only recently become clear. With our gradual awakening to the concept of the F araday spectrum over the last decade\, we could design sky surveys that fo r the first time are sensitive to the full range of rotation measure of th e polarized emission. The Global Magneto-Ionic Medium Survey (GMIMS) is a combination of such polarization surveys using different telescopes at dif ferent wavelengths. Now the results of two GMIMS surveys are available\, f rom Parkes and the Dominion Radio Astrophysical Observatory (DRAO). In thi s talk I will explain the Faraday spectrum\, show images of the sky that a re sensitive to the full range of rotation measures for the first time\, a nd then show how we can determine the distance to the emission regions. T he polarization horizon is an analog to optical depth in an ordinary spect rum\, that sets the limit for how far we can see. LAST-MODIFIED:20180205T061605Z LOCATION:Duffield Lecture Theatre (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:John Dickey (University of Tasmania) "GMIMS: Steps to the Polarizat ion Horizon" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250530T040000Z DTEND:20250530T043000Z DTSTAMP:20261011T152430Z UID:lgpt07t925pp89j1gh74hlpni4@google.com CREATED:20250518T235610Z DESCRIPTION:This month of May I had the experience of observing at the AAT with KOALA. For the first time in my career\, I used an instrument I had n ot built/worked on before. And now I get it: I know how astronomers might feel when using our instruments! LAST-MODIFIED:20250518T235610Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Noelia Martinez Rey (RSAA) "My experience as AO scientist observing at the AAT with an instrument I have not built" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230606T010000Z DTEND:20230606T020000Z DTSTAMP:20261011T152429Z UID:n1ij79m602ru8imqm9h9vco4t0@google.com CREATED:20230521T073609Z DESCRIPTION:The LIFE initiative has the goal to develop the science\, the t echnology and a roadmap for an ambitious mid-infrared nulling interferomet er space mission. Such a mission will allow humankind to detect and charac terize the atmospheres of hundreds of nearby extrasolar planets - includin g dozens that are similar to Earth - by probing the objects' thermal emiss ion spectra. As underlined in the "Voyage 2050" recommendations from the E SA Senior Committee\, the direct detection of the thermal emission of temp erate terrestrial exoplanets is given very high scientific priority in ESA 's future science program and is considered as a candidate theme for a fut ure L-class mission. By now\, the LIFE initiative is supported by more tha n 300 international colleagues from various ESA member states\, the USA\, Australia\, and Japan. In this talk I will demonstrate the unique discover y space for a large mid-infrared exoplanet mission\, in particular for the detection and characterization of terrestrial exoplanets similar to Earth and Venus in the Solar System and the search for atmospheric biosignature s. Synergies between LIFE\, ground-based efforts with the ELTs\, and futur e ESA and NASA missions will be mentioned and a short overview of ongoing technology developments and related challenges will be given. LAST-MODIFIED:20230531T030108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Bailey) \nZoom: https://an u.zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sascha Quanz (Institute for Particle Physics and Astrophysics) "The LIFE initiative - atmospheric characterization of terrestrial exoplanets in the mid-infrared with a large space-based nulling interferometer" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151022T000000Z DTEND:20151022T010000Z DTSTAMP:20261011T152429Z UID:hulbb9e4am7901rbl1p1ebvr7o@google.com CREATED:20150705T081116Z DESCRIPTION:Thanks to numerous ground and space-based surveys\, we are now aware of over 1800 planets orbiting other stars\, with another nearly 5000 candidates from the Kepler Mission awaiting confirmation. The Universe is teeming with rocky and gaseous bodies. How did these planet systems form and evolve toward their present configurations? The answer to this questio n lies in the study of young planets and their formation environments. In this talk I will show how high-precision time series data from space teles copes is beginning to illuminate the conditions surrounding planet formati on and the star-disk connection. Progress is being made on two fronts. Fir st\, high cadence photometry of accreting young stars is revealing the str ucture of the inner circumstellar disk on spatial scales inaccessible to d irect imaging. Second\, the onset of the K2 mission is enabling an unprece dented search for exoplanets at ages of a few to 100 Myr. I will present a selection of exquisite photometric time series from several recent campai gns\, highlighting the diversity of variability seen in young stars with p rotoplanetary disks. In some cases\, we observe occultations by coherent d ust clumps which may be the precursors to planetesimals. I will discuss th e prospects for detecting transits of newly formed planets around young st ars\, as well as upcoming space missions. LAST-MODIFIED:20151014T004108Z LOCATION:Duffield Lecture Theatre (host: Michael Ireland) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ann Marie Cody (NASA Ames) "The Youngest Planets and their Host Sta rs" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201208T000000Z DTEND:20201208T010000Z DTSTAMP:20261011T152430Z UID:csg2fj39441ji8kvqc1jj0ru1s@google.com CREATED:20200826T081718Z DESCRIPTION:Elders teach that everything on the land is reflected in the sk y. The stars serve as a map\, a text\, a law book\, and a memory space. Em erging research in collaboration with Indigenous and First Nations communi ties is revealing a wealth of knowledge about the movements of the stars a nd the myriad ways changes in stellar properties are read to interpret sea sonal change\, atmospheric conditions and much more. Western science is al so realising that many of the discoveries attributed to European thinkers had been observed\, understood\, and encoded in traditional knowledge long ago but was never given proper recognition or credit due to the casual di smissal of non-Western ways of thinking as myth and legend. But our connec tion to the stars\, and the foundations of these ancient knowledge systems \, are under constant threat. The advent of satellite networks overlapping the rapidly decreasing numbers of stars we can see due to light pollution is actively erasing this connection. This talk will discuss some of the a stronomical traditions and their links to land and sky\, and why the erasu re of the stars is a form of ongoing cultural genocide. LAST-MODIFIED:20201206T223806Z LOCATION:ZOOM 997 8534 1005 (host: Kenchington Goldsmith) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Duane Hamacher (U/Melb) "Invited Colloquium: Safeguarding Australia 's Astronomical heritage" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260804T010000Z DTEND:20260804T020000Z DTSTAMP:20261011T152430Z UID:ajllg2ugjpos952i2f8rktfku8@google.com CREATED:20260605T021622Z DESCRIPTION:To understand how galaxies evolve\, we must look beyond their s tellar disks. Galaxies are embedded within vast reservoirs of diffuse gas known as the circumgalactic medium\, which contain the fuel for future sta r formation\, material expelled by feedback\, and a record of the interact ions between galaxies and their environments. Yet this gas is faint\, mult iphase and difficult to observe.\n\nIn this talk\, I will show how backgro und quasars and gravitationally lensed galaxies can be used as cosmic flas hlights to map the gas surrounding galaxies. By combining absorption line spectroscopy with galaxy imaging\, kinematics\, chemical abundances and sp atially resolved emission\, we can connect the location\, motion and metal licity of halo gas to galaxy orientation\, rotation and star formation. I will present evidence for gas accretion\, recycling and outflows\, while h ighlighting the challenges involved in distinguishing these processes obse rvationally. I will also discuss new approaches that move beyond individua l quasar sightlines\, using gravitational arcs and integral field spectros copy to build tomographic maps of the circumgalactic medium. Together\, th ese observations are transforming the circumgalactic medium from an unseen reservoir into a measurable ecosystem\, and clarifying how galaxies acqui re gas\, regulate their star formation and ultimately shut down. LAST-MODIFIED:20260721T000009Z LOCATION:Zoom or Duffield Lecture Theatre (host: Tomasz Rozanski) \nZoom: h ttps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:2 STATUS:CONFIRMED SUMMARY:Glenn Kacprzak (Swinburne) "Beyond the Galaxy: Tracing the Baryon C ycle through the Circumgalactic Medium" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250527T010000Z DTEND:20250527T020000Z DTSTAMP:20261011T152429Z UID:q4tqdnqmnc2hfbi7cmuvpkgdqo@google.com CREATED:20250106T230130Z DESCRIPTION:The SKA Observatory (SKAO) is an intergovernmental project to b uild the world's largest radio telescopes. In order to fully exploit the s cientific output of the immense amount (~700 PB / year) of data flowing fr om the Observatory\, international cooperation through nationally lead hub s -- referred to as SKA Regional Centres (SRCs) -- is required. The Austra lian SKA Regional Centre (AusSRC) is part of this global computing and dat a delivery network -- referred to as SRCNet -- that will enable ground-bre aking science by providing the connection between the SKA telescopes and t he research community. AusSRC is current working with SKA precursor telesc opes\, such as ASKAP\, to build up its own capabilities and local expertis e while supporting developments of the international SRCNet. I will presen t an overview of recent AusSRC and SRCNet activities. I will also include details about my research work with neutral hydrogen (HI) and fast radio b usts (FRBs). Hydrogen is the fuel for star-formation and comprises majorit y of the baryonic matter in our Universe. Using radio telescopes such as A SKAP and eventually the SKA\, HI is readily detectable in and around galax ies\, giving information about the composition\, dynamics\, and evolutiona ry history of these galactic systems. FRBs are extremely energetic and par ticularly peculiar astronomical events arising from unknown origins. As mo re FRBs are detected and localised to host galaxies\, we are starting to c onstrain the environments that could trigger these millisecond pulses. Sev eral FRBs have been localised to extragalactic systems that are close enou gh for HI observations and further detailed analysis\, shedding light on t hese mysterious events. LAST-MODIFIED:20250520T113109Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Vanhiep Nguyen) \nZoom: ht tps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Karen Lee-Waddell (Australian SKA Regional Centre) "ASKAP and AusSR C: finding a path to enable science with SKAO" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220405T060000Z DTEND:20220405T070000Z DTSTAMP:20261011T152429Z UID:lappjh32abuea4lodg9hg04740@google.com CREATED:20220326T090110Z DESCRIPTION:The Milky Way's magnetic field has coherent structures on Galac tic scales\, following spiral arms but also Galactic outflows. It also has a turbulent component\, which influences the galactic ecosystem in many w ays\, such as delaying star formation\, isotropizing Galactic cosmic rays\ , and providing significant pressure component. These magnetic field compo nents can only be detected indirectly\, through the signature they leave o n various kinds of radiation and particles\, observations of which are fit ted to models of the Galactic magnetic field. Traditionally\, radio polari metry is most used to probe Galactic magnetic fields\, with radio detector s in frequency ranges from LOFAR to Planck. However\, recently\, optical p olarimetry of stellar light is an increasingly important tracer\, giving u nique information. I will introduce some of the outstanding problems\, and discuss how we are trying to shed light on the coherent and turbulent mag netic fields in the Milky Way\, using radio polarimetric and optical polar imetric observational methods\, and modeling. LAST-MODIFIED:20220326T090110Z LOCATION:DLT & ZOOM (host: Jackie Ma) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Marijke Haverkorn (Radboud University Nijmegen\, Netherlands) "Invi ted Colloquium: The Magnetic Field of the Milky Way" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191018T033000Z DTEND:20191018T040000Z DTSTAMP:20261011T152429Z UID:o5nj3ff2ips061akbqgh36qip4@google.com CREATED:20191004T042609Z DESCRIPTION:As instruments in space become more complex they produce more d ata. We are at the limit of what is possible to transmit with radio-freque ncy transmissions\, and must move into the optical domain to continue to g row the scientific output of space. This has the added benefit of having n o license fees\, and can enabling new techniques such as quantum encryptio n on a global scale. This presentation will focus on what ANU is doing in the optical communications domain\, and how it might impact on ANU science for remote locations and space. LAST-MODIFIED:20191017T013106Z LOCATION:Duffield Lecture Theatre (host: Monty) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:The Optical Communications Group (RSAA/AITC) "AITC Series - Stop de leting data in space: how optical communications can provide better access to space instruments" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220714T230000Z DTEND:20220715T034000Z DTSTAMP:20261011T152429Z UID:9l5tgvke9dgcr3vbbj76vs7pp8@google.com CREATED:20220705T052109Z DESCRIPTION:Schedule available at : https://anu365-my.sharepoint.com/:x:/g/ personal/u1057001_anu_edu_au/EX00_zlqLHdKpjR-rZiRGBABRC1a20hn3dM4wEmmIMyoT Q?e=DpJnwu LAST-MODIFIED:20220705T052109Z LOCATION:DLT & ZOOM (host: Tony Travouillon) \nZoom: https://anu.zoom.us/j/ 99785341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA HDR Students (RSAA) "RSAA HDR Students Thesis Proposals and An nual Reviews" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261013T000000Z DTEND:20261013T010000Z DTSTAMP:20261011T152430Z UID:jhoqq8oflr4pp7lmlma42vlcv8@google.com CREATED:20260503T114416Z DESCRIPTION:One of the key questions in galaxy evolution is why galaxies st op forming stars. Environmental processes such as gas stripping are known to play an important role\, especially in the local Universe\, yet many ga laxies\, even in massive clusters\, retain significant gas reservoirs long after star formation begins to decline. Understanding what happens to thi s remaining gas\, and why it ultimately fails to form stars\, has therefor e emerged as a key missing piece of the quenching puzzle.\n\nIn this collo quium\, I will present recent results from the Multiphase Astrophysics to Unveil the Virgo Environment (MAUVE)\, a new observational program designe d to probe the state\, dynamics and chemistry of the gas and stars in gala xies undergoing transformation within the Virgo Cluster. By combining obse rvations from VLT/MUSE\, the Hubble Space Telescope and ALMA\, MAUVE follo ws galaxies across different stages of quenching while resolving physical scales of only 100-200 parsecs. In a nutshell\, MAUVE aims to provide for cluster galaxies the same physical insight that PHANGS has delivered for n earby main sequence systems.\n \nAlthough still in its early stages\, MAUV E is already revealing a more complex picture of the quenching process\, i n which outflows remain important beyond the peak of star formation activi ty\, ionised gas can persist after star formation has largely ceased\, and residual gas reservoirs frequently exhibit disturbed kinematics rather th an settled rotating discs. I will also discuss emerging evidence that the relationship between metallicity and star formation may be more complicate d than traditionally assumed. Together\, these results suggest that quench ing is not simply a consequence of gas removal\, but reflects a broader tr ansformation of the physical\, dynamical and chemical state of the gas its elf. LAST-MODIFIED:20260923T130008Z LOCATION:Zoom or Duffield Lecture Theatre (host: Tomasz Rozanski) \nZoom: h ttps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Luca Cortese (U. Western Australia) "Beyond gas removal: early insi ghts into star formation quenching from MAUVE" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190801T010000Z DTEND:20190801T020000Z DTSTAMP:20261011T152429Z UID:oaud88lqtm3qsmjv7abkdr5nr4@google.com CREATED:20190704T023109Z DESCRIPTION:An important shortcoming of the classical model of low-mass sta r formation is the so-called luminosity problem\, whereby embedded protost ars are observed to be under-luminous compared to what is expected from a steady mass accretion. An effect of this is observed in the Hertzsprung-Ru ssell diagrams of star forming regions that show a large luminosity spread \, which is incompatible with well-defined isochrones based on classic non -accreting protostellar evolution models. A possible solution is that accr etion is not steady\, but varies with time. It is not clear if the time ev olution of accretion rates in deeply embedded protostars is best character ised by a smooth decline from early to late stages\, or by intermittent bu rsts of high accretion. Furthermore\, while an age can be defined for a st ar forming region\, the ages of individual stars in the region will vary. I will discuss how we can trace the accretion history of young stars\, how non-steady accretion impacts the evolution of the protostellar structure\ , and how the observed luminosity spread can be explained through the comb ined effect of a protostellar age spread\, a consequence of sustained star formation in star forming regions\, and time-varying protostellar accreti on for individual protostars. LAST-MODIFIED:20190729T080606Z LOCATION:Duffield Lecture Theatre (host: Zhang) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Troels Haugbolle (University of Copenhagen) "Explaining the luminos ity spread in young clusters" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170608T010000Z DTEND:20170608T020000Z DTSTAMP:20261011T152429Z UID:22tuh005hosmt7tkdjrs3aseso@google.com CREATED:20170423T231614Z DESCRIPTION:Machine learning is the study of algorithms that infer patterns from data\, typically with the express goal of making good predictions ab out future data. Classic examples of such techniques are neural networks a nd support vector machines\, which have seen a wide impact far beyond thei r humble origins\; indeed\, the last decade has seen a flurry of applicati ons of machine learning techniques to areas ranging from e-commerce (Netfl ix's video recommendations) to environmental science (MAXENT for species d istribution modelling) to game playing (Google’s champion-beating Go pro gram). Despite these successes\, it is not always obvious how to apply ma chine learning to a new problem. In part\, this is because to the uninitia ted\, it can appear to be a black box comprising an overwhelming number of techniques and terms. In this talk\, we open this box and de-mystify some of these techniques. We introduce some simple ideas -- matrix factorisati on\, logistic regression\, and neural networks -- and show how they underp in many recent advances in machine learning. We illustrate some of these a dvances via a series of vignettes that illustrate their applications to re al-world problems\, including: - determining what makes YouTube videos pop ular (via self-exciting stochastic processes) - recommending trips to trav ellers in a city (via structured prediction) - generating realistic images of cats\, dogs and more! (via adversarial neural networks) Our aim is to stimulate discussion and generate ideas as to how machine learning could be applied in the astronomical sciences. In presenting these applications\ , care will thus be taken to emphasise the abstract problems underpinning each of them. LAST-MODIFIED:20170602T025604Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Lexing Xie and Aditya Menon (CSIRO/ANU) "Opening the Black Box: Rec ent Advances in Machine Learning" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230818T040000Z DTEND:20230818T041500Z DTSTAMP:20261011T152429Z UID:n4t1qolvqrl0mefeq1gfn2959o@google.com CREATED:20230726T060614Z DESCRIPTION:The 2.3m telescope and the WiFeS instrument transitioned to aut omated operation in March 2023 and has been operating robustly for several months. The project required a major overhaul of the software control sys tem and user interface\, with almost no changes to the hardware. The talk will present the architecture of the system\, the underlying design princi ples\, and an explanation of how it actually works in practice. The featur es available will be briefly outlined and I'll discuss the change in minds et required by WiFeS observers to move from classical scheduling to queue scheduling\, and the advantages and disadvantages of the latter. LAST-MODIFIED:20230726T060614Z LOCATION:Duffield Lecture Theatre (host: Mark) \nZoom: https://anu.zoom.us/ j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ian Price (RSAA) "Automating the ANU 2.3m telescope" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240213T000000Z DTEND:20240213T013000Z DTSTAMP:20261011T152429Z UID:fffrd91ub8k5ra3s6k43l7dv74@google.com CREATED:20231212T003613Z DESCRIPTION:I will describe current efforts to model strong binary interac tions\, such as common envelopes\, using 3D hydrodynamic codes and connect these simulations to a number of diverse observations\, particularly thos e of a type of transient known as luminous red novae. In particular I will discuss the implementation of dust nucleation in simulations\, a necessar y ingredient to connect simulations to the observed light curves of the ob jects. LAST-MODIFIED:20240123T030111Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Orsola De Marco (Macquarie U.) "Strong\, dusty binary interactions\ , and the transients they cause" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230216T000000Z DTEND:20230216T010000Z DTSTAMP:20261011T152429Z UID:87tp87hnedmja4udmi4rjp9860@google.com CREATED:20230201T134312Z DESCRIPTION:We studied large-scale magnetic field reversals of a galaxy bas ed on a magnetic vector map of some galaxy. It is known that the magnetic field of galaxies is universal and align with a spiral arm structure. Howe ver\, how these structures are formed is not fully understood. We have dev eloped a new method to determine the magnetic vector structure of galaxies . We also performed a modal analysis of the magnetic field and stellar arm s to investigate their relationship. In this talk\, I will present the rel ationship which is we have found between the magnetic field structure and stellar disks. I would also be happy to share some memories from my stay i n ANU for about a month. LAST-MODIFIED:20230207T001112Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hiep) \nZoom: https://anu. zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kohei Kurahara (NAOJ) "Large-scale magnetic field structure based o n a magnetic vector map" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250213T000000Z DTEND:20250213T010000Z DTSTAMP:20261011T152429Z UID:2s78djsndpdc2mj2jrp9hb7h3k@google.com CREATED:20250106T230711Z DESCRIPTION:Type Ia supernova science holds steady as one of the leading pr obes to study the behavior of our universe\, and yet\, even the most compl ete and advanced datasets to date suffer from poor statistics and systemat ics at low redshift. To combat these pitfalls\, the Dark Energy Bedrock Al l-Sky Supernovae (DEBASS) program will provide the largest consistently ca librated low-z SN Ia data in the southern hemisphere\, helping improve mea sures of bulk flow and universe isotropy. At this time\, DEBASS has accumu lated more than 350 spectroscopically confirmed SN Ia within the redshift range out to z~0.08 using the Dark Energy Camera for 3.5 nights per semest er over the last 4 years. In this talk\, we will introduce the DEBASS prog ram\, discuss its science goals and the advantages it presents to supernov a cosmology\, and introduce the upcoming DEBASS early data release\, compo sed of 56 SNe located within the Dark Energy Survey footprint. LAST-MODIFIED:20250131T060613Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Bailey Martin) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Nora Sherman (Boston U.) "The Dark Energy Bedrock All-Sky Supernova e Survey" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190822T010000Z DTEND:20190822T020000Z DTSTAMP:20261011T152429Z UID:7189e9c99odu71hrbvtiqmru20@google.com CREATED:20190704T051611Z DESCRIPTION:Relativistic jets from active galactic nuclei may have a profou nd impact on their environment\, both enhancing ('positive feedback') and inhibiting ('negative feedback') star formation under certain conditions. On cluster scales\, powerful jets are believed to drive negative feedback by preventing cooling of the intracluster medium (ICM)\, depriving galaxie s of dense gas for star formation (e.g.\, McNamara & Nulsen 2012). On much smaller scales\, however\, the role that jet-driven feedback processes pl ay in shaping the properties of their host galaxies and environment remain s elusive. In particular\, efforts to catch feedback in the act have been hampered by the sub-kpc spatial resolution required to resolve the jets' e nvironment. In this talk I will discuss my PhD research\, in which I have used high-resolution optical and near-infrared integral field spectroscopy (IFS) in conjunction with state-of-the-art hydrodynamical simulations to shrink this gap in our understanding of jet-driven feedback on sub-kpc sca les. To investigate feedback processes driven by young jets\, I led studie s of the local radio galaxies 4C 31.04 and UGC 05771. Both galaxies harbou r young jets confined to the ISM\, with very long baseline interferometry (VLBI) revealing jets ~100 pc and ~10 pc in size in 4C 31.04 and UGC 05771 respectively. Using AO-assisted near-IR IFS from Gemini/NIFS and Keck/OSI RIS\, we found signatures of jet-ISM interactions at radii up to 100 times larger than the apparent size of the jets in both galaxies\, a surprising result indicating the existence of low surface-brightness jet plasma belo w the detection threshold of the VLBI observations. This is consistent wit h contemporary hydrodynamical simulations which show that the main jet str eam may become temporarily halted by a dense clump in the ISM\, whilst sec ondary plasma streams---which have a much lower surface brightness---can p ercolate through channels in the ISM\, reaching much larger radii. To inve stigate jet-driven feedback in the intracluster medium\, I led a study of Minkowski's Object\, a peculiar star-forming region triggered by the jet f rom a neighbouring galaxy. Using observations from the WiFeS spectrograph on the ANU 2.3 m telescope\, we discovered a metallicity gradient across M O. We concluded that the gradient has been caused by metal-rich material e ntrained by the jet mixing with the pristine ICM. This is the first study of optical emission-line gas that has confirmed this phenomenon\, which ha s previously only been observed in clusters using X-ray observations. LAST-MODIFIED:20190819T012605Z LOCATION:Duffield Lecture Theatre (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Henry Zovaro (RSAA) "Resolving jet-driven feedback on sub-kpc scale s (End-of-Thesis Colloquium)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221201T000000Z DTEND:20221201T010000Z DTSTAMP:20261011T152429Z UID:bm7r1rfj9p9kem3fc7evedt5pk@google.com CREATED:20221107T223614Z DESCRIPTION:The Fermi Gamma-ray Burst Monitor (GBM) triggers on-board in response to ~ 40 short gamma-ray bursts (SGRBs) per year\; however\, thei r large localization regions have made the search for optical counterparts a challenging endeavor. We have developed and executed an extensive progr am with the wide field of view of the Zwicky Transient Facility (ZTF) came ra\, mounted on the Palomar 48-inch Oschin telescope (P48)\, to perform ta rget-of-opportunity (ToO) observations on 10 Fermi-GBM SGRBs during 2018 and 2020-2021. Bridging the large sky areas with small field of view optic al telescopes in order to track the evolution of potential candidates\, we look for the elusive SGRB afterglows and kilonovae (KNe) associated with these high-energy events. No counterpart to a binary neutron star merger h as yet been found in our searches\, however\, interesting transients (such as GRB 200826A) have appeared in our searches. More than 10 ground-based telescopes\, part of the Global Relay of Observatories Watching Transient s Happen (GROWTH) network\, have taken part in these efforts. The candidat e selection procedure and the follow-up strategy have shown that ZTF is an efficient instrument for searching for poorly localized SGRBs\, retrievin g a reasonable number of candidates to follow-up and showing promising cap abilities as the community approaches the multi-messenger era. Based on th e median limiting magnitude of ZTF\, our searches would have been able to retrieve a GW170817-like event up to ~200 Mpc and SGRB afterglows to z = 0.16 or 0.4\, depending on the assumed underlying energy model. Future ToO s will expand the horizon to z = 0.2 and 0.7 respectively. LAST-MODIFIED:20221107T224614Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/99785341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tomas Ahumada (California Institute of Technology) "Optical searche s of Fermi GRBs using the Zwicky Transient Facility" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170808T000000Z DTEND:20170808T010000Z DTSTAMP:20261011T152429Z UID:l8pm865tkajuebkl888dg3u2mg@google.com CREATED:20170807T010603Z DESCRIPTION:A major goal of modern astrophysics is to understand how galaxi es evolved across cosmic time from small fluctuations in the primordial Un iverse to the variety of galaxies we observe today. Significant observatio nal advances in the last few decades have allowed us to obtain snapshots o f the galaxy population at different cosmic times in different parts of th e electromagnetic spectrum. These snapshots give us a census of baryonic c omponents - stellar populations and interstellar matter - for large statis tical samples of galaxies at each epoch. In this talk\, I will describe ga laxy spectral models that allow us to translate these multi-wavelength int o physical properties of galaxies that can be used to contrast different g alaxy populations and compare with predictions from theoretical models. Su ch comparisons have yielded valuable insight into the complex lives of gal axies\, however many questions remain regarding the evolution of star form ation and the interstellar medium of galaxies\, particularly in the young Universe\, which has been hard to access observationally. New facilities s uch as the Atacama Large Millimetre Array\, the James Webb Space Telescope \, the Square Kilometre Array\, and Integral Field Unit Spectrographs on a variety large telescopes promise to revolutionise this field. I will outl ine the next-generation spectral models that will be vital in unlocking ke y physics from these ever more sophisticated observations\, all the way fr om our local Universe to the epoch of re-ionisation. LAST-MODIFIED:20170807T010603Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Elisabete da Cunha (RSAA) "Galaxy evolution across the spectrum" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220426T010000Z DTEND:20220426T020000Z DTSTAMP:20261011T152429Z UID:d9sbkelfhfracn72tes0kj7pas@google.com CREATED:20220207T002112Z DESCRIPTION:Since the detection of the first gravitational wave transient i n 2015\, there has been a small revolution in our understanding of the mas s distribution of black holes. But\, there are still many unknowns and the ory is still struggling to understand how the observed distribution is det ermined. There are also other windows onto black holes that are showing th at the GW transient masses are only half the story. I'll present the main samples of black holes that are available to us today\, and in the not-too -distant future. Then describe how theoretical work will allow us to under stand what physics is in play in determining the birth and evolution of bl ack holes\, their ecology within galaxies and the Universe. LAST-MODIFIED:20220427T002606Z LOCATION:DLT & ZOOM (host: Jackie) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jan J. Eldridge (University of Auckland\, NZ) "Invited Colloquium: Insights into black hole ecology" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160209T000000Z DTEND:20160209T010000Z DTSTAMP:20261011T152429Z UID:4h7qqbrioejl9sltdc3pfk8pl8@google.com CREATED:20151214T225609Z DESCRIPTION:The bulge is one of the oldest\, yet very metal-rich Galactic c omponents suggesting that it experienced early\, rapid chemical enrichment . Yet\, the first\, metal-poor stars to have formed in the Universe are pr edicted to be found in this central region of the Milky Way. I will presen t results from our endeavour to detect and characterize signatures from su ch stars. The chemical abundances of our candidates (at [Fe/H] of -1.5 to -2.6 dex) vastly overlap with those of halo stars and our sample also cont ains one CEMP-s and a CH-star - the first detections of such objects in th e bulge. While we do not see any evidence of Population III enrichment in our sample\, the chemical abundance patterns still give a deep insight int o the dominant enrichment mechanisms in the early phases of galaxy assembl y. This can be contrasted to observations of other\, most metal-poor stell ar systems such as globular clusters. LAST-MODIFIED:20160131T231606Z LOCATION:Duffield Lecture Theatre (host: Helga Denes) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Andreas Koch (University of Heidelberg) "Bulge vs. Halo: a mixed b ag of chemical enrichments" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190228T000000Z DTEND:20190228T003000Z DTSTAMP:20261011T152429Z UID:hougv40nm2ph5sj0ukntlqm4n0@google.com CREATED:20190128T232717Z DESCRIPTION:Outflows are ubiquitous at the peak epoch of star formation (z~ 1-3)\, and are likely to play an important role in shaping the growth and evolution of galaxies. Near-IR integral field spectroscopy is a powerful t ool to investigate the physical properties of galactic winds at this epoch because it enables us to kinematically disentangle them from gravitationa l motions\, and to map the launch sites\, extent\, and geometry of outflow s. In this talk I will present the most recent results from our integral f ield studies of outflows at z~1-3. I will summarise the properties and sca ling relations of outflows resolved on 1-2 kpc scales using SINFONI with a daptive optics\, and place these results in the context of our study of gl obal outflow properties and demographics from the KMOS3D survey. LAST-MODIFIED:20190226T231105Z LOCATION:CSO Common Room (host: Oh) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rebecca Davies (MPE) "Resolved Properties and Demographics of Ioniz ed Gas Outflows at" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160809T010000Z DTEND:20160809T020000Z DTSTAMP:20261011T152429Z UID:481let1j6je498oeqhpuikctg4@google.com CREATED:20160727T182113Z DESCRIPTION:Magnetic fields are an elemental part of the interstellar mediu m (ISM) that have a large impact on the dynamics of the ISM on various spa tial scales. Here\, I'll talk about the long-standing issue of how to gene rate magnetically supercritical cloud cores\, which are essential to under standing star formation in our own Galaxy. Furthermore on a related issue\ , I'll discuss how to circumvent the 'magnetic braking catastrophe'\, whic h was thought to be a major problem for the formation of protostellar disc s. LAST-MODIFIED:20160801T011105Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Robi Banerjee (University of Hamburg) "Star formation out of the Ma gnetised Interstellar Medium" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190510T010000Z DTEND:20190510T013000Z DTSTAMP:20261011T152429Z UID:m2ma6u2b2ov7c51i4ahj750r9k@google.com CREATED:20190509T030203Z DESCRIPTION:Internationally acclaimed pianist\, composer and one-time astro physics student Dan Tepfer delves into the music that arises when the orbi ts of planets around their host star are turned into sound. Part musical p erformance\, part lecture\, a 21st century update on the Music of the Sphe res. LAST-MODIFIED:20190509T030203Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dan Tepfer (Music Festival) "Listening to planetary orbits: Finding music in the Solar System and beyond" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230613T230000Z DTEND:20230614T020000Z DTSTAMP:20261011T152429Z UID:4pr9vi25d2v4ipt973uei2qlp0@google.com CREATED:20230521T073610Z DESCRIPTION:Schedule: 9.15: Deon Hickey "Spatially Variable Filters Special ised for Wide Field Spectral Kilonova Searches" 9.45: Jim Chung "Prototypi ng the Differential Astrometric Calibration Technique for MAVIS" 10.15: Ru izhou Hua "The high energy gamma-ray emission of 27 globular clusters and its correlations" 10.50-11.10: Coffee break (CSO Common room) 11.10: Fan X u "An Integral Field Spectroscopy Study of Thick Disc in 2531" 11.45: Yanj un Sheng "Exploring the LMC's orbital history through its dynamical pertur bations in the Milky Way halo" LAST-MODIFIED:20230609T064110Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Luca Casagrande) \nZoom: h ttps://anu.zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Honours and Masters talks (RSAA) "Honours and Masters Talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191122T030000Z DTEND:20191122T033000Z DTSTAMP:20261011T152430Z UID:2c1bo0itvp232pklihun9vpnp4@google.com CREATED:20191022T041612Z DESCRIPTION:We're all familiar with geostationary satellite antennas – th e Foxtel dishes atop many rooftops that point to a fixed location in space . The AITC has a number of programs\, however\, that rely on our ability to interact with satellites that freely zip across the sky under the influ ence of a plethora of perturbing forces. Understanding these forces is th e first step to being able to predict where any of the 20\,000+ catalogued orbital objects are at any particular instant so we know where – and wh en – to point our telescopes at them. In this talk I’ll outline how s atellites move\, how we find them and the challenges and opportunities the y afford to our communications and space environment research programs. LAST-MODIFIED:20191022T041612Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:James Webb (RSAA/AITC) "AITC Series – Space is big\, satellites a re (comparatively) small… the joys of finding\, tracking\, and using th em!" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231101T221500Z DTEND:20231102T041500Z DTSTAMP:20261011T152430Z UID:d7ril9bra6b2d48d2k4vkmffrs@google.com CREATED:20231011T104613Z DESCRIPTION:TBC LAST-MODIFIED:20231011T104613Z LOCATION:Duffield Lecture Theatre (host: Christian Wolf) \nZoom: https://an u.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Honours and MSc Talks (RSAA) "Honours and MSc Talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150821T042000Z DTEND:20150821T044000Z DTSTAMP:20261011T152429Z UID:1il16vl4rhlmjfp33lloonu2eo@google.com CREATED:20150625T051617Z DESCRIPTION:I will present an update on the Keck telescope and instrumentat ion from the recent Keck Science Steering Committee Meeting. I will discus s the status of current instrumentation for the next semester\, and provid e an update of instruments in the development or proposal phase. I will de scribe the new Australian Keck TAC process\, and I will briefly discuss a potential future Keck-Subaru partnership. LAST-MODIFIED:20150820T021607Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Lisa Kewley (RSAA) "Keck Update" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150428T010000Z DTEND:20150428T020000Z DTSTAMP:20261011T152429Z UID:ts6jce90or3f7u3q4bu4l29o1c@google.com CREATED:20150227T012624Z DESCRIPTION:Molecular clouds in the central 200 pc of the Galaxy (the 'Cent ral Molecular Zone') exhibit different (and more extreme) physical propert ies than those in the disk\, yet because this is the closest galactic nucl eus\, detailed studies of this region can provide insight on galactic nucl ei in general in the nearby universe. We have recently undertaken a high s patial and spectral resolution study of a sample of molecular clouds in th is region to try to get a better understanding of their detailed propertie s and what mechanisms might be heating them. In this talk I will present a case study of one of the clouds - a dense and unusual cloud\, GCM0.253+0. 016 - also known as 'The Brick'. Observations were made using the Very Lar ge Array in New Mexico\, USA at K (24 to 26 GHz) and Ka (27 and 36 GHz) ba nds. I will describe results from sensitive continuum images and studies o f 12 molecular lines\, including 8 transitions of ammonia (NH3) and the ab undant CH3OH maser. LAST-MODIFIED:20150421T023606Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Cornelia Lang (University of Iowa) "A case study of an unusual mole cular cloud in the Galactic Center: Abundant CH3OH Masers but no new star formation in GCM0.253+0.016" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230203T020000Z DTEND:20230203T030000Z DTSTAMP:20261011T152429Z UID:arhb9ql854uaa2d87uhg66tpo4@google.com CREATED:20230116T001611Z DESCRIPTION:The nucleus of our Galaxy is home of several high-energy proces ses (black hole\, intense star formation) that have generated a large-scal e\, multiphase\, nuclear wind. In the past few years\, we have extensively studied the colder components of this outflow thanks to dedicated surveys of the Galactic Centre region in neutral hydrogen (HI) and molecular line s. These observations have revealed for the first time the resolved struct ure of cold gas clouds entrained in a galactic wind and have returned a nu mber of new\, puzzling aspects of these fascinating phenomena. In this tal k\, I will review the main discoveries and findings about the cold gas pha ses of the Milky Way's nuclear outflow and I will discuss its possible ori gin and impact on the central regions of the Galaxy. LAST-MODIFIED:20230130T003610Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Callum Lynn) \nZoom: https ://anu.zoom.us/j/99785341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Enrico Di Teodoro (University of Florence) "The cold outflow from t he nucleus of the Milky Way" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220524T010000Z DTEND:20220524T020000Z DTSTAMP:20261011T152429Z UID:sgstne6u7b3or6o1uuhgddf1vk@google.com CREATED:20220201T005114Z DESCRIPTION:Over 2/3 of all star formation in the Universe occurs in gas-ri ch\, super-high pressure clumpy galaxies in the epoch of redshift z~1-3. H owever\, because these galaxies are so distant we are limited in the infor mation available to study the properties of star formation and gas in thes e systems. I will present results using a sample of extremely rare\, near by galaxies (from the DYNAMO survey and the new DUVET survey) that are ver y well matched in gas fraction (fgas~20-80%)\, kinematics (rotating disks with velocity dispersions ranging 20-100 km/s)\, structure (exponential di sks) and morphology (clumpy star formation) to high-z main-sequence galaxi es. We therefore use these galaxies as laboratories to study the processes inside galaxies in the dominate mode of star formation in the Universe. I n this talk I will report on results that are aimed at testing models of s tar formation in galaxies. Feedback regulated star formation theories aim to explain properties like the velocity dispersion of disks\, the relation ship between gas and star formation and the vertical scale height of thin disks in galaxies. I will show that while these theories explain the prope rties in spiral galaxies\, like the Milky Way\, they fail to recover the k inematics and star formation in gas rich disks\, and thus are not able to describe galaxies in the epoch when most stars formed. Finally\, I will di scuss very recent efforts to connect the regulation of gas via outflows to the picture of how galaxies maintain their star formation rates and posit ions in Kennicutt-Schmidt relationship. LAST-MODIFIED:20220517T004309Z LOCATION:DLT & ZOOM (host: Stefania) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Deanne Fisher (Swinburne University) "Invited Colloquium: Testing F eedback Theories in Clumpy\, Gas Rich Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150130T030500Z DTEND:20150130T032000Z DTSTAMP:20261011T152430Z UID:mnftdt3lc7d4lcd3v22kp7h7bk@google.com CREATED:20250925T231033Z DESCRIPTION:I will briefly summarise the methods to estimate the magnetic f ield strengths of different types of neutron stars and the caveats associa ted with them. In this context I will present some recent results we have obtained in finding the limits to the field strengths of accreting millise cond X-ray pulsars from the interaction between the accretion disk and neu tron star magnetosphere. LAST-MODIFIED:20250925T231033Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dipanjan Mukherjee (RSAA) "Measuring magnetic field strengths of ne utron stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181212T032000Z DTEND:20181212T034000Z DTSTAMP:20261011T152429Z UID:086ebjng9qo90jgnpj9t0bae8k@google.com CREATED:20181123T013123Z DESCRIPTION:A new method for refining the physical and behavioural characte ristics of near-earth orbiting objects is being developed. The method can be thought of as orbit determination using more object characteristic para meters and with geophysical\, atmospheric and third-body models of greater fidelity than are typically used. The method is similar to cell-based eng ineering analyses in that it is solved through linear algebraic methods. I n this first PhD annual report\, the progress on developing the method wil l be presented. Convergence to a theoretically valid solution has been ach ieved but the solutions are not unique and vary with infinitesimal changes to the initial estimates\; a consequence of a non-linear system of equati ons with limited diversity. Current work on characterising and improving e quation diversity as well as the opportunity to incorporate additional ana lytic features will be presented. Collaboration opportunities for the next twelve months will also be discussed. LAST-MODIFIED:20181202T103609Z LOCATION:CSO Common Room (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Richard Samuel (SERC) "Refinement of near-earth object characterist ics through numerical synthesis (PhD annual report)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151201T000000Z DTEND:20151201T010000Z DTSTAMP:20261011T152429Z UID:p90k42o9viatvcd5g94cchhcsg@google.com CREATED:20151109T020113Z DESCRIPTION:Filamentary structures are ubiquitous in the interstellar mediu m\, yet their formation\, internal structure and longevity have not been s tudied in detail. In this talk I present a summary of my PhD thesis\, whic h investigates the characteristics\, formation and dynamics of filaments a rising from wind-cloud interactions. I use magnetohydrodynamic numerical s imulations with gas multi-tracking techniques to shed light on the physica l mechanisms acting upon wind-swept clouds and provide measurements of the aspect ratios\, internal velocity dispersions\, energy densities\, and ma gnetic field strengths and orientations in the resulting filaments. Using state-of-the-art visualisation techniques\, I also explain the roles of pl asma instabilities\, turbulence and magnetic dynamos in the evolution of f ilaments. At the end of the talk I discuss the relevance of this work for the study of clouds and filaments in the Galactic centre region and provid e my perspectives of potential future research in this field. LAST-MODIFIED:20151201T041104Z LOCATION:Woolley Seminar Room (NOTE CHANGE OF LOCATION!) (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Wladimir Banda-Barragan (RSAA) "Magnetohydrodynamics of Wind-Cloud Interactions: Filament Formation in the Interstellar Medium" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160802T010000Z DTEND:20160802T020000Z DTSTAMP:20261011T152429Z UID:gtnr467iraqovbvvbgctc3g200@google.com CREATED:20160720T033107Z DESCRIPTION:Measurement of the matter distribution in the universe is one o f the key components in observational cosmology. This provides an importan t test of structure formation scenarios and cosmological models. I discuss two aspects of this test: (1) comparing the matter distribution around ga laxy clusters from galaxy redshift surveys with that from weak-lensing sur veys and (2) statistical comparison of large-scale structure between obser vations and cosmological simulations. These tests underscore the importanc e of mapping the large-scale structure of the universe for exploring and u nderstanding cosmology and structure formation. I emphasize the power of c ombining observations including redshift and weak-lensing surveys with cos mological simulations. LAST-MODIFIED:20160801T230604Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ho Seong Hwang (Korea Institute for Advanced Study) "Mapping the Di stribution of Galaxies at Intermediate Redshifts: Galaxy Clusters and Larg e-scale Structure of the Universe" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180412T010000Z DTEND:20180412T020000Z DTSTAMP:20261011T152429Z UID:n0ftrsco39dsk1vsrvsn0jm0eo@google.com CREATED:20180319T125611Z DESCRIPTION:The origin of the star to star abundance variations for light e lements shown in galactic globular clusters (GGCs) is not well understood\ , which represents a significant problem for stellar astrophysics. While t he light element abundance variations are very common in globular clusters \, they are comparatively rare in the galactic halo field population. Howe ver\, very little is known regarding the occurrence of the abundance anoma lies in other environments such as dwarf spheroidal galaxies and massive s tar clusters younger than the ancient globular clusters. Consequently\, du ring my Ph.D. thesis was investigated the anti-correlation and bimodality of CH and CN band strengths through the measurement of CH(lambda ~ 4300)\, S(3839) and S(4142) indices for 45 red giants stars in Sculptor dwarf sph eroidal galaxy. We report the discovery of a third carbon-enhanced metal p oor star in Sculptor\, which shows evidence of a strong s-process element enhancement. Through the calibration of five GCs (NGC 1851\, NGC 288\, NGC 6752\, M 55 and M 30) we also have studied the correlation CN/Na in the S culptor red giant sample. Our results indicate that variations analogous t o those seen in GGCs are not present in our Sculptor sample. Instead we fi nd a positive correlation between CH and CN\, and no correlation between N a and CN. Also\, we have found a deficiency of [Na/Fe] in Sculptor relativ e to GGCs\, which is consistent with previous works for dSph galaxies. The outcome reinforces the apparent need for a high stellar density environme nt to produce the light element abundance variations. In addition\, we hav e investigated CN and CH band strengths along with carbon and nitrogen abu ndances in massive star clusters of Small Magellanic Cloud. These clusters have metallicity and luminosity comparable to GGCs but shows differences in age. The investigated clusters are Lindsay 1\, Kron 3 and NGC 339\, whi ch have ages between 6 and 7.5 Gyr. Our results show large spread in nitro gen in these three clusters\, which is an indicator of multi population. D ue to the possibility of evolutionary mixing on the red giant branch\, the existence of CN-CH anti-correlation is not sufficient in itself to indica te the presence of abundance anomalies. Consequently\, we have investigate d the Na\, CN correlation through the measurement of sodium D-lines and Na abundances. At least for NGC339 we can confirm the positive correlation b etween nitrogen and sodium. Our results are a key factor in gaining unders tanding on the origin and evolution of stellar systems and also it will pr ovide an accurate context for studying the problem of origin of anomalies constraining the age dependence of them in the unexplored 6-11 Gyr age ran ge. LAST-MODIFIED:20180405T051105Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Carolina Salgado Escalona (RSAA) "Investigating globular cluster ab undance anomalies in different environments (End-of-Thesis Colloquium)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160715T040000Z DTEND:20160715T042000Z DTSTAMP:20261011T152429Z UID:u3jkg3sibde7vd7hehgp9reo9s@google.com CREATED:20160704T074106Z DESCRIPTION:TBD LAST-MODIFIED:20160704T074107Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dilyar Barat (RSAA) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240820T010000Z DTEND:20240820T020000Z DTSTAMP:20261011T152429Z UID:f4vhjg5imge010idcc8kps4j3g@google.com CREATED:20240415T054237Z DESCRIPTION:As climate change worsens fire weather and increases the number of areas burned by wildfires worldwide\, high-tech solutions are critical to changing how wildfires are battled. Remote sensing technologies provid e access to dynamic and real-time information that helps fire managers to better understand the likelihood of a catastrophic bushfire\, the whereabo uts and intensity of active fires and accurately assess wildfire scale and environmental impacts. This remote sensing-derived information is critica l to plan\, prepare and respond to future wildfires. In my talk\, I will p rovide an overview of the technological trends including sensor integratio n\, planned satellite earth observing missions and state-of-the-art modell ing approaches. LAST-MODIFIED:20240801T171111Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Marta Yebra (ANU Fenner School of Environment and Society) "Remote Sensing for Climate Change Resilient Wildfire Management" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230509T010000Z DTEND:20230509T020000Z DTSTAMP:20261011T152430Z UID:c3521j9ca6jgc6b3o695ecd5bs@google.com CREATED:20230501T022109Z DESCRIPTION:Large\, spatially-resolved galaxy surveys like MaNGA and SAMI h ave provided an unprecedented look at the internal structure and compositi on of the nearby galaxy population. Here I will describe our investigation of stellar chemical enrichment across a range of galaxy properties and en vironments as a way to probe early-type galaxy assembly. We see difference s in outer metallicity profiles that may be evidence for late-time accreti on in massive galaxy outskirts. And\, when we look at the inner profiles of central galaxies\, we find enrichment histories that\, at fixed halo ma ss\, reveal a surprising secondary dependence on stellar mass. Halos that host galaxies with more stars seem to have experienced accelerated format ion and assembly\, leading to older and more alpha-enhanced populations to day. I'll conclude with an update on the Starbugs-enabled FOBOS instrument \, which will enabled resolved studies like these at redshift one and beyo nd. LAST-MODIFIED:20230504T014402Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Callum) \nZoom: https://an u.zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kevin Bundy (UCSC) "The Impact of Halo-Driven Assembly on the Enric hment of Spatially-Resolved Stellar Populations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150528T010000Z DTEND:20150528T020000Z DTSTAMP:20261011T152429Z UID:gkeufk678iltd052k89khhngrs@google.com CREATED:20150420T101614Z DESCRIPTION:Transiting systems offer us unique opportunities to study indiv idual systems in great detail. This talk will present discoveries of new t ransiting planets and low mass stars\, and the characterisation of their f undamental properties: mass\, radius\, temperature\, and composition. I wi ll introduce the HATSouth survey\, the only global network of telescopes d edicated to searching for transiting exoplanets. The planets discovered by HATSouth orbit a diverse range of host stars\, and the candidates identif ied have a wide range of orbital periods. I will present some of the highl ight discoveries of the HATSouth program. The goal of these planet searche s is to identify the most characterisable planets for further study. We ar e using the Anglo-Australian Telescope to survey the near infrared seconda ry eclipses of a series of hot-Jupiters. These observations represent some of the highest precision near-infrared time-series photometry performed f rom the ground\, and probe a diverse range of planet atmospheres. We find a diverse\, but continuous distribution of spectral properties for the hot -Jupiter population. We explore this in the context of climate and global circulation in the atmospheres of these planets. LAST-MODIFIED:20150523T090606Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:George Zhou (RSAA) "Discovering and characterising transiting plane ts and low mass stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20211028T000000Z DTEND:20211028T003000Z DTSTAMP:20261011T152429Z UID:u9umr0m59hm8vqtdmh0p6hoslg@google.com CREATED:20211022T085109Z DESCRIPTION:Peculiar velocity analysis is currently a growing field due to the advent of new data from various surveys. One statistic that can be der ived from peculiar velocity analyses is the bulk flow within the survey vo lume\, which is closely related to the cosmological model and so can be us ed to test theories.To measure the bulk flow accurately\, a sky coverage a s complete as possible is needed to disentangle the dipole from the monopo le component of the velocity field. In this work\, we use the Fundamental Plane (FP) relation for early-type galaxies to measure distances. We measu re peculiar velocities as the logarithmic ratio of the distances inferred from observed redshifts and comoving distances derived from the FP. Our fi nal peculiar velocity sample consists of 15525 individual galaxies. We mea sure the bulk flow within the survey volume directly from the log-distance ratio measurements using a maximum likelihood method. These amplitudes ar e consistent at 1 sigma with the root-mean-square bulk motions expected in a standard LCDM cosmology. LAST-MODIFIED:20211022T085109Z LOCATION:ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rafif Rabbani (Institut Teknologi Bandung) "Bulk flow in the local universe from 6dfGS\, SDSS\, and LAMOST peculiar velocities" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151218T030000Z DTEND:20151218T033000Z DTSTAMP:20261011T152429Z UID:t7hdqa9b98rua55divvsrnphi0@google.com CREATED:20151209T041109Z DESCRIPTION:Space debris is a serious and growing threat to operating space craft. Potential debris collisions with satellites are becoming increasin gly likely and can cause economic loss of between $25 million and $500 mil lion per event. An avalanche where one collision quickly triggers another until many satellites are destroyed is increasingly likely. Such an even t could destroy hundreds of satellites and impair the global economy for d ecades. The Space Environment Research Centre consolidates formerly indep endent research efforts to develop technologies to address the global issu e of space debris. National and international partners include EOS Space Systems\, Lockheed Martin Space Systems (US)\, Optus Satellite Systems\, t he Australian National University\, RMIT University and the National Insti tute of Information and Communication's Technology (Japan) LAST-MODIFIED:20151214T010106Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ben Greene (SERC) "CRC for Space Environment Management - Space Env ironment Research Centre (SERC)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260512T013000Z DTEND:20260512T023000Z DTSTAMP:20261011T152430Z UID:36f20pdgu3kf16u1hl1m9undj4@google.com CREATED:20260503T015638Z DESCRIPTION:Over the past decade\, the advancement of large optical surveys and the emergence of gravitational wave observatories have opened a new p athway to finding and characterising black holes. These developments have led to new exciting insights on how black holes form and evolve. We are fi nding black holes in binary (and triple) configurations never observed bef ore\, and we are finding stellar-black holes in mass ranges that were deem ed unfeasible. Alongside these revelations\, new questions have emerged ar ound how to interpret these findings\, in the context of black hole format ion and evolution and what they imply for the population of black holes in our Galaxy. In this talk\, I'll review some of the recent discoveries\, a nd showcase how they are shaping our journey in understanding black holes in our Galaxy. LAST-MODIFIED:20260503T112611Z LOCATION:Zoom or DLT (host: Tomasz Rozanski) \nZoom: https://anu.zoom.us/j/ 82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Arash Bahramian (Curtin U.) "Chasing stellar-mass black holes in ou r Galaxy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200924T010000Z DTEND:20200924T013000Z DTSTAMP:20261011T152430Z UID:41dj6srmmt0puj0f3qg3nsq028@google.com CREATED:20200907T051111Z DESCRIPTION:TBD LAST-MODIFIED:20200907T051111Z LOCATION:ZOOM 997 8534 1005 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dávid Guszejnov (UT Austin (USA)) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221213T000000Z DTEND:20221213T010000Z DTSTAMP:20261011T152429Z UID:efald37nokov7jkjb87f9ov5cc@google.com CREATED:20220812T005614Z DESCRIPTION:Intense star formation and rapid black hole accretion in the ce nters of galaxies produce energy that propels gas outward. These galactic winds affect the evolution of their host galaxies\, and may self-regulate the future growth of stars and black holes. Galaxies are also known to be surrounded by enormous reservoirs of gas. Galactic winds are a likely mech anism by which these reservoirs are created. However\, we don't know how f ar most galactic winds extend into their surroundings. I will discuss obse rvations of galactic winds driven by star formation and black holes that p robe their extent and illuminate the connection between galaxies and their surroundings. These observations come from sensitive ground-based spectro graphs\; the ultraviolet capabilities of HST\; and newly deployed space-ba sed\, infrared IFSs on JWST. LAST-MODIFIED:20221205T094111Z LOCATION:DLT & ZOOM (host: TBD) \nZoom: https://anu.zoom.us/j/99785341005?p wd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:David Rupke (Rhodes College) "How big are galactic winds?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190416T010000Z DTEND:20190416T020000Z DTSTAMP:20261011T152430Z UID:bidsbn8dcdd4uboauciok07g1s@google.com CREATED:20190308T010120Z DESCRIPTION:Cosmic rays and magnetic fields are important non-thermal compo nents of the ISM of spiral galaxies. Cosmic ray electrons in the presence of the ISM magnetic fields give rise to synchrotron emission\, which is on e of the most powerful probes of magnetic fields in galaxies. Interpretati on of synchrotron intensity data requires knowledge of the cosmic ray numb er density\, which is often assumed to be in energy equipartition (or othe rwise tightly correlated) with the magnetic field energy density. We exami ne the energy equipartition assumption between cosmic rays and magnetic fi elds using both: test-particle simulations (important to capture the effec t of the magnetic field structure) and MHD simulations by considering cosm ic rays as an additional diffusive fluid (important to consider the effect s of gas pressure). We find no spatial correlation between the cosmic rays and magnetic field energy densities at turbulent scales. Moreover\, the c osmic ray number density and magnetic field strength are statistically ind ependent. Nevertheless\, small-scale cosmic ray structures are abundant a t low energies. These are particles trapped in random magnetic bottles. Th ese conclusions can significantly change the interpretation of synchrotron observations and thus our understanding of strength and structure of magn etic fields in the Milkyway and nearby spiral galaxies. LAST-MODIFIED:20190412T004106Z LOCATION:CSO Common Room (host: Monty) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Amit Seta (RSAA) "Cosmic rays and magnetic fields in the ISM of spi ral galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150318T030000Z DTEND:20150318T040000Z DTSTAMP:20261011T152429Z UID:orq06aeu34g2tb5l8ma87agq8o@google.com CREATED:20150313T040606Z DESCRIPTION:Brian Boyle will give us an update on the Square Kilometre Arra y project\, particularly the recently completed process of re-baselining a nd the implications for Australia. LAST-MODIFIED:20150316T234104Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Brian Boyle (Australian SKA Director\, Department of Industry) "Squ are Kilometre Array (SKA) Update" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201124T000000Z DTEND:20201124T010000Z DTSTAMP:20261011T152429Z UID:elbp3ik3gg19719eqmo02c590g@google.com CREATED:20200929T071621Z DESCRIPTION:TBD LAST-MODIFIED:20201123T221106Z LOCATION:DLT and ZOOM 997 8534 1005 (host: Menon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Yixiao Zhou (RSAA) "End-of-Thesis Talk: Asteroseismology with 3D ma gneto-hydrodynamical simulations of stellar convection" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240912T010000Z DTEND:20240912T020000Z DTSTAMP:20261011T152430Z UID:82lr4hg2fnksbf7lfbj6v1luh0@google.com CREATED:20240417T012651Z DESCRIPTION:Since the watershed discovery of GW170817 - a binary neutron st ar merger with a definitive electromagnetic counterpart - there has been a great deal of hope that similar gravitational wave events identified by t he LIGO-Virgo-KAGRA experiments would yield similar exciting discoveries. Since 2017\, only one more binary neutron star merger has been identified: GW190425. Using this example\, we will study the process of gravitational wave detection: from candidate identification to localization to astrophy sical implications\, and how we associate GW events with EM counterparts. I'll delve into how we can learn more about the astrophysics of the most e xtreme neutron stars. I will show how hierarchical models can be applied t o gain both potentially fascinating and statistically robust insights into the compact object population detected via gravitational wave emission. LAST-MODIFIED:20240829T011114Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hayden Park) \nZoom: https ://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Fiona Panther (UWA) "The last neutron star merger: what can we lear n from GW190425?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200312T000000Z DTEND:20200312T010000Z DTSTAMP:20261011T152430Z UID:1597hsdos94l22mp8kvu3j2la0@google.com CREATED:20200227T050106Z DESCRIPTION:Physical properties of the interstellar medium (ISM) such as m etallicity\, ionisation parameter\, temperature\, density and pressure re gulate star-formation in galaxies\, and thus are the prime drivers of gala xy evolution. In order to understand how galaxies evolved through cosmic t ime\, it is important to study these properties better\, particularly at h igh redshift. I will talk about the high-redshift ISM studies we performed \, the challenges involved\, and the possible solutions. I will present ou r pilot study comparing new rest-frame UV and optical emission line nebul ar diagnostics\, for the first time\, to the brightest known lensed galaxy at cosmic noon followed by the full high-redshift sample. I will demonst rate the power of rest-frame UV spectra surveys when combined with these d iagnostics and unprecedented sensitivity of the upcoming space-based and l ate ground-based observatories. However\, the spatial resolution of these surveys might impact the accuracy of measuring the distribution of metals in galaxies. I will present a suite of synthetic Integral Field Unit (IFU) data cubes\, produced from simulations\, to quantify the said effect of s patial resolution. I will finish by demonstrating our novel method of corr ecting existing measurements of nearby galaxies\, for their insufficient s patial resolution and signal-to-noise levels. Our method will be crucial f or planning high-redshift IFU surveys with future telescopes. LAST-MODIFIED:20200310T001605Z LOCATION:Duffield Lecture Theatre (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ayan Acharyya (ANU) "Evolution of ISM conditions across the cosmic time - probing farther\, seeing better (End-of-Thesis Colloquium)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160811T010000Z DTEND:20160811T020000Z DTSTAMP:20261011T152429Z UID:8ggl3rh2sr9i310fb18183utn4@google.com CREATED:20160706T081111Z DESCRIPTION:DST Group has been actively involved in research into free spac e optical communications (FSOC) for over a decade\, and in this seminar I will present an overview of this programme. We have conducted studies of laser atmospheric propagation\, including numerical simulations and experi mental measurement campaigns. This has underpinned work conducted in conj unction with the University of South Australia on the development of forwa rd error correcting modems for the free space channel. We have developed novel FSOC systems based on modulating retroreflectors for applications wi th low size\, weight and power constraints. With support from the Royal A ustralian Navy\, we have developed a laser-based communications system to replace their 'flashing light' signalling. I will conclude with a look at our emerging research directions and collaborative opportunities. LAST-MODIFIED:20160803T235606Z LOCATION:Duffield Lecture Theatre (host: Francis Bennet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ken Grant (Defence Science and Technology Group) "Free Space Optica l Communications Research at DST Group" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250522T010000Z DTEND:20250522T020000Z DTSTAMP:20261011T152429Z UID:qsuhkhnd5e8a5a70glip89cpnc@google.com CREATED:20250226T045119Z DESCRIPTION:As First Light from the First Stars transforms the universe fro m Dark Ages into Cosmic Dawn\, the thermal history may be traced in redshi fted 21-cm from neutral hydrogen in the gas. Efforts to build radiometers to detect this faint signal are yielding results of significance to the theory\, thus constraining the starlight of the earliest galaxies and thei r impact on the gas. I will present the progression in astrophysical cons traints that have resulted from radiometers deployed in remote sites in In dia - at the Timbaktu collective\, in the trans-Himalayan plateau and floa ted on remote lakes. Progress in precision has led to building of a GINA N radiometer in CSIRO\, which has been trialed at the Inyarrimanha Ilgari Bundara\, the Murchison Radio-astronomy Observatory in remote radio-quiet Western Australia\, with an SKA-Low antenna element. LAST-MODIFIED:20250518T235607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Stu Wyithe) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ravi Subrahmanyan (CSIRO Space and Astronomy) "Radio discovery of C osmic Dawn" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170224T033000Z DTEND:20170224T035000Z DTSTAMP:20261011T152430Z UID:807n4mo1eb6s0f6h2as2tvbl6s@google.com CREATED:20170217T054606Z DESCRIPTION:The gender gap in the sciences is a global phenomenon\, and app ears to be the result of both discipline-driven and societal culture-drive n factors\, among others. Several initiatives towards gender parity in the sciences in India have occurred at the national\, governmental levels. Da ta for India suggest that the gender gap is due neither to lack of interes t in science nor to a lack of career goals in science among girls. The dri vers of the gap in India are explored using available empirical investigat ions and theoretical insights from gender studies. The implications for po licy will be discussed. LAST-MODIFIED:20170224T005106Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Prajval Shastri (Indian Institute of Astrophysics) "Interventions f or Gender Equity in Physics: Seeding or Hindering Cultural Change?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190507T010000Z DTEND:20190507T020000Z DTSTAMP:20261011T152429Z UID:dnchfsccbrlnmvov8vv27lgmt0@google.com CREATED:20190402T030111Z DESCRIPTION:Dust plays critical roles in many of the processes occurring in the interstellar medium and dust’s infrared emission serves as a tracer for the ISM and star formation from the nearby universe out to high redsh ift. While most of our knowledge of dust is built from observations of th e local area of the Milky Way\, it is clear that dust properties change dr amatically in low metallicity conditions which may be prevalent at high re dshift and in nearby dwarf galaxies. I will discuss what we know about ho w dust properties change with metallicity and how this can impact physical processes occurring in the ISM. I will also present new results studying low-metallicity dust in the Small Magellanic Clouds and other nearby gala xies. Finally\, I will describe some of the exciting prospects for learni ng more about low metallicity dust with new and upcoming observational fac ilities like the James Webb Space Telescope. LAST-MODIFIED:20190426T061108Z LOCATION:Duffield Lecture Theatre (host: Zhang) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Karin Sandstrom (University of California) "Interstellar Dust at Lo w Metallicity" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260922T050000Z DTEND:20260922T061500Z DTSTAMP:20261011T152430Z UID:e95urlqtpddqkurjbekqagoms8@google.com CREATED:20260803T010016Z DESCRIPTION:Our monthly Skillshare sessions provide an informal\, supportiv e\, and practical space for students and postdoctoral researchers to devel op and exchange research skills\, professional-development tools\, and eff ective workflows. The format is primarily focused on students\, in particu lar those enrolled in the ASTR8030 course Astronomy and Astrophysics Resea rch Skills. However\, everyone is very warmly invited to join and contribu te.\n\nSessions are held on selected Tuesdays from approximately 3:00-4:15 ish pm in the CSO Common Room. Depending on the topic\, they may include s hort introductions\, demonstrations\, panel discussions\, interactive exer cises\, or open-ended hands-on activities. LAST-MODIFIED:20260803T020019Z LOCATION:Zoom or CSO Common Room (host: Sven Buder and Melanie Kaasinen) \n Zoom: https://anu.zoom.us/j/89544552112?pwd=Bdoo5fgMVS2Ls6e3Fs0NSNk9OMpaXn .1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA Skillshare (RSAA) "Software Engineering 101" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200618T010000Z DTEND:20200618T013000Z DTSTAMP:20261011T152429Z UID:b27unl1276ofgpfjjov0ug9n0s@google.com CREATED:20200604T000604Z DESCRIPTION:The magnetic fields in interstellar medium (ISM) of spiral gala xies can be observationally studied by Faraday rotation measures (RM)\, wh ich depends on the thermal electron density and magnetic field strength pa rallel to the line of sight. The spatially intermittent structure of magne tic field and thermal electron density might affect the interpretation of RM observations. We aim to study the effect of structures in magnetic fiel d and electron density on the statistical properties of RM using numerical simulations. First\, we would generate idealized magnetic and electron de nsity structures (random ellipsoids in a triply periodic domain) and gener ate a mock RM map. We would then calculate the statistical properties of R M as a function of size of structures and angle between the magnetic field and electron density structure. Finally\, we would calculate RM propertie s from magnetohydrodynamic (MHD) simulations (as a function of Mach number \, which quantifies the compressibility of the medium) and then compare it with results obtained using idealized structures to constrain the propert ies of structures\, as imprinted in the RM map\, in MHD simulations. The p roject would inform us about the effect of structures on the RM and provid e an algorithm to convert observed statistical properties of the RM to phy sical size of magnetic and electron density structures in the ISM. Please see separate reminder email for zoom details. LAST-MODIFIED:20200612T015108Z LOCATION:ZOOM (host: Seta) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rhea Laverock (RSAA) "PhB talk: Magnetic and Electron Density Struc tures in the Interstellar Medium" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160726T010000Z DTEND:20160726T020000Z DTSTAMP:20261011T152429Z UID:vvvqjbvkt9t3kdnk5ng959uuc4@google.com CREATED:20160715T051105Z DESCRIPTION:Studies of data from the Fermi Gamma-Ray Space Telescope have r evealed new and striking features of the Milky Way\, from the giant struct ures known as the Fermi Bubbles to a spherical glow of bright gamma-ray em ission from around the Galactic Center. The latter has garnered great inte rest as a possible signal of annihilating dark matter\, but new analyses s uggest that it may instead be the first sign of an unexpected pulsar popul ation with unusual properties. I will discuss the techniques used to unvei l and study these signals\, and what they may reveal about the deep histor y of our Galaxy. LAST-MODIFIED:20160725T003604Z LOCATION:Duffield Lecture Theatre (host: Francis Bennet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tracy Slatyer (MIT) "Galactic Puzzles in the Gamma-Ray Sky" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170105T030000Z DTEND:20170105T040000Z DTSTAMP:20261011T152429Z UID:4fhbu0tb1rupg6cegtp18t59qg@google.com CREATED:20161209T022106Z DESCRIPTION:Radio astronomy is currently exploring an intriguing new phase space that probes the dynamic Universe on timescales of milliseconds. Rece nt development of sensitive\, high time resolution instruments has enabled the discovery of millisecond duration fast radio bursts (FRBs) and the er ratic rotating radio transients (RRATs). My thesis focusses on discovering these FRBs and understanding how we can exploit them as a cosmological pr obe of the intergalactic medium using RRATs as a test case. The class Fast radio Bursts encompasses a number of single pulses\, each unique in its o wn way\, hindering a consensus for their origin. The key to demystifying F RBs lies in discovering many of them in realtime in order to identity comm onalities. The recently upgraded UTMOST in Australia operating at 843 MHz\ , is undergoing a backend transformation to rise as a fast transient detec tion machine. Until 2015\, FRBs had been detected exclusively at 1.4 GHz. In my talk\, I will describe the Monte Carlo simulations I performed\, of a cosmological population of FRBs to predict the estimated FRB rate at UTM OST's's operating frequency scaling from the observed rate at 1.4 GHz. I w ill present the FRB surveys undertaken at UTMOST which yielded the first i nterferometric detections of FRBs and compare them to the expectations fro m the simulations. I will also talk about the method developed to potentia lly for the very first time\, map the intergalactic magnetic field\, using a recently discovered FRB. This method has enabled the determination of t he first ever rotation measures of 18 known RRATs. LAST-MODIFIED:20161227T102606Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Manisha Caleb (RSAA) "A pursuit of fast radio transients using the UTMOST and Parkes radio telescopes - End of Thesis Colloquium" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250219T030000Z DTEND:20250219T040000Z DTSTAMP:20261011T152429Z UID:0ubtrbc8aqocu9u7kc7mcsr47g@google.com CREATED:20250212T114607Z DESCRIPTION:Atmospheric distortions limit seeing from earth into space\, af fecting optical astronomy and optical communication to satellites. Adaptiv e optics can compensate these distortions using measurements from guide st ars. Bright natural guide stars are only available in a fraction of the sk y. Instead\, one can use lasers for creating artificial guide stars\, eith er by Rayleigh scattering in the atmosphere or using fluorescence from an atomic sodium layer in the mesosphere. Only latter allows full compensatio n of the atmospheric distortions and requires a high power narrow line wit h laser resonant with the D2 sodium transition (589.2 nm). Today\, most bi g telescopes use so-called 3rd generation sodium guide star lasers. These lasers use a master oscillator\, which is amplified in a Raman fiber ampli fier and then resonant frequency doubled delivering more than 20 W of opti cal output at 589 nm. In this presentation\, we will review the current st ate of guide star lasers\, their current use in astronomy as well as upcom ing applications such as optical communication. LAST-MODIFIED:20250212T114607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Elisa Jager) \nZoom: https ://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Armin Zach (Toptica) "Sodium Guide Star Lasers for Astronomy and Hi gh Power Fiber Amplifier for Free Space Optical Communication" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251106T000000Z DTEND:20251106T010000Z DTSTAMP:20261011T152430Z UID:1ndff5drsqgarbg86ogk0eitp4@google.com CREATED:20250902T070116Z DESCRIPTION:The Universe was born without magnetic fields\, yet we see dyna mically important magnetic fields threading galaxies young and old. While many processes could have seeded the first magnetic fields\, none of those initial fields resemble the coherent galactic fields we see today\; inste ad\, coherence has been generated over time. In my thesis I have studied h ow small-scale dynamos have shaped magnetic fields during the formation of the first galaxies and in subsequent galaxy mergers. Using direct numeric al simulations\, I have revealed how compressibility and shocks\, inherent to supersonic flows in the interstellar medium (ISM)\, modifies magnetic- field growth\, spectra\, and their coupling to the gas in which they are e mbedded. I have also implemented magnetic physics in the Quokka code\, Str omlo's own astrophysics code\, which will allow us to tackle the next part of the problem: when and how large-scale coherence emerges in galaxies! LAST-MODIFIED:20251102T061607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Neco Kriel (RSAA) "Simulating Magnetic Field Amplification and Stru cture Formation in Compressible Galactic Turbulence (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180502T010000Z DTEND:20180502T020000Z DTSTAMP:20261011T152429Z UID:pols77ctob3tgr344h1545mi68@google.com CREATED:20180424T021608Z DESCRIPTION:The energy balance sets the structure of the interstellar mediu m (ISM) phases\, which in turn control the processes of star-formation (SF ). We investigate the balance between the heating by stellar radiation\, a nd neutral gas cooling dominated by [CII] emission line. [CII] is typicall y the brightest far-IR emission line from star-forming galaxies\, and it h as been proven to be a useful SFR tracer\, both locally and at high redshi fts\, however\, with some vital caveats. Specifically\, we are interested wheather there are any changes in the efficiency of the photoelectric heat ing (PEeff)\, the dominant heating mechanism of the neutral gas\, that mig ht affect reliability of the [CII] as a SFR tracer. To address these issue s\, we have assembled a unique set of observations in two nearby galaxies\ , M31 and M51. Multi wavelength FUV-FIR photometric coverage enables a wel l constrained SED modelling. Key observations of [CII] emission at high\, 50pc\, resolution in five SF regions in M31 (Herschel)\, and the first ful ly mapped galaxy at ~650pc resolution in M51 (SOFIA)\, enable a local and a global studies. Finally\, we model individually resolved stars with 6 ba nd HST photometry down to spectral type F0 with PHAT survey in M31 using B EAST (Bayesian Extinction and Stellar Tool) for an independent measurement of the heating at smallest scales. A commonly used ratio [CII]/TIR (total IR emission)\, fails as a proxy for PEeff\, because the TIR measures all dust heating\, not just the FUV photons capable of ejecting electrons from dust grains (Kapala et al. 2017). We find [CII]/TIR to be strongly correl ated with UVatt/TOTatt (inferred from MAGPHYS SED fitting)\, indicating th at\, in M31 at least\, one of the dominant drivers for [CII]/TIR variation is the relative hardness of the absorbed stellar radiation field. We defi ne PEeff(UV)\, [CII]/UVatt which should be more closely related to the tru e PE efficiency\, which we find to be essentially constant (1.85 ± 0.8%) in all explored 700x700pc fields in M31\, regardless of the value of [CII] /TIR (varying by a factor of 3). I will present the above findings and the preliminary results of the [CII] - SFR relation\, and the PEeff(UV) on 65 0pc scales in M51. I will also explore environmental dependencies on those relations. LAST-MODIFIED:20180503T001607Z LOCATION:Duffield Lecture Theatre (host: Oh) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Maria Kapala (University of Capetown) "[CII] as a SFR tracer in M31 and M51: A ~constant photoelectric heating efficiency links [CII] 158 um with young stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191122T030000Z DTEND:20191122T033000Z DTSTAMP:20261011T152429Z UID:jht8busc858l738rd9cnqetvbs@google.com CREATED:20191022T233613Z DESCRIPTION:We're all familiar with geostationary satellite antennas – th e Foxtel dishes atop many rooftops that point to a fixed location in space . The AITC has a number of programs\, however\, that rely on our ability to interact with satellites that freely zip across the sky under the influ ence of a plethora of perturbing forces. Understanding these forces is th e first step to being able to predict where any of the 20\,000+ catalogued orbital objects are at any particular instant so we know where – and wh en – to point our telescopes at them. In this talk I’ll outline how s atellites move\, how we find them and the challenges and opportunities the y afford to our communications and space environment research programs. LAST-MODIFIED:20191022T233613Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:James Webb (RSAA/AITC) "AITC Series – Space is big\, satellites a re (comparatively) small… the joys of finding\, tracking\, and using th em!" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141204T000000Z DTEND:20141204T010000Z DTSTAMP:20261011T152430Z UID:flfil7odihigaf9ro67b0tb6lc@google.com CREATED:20141117T060341Z DESCRIPTION:It has been known only since 2010 that the nucleus of the Galax y launches two giant outflows into north and south Galactic hemispheres. D iscovered originally in Fermi gamma-ray telescope data and labelled the 'F ermi Bubbles'\, the polarized radio counterparts of these structures were discovered with the Parkes telescope in 2012. The origin of the Bubbles re mains enigmatic and controversial with many researchers favouring the idea that they were launched within the last few million years during an activ e period of the Galaxy's super-massive black hole. Our theoretical and obs ervational work makes us increasingly confident\, however\, that the Bubbl es were inflated\, over much longer timescales\, by the intense star-forma tion occurring around the SMBH. Whatever their origin\, the Bubbles repres ent an up-close-and-personal view of feedback from the nucleus to the Gala xy-at-large. I will present an important\, recent discovery we have made a bout the Bubbles: they contain giant shocks at heights of ~2 kpc above the plane. These shocks reveal themselves as huge linear structures in radio polarization\, microwave\, gamma-ray\, and H-alpha data. The shocks are si tes for cosmic ray acceleration. Emission from these cosmic rays explains the 'WMAP Haze' observed at microwave wavelengths around the Galactic cent re as well as the Bubbles' wider-scale radio polarization and gamma-ray em ission. These giant shocks may also be the dominant source of cosmic rays in the Galaxy-as-a-whole above energies of ~10^15 eV. LAST-MODIFIED:20250925T231024Z LOCATION:Duffield Lecture Theatre (host: David Nataf) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Roland Crocker (RSAA) "Unravelling the Milky Way's Giant Gamma-Ray and Radio Lobes" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141121T032000Z DTEND:20141121T033500Z DTSTAMP:20261011T152430Z UID:pmg19ooa6mdfdo8b7r1c8kbs50@google.com CREATED:20250925T231020Z DESCRIPTION:We use Integral Field Spectroscopic data from the Gemini Multi- Object Spectrograph to analyse the 3D kinematics\, ionization state\, temp erature and density of ionized gas in the "Green Bean" (GB) galaxy quasar ionization echo candidate J2240-0927. We model the emission line spectrum of each spaxel as a superposition of up to three Gaussian components and a nalyse the physical properties of each component individually. Two narrow components\, tracing the velocity fields of the disc and the ionized gas c loud\, are superimposed over the majority of the galaxy. A broader kinemat ic component is also ubiquitous across the galaxy disc. Fast shocks produc e hot\, dense\, turbulent\, [O III]-bright regions with large [N II]/Halph a and [S II]/Halpha ratios. The most prominent such spot is consistent wit h a radio jet shock-heating the interstellar medium. However\, the active galactic nucleus (AGN) is still responsible for > 82% of the galaxy's tota l [O III] luminosity\, confirming that J2240 is a quasar ionization echo. The ionized gas cloud has a strong kinematic link to the central AGN and i s co-rotating with the main body of the galaxy\, suggesting that it may be the remnant of a quasar-driven outflow. The extremely low space density o f GB galaxies suggests that they may be manifestations of normal but short -lived stages in the lives of quasar host galaxies. Detailed 3D spectrosco pic analysis of other GB galaxies will provide further insight into the ev olutionary history of this unique class of objects. LAST-MODIFIED:20250925T231020Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rebecca Davis (RSAA) "The Extended Emission Line Region of the "Gre en Bean" Galaxy SDSS J2240-0927: a quasar ionization echo illuminating the remnant of a quasar-driven outflow?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190417T010000Z DTEND:20190417T020000Z DTSTAMP:20261011T152429Z UID:5muukm98luhqc4kd1f8lv8u6nk@google.com CREATED:20190325T100611Z DESCRIPTION:All massive galaxies host a supermassive black hole - with mass es of millions to billions of times that of the Sun - in their centers. Th ese black holes act as the power engine of Active Galactic Nuclei (AGN)\, which can release tremendous amounts of energy into the surrounding medium \, potentially heating and/or ejecting the gas reservoirs of galaxies. AGN feedback and outflows have often been proposed as necessary ingredients f or the regulation of star formation in galaxies\, but the observational ev idence has been mixed. After a brief overview\, I will present observation al and numerical constraints on the fueling of black holes\, and on the ex tent to which they can change the fate of galaxies. I will then highlight findings from a multi-scale analysis of gas ionization and dynamics thanks to 3D spectroscopy with the VLT/MUSE instrument. Lastly\, I will conclude with a global view of black hole growth and feedback in galaxies\, includ ing major questions that remain open for new capabilities such as the Jame s Webb Space Telescope (JWST)\, and large galaxy survey experiments such a s DESI and Euclid. LAST-MODIFIED:20190409T055107Z LOCATION:CSO Common Room (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Stephanie Juneau (NOAO) "The Influence of Supermassive Black Holes on the Fate of Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190221T000000Z DTEND:20190221T010000Z DTSTAMP:20261011T152429Z UID:qkmn96bdqqdf5trbsmo64uu1jg@google.com CREATED:20181220T031117Z DESCRIPTION:After aLIGO detected the gravitational wave produced by mergers of binary black holes (BHs)\, researchers have aggressively studied the o rigin of the BHs with masses of the order of O(10) M_sun. In addition to a strophysical origins through evolutions of Pop.III stars\, one of the attr active candidates of those BHs should be Primordial Black Holes (PBHs). Th e PBHs can be produced in the early radiation dominated Universe due to s pherical collapses of regions which have a large density perturbation. I w ill review the current status of cosmological and astrophysical constraint s on PBHs with introducing my own latest bounds on PBHs in terms of polari zation of Cosmic Microwave Background photons (arXiv:1707.04206 [astro-ph. CO])\, cosmological bounds on evaporating PBHs (arXiv:0912.5297 [astro-ph. CO])\, Higgs phenomenology (arXiv:1708.02138 [hep-ph]) and so on. If time permitted\, I will mention cosmological accretions of baryon onto PBHs an d implications for a seed of Super-Massive BHs (in progress). LAST-MODIFIED:20181221T032115Z LOCATION:CSO Common Room (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kazunori Kohri (KEK) "Primordial Black Hole Cosmology" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220518T030000Z DTEND:20220518T040000Z DTSTAMP:20261011T152429Z UID:qdml9crtqr5vd5krglu36lflr4@google.com CREATED:20220517T003707Z DESCRIPTION:The first stars mark the transition from the cosmic dark ages t o the modern universe that we know today\, a universe that is filled with stars\, galaxies\, and heavy elements essential to life. The first stars stand out because of their pristine primordial initial composition and the ir pre-galactic formation environment. Their unique composition dramatica lly alter their evolution\, their structure\, the way they die as supernov ae\, and their resulting nucleosynthesis. The special circumstances under which these stars were formed also impacts their characteristic initial m ass distribution\, the initial mass function. Generally it is assumed tha t these stars\, on average\, were significantly more massive than present- day stars. No low-mass Population III star that could have survived to t he present day has ever been found. Some speculations exist that even sup ermassive primordial stars may have formed that laid the basis for superma ssive black holes in the centres of early galaxies including high-red shif t quasars. I will give an overview of the evolution and death of these fi rst stars and their supernova. I will also discuss nucleosynthesis signatu res as possible diagnostics that have survived to the present day. LAST-MODIFIED:20220517T003707Z LOCATION:DLT & ZOOM (host: Thomas Nordlander) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alexander Heger (Monash University) "Life and Death of the First St ars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190125T030000Z DTEND:20190125T032000Z DTSTAMP:20261011T152429Z UID:rtbdu9gs9nidrhd5cho088tklc@google.com CREATED:20181119T225615Z DESCRIPTION:We investigate the stellar population properties of passive spi ral galaxies in the CALIFA survey. Nine spiral galaxies that have NUV-r > 5 and no/weak nebular emission lines in their spectra are selected as pass ive spirals. They clearly lie in the domain of early-type galaxies in the WISE IR color-color diagram. We analyze the stellar populations out to one effective radius\, using the best-fitting model to the measured absorptio n line-strength indices in the Lick/IDS system. We find that stellar popul ations of the passive spirals span a wide range\, even in their centers\, and hardly show any common trend amongst themselves either. We compare the passive spirals with S0s selected in the same mass range. S0s cover a wid e range in age\, metallicity\, and [alpha/Fe]\, but stellar populations of the passive spirals are encompassed in the spread of the S0 properties. H owever\, the distribution of passive spirals are skewed toward higher valu es of metallicity\, lower [alpha/Fe]\, and younger ages at all radii. Thes e results show that passive spirals are possibly related to S0s in their s tellar populations. We infer that the diversity in the stellar populations of S0s may result from different evolutionary pathways of S0 formation\, and passive spirals may be one of the possible channels. LAST-MODIFIED:20190115T002606Z LOCATION:CSO Common Room (host: Oh) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mina Pak (KASI and UST) "Stellar populations of nine passive spiral galaxies from the CALIFA survey" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251114T030000Z DTEND:20251114T033000Z DTSTAMP:20261011T152430Z UID:sn1hmk8jvubs58agq0h25agmto@google.com CREATED:20251110T022108Z DESCRIPTION:A discussion of plans for the reopening of the MSO Visitor Cent re and Cafe. LAST-MODIFIED:20251110T022108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Brad Tucker (RSAA) "Plans for the Visitor Centre and Cafe" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231204T023000Z DTEND:20231204T033000Z DTSTAMP:20261011T152429Z UID:qa820pfue650ds2du3omk9fj80@google.com CREATED:20231201T063607Z DESCRIPTION:The Optical Commnications team in AITC will detail their ongoin g development of the newly constructed Optical Ground Station at Mt Stroml o. Optical communications provides higher data rates than traditional radi o frequencies and smaller resource consumption. The technology will unlock high bandwidth communications to deep space (the Moon\, Mars and beyond). Instrument development in this project is being performed in collaboratio n with NASA and aims to support the Optical to Orion (O2O) mission on Arte mis II\, the next crewed flyby of the Moon. Visiting collaborators from NA SA heading up the O2O program will also present on some of their work and pioneering advancements in the field. There will be a catered afternoon te a to follow in Possum Hall. LAST-MODIFIED:20231201T063607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBC) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Francis Bennet and Steven Horowitz (RSAA\, NASA Goddard Space Fligh t Center) "Joint Efforts of AITC and NASA in developing Lunar Optical Comm unications" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180227T000000Z DTEND:20180227T010000Z DTSTAMP:20261011T152429Z UID:g0sf349sgrbvoi9a56pba3ppr0@google.com CREATED:20180127T080610Z DESCRIPTION:We infer the star formation rates in dark matter halos at diffe rent redshifts from halo merger histories expected in a Lambda CDM cosmolo gy using Bayesian inference and Bayes ratios to restrict the model complex ity\, constrained to match the observed stellar mass/luminosity functions of galaxies at different redshifts and the local cluster galaxy luminosity function\, which has a steeper faint end than that of field galaxies. Th e only other assumptions that we make are that the star formation rate of central galaxies depends on the halo mass and redshift and that when a gal axy becomes a satellite its star formation rate is quenched exponentially and it can eventually merge with the central galaxy on a dynamical frictio n timescale. We find that 1) the star formation in the central galaxies of high mass halos (>10e12) has to be boosted at high redshift beyond what i s expected from a simple scaling of the dynamical time\; 2) below z=2 the star formation in halos below 1e11 must be quenched\, which is not directl y expected in standard stellar feedback models and is most easily explaine d by some form of preheating\, and implies that there is a significant old stellar population in present-day dwarf galaxies with M_star < 10e8 and s teep slopes for the high redshift stellar mass and star formation rate fun ctions 3) the stellar mass of galaxies assembles in one of three ways depe nding on halo mass: > 1e12 the galaxies assemble through mergers and shoul d hence have a spheroidal morphology and between 1e11 and 1e12 (e.g MW) it assembles slowly and at z>2 has less than 5% of its mass in place\, which has extreme observational consequences. LAST-MODIFIED:20180225T011605Z LOCATION:Duffield Lecture Theatre (host: Battisti) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Neal Katz (UMass) "Letting the Data Speak for Themselves: What Obse rvations Tell Us About" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151001T010000Z DTEND:20151001T020000Z DTSTAMP:20261011T152429Z UID:r3v050u2jvvts9go1b7p7kdhj8@google.com CREATED:20150924T141604Z DESCRIPTION:ZFOURGE and ZFIRE are deep near-IR surveys that track how galax ies assemble over cosmic time. ZFOURGE identifies approximately 30\,000 ga laxies up to redshifts of z~7 using a custom set of medium-band near-IR fi lters that provide high precision photometric redshifts. ZFIRE selects gal axies from ZFOURGE for spectroscopic follow-up with Keck/MOSFIRE to measur e how baryons cycle between stars\, winds\, and the Inter-Stellar Medium a t z~2. Here I summarize our results that include stellar mass functions at 0.5 1 0^6 stars\, and Gaia mapping >10^9 stars in the Galaxy\, we have learned t hat the inner stellar halo is dominated by the accretion of Gaia Enceladus . With the richness of data at hand\, there are a myriad of ways these acc reted stars have been selected: from kinematics\, to dynamics\, to even ch emistry. In this work\, we explore these different selections and their ef fects on the inferred progenitor properties using APOGEE DR17 and Gaia dat a. Specifically\, we investigate the selections made in eccentricity\, E-L z\, Vphi-Vr\, Jr-Lz\, and [Mg/Mn] vs [Al/Fe] and quantify the overlap betw een and contamination in each selection method. To ultimately understand t heir efficacy\, we apply similar selections in Milky Way like galaxies wit h a known Gaia Enceladus progenitor in the AURIGA hydrodynamical simulatio ns and similarly infer progenitor properties. Through this\, we are able t o understand which selection is best to recover true Gaia Enceladus stars in terms of completeness and purity\, how much contamination from other ac cretion events and from in-situ population is present depending on the met hod\, and ultimately which selection is best for inferring Gaia Enceladus mass. LAST-MODIFIED:20221205T230310Z LOCATION:DLT & ZOOM (host: Lindsey Oberhelman) \nZoom: https://anu.zoom.us/ j/99785341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Andreia Carrillo (Durham University) "Can we really pick and choose ? Benchmarking various selections of accreted halo stars in observations w ith simulations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150804T010000Z DTEND:20150804T020000Z DTSTAMP:20261011T152429Z UID:apng84nh785mdlf0c8riv3t4b4@google.com CREATED:20150727T104607Z DESCRIPTION:Some astronomers ignore low-mass stars because they aren't very bright. However\, stars with initial masses between about 0.8 Msun and 8 Msun (AGB stars) play an important role as the main site of the slow neutr on capture (s-)process\, which produces roughly half of the elements heavi er than iron. In this talk\, I will present results from my PhD thesis whi ch explores several topics related to AGB stars and the s-process. The foc us is on comparing theoretical models with observations the literature on planetary nebulae\, post-AGB stars\, and globular cluster stars. From thi s work\, we will see have a better understanding of AGB nucleosynthesis\, the chemical evolution of globular clusters\, and the properties of helium -rich stars. LAST-MODIFIED:20150803T071605Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Luke Shingles (RSAA) "Final Thesis Talk: Neutron-Capture Nucleosynt hesis and the Chemical Evolution of Globular Clusters" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180802T010000Z DTEND:20180802T020000Z DTSTAMP:20261011T152429Z UID:dol86qcucjs29ci09d3qna2nu4@google.com CREATED:20180612T061611Z DESCRIPTION:The Planck Era cannot be given a precise mathematical descripti on until the full theory of quantum gravity is available. However\, some a spects of the physical state of the Planck Era can be revealed by order of magnitude considerations which also have implications for the low entropy of the very early universe. LAST-MODIFIED:20180720T134609Z LOCATION:Duffield Lecture Theatre (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Peter Riggs (Research School of Physics and Engineering) "On The Ph ysical State of the Universe in the Planck Era" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170302T000000Z DTEND:20170302T010000Z DTSTAMP:20261011T152430Z UID:a2icng5o35omjn5kj2o6ddort8@google.com CREATED:20170123T204110Z DESCRIPTION:New spectroscopic surveys now allow to measure the detailed abu ndance and ages of stars throughout the Galactic disk. Having this informa tion star‐by‐star\, including ages\, allows a qualitatively exploratio n of the evolution of the Milky Way's stellar body: which processes set th e overall radial profile of the disk\, which the present-day orbital of an y star? To which extent is the disks' thickness a birth property\, as opp osed to a consequence of subsequent heating or flaring. How much formation memory does the Milky Way's disk retain? I will aim at providing (current ) answers to these questions\, and sketch out briefly my view of what is y et to come in the age of Gaia data. LAST-MODIFIED:20170215T225611Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Hans-Walter Rix (Max Planck Institute for Astronomy) "How the Milky Way Shaped Its Disk" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201104T230000Z DTEND:20201104T231500Z DTSTAMP:20261011T152429Z UID:glnlo9u69gbllvfccm9fuookeo@google.com CREATED:20201025T225107Z DESCRIPTION:A 1.772GHz Phase Locked Loop (PLL) Radio Frequency Synthesiser has been designed and built for sodium laser guide star adaptive optics (L GS AO) applications include Space Situational Awareness (SSA) and Satellit e and Debris Tracking. The PLL has been designed to be used in combination with an electro-optic modulator (EOM) to produce the sodium D2b emission sideband from a monochromatic laser operating at the sodium D2a emission f requency. LAST-MODIFIED:20201103T011605Z LOCATION:ZOOM 997 8534 1005 (host: Martinez) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:David Ashworth (RSAA) "Honours project presentation: 1.772GHz Phase Locked Loop Radio Frequency Synthesiser For Sodium Laser Guide Star Photo n Return Optimisation" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221124T000000Z DTEND:20221124T003000Z DTSTAMP:20261011T152429Z UID:bua51l2pqno4tuele0p7nqe47k@google.com CREATED:20220926T055116Z DESCRIPTION:Bars are large triaxial structures in the centers of galaxy dis ks\, having sizes varying from a few 100 pc to several kpc. Nearly 2/3rd o f all disk galaxies in our local universe are barred. Bars play a crucial role in galaxy formation\, shaping the structure of a galaxy’s dark matt er halo\, bulge\, and disk and influencing its star formation history. De spite decades of research\, the mechanism of bar formation in galaxies is still a subject of debate. From isolated galaxy simulations we have gained valuable insight to how bars form and evolve. However\, bars in the Unive rse evolve in galaxies in highly complex environments with multiple satell ite interactions\, mergers\, gas accretion events\, star-formation and gas in-fall to the central supermassive blackhole (SMBH)\, while simultaneous ly interacting with their dark matter halo. Investigating bar formation an d reproducing their observed properties in cosmological simulations is imp ortant for understanding galaxy formation\, as well as understanding the f ormation of galactic bars. In this talk\, I will present our work with the zoomed-in cosmo-hydro simulation FIRE-2 (Feedback in Realistic Environmen ts). We study 13 high resolution MW-mass galaxies from FIRE2 to first ask: Do the FIRE galaxies have bars? If so\, how do bars form and when does ba r formation fail? We find examples where bars form due to satellite intera ctions and others where bars form secularly in the disk. The stellar feedb ack prescription in FIRE2\, which affects starburst and gas dynamics\, and the lack of blackhole feedback to mitigate the gas in the galaxy center\, together make the disk kinematically hot\, such that bars are shorter tha n the MW-bar\, rotate faster\, and are mostly short-lived. Using predictio ns from controlled simulations for varied dark matter and stellar distribu tions at the galaxy center\, we explain the morphological differences betw een the bars in FIRE2 and TNG50 and connect them to differences in the phy sics implementations of the two codes. In addition to known influences on bar formation such as mergers and the mass ratio of stellar to dark matter in the inner galaxy\, we argue that the burstiness of stellar feedback pl ays a crucial role in bar formation. In the end\, I will touch upon some other works I have been involved with\, to study the dark matter halo prop erties using the baryonic disk properties using N-body and cosmological si mulations. LAST-MODIFIED:20221116T011111Z LOCATION:DLT & ZOOM (host: Neco Kriel) \nZoom: https://anu.zoom.us/j/997853 41005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sioree Ansar (Indian Institute of Astrophysics) "Bar Formation and Destruction in the FIRE-2 Simulations." TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160728T010000Z DTEND:20160728T020000Z DTSTAMP:20261011T152429Z UID:tst40p1opabfo958eicts43qi8@google.com CREATED:20160614T064613Z DESCRIPTION:TBD LAST-MODIFIED:20160725T003605Z LOCATION:Duffield Lecture Theatre (host: Francis Bennet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anna Zovaro\, Michael Copeland and Elliott Thorn (RSAA) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260210T000000Z DTEND:20260210T010000Z DTSTAMP:20261011T152430Z UID:1phd3cqfgip0r92b7net4c1s20@google.com CREATED:20251203T021610Z DESCRIPTION:ALMA and JWST are at the forefront of a transformative era in o ur understanding of galaxy formation and evolution. These observatories of fer unprecedented high-angular-resolution capabilities\, enabling a multi- phase view of the interstellar medium (ISM)\, the spatial distribution of stars within galaxies\, and new avenues to robustly constrain the properti es of dark matter through galaxy dynamics. In this talk\, I will present h ow recent high-resolution observations from ALMA and JWST are challenging our current view of the physical mechanisms that shape the structure and d ynamics of galaxies at z > 1\, forcing a revision of our theoretical frame work. I will then briefly highlight how these results provide insights int o the assembly pathways of present-day early-type galaxies at z = 0. LAST-MODIFIED:20260202T005607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Melanie Kaasinen) \nZoom: https://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Francesca Rizzo (U. Groningen) "A Transformative era for galaxy dyn amics at high redshift: insights from ALMA and JWST" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261020T000000Z DTEND:20261020T010000Z DTSTAMP:20261011T152430Z UID:d60aod7d5pg0ofucb23r5gok58@google.com CREATED:20260605T021628Z DESCRIPTION:Research at the intersection of astrophysics and Indigenous ast ronomy has rapidly accelerated over the last two decades. But during this time\, motivations\, approaches\, and methods have shifted and evolved. We are now seeing astronomers\, Elders\, and those who walk in both worlds c ollaborate in ways that are mutually beneficial by showcasing the scientif ic achievements of Aboriginal and Torres Strait Islander people that were not previously recognised while altering the way we conduct astrophysics r esearch\, addressing pressing issues of who benefits\, who is allowed to p articipate\, and how this knowledge is shared and applied. In this talk\, Duane Hamacher will discuss how these worlds are working together and what this means for the future of astronomy. LAST-MODIFIED:20260915T030011Z LOCATION:Zoom or Duffield Lecture Theatre (host: TBC) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Duane Hamacher (U. Melbourne) "Innovation at the cultural interface of Indigenous Knowledge and Astrophysics" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191101T030000Z DTEND:20191101T033000Z DTSTAMP:20261011T152429Z UID:4qamitu7p8hop1am08t58vgvcs@google.com CREATED:20191004T042614Z DESCRIPTION:MAVIS just passed its conceptual design mid term review. During the past eight month since the start of the conceptual design phase\, the international MAVIS team came up with a baseline design that fulfils the ambitious instrument requirements: provide both an imager and a spectrogra ph with diffraction limited images down to 450nm and over a field of view of 30x30 arcsec. Numerical simulations and optical design fed trade-off st udies that eventually resulted in the baseline design. We will present a s napshot of the MAVIS current status\, including programmatic\, performance \, science\, funding and the future of MAVIS. LAST-MODIFIED:20191024T031608Z LOCATION:Duffield Lecture Theatre (host: Zhang) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Francois Rigaut & David Broderick (RSAA/AITC) "AITC Series - MAVIS status update: going strong" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191122T030000Z DTEND:20191122T033000Z DTSTAMP:20261011T152429Z UID:p04q8bo8mainhtcq2p4p7emers@google.com CREATED:20191022T050511Z DESCRIPTION:We're all familiar with geostationary satellite antennas – th e Foxtel dishes atop many rooftops that point to a fixed location in space . The AITC has a number of programs\, however\, that rely on our ability to interact with satellites that freely zip across the sky under the influ ence of a plethora of perturbing forces. Understanding these forces is th e first step to being able to predict where any of the 20\,000+ catalogued orbital objects are at any particular instant so we know where – and wh en – to point our telescopes at them. In this talk I’ll outline how s atellites move\, how we find them and the challenges and opportunities the y afford to our communications and space environment research programs. LAST-MODIFIED:20191022T050511Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:James Webb (RSAA/AITC) "AITC Series – Space is big\, satellites a re (comparatively) small… the joys of finding\, tracking\, and using th em!" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180906T010000Z DTEND:20180906T020000Z DTSTAMP:20261011T152430Z UID:9ogoidutv11gf7mq27nf8ta3pc@google.com CREATED:20180822T015206Z DESCRIPTION:Key information about the formation and evolution of galaxies c an be obtained from the diffuse stellar component that surrounds galaxies and clusters\, and recent studies (e.g.\, Morishita et al\, 2017\; Merritt et al\, 2016)\, have provided some insight on the formation and evolution of these structures in different environments. However\, conclusions are still limited by the surface brightness detection limit and the size of th e samples in observations. Numerical simulations hence provide an excellen t complementary tool to track the evolution of these structures in a cosmo logical context. Using a new\, improved version of the 6-D halo finder VEL OCIraptor\, we measure and characterise the diffuse\, Intra-Halo Stellar C omponent (IHSC) of halos in a wide dynamic range\, from MW-like halo masse s to galaxy clusters\, in state-of-the-art simulations of galaxy formation (Horizon-AGN\, EAGLE and Illustris). This is the first time that such mea surement is possible in such a wide dynamic range. In this talk I will be presenting the simulation predictions throughout cosmic time and what we c an learn of the build-up of galaxies and halos from their IHSC. LAST-MODIFIED:20180827T084106Z LOCATION:Duffield Lecture Theatre (host: Zerjal) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rodrigo Canas (ICRAR UWA) "Diffuse stellar component in state-of-th e-art simulations of galaxy formation" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191122T030000Z DTEND:20191122T033000Z DTSTAMP:20261011T152429Z UID:sg1ibk5im2j8j0nlf0kbnmdog0@google.com CREATED:20191023T052111Z DESCRIPTION:We're all familiar with geostationary satellite antennas - the Foxtel dishes atop many rooftops that point to a fixed location in space. The AITC has a number of programs\, however\, that rely on our ability to interact with satellites that freely zip across the sky under the influen ce of a plethora of perturbing forces. Understanding these forces is the first step to being able to predict where any of the 20\,000+ catalogued o rbital objects are at any particular instant so we know where - and when - to point our telescopes at them. In this talk I'll outline how satellite s move\, how we find them and the challenges and opportunities they afford to our communications and space environment research programs. LAST-MODIFIED:20191024T031612Z LOCATION:Duffield Lecture Theatre (host: Monty) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:James Webb (RSAA/AITC) "AITC Series - Space is big\, satellites are (comparatively) small... the joys of finding\, tracking\, and using them! " TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141219T030000Z DTEND:20141219T032000Z DTSTAMP:20261011T152430Z UID:lih1tafidnaah2g4jfpcs7v8p0@google.com CREATED:20141117T060343Z DESCRIPTION:The properties of the midplanes of planet-forming protostellar disks remain largely unprobed by observations due to the high optical dept h of dust and commonly observed molecules. However\, rotational emission l ines from rare molecules may have optical depths near unity in the vertica l direction\, so that the lines are strong enough to be detected\, yet rem ain transparent enough to trace the disk midplane. In this talk\, I will p resent a chemical evolution model of an MRI-active T-Tauri disk. The optic al depths of low-order rotational lines of C17O are around unity\, which s uggests it may be possible to see into the disk midplane using C17O. With our computed C17O/H2 abundance ratio\, such ALMA observations would provid e estimates of the disk masses by measuring the intensity of gas emission. LAST-MODIFIED:20141119T225629Z LOCATION:Duffield Lecture Theatre (host: Tiantian Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mo (Emma) Yu (University of Texas at Austin) "Probing planet nurser ies with rare CO isotopologues" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191217T000000Z DTEND:20191217T010000Z DTSTAMP:20261011T152429Z UID:bh66so5t1f48g7eeso11l72q4o@google.com CREATED:20191106T112117Z DESCRIPTION:In this talk\, I will go through a brief history in the field o f ultracold atomic experiments before leading into the work I did during m y PhD at Swinburne. This work involved the use of Bragg spectroscopy to me asure the dynamic properties of unitary Fermi gases. I will also cover som e of the current and future applications for ultracold atom experiments. LAST-MODIFIED:20191210T032605Z LOCATION:Duffield Lecture Theatre (host: Pingel) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Marcus Lingham (RSAA/AITC) "Cold atoms\, Fermi gases\, and Bragg sc attering" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241025T030000Z DTEND:20241025T040000Z DTSTAMP:20261011T152429Z UID:jv86abhfer3urcbq9bm68gbboo@google.com CREATED:20241024T030108Z DESCRIPTION:This cross-disciplinary collaboration between the College of Bu siness and Economics (CBE) and AITC/RSAA is focused on improving operation al efficiency for instrumentation projects. As part of the CBE Internship Program\, AITC has welcomed three master’s students -- Belinda\, Simant\ , and Tyra -- since July 25\, 2024. Their primary objective is to map and analyse current workflows in critical areas such as project management\, o pto-mechanical engineering\, and the integration of lessons learned from p ast projects. Through close engagement with key staff members\, the studen ts have made significant progress in identifying opportunities to streamli ne our processes\, ultimately contributing to more efficient and innovativ e astronomical research. Join us for a series of talks where they will pre sent their findings\, which would contribute to informing and refining our technical approaches in future projects. Presentations are as follows: Qi nqi Gu (Belinda): Project Management workflow mapping: map a project from the start to the end\; Simant Gupta: Engineering workflow mapping for opto -mechanics\; Xinyi Xie (Tyra): lessons learned process mapping. LAST-MODIFIED:20241024T030108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Jenny Jiang) \nZoom: https ://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Xinyi Xie (Tyra)\, Qinqi Gu (Belinda) and Simant Gupta (AITC/RSAA) "CBE Internship Program-AITC Placement -- Final presentations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221028T000000Z DTEND:20221028T010000Z DTSTAMP:20261011T152429Z UID:m3806lgso1m6n4al4n5lgfrtr0@google.com CREATED:20221017T025110Z DESCRIPTION:Accurate predictions of the physics of interstellar medium are vital for understanding galaxy formation and evolution. Modeling photoioni zed regions with complex geometry produces realistic ionization structures within the nebulae\, providing the necessary physical predictions to inte rpret data. 3D photoionization codes built with Monte Carlo techniques pro vide powerful tools to produce the ionizing radiation field with fractal g eometry\, which includes the regions ionized by both stellar and diffuse p hotons. In this talk\, we will present a new self-consistent three-dimensi onal photoionization code -- Messenger Monte-Carlo MAPPINGS V (M^3)\, whic h is designed for modeling nebulae in arbitrary three-dimensional geometri es. We will present nebula models with complex geometries created by M^3\, and will further show how nebular geometry influences the ionizing radiat ion field and emission-line ratios. Our research has important implication s for studies of emission-line behaviors in the era of large IFU surveys a nd JWST. LAST-MODIFIED:20221027T120607Z LOCATION:DLT & ZOOM (host: Neco Kriel) \nZoom: https://anu.zoom.us/j/997853 41005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Yifei Jin (RSAA) "Modeling nebula with the next generation photoion ization code." TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261006T000000Z DTEND:20261006T010000Z DTSTAMP:20261011T152430Z UID:hg7qv7bj0fjt5ptb69a6a187mc@google.com CREATED:20260605T021626Z DESCRIPTION:I'll talk about the discovery of odd radio circles (ORCs) with ASKAP and present what we know about their properties and possible formati on mechanisms. Since our understanding of ORCs is still evolving\, questio ns and ideas are welcome. I will take this opportunity to also present oth er science highlights from my recent work\, including the Corkscrew Galaxy and a huge hour-glass outflow from a nearby galaxy. LAST-MODIFIED:20260923T120007Z LOCATION:Zoom or Duffield Lecture Theatre (host: Tomasz Rozanski) \nZoom: h ttps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Baerbel Koribalski (CSIRO) "Odd Radio Circles - what are they?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150327T030000Z DTEND:20150327T032000Z DTSTAMP:20261011T152429Z UID:447cu0qnqg05u2nv2hgubsvu9g@google.com CREATED:20150323T062606Z DESCRIPTION:Snapshot Supernova\, a collaboration between Skymapper\, Zooniv erse and BBC Stargazing Live\, is a recent citizen scientists project wher e Zooites and BBC viewers were asked to scan for supernova candidates in S kyMapper data and the candidates were then followed up using the NTT as pa rt of the PESSTO survey. The program successfully engaged the public and b rought lots of excitement and activity in the UK and world wide. Thanks to the amazing efforts of our volunteers\, we managed to discover four confi rmed supernovae within the first three days and more discoveries are still being made. We will take you behind the scenes and reflect on what we hav e learned (a lot) through this project. LAST-MODIFIED:20150323T062606Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Richard Scalzo and Fang Yuan (RSAA) "Snapshot Supernova" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181128T220000Z DTEND:20181129T060000Z DTSTAMP:20261011T152429Z UID:rinfa876j9mi9tnp2i9mop76c0@google.com CREATED:20180822T015208Z DESCRIPTION:This is the annual christmas seminars at Mount Stromlo. Student s from RSAA and elsewhere flock to the mountain to share their research wi th others. Invited talks from members of RSAA will also feature. LAST-MODIFIED:20181117T102111Z LOCATION:CSO Common Room (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Student Christmas Seminars (RSAA) "Student Christmas Seminars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190801T010000Z DTEND:20190801T020000Z DTSTAMP:20261011T152429Z UID:7psfctima9aljar9uq275f4md0@google.com CREATED:20190703T060508Z DESCRIPTION:Jupiter and Saturn played an important role opening gaps and fo rming dust traps in the protosolar accretion disk. This is reflected in th e distribution of chondrules and calcium-aluminum-rich inclusions (CAIs) i n chondritic meteorites. CAIs are almost exclusively present in chondrites that accreted in the outer Solar System\, and isotopic fingerprints show that chondrules were transported to the outer Solar System\, but no outer Solar System chondrules returned to the inner Solar System. A dust trap ca n only stop particles above a certain size\, while small particles flow th rough the trap together with the gas. Using a suite of simulations of the protosolar disk including gas\, dust\, and planets advanced for up to 50\, 000 Jupiter orbits\, I investigate the efficiency of planetary dust traps for different physical conditions. These models are compared to cosmochemi cal evidence from a systematic search for CAIs using electron microscope s cans of the ordinary chondrite NWA5697. Combining models and data gives ne w insight into the architecture of the young Solar System\, and novel cons traints on the gas surface density in the protosolar disk. Furthermore\, I show having Jupiter and Saturn initially in a 3:2 resonance\, as expected in the Nice II model\, is difficult to reconcile with the CAI size cut-of f in NWA5697. LAST-MODIFIED:20190703T060508Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Troels Haugbølle (University of Copenhagen) "Probing the protosola r disk using dust filtering of the gas giants in the early Solar System" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181109T030000Z DTEND:20181109T032000Z DTSTAMP:20261011T152429Z UID:nir9d1tldgn1ptah2ct4ak7atg@google.com CREATED:20181017T030106Z DESCRIPTION:Turbulence is a major problem in astronomy\, limiting telescope resolution and the ability to resolve small\, distant objects. However\, current efforts to minimise this turbulence focus on the turbulence in the atmosphere\, discounting the turbulence inside the telescope dome. Here\, we present an instrument that can measure turbulence inside the telescope dome\, while also separating out vibrations caused by the telescope mount and related instruments. With this information\, astronomers and telescop e dome operators will be able to get a better understanding of the exact c onditions in their dome so that they can minimise the inside seeing. LAST-MODIFIED:20181030T233107Z LOCATION:Duffield Lecture Theatre (host: Zerjal) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jonah Hansen (AITC) "Dome Seeing Probe: An instrument to measure op tical turbulence inside an observatory dome." TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221011T000000Z DTEND:20221011T010000Z DTSTAMP:20261011T152429Z UID:iat63705qfepuvvv9h59cjoqec@google.com CREATED:20220830T015112Z DESCRIPTION:Molecular gas is the fuel for star formation in galaxies. Using observations from the mm-Wave Interferometric Survey of Dark Object Masse s (WISDOM) survey\, that spatially resolve (1-30 pc) individual molecular clouds across the Hubble sequence\, we reveal a clear dependence of the na ture of the molecular interstellar medium of galaxies on Hubble type\, and present a simple diagnostic of cloud formation. In particular\, we highli ght the shortcomings of the usual virial approach to clouds as self-gravit ating objects\, and stress the importance of the external galactic potenti al and in-plane shear to regulate the dynamical states of clouds. We also introduce a simple but powerful cloud-cloud collision formalism that accou nts for the cloud properties in both nearby and high-redshift systems. Fin ally\, we discuss the impact of these different mechanisms on the star for mation efficiency of the clouds and thus the quenching of star formation\, particularly in galaxy nuclei and spheroids (morphological quenching). LAST-MODIFIED:20220830T015112Z LOCATION:DLT & ZOOM (host: TBD) \nZoom: https://anu.zoom.us/j/99785341005?p wd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Martin Bureau (University of Oxford) "WISDOM: Molecular cloud prope rties and star-formation quenching" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170103T000000Z DTEND:20170103T010000Z DTSTAMP:20261011T152429Z UID:v7sfjhl9mei0dks21itt3bqqhc@google.com CREATED:20161107T004614Z DESCRIPTION:The motivation of this research came from a desire to accuratel y trace the underlying stellar distributions of low mass irregular galaxie s in the Local Volume and utilize the derived properties in various avenue s of research. To this effect\, deep H-band surface photometry and analysi s of 40 Local Volume galaxies was performed\, a sample primarily composed of dwarf irregulars in the Cen A group\, obtained using the IRIS2 detector at the 3.9m Anglo- Australian Telescope. The imagery probes to a surface brightness of 25 mag per square arcsec\, reaching a 40 times lower stellar density than the Two Micron All Sky Survey (2MASS) which had insufficient image depth to study dwarf galaxies in the NIR. Given available evidence in the literature\, and from analysis of the NIR imagery it was suspected that the structural properties of irregular galaxies were similar to othe r dwarf sub-types. I tested this suspicion through structure-luminosity re lationships for the low mass irregulars in the sample and dwarf elliptical s and spheroidal galaxies obtained from other catalogues. I demonstrate th at a significant fraction of the Local Volume dwarf irregular population h ave underlying structural properties similar to both Local Volume and Virg o Cluster dwarf ellipticals. Spatially resolved Hi studies of dwarf galax ies have provided a wealth of precision data. However these high quality r esolved observations are only possible for handful of dwarf galaxies in th e Local Volume. Future Hi surveys are unlikely to improve the current situ ation. I therefore explored a method for estimating the surface density of the atomic gas from global Hi parameters\, which are conversely widely av ailable. LAST-MODIFIED:20161230T051105Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tye Young (RSAA) "Physical Properties of low mass Galaxies in the L ocal Volume - End of Thesis Colloquium" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150402T000000Z DTEND:20150402T010000Z DTSTAMP:20261011T152429Z UID:lccas7j7dvs7o01n8gmo9v1fmo@google.com CREATED:20150303T003618Z DESCRIPTION:The upper limit to stellar masses is unclear\, as is the relati ve importance of 'nature' (stellar physics) and 'nurture' (formation envir onment) to the limit. I will show that quasar disks may form stars with m asses much larger than in giant molecular clouds. This encourages a re-exa mination of the limits imposed by stellar physics. We have studied pulsat ional instabilities of modern solar-metallicity models up to 938 solar mas ses. Despite some uncertainties in the linear growth rate\, we conclude th at these modes saturate nonlinearly at small and harmless amplitudes. Vigo rous\, optically thick winds driven by the Rosseland-mean opacity near 100 \,000 K are more likely to limit the main-sequence lifetime. LAST-MODIFIED:20150327T044609Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jeremy Goodman (Princeton University) "Very Massive Stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260604T013000Z DTEND:20260604T023000Z DTSTAMP:20261011T152430Z UID:so0tje3m3f9vkklin3bcpqvgek@google.com CREATED:20260527T013423Z DESCRIPTION:I will give a < 30-minute talk introducing the After Sloan-V (A S5) Survey. This is a next-generation dual-hemisphere spectroscopic progra m set to address major questions in astrophysics. Using optical and near-i nfrared instruments spanning a range of spectral resolutions\, AS5 is desi gned to study both dynamic astrophysical phenomena and the structure and e volution of galaxies. Its science goals include characterising transient a nd variable phenomena across the sky\, mapping the central and far side of the Milky Way\, resolving the interplay between stars and gas in galaxies \, and uncovering the origins of the chemical elements. These goals are pu rsued through four complementary survey components: the Dynamic Universe E xplorer (DUE)\, Hidden Galaxy Explorer (HGE)\, Local Volume Mapper 2 (LVM2 )\, and Atomic Genesis Explorer (AGE). LAST-MODIFIED:20260527T013423Z LOCATION:Zoom or Duffield Lecture Theatre (host: N/A) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Melissa Ness (RSAA) "The After Sloan V Survey" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261027T000000Z DTEND:20261027T010000Z DTSTAMP:20261011T152430Z UID:u4ivehamjfi4k43l6at45d6c74@google.com CREATED:20260605T021628Z DESCRIPTION:TBC LAST-MODIFIED:20260716T070022Z LOCATION:Zoom or Duffield Lecture Theatre (host: TBC) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Johanna Hartke (U. Turku) "TBC" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191206T000000Z DTEND:20191206T010000Z DTSTAMP:20261011T152429Z UID:c5o0u511ra9i00592i2cipboj4@google.com CREATED:20190805T042115Z DESCRIPTION:Las Cumbres Observatory is a global network of 23 robotic teles copes providing nearly continuous coverage of the sky. I lead the Global Supernova Project\, a nearly six year effort to obtain lightcurves and spe ctra of 800 supernovae. I'll talk about a few highlights\, including: iPT F14hls\, a surprising supernova with a 3+ year lighcurve with 5 peaks\, wh ich may be the first example of the long-theorized puslational pair instab ility supernova. I'll also mention several type Ia supernovae with early blue bumps in their lightcurves\, which may indicate interaction with a co mpanion star. Finally\, I'll talk about our search for kilonovae\, includ ing the co-discovery of the optical counterpart of GW170817. LAST-MODIFIED:20191206T013104Z LOCATION:Duffield Lecture Theatre (host: Pingel) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Andy Howell (Las Cumbres Observatory) "Explosive Discoveries from L as Cumbres Observatory" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180525T010000Z DTEND:20180525T020000Z DTSTAMP:20261011T152429Z UID:sdru8jbjg4564k75tc06cqrkqc@google.com CREATED:20180509T120610Z DESCRIPTION:I will present findings from our ongoing UK KMOS GTO programme that has measured the spatially-resolved gas properties for over 1000 emis sion-line galaxies at z~0.6-2. Combining this sample with ~800 galaxies at z~0 from the SAMI Galaxy Survey and ~400 more at intervening redshifts (z ~0.4) observed with MUSE\, we are able to probe the dynamics of star-formi ng galaxies over an interval of ~10 Gyr. This period encompasses ~70 perce nt of cosmic history and includes key epochs for galaxy growth and evoluti on. I will highlight recent results from our programme\, including a measu re of the redshift evolution of the Tully-Fisher relation since z~1 and an examination of the shapes of galaxy rotation curves between z~0.6-2. I wi ll discuss how these analyses provide insights into the processes governin g galaxy evolution in our Universe. LAST-MODIFIED:20180520T024109Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alfie Tiley (Durham) "Galaxy Kinematics from Integral Field Spectro scopy of ~1000 z~0.6-2 Star-forming Galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170720T010000Z DTEND:20170720T020000Z DTSTAMP:20261011T152429Z UID:3ldf9ro4muieck4o1pikpp7p0k@google.com CREATED:20170622T010109Z DESCRIPTION:One of keys to understanding how star-forming galaxies evolve i s to study the inter-stellar medium (ISM). The last decade of high-redshif t\, observational studies have shown that the conditions within the ionize d ISM of high-redshift (z>1) star-forming galaxies are very different to w hat is observed in local galaxies. Unfortunately this is where the consens us ends. There still exists a somewhat confusing and heated debate over wh at is driving the observed changes. My Masters project aimed to address th e lack of consensus over the evolution of two properties of the ionized IS M\; the electron density and ionization parameter. By analysing matched sa mples of local and high-redshift galaxies we showed how these two properti es evolve over cosmic time. In this talk I present our strategy of matchin g (and stacking) galaxies and the key findings of our work. LAST-MODIFIED:20170710T070106Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Melanie Kaasinen (ANU) "Playing the cards at high redshift: the evo lution of electron density and ionization parameter" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250225T000000Z DTEND:20250225T010000Z DTSTAMP:20261011T152429Z UID:pqiju6plfac1g4rhekke110kig@google.com CREATED:20250106T225613Z DESCRIPTION:LIGO\, Virgo and KAGRA have unveiled a population of merging ne utron star and black hole binaries. The origin of these binaries is curren tly uncertain\; they may be produced by pairs of massive stars evolving vi a mass transfer episodes\, or they may form dynamically in dense stellar e nvironments such as globular clusters or active galactic nuclei\, or perha ps some combination of both. We have developed the open-source population synthesis and inference suite COMPAS (https://compas.science) to model th e formation of merging compact object binaries from massive binary stars. COMPAS incorporates several recent developments in population modelling\, including an updated treatment of common envelope evolution\, improved mod elling of chemically homogeneous evolution and a new prescription for wind s and tides of massive stars. I will present an overview of predictions fo r the binary evolution channel utilising these recent updates\, and our ef forts to use gravitational-wave observations to place constraints on uncer tain phases of massive binary stellar evolution. LAST-MODIFIED:20250122T035118Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hiep Nguyen) \nZoom: https ://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Simon Stevenson (Swinburne U.) "Probing massive binary stars with g ravitational waves" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220118T223000Z DTEND:20220119T001500Z DTSTAMP:20261011T152429Z UID:ph1ukkangpaen8pdvi3q7hl5r4@google.com CREATED:20220111T071606Z DESCRIPTION:Schedule: 09:30: Andrew Rapp 09:45: William Wall 10:00: Saakshi Dhakal 10:15: Hank Hua 10:30: Nicholas Bholsen 10:45: Erin Holdorf 11:00: Eric Muller LAST-MODIFIED:20220111T071606Z LOCATION:ZOOM only (host: Tony Travouillon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA Summer Students (RSAA) "Summer Student Presentations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150507T010000Z DTEND:20150507T020000Z DTSTAMP:20261011T152429Z UID:379glvr1h2s2ar0ft2s2ghs46o@google.com CREATED:20150210T000129Z DESCRIPTION:We often describe galaxies at z=0 as a bimodal population. On o ne side we have gas-rich\, star-forming spirals\; on the other\, passively -evolving\, gas-poor\, early-types. The former\, with their star formation activity and complex hydrodynamics\, sound like much more fun than the la tter -- but is this really the case? In this talk I will present results f rom a large survey of neutral hydrogen gas (HI) in early-type galaxies car ried out as part of the Atlas3D project. I will show that early-type galax ies form a surprisingly heterogeneous family when it comes down to HI\, co vering four orders of magnitude in M(HI)/M(star) and a wide range of gas m orphologies. I will discuss the role of environment in shaping these prope rties and present results on the misalignment between the angular momenta of stars and HI in these objects\, as well as a comparison to hydrodynamic al cosmological simulations. Future HI surveys will allow us to greatly ex pand this line of investigation and I will discuss this by giving a brief update on ASKAP commissioning. LAST-MODIFIED:20150501T032105Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Paolo Serra (CSIRO) "Neutral hydrogen gas in early-type galaxies: r esults from the Atlas3D survey" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190118T030000Z DTEND:20190118T032000Z DTSTAMP:20261011T152429Z UID:0fdg9kb2kh0easo8dq2lftvat8@google.com CREATED:20180926T072613Z DESCRIPTION:I will talk about the research I have done during my 5 month in ternship here. This includes two projects. The main project: Constructing a contamination-free sample of supernova DES16C2ayx. Here I will try diffe rent methods of normalizing the supernova spectra and find a method that w ill provide the best contamination-free spectra. The second project will t est the feasibility of a new measuring method. This method will make it po ssible to constrain cosmological parameters from SNe without the need of a spectroscopic follow-up. I have tested the feasibility of the method usin g already available data from DES\, OzDES and other telescopes. LAST-MODIFIED:20190108T042105Z LOCATION:CSO Common Room (host: Monty) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jesse Roomer (Fontys university) "Construction of a contamination-f ree supernova sample and testing the feasibility of a measuring method tha t will make it possible to constrain cosmological parameters from SNe with out the need of a spectroscopic follow-up." TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190208T033000Z DTEND:20190208T035000Z DTSTAMP:20261011T152429Z UID:sv88ntaj2tdboljo5gj6n246to@google.com CREATED:20190203T012107Z DESCRIPTION:The MSATT telescope allows high school/college students through out the ACT to conduct their own research projects in astronomy. Now enter ing its third year\, MSATT has a record number of 19 eager students who wa nt to do astronomy projects\, but more mentors are needed. I'll talk about the MSATT programme and convince you to mentor one of the many fantastic students. LAST-MODIFIED:20190203T213606Z LOCATION:CSO Common Room (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ryan Ridden-Harper (RSAA) "MSATT Mentor Program" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160520T040000Z DTEND:20160520T042000Z DTSTAMP:20261011T152429Z UID:sjmabllgj1e3fdfp2d1crb2nqs@google.com CREATED:20160309T043121Z DESCRIPTION:Astronomy Australia Ltd (AAL) is an independent not-for-profit company that has invested over $100M since 2007 to advance the vision that astronomers in Australia will have access to the best astronomical resear ch infrastructure. The goals of AAL are to implement the infrastructure pr iorities of the Decadal Plan\, advise the Government on new astronomy infr astructure investments\, and manage some of those investments. This talk g ives an update on the current status of AAL-supported project and faciliti es. We will also discuss AAL's future plans and opportunities in the conte xt of the Government's recently announced long-term NCRIS research infrast ructure program\, astronomy governance discussions that are underway\, and the new Decadal Plan. LAST-MODIFIED:20160517T002606Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Lisa Kewley and Yeshe Fenner (AAL/RSAA) "Astronomy Australia Ltd: U pdate on current activities and future plans" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240924T010000Z DTEND:20240924T020000Z DTSTAMP:20261011T152429Z UID:bqqjifoammd6eubnt1lctkm398@google.com CREATED:20240815T064124Z DESCRIPTION:Big-data challenges associated with large radio surveys\, such as the Evolutionary Map of the Universe (EMU) conducted with the ASKAP tel escope\, will require non-traditional approaches. We have applied self-sup ervised algorithms for discovering new radio sources such as Odd Radio Cir cles. I will discuss how we use weakly-supervised deep learning techniques for detecting extended radio sources\, along with the integration of nove l semi/fully supervised object detection methods to identify\, categorize and group complex radio galaxies with multiple components. These novel com puter vision methods produce value-added catalogues of radio galaxies whic h are essential for astronomical and cosmological studies. LAST-MODIFIED:20240906T100715Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Vanhiep Nguyen) \nZoom: ht tps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Minh Huynh (CSIRO - WA) "Novel Computer Vision Applications for Big Data in Astronomy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150612T042000Z DTEND:20150612T044000Z DTSTAMP:20261011T152429Z UID:lv48s52ahhgv4c3jpg569tun4s@google.com CREATED:20150612T083227Z DESCRIPTION:Can quantum computers indeed meet the promise of doing complex calculations faster than classical computers based on transistor technolog ies? While the holy grail of a programmable universal quantum computer wil l probably still take decades to reach\, one can already begin to answer t his question by testing programmable quantum annealing machines that are c urrently being built. These machines\, such as D-Wave Two\, use a non-main stream method known as adiabatic quantum annealing to perform optimization tasks. Very recently\, tests performed by different research teams on the D-Wave Two machine using hard optimization problems as a benchmark have s hown that it shows no speedup over traditional computing architectures. Af ter an introduction to optimization problems\, I briefly present our resul ts on detecting signatures of a quantum advantage on the D-Wave Two machin e. LAST-MODIFIED:20150612T083227Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Helmut Katzgraber (Texas A&M University\, Santa Fe Institute\, Cove ntry University) "Beyond Moore's Law: Seeking Quantum Speedup" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170519T040000Z DTEND:20170519T042000Z DTSTAMP:20261011T152429Z UID:ib2un3j8bpoovavti1ebo153ko@google.com CREATED:20170511T063107Z DESCRIPTION:TBD LAST-MODIFIED:20170511T063107Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mike Ireland (RSAA) "ESO Instrumentation at Paranal and La Silla Ob servatories" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191017T000000Z DTEND:20191017T010000Z DTSTAMP:20261011T152430Z UID:eh1sujo0hlagbn5eituh89kidc@google.com CREATED:20190916T031608Z DESCRIPTION:Using images from the GaLactic and Extragalactic All-sky Murchi son Widefield Array (GLEAM\; MWA) survey\, I have discovered 27 new supern ova remnants (SNRs) via their non-thermal emission at low radio frequencie s. Some of these are quite unusual objects with very low surface brightnes s\, while others were simply hidden from view due to confusion between the rmal and non-thermal emission at higher radio frequencies. For six candida tes I have suggested pulsar associations and can derive physical character istics. I will conclude the talk with other recent developments in low-fre quency Galactic science\, and future prospects for further discoveries usi ng upcoming MWA surveys. LAST-MODIFIED:20191017T013104Z LOCATION:Duffield Lecture Theatre (host: Pingel) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Natasha Hurley-Walker (ICRAR/UWA) "Detecting new supernova remnants with GLEAM" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260602T013000Z DTEND:20260602T023000Z DTSTAMP:20261011T152430Z UID:nsobrcn2kb2lh9qp6dm828hhr8@google.com CREATED:20260503T113602Z DESCRIPTION:Pulsar timing arrays\, which probe nanohertz-frequency gravita tional waves\, have recently reported the very first evidence for the pres ence of a stochastic background. This background most likely originates fr om a superposition of inspiraling supermassive black hole binaries. Howeve r\, more speculative sources such as cosmic strings and phase transitions cannot be ruled out. As we may now be entering the detection era\, pulsar timing arrays will focus on identifying and characterising the source of t he signal. \n\nIn the talk I will review the recent efforts of the pulsar timing community towards understanding the emerging signal. In particular\ , I will show how this goal can be targeted from many different angles\, s tarting from radio data acquisition and analysis up to multi-messenger ast rophysical studies in the context of galaxy evolution. LAST-MODIFIED:20260527T013422Z LOCATION:Zoom or DLT (host: Maja Jablonska) \nZoom: https://anu.zoom.us/j/8 2974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Gosia Curylo (Monash U.) "On the hunt for supermassive black hole b inaries with Pulsar Timing Arrays" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200924T010000Z DTEND:20200924T013000Z DTSTAMP:20261011T152429Z UID:ehe68s461b2ei5map8j3h00l80@google.com CREATED:20200906T234610Z DESCRIPTION:TBD LAST-MODIFIED:20200906T234610Z LOCATION:ZOOM 997 8534 1005 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dávid Guszejnov (UT Austin (USA)) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20211005T000000Z DTEND:20211005T010000Z DTSTAMP:20261011T152429Z UID:ba64t3clu298nhtg4mp0cpf980@google.com CREATED:20210805T045611Z DESCRIPTION:The archaeological record of the Milky Way is being unveiled th rough measurements of its stars. This is an endeavour across a huge range of scales\, where both individual stellar atmospheres and million star sur veys are revealing the connection of present to past. I will present my re cent work that makes measurements of stellar ages\, and uses these ages as the fundamental variable to learn the formation and evolutionary properti es of the Galaxy: where stars were born\, how they have moved over time\, and how individual abundances can quantify the diversity of the environmen t in which they formed. The overarching goal of this ensemble of studies i s to link the chemical to the structural evolution of the Milky Way\, show ing relationships that directly enable comparisons to other galaxies. LAST-MODIFIED:20210927T025107Z LOCATION:ZOOM (host: Sven Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Melissa Ness (Columbia University and Flatiron Institute\, USA) "In vited Colloquium: The Archaeological Record of the Milky Way" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250207T030000Z DTEND:20250207T040000Z DTSTAMP:20261011T152429Z UID:3ia7qmsbppq4vchn1p857eb78g@google.com CREATED:20250129T035611Z DESCRIPTION:An introduction to the thesis oversight committee for students LAST-MODIFIED:20250129T035611Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Emily Wisnioski) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Thesis oversight committee (RSAA) "Thesis oversight committee intro duction" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220218T000000Z DTEND:20220218T010000Z DTSTAMP:20261011T152429Z UID:f3abnnsumltv7tccovq80cpo9c@google.com CREATED:20220207T002104Z DESCRIPTION:Schedule: 11:00-11:15am Ashley Hai Tung Tan 11:15-11:30am Jessi ca Ross 11:30-11:45am Luka Mijnarends 11:45-12:00am Isaac Kanowski LAST-MODIFIED:20220207T002104Z LOCATION:DLT and ZOOM (host: Emily Wisnioski) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA ASTR3005 Students (RSAA) "ASTR3005 Student Presentations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240829T010000Z DTEND:20240829T020000Z DTSTAMP:20261011T152429Z UID:n7qd4ksk0oooucofpg2vavu9c8@google.com CREATED:20240417T012646Z DESCRIPTION:The magnetic field is a crucial constituent of the interstellar medium\, and accurately understanding its strength and structure in galax ies has significant implications for various areas of galactic astrophysic s. Recent advancements in sensitivity and frequency coverage of radio tele scopes have provided clearer insights into the magnetic fields of our Milk y Way Galaxy and its neighbouring Small Magellanic Cloud (SMC). In this se minar\, I will share the new magnetic knowledge gained from these advanced radio instruments\, using both linear polarisation and high-resolution HI measurements. In the case of the Milky Way\, I utilised the Faraday rotat ion experienced by linearly polarised emission from extragalactic radio so urces to find hints of Galactic magnetic structures at <2.5" scales. Meanw hile in the SMC\, I find that the filamentary HI structures near its centr e are preferentially aligned with the magnetic fields traced by starlight polarisation\, suggesting that these HI structures can have the potential of being a new 3D tracer of the SMC's plane-of-sky magnetic field. I will conclude by highlighting the exciting prospects in magnetism studies offer ed by on-going southern sky radio survey\, such as the POSSUM survey in po larisation and the GASKAP survey in HI. LAST-MODIFIED:20240820T040113Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jackie Ma (RSAA) "Magnetic Fields in the Milky Way and the Small Ma gellanic Cloud" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221117T000000Z DTEND:20221117T003000Z DTSTAMP:20261011T152430Z UID:2maveq177l78karip4n6eatgjs@google.com CREATED:20221005T052917Z DESCRIPTION:The abundances of chemical elements across cosmic epochs provid e unique information on the physical processes driving the evolution of ga laxies. Over the past decades many attempts have been made to measure meta llicities using emission lines from photoionized gas in galaxies\, ranging from direct measurements based on electron temperature and densities (Te- based metallicities)\, to calibration of relations between line ratios and metallicities\, to the use of photoionization models. However\, these met hods are often based on simplifying assumption which does not adequately d escribe the complexity of the emitting regions\, and their reliability is questioned. We will analyze a set of galaxy spectra using our new multi co mponent photoionization models which are able to reproduce all observed em ission lines with a very high accuracy\, down to a few percent. Our models thus allow for accurate metallicity measurements and to recover the well- known trends between ionization parameter and metallicity\, and N/O versus Oxygen abundance. we will show that while our models do reproduce all obs erved line ratios\, hence providing the same Te-based metallicities as obs ervations\, the true model metallicities are sometimes very different\, qu estioning the use of Te-based metallicities. we finally present newly cali brated metallicity estimators based on ratios between strong emission line s. LAST-MODIFIED:20221005T052917Z LOCATION:DLT & ZOOM (host: TBD) \nZoom: https://anu.zoom.us/j/99785341005?p wd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Amirnezam Amiri (University of Florence) "A New \, Multi-Cloud meth od to model emission lines in starforming galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260616T013000Z DTEND:20260616T023000Z DTSTAMP:20261011T152430Z UID:7ippg8khddafptdmb6ovsp0n0c@google.com CREATED:20260527T013426Z DESCRIPTION:In ancient times\, looking at the stars was essential for navig ation. Today\, we make use of artificial satellites for our position\, nav igation and timing applications\, giving the impression that there is no n eed for astronomers any more telling us where to go or what time it is. We ll\, this is not the case. Modern satellite techniques rely on precise kno wledge of their orbits in space\, which needs to be determined in an absol ute manner. In geodetic Very Long Baseline Interferometry (VLBI)\, we use extra-galactic black holes (quasars) as anchor points\, allowing to disent angle satellite orbits from the irregular movements of the Earth. It is th e only technique capable of measuring the full set of Earth orientation pa rameters\, which are precession and nutation\, polar motion and dUT1\, the difference between the actual rotational speed of the Earth to an atomic time scale. \n\nVLBI is a global instrument which is currently organised o n a best effort basis only\, relying on the voluntary contributions from n ational mapping authorities\, research institutions\, observatories\, and Universities. This is a major gap in resilience in our modern world\, a to pic recently highlighted by the United Nations.\n\nIn this talk\, I will p resent Australia’s contribution to international geodetic VLBI and its l inks to the radio astronomy community. While the core products mainly find their way into enabling sciences such as the world’s most precise coord inate frame\, more recent applications of VLBI can be found in upcoming sp ace missions (e.g. ESA’s NovaMoon) or intercontinental time and frequenc y transfer. Current risks and challenges will also be discussed\, such as the rapidly increasing man-made radio emissions in space caused by provide rs of internet via satellites. Improved protection of VLBI frequencies on a global scale is an urgent need if we want satellite services being able to continue operations. This is where science meets policy and internation al treaties and I will report about current work on this matter at the nat ional level. LAST-MODIFIED:20260605T021609Z LOCATION:Zoom or Duffield Lecture Theatre (host: Hiep Nguyen) \nZoom: https ://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Lucia McCallum (U. Tasmania) "Geodetic Very Long Baseline Interfero metry – why listening to the stars is essential for modern life" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151013T003000Z DTEND:20151013T010000Z DTSTAMP:20261011T152429Z UID:34c9n09e11bufv00nhdnvr1kls@google.com CREATED:20151004T121108Z DESCRIPTION:As a part of Mahalo-Subaru project\, we performed a deep narrow -band imaging with Subaru/MOIRCS in the SXDF-CANDELS field. We construct s amples of [OIII] emission line galaxies at z=3.2 and 3.6\, and investigate their global physical properties\, such as stellar mass and star formatio n rate (SFR). The stellar mass and SFR of the [OIII] emitters show clear c orrelation known as the 'main sequence' of star-forming galaxies. Comparin g with the Hα emitters at z~2\, we find that the location of the sequence of the [OIII] emitters is almost identical to that of the Hα emitters. H owever\, the distribution of galaxies along the sequence is systematically different between the two samples. In this talk\, I will show our results about NB-selected [OIII] emitters at z > 3\, and discuss what is suggeste d from the different distribution of galaxies on the main sequence diagram between the two different epochs. LAST-MODIFIED:20151012T040609Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tomoko Suzuki (NAOJ) "Star formation activities of galaxies before the peak epoch explored with [OIII] emission line galaxies at z > 3" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250814T010000Z DTEND:20250814T020000Z DTSTAMP:20261011T152429Z UID:f1v154ql19bcgd3f18mhn94ve0@google.com CREATED:20250728T232107Z DESCRIPTION:The Gaia mission has made more than three trillion observations of two billion stars and other objects throughout the Milky Way galaxy an d beyond\, mapping their motions\, luminosity\, temperature and compositio n. Thanks to a powerful large statistics\, homogeneity\, precision and spe ctral fidelity\, the Gaia RVS chemical cartography is revolutionising our understanding of the disc chemical abundances. In this talk\, I will prese nt several aspects of this revolution. First of all\, I will illustrate th e Gaia RVS spectral fidelity\, unexpected for a large part of the scientif ic community\, showing comparisons with asteroseismic data and other scien tific validation examples. Then\, I will present different results on Gala ctic disc populations as the chemical signature of the spiral arms\, the d ouble RGB sequences of the thin and thick disc\, the chemical pattern of t he disc kinematical perturbances\, and evidence of a recent gas infall eve nt. Finally\, I will present the future prospects of the Gaia mission for the next two data releases (DR4\, December 2026 and DR5 in 2030). LAST-MODIFIED:20250807T003608Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Sven Buder) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alejandra Recio-Blanco (Nice Observatory) "The chemistry of the Mil ky Way disc with the Gaia space mission" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251111T000000Z DTEND:20251111T010000Z DTSTAMP:20261011T152430Z UID:c4he1mm0kb26639hc97gj60ik8@google.com CREATED:20250623T121118Z DESCRIPTION:The presence of a supermassive compact object was envisaged fai rly quickly after the detection of the radio source Sagittarius A* at the centre of the Milky Way in 1974. Confirmation of this hypothesis took seve ral decades\, thanks in particular to the development of high angular reso lution techniques at optical wavelengths. The precise measurement of the o rbit of the star S2\, notably with the VLTI's GRAVITY interferometer\, mad e it possible to carry out tests of general relativity\, the results of wh ich proved compatible with the hypothesis of a supermassive black hole. Th e measurement of heated plasma orbits close to Sgr A*\, also by GRAVITY\, made it possible to establish a maximum size for the central object that i s also compatible with the black hole hypothesis\, in agreement with the i mage made later by the Event Horizon Telescope at 1.3 mm wavelength. I wil l come back to these results during the seminar and describe the measureme nts currently underway and those to come in order to continue the tests of general relativity in the strong field regime and the test of the superma ssive black hole hypothesis. I will also briefly present results obtained supermassive black holes at the core of AGNs and quasars and the prospects with the GRAVITY+ upgrade of the instrument. LAST-MODIFIED:20251006T215612Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Brian Schmidt and Francois Rigaut) \nZoom: https://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuA veyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Guy Perrin (Observatoire de Paris) "Sagittarius A*\, the supermassi ve black hole at the centre of the Milky Way: exploration and tests of gen eral relativity" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210427T010000Z DTEND:20210427T020000Z DTSTAMP:20261011T152429Z UID:sbt60113c13ikfsl9aevh5gu7c@google.com CREATED:20210128T023118Z DESCRIPTION:The focus of this talk is to address the spatial structure and evolution of star formation and the interstellar medium (ISM) in interacti ng galaxies. We use an extensive suite of parsec-scale galaxy merger simul ations\, which employs the 'Feedback In Realistic Environments' model (FIR E). This framework resolves star formation\, feedback processes\, and the multi-phase structure of the ISM. We find that close encounters augment mo lecular gas and star formation in the centre of galaxies\, and suppress th ese budgets at large galactocentric radii. We also find that nuclear enhan ced star formation is primarily driven my the increased presence of molecu lar gas fuel\, but the most intense starbursts are driven by star-formatio n efficiency. Our numerical predictions underscore the need of substantia lly larger\, and/or merger-dedicated\, spatially-resolved (integral-field spectroscopic) galaxy surveys -- capable of examining vast and diverse sam ples of interacting systems -- coupled with multi-wavelength campaigns aim ed to capture their internal ISM structure. Lastly\, if time allows\, I wi ll also speak of dark matter free dwarf galaxies in FIREBox\, a cosmologic al simulation of galaxy formation with FIRE. See also: https://arxiv.org/a bs/2009.11289 LAST-MODIFIED:20210420T014108Z LOCATION:ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jorge Moreno (Pomona\, USA) "Invited Colloquium: Spatially resolved galaxy interactions." TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190820T010000Z DTEND:20190820T020000Z DTSTAMP:20261011T152430Z UID:ku1cv0d1eibisu22qjkr8dmsj4@google.com CREATED:20190805T025609Z DESCRIPTION:Blue straggler stars (BSS) have been identified in star cluster s and in field populations in our own Milky Way galaxy and in its satellit e galaxies. They manifest as stars bluer and more luminous than the domin ant old population\, and usually have a spatial distribution that follows the old population. Their progenitors are likely to have been close binari es. We investigate trends of the BSS population in dwarf spheroidal galaxi es (dSph) and in the bulge of the Milky Way and find an anti-correlation b etween the relative frequency of BSS and the mean metallicity of the paren t population. This trend mirrors that found for the close-binary fraction in the field populations of the Milky Way. We argue that the dominant mod e of BSS formation in low-density populations is likely to be mass transfe r in primordial close binary systems and thus that the similarity between the results for BSS in the dSph and field stars in our Galaxy supports the proposal that the small-scale fragmentation during star formation is driv en by the same dominant physical process\, despite the diversity in enviro nment. LAST-MODIFIED:20190815T005606Z LOCATION:Duffield Lecture Theatre (host: Monty) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rosemary Wyse (Johns Hopkins University) "The Rich Lack Close Neigh bours: The Dependence of Blue-Straggler Fraction on Metallicity" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260521T013000Z DTEND:20260521T023000Z DTSTAMP:20261011T152430Z UID:8u0vkhu3l6nhdagbc7jj2rv1q0@google.com CREATED:20260503T114408Z DESCRIPTION:Motivated by the discovery of a repeating FRB associated with a globular cluster in the nearby galaxy M81\, this thesis investigates whet her old stellar environments can produce FRBs and examines the relationshi p between FRBs and other coherent radio transients associated with neutron stars. Using MeerKAT ultra-high frequency baseband observations of the mi llisecond pulsar PSR~J1823$-$3021A in the globular cluster NGC~6624\, we d etect more than $3.7\\times10^{4}$ GPs per hour\, establishing it as one o f the most prolific GP emitters known. Although the pulses exhibit complex temporal and spectral structures\, their energetics\, periodicity\, and s tatistical properties distinguish them from FRBs\, suggesting that GPs are unlikely to be direct low-energy analogues of the FRB population. We also investigate scintillation and coherent descattering\, demonstrating the f easibility of recovering intrinsic pulse structures from highly scattered radio pulses. Extending this work to extragalactic systems\, we conduct a deep FAST search for FRBs from globular clusters in the nearby elliptical galaxy M49 (NGC~4472)\, covering $\\sim4000$ globular clusters. No FRBs ar e conclusively detected\, yielding stringent upper limits on FRB activity in globular clusters. Finally\, we explore the cosmological potential of f uture wide-field FRB surveys with the BURSTT experiment\, showing that lar ge FRB samples could constrain primordial black holes through gravitationa l lensing. LAST-MODIFIED:20260527T014009Z LOCATION:Zoom or DLT (host: TBD) \nZoom: https://anu.zoom.us/j/82974980739? pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Simon Ho (RSAA) "Fast Radio Transients in the nearby Universe (End- of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20211116T000000Z DTEND:20211116T010000Z DTSTAMP:20261011T152429Z UID:sighpr4586oad98vk45933kf90@google.com CREATED:20210927T081612Z DESCRIPTION:Deep\, optical wide-field imaging is essential in nearly every area of astronomy and for science at all wavelengths for source localisati on and other applications. As a testament\, wide-field imagers are the hig hest demand instruments on their respective telescopes. The Australian-led Keck Wide-Field Imager (KWFI) is a 1-degree diameter field of view UV-sen sitive optical camera for Keck telescopes. KWFI will be the most powerful wide-field camera in the world for the foreseeable future and the only suc h 8m-class camera sensitive from 1000 nm down to 300 nm. KWFI can reach ga me-changing magnitudes of m ~ 28 - 30 (~25 - 4 nano-Jy) depths over wide f ields\, including the u-band as a result of Keck's 10m aperture and 4100m elevation. KWFI performs a critical role for existing and new spectroscopi c instruments for 8m and 30m-class telescopes in which Australia is invest ed\, for SKA\, CTA\, GMT\, E-ELT\, and JWST science\, upcoming wide-field space missions Roman and Euclid\, and current and next-generation gravitat ional wave detectors. In this talk\, I will discuss the KWFI instrument\, its status\, and path forward\, as well as associated Keck access for Aust ralians. KWFI will enable world-leading science that cannot be done on any other telescope anywhere else in the world or in space\, not even with 30 -metre telescopes. Examples include: Epoch of Reionisation science mapping ionising flux to complement SKA's goal to map neutral gas\; discovering n early all kilonovae detected by gravitational wave detectors that will be missed by current facilities (> 90%)\; and many other areas of science fro m the solar system\, to the Milky Way and local/low-redshift galaxy stella r populations and metallicities\, low surface brightness and diffuse galax ies\, to large-scale structure and the high redshift Universe\, to time do main science. KWFI reaches 2/3rds of the Southern Hemisphere sky\, as well as the full Northern Hemisphere sky\, enabling Australians to lead the wo rld in all these science areas and more. LAST-MODIFIED:20211112T043106Z LOCATION:ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jeff Cooke (Swinburne University) "Invited Colloquium: The Australi an-led Keck Wide-Field Imager" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240827T010000Z DTEND:20240827T020000Z DTSTAMP:20261011T152430Z UID:76kclv0170k7vtq1i11kkfqh74@google.com CREATED:20240415T054238Z DESCRIPTION:Much of our knowledge of the early Universe comes from measurem ents of the Cosmic Microwave Background\, and it is the driving force behi nd modern cosmological models. Approximately one billion years later\, the first stars were born from the primordial gas during the Epoch of Reionis ation. These first stars and galaxies represent the most basic experimenta l setup we will ever have on the intersection of cosmology and astrophysic s\, and as such\, they hold the last keys to some of the greatest mysterie s of our early Universe. However\, the Epoch of Reionisation signal is fai nter than a light bulb on Pluto. Everything between us and this time perio d is extremely bright\, like stadium lights\, in comparison. Nevertheless\ , the allure of its science potential inspires astrophysicists from around the world to search for this signal. Using the 21-cm hyperfine transition of Hydrogen\, we aim to map out the structure of primordial gas as it ion ises around the first stars and galaxies\, giving us bulk statistics on th e young Universe. In principle\, instruments from around the world have re ached the required sensitivity to measure this signal\, including the Murc hison Widefield Array. Understanding how to perform the order-petabyte dat a reductions whilst reducing the causes of contamination that render the s ignal immeasurable is the focus of my research. I will discuss the range o f approaches my collaborators and I are taking in order to reveal the elus ive 21-cm signal as we approach the era of the Square Kilometre Array. LAST-MODIFIED:20240801T171113Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Nichole Barry (Curtin U.) "Pursuing the Faint 21-cm Signal of the E poch of Reionisation" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180607T010000Z DTEND:20180607T020000Z DTSTAMP:20261011T152429Z UID:c08p1dlin5o77p1mfvlnle1u00@google.com CREATED:20180410T235620Z DESCRIPTION:For more than 50 years\, the rate and distribution of positron (anti-electron) annihilation in the Milky Way has puzzled gamma ray astron omers. Positrons with low (~MeV) initial energies are predominantly produc ed by beta+ unstable radioactive elements\, however\, the observed rate of positron annihilation in the Milky Way far exceeds the inferred rate of p ositron production by 'conventional sources' such as core-collapse and Typ e Ia supernovae. Moreover\, the observed distribution of positron annihila tion in the Milky Way appears to trace the older stellar populations of th e Galaxy (the Galactic bulge and thick disk)\, while radioactive material is predominantly synthesised in the thin disk of the Galaxy. My PhD has fo cused both on investigating the transport of positrons in the interstellar medium\, to constrain the production sites of this Galactic antimatter\, as well as investigating phenomena associated with SN1991bg-like supernova e\, which have been implicated as potential antimatter factories in the Mi lky Way. In this talk I will discuss some of my exciting new results on po sitron transport\, and SN1991bg-like supernovae\, and the implications of this work beyond high-energy astrophysics. LAST-MODIFIED:20180605T002110Z LOCATION:Duffield Lecture Theatre (host: Panther) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Fiona Panther (RSAA) "Antimatter in the Milky Way" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170509T010000Z DTEND:20170509T020000Z DTSTAMP:20261011T152429Z UID:pf66r8i30q2eejkq79hs9ajkj8@google.com CREATED:20170324T022106Z DESCRIPTION:I will describe how spectroscopic monitoring from the Global Je t Watch observatories (www.globaljetwatch.net/solar of the Galactic microq uasar SS433 elucidates the mass-loss via its accretion disc\, circumbinary disc and jets and show evidence of how these are evolving\, and of how th ey are coupled when the microquasar goes into flare. I will also present a succession of spectra of a Galactic nova (V5668 Sgr) which illuminate it s evolution in dust production and metallicity measured since shortly afte r detonation in March 2015 up to the present. LAST-MODIFIED:20170404T233610Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Katherine Blundell (University of Oxford) "Phase-resolved spectrosc opy of Galactic explosive energetic evolving ejecta" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161007T030000Z DTEND:20161007T032000Z DTSTAMP:20261011T152430Z UID:lij3jif4ce1bp2ncq0fca30gpk@google.com CREATED:20160904T235610Z DESCRIPTION:The high redshift regime presents an interesting laboratory to test radiative feedback from AGNs owing to their peak accretion density du ring this epoch. Observational efforts are underway to quantify the impact of AGN feedback\, if it exists\, on their host galaxies. We will present the first statistically sound investigation with ALMA of the molecular gas content\, CO(2-1)\, in a sample AGNs hosted in main-sequence galaxies at z~1.5. We compare the molecular gas content of these AGN hosts with a samp le of inactive galaxies matched in redshift\, stellar mass and star format ion rate. Our results indicate a statistically significant depletion of mo lecular gas in AGN hosts with respect to the inactive comparison sample. W e will discuss the implication of these observations on the impact that AG N feedback may have on the star-formation efficiency of z>1 galaxies. LAST-MODIFIED:20161004T234605Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Darshan Kakkad (ESO) "ALMA observations of cold molecular gas in AG N hosts at high redshift - Evidence of AGN feedback ?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250501T010000Z DTEND:20250501T020000Z DTSTAMP:20261011T152429Z UID:h3t2iolrmutlnm9knkjh21i410@google.com CREATED:20250426T021706Z DESCRIPTION:The Initial Mass Function (IMF) describes the distribution of s tellar masses formed through an episode of star formation. For any physica l interpretation of optical light\, especially for external galaxies\, an IMF is needed --- that is\, assumed. But measuring the IMF directly is com plicated. There are many technical (i.e. measurement) and intrinsic diffic ulties in ascertaining the masses that stars were at their birth\, often b illions of years in the past. Many different methods exist to indirectly c onstrain this concept\, each with their own strengths and pit-falls. They are routinely applied to heterogeneous samples of galaxies with heterogene ous data sets\, yet then compared in an attempt to constrain the IMF and i ts variability across space and time. I will tell the story of ESO286-G022 \, a massive early-type galaxy for which we have many independent probes o f the IMF. Even for this one galaxy\, these methods do not agree in their predicted IMF. I will describe our increasingly-sophisticated attempts to determine why they do not agree\, and what we learn in the process. LAST-MODIFIED:20250427T065607Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Emily Wisnioski) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Adriano Poci (Oxford U.) "The Peculiarities of the Massive Early-Ty pe Strong-Lens Galaxy ESO286-G022" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260224T220000Z DTEND:20260224T230000Z DTSTAMP:20261011T152430Z UID:3f6jcq22qva44jgn2j3a0u5gcg@google.com CREATED:20260210T105609Z DESCRIPTION:Over the past two decades\, wide-field radio surveys conducted with SKA precursor facilities such as ASKAP\, MeerKAT\, and LOFAR have tra nsformed our understanding of fast radio transients -- millisecond to minu te-duration bursts produced by some of the most extreme objects in the Uni verse. Among these are radio neutron stars and white dwarfs: pulsars\, mag netars\, rotating radio transients\, and recently discovered long-period r adio emitters that challenge traditional models of coherent radio emission . In this talk\, I will review how SKA precursor instruments have enabled systematic exploration of this diverse population and revealed intriguing connections between previously distinct sub-classes of radio neutron stars . The emerging picture suggests a continuum of behaviours\, from classical pulsars to highly magnetised neutron stars (magnetars)\, with long-period transients occupying a newly recognised parameter space. I will discuss h ow these discoveries inform our understanding of radio emission from compa ct objects. I will also discuss the recently discovered phenomenon of fast radio bursts (FRBs)\, which have opened a new frontier in high-energy ast rophysics. By localising FRBs to distant galaxies and measuring their disp ersion through intergalactic plasma\, SKA precursors have demonstrated the ir power as cosmological probes -- offering a novel means of tracing baryo nic matter and studying the large-scale structure of the Universe. Togethe r\, these advances illustrate how next-generation radio surveys are reshap ing our view of compact objects and transforming fast radio transients fro m rare curiosities into precision tools for astrophysics and cosmology. LAST-MODIFIED:20260216T232107Z LOCATION:ZOOM only (will be shown in Duffield Lecture Theatre) (host: Stu W yithe) \nZoom: https://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAve yEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kaustubh Rajwade (Oxford) "Unravelling the mysteries of fast radio transients with SKA precursors (Stromlo Radio Fellow candidate talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261231T000000Z DTEND:20261231T010000Z DTSTAMP:20261011T152430Z UID:8gss1ek88a8mq3jfvv24ll9l0c@google.com CREATED:20260527T013434Z DESCRIPTION:TBC LAST-MODIFIED:20260716T070033Z LOCATION:Zoom or Duffield Lecture Theatre (host: TBC) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:2 STATUS:CONFIRMED SUMMARY:Karl Glazebrook (Swinburne) "TBC" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231117T030000Z DTEND:20231117T031500Z DTSTAMP:20261011T152430Z UID:k8d718t08iugm0hmf6tnuvju38@google.com CREATED:20231113T131707Z DESCRIPTION:Compressible hydrodynamic simulations of turbulence have applic ations including astrophysical modelling of star formation\, and such simu lations are simplified if numerical energy dissipation effects can act as a proxy for viscous forces. In an effort to further understanding of these effects\, we implemented the kinetic energy equation to quantify and anal yse the structure of this dissipation. I will discuss the fractal nature o f turbulence and how these results parallel the structure observed in real -life turbulence. This is an ASC presentation by a PhB student. LAST-MODIFIED:20231113T131707Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Christoph Federrath) \nZoo m: https://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Thomas Shaddock (RSAA) "Characterising Structures of Numerical Diss ipation in Compressible Hydrodynamic Simulations of Turbulence" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240606T010000Z DTEND:20240606T020000Z DTSTAMP:20261011T152429Z UID:6reo0kts9abbn4j0e6728622nc@google.com CREATED:20240415T051624Z DESCRIPTION:Laser communication will revolutionise telecommunication by amp lifying the data capability of satellites\, supporting future space explor ation\, and bringing the world closer through high-speed relays. Despite t his\, laser communication has long struggled with adoption due to clouds a nd atmospheric turbulence. I present new tools to analyse optical ground station (OGS) networks for optimisation against clouds\, with a focus on A ustralia and the poles that includes utilising instruments installed in An tarctica. I also present development of a novel atmospheric turbulence mon itor which is tested at SSO\, the North pole\, and the NASA/Jet Propulsion Laboratory. These are novel solutions which are helping to commission the recently installed Quantum Optical Ground Station at MSO\, and more broad ly support a regional network of ground stations. LAST-MODIFIED:20240528T230112Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Francis Bennett) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Marcus Birch (RSAA) "Building resilient optical ground station netw orks with atmospheric characterisation and modelling (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260806T010000Z DTEND:20260806T020000Z DTSTAMP:20261011T152430Z UID:658r6cun77hdkb8ag1fsssepv4@google.com CREATED:20260605T021618Z DESCRIPTION:Type Ia supernovae (SNe Ia) are among the most powerful distanc e indicators in observational cosmology\, enabling precise measurements of cosmological parameters\, such as the dark energy equation of state param eter. Recent findings suggest that dark energy may be varying in time\, ra ther than following Einstein’s cosmological constant Lambda. Our ability to verify these results relies on our ability to accurately account for s ystematic biases in SN Ia distances\, the most prominent of which is the i nfluence of host galaxy environments. In this end-of-thesis talk\, I will present the spectroscopic follow up of SNe Ia and their host galaxies I ha ve completed for the Dark Energy Bedrock All-Sky Supernova Survey\, the ne w benchmark sample of low-redshift SNe Ia. A concurrent host follow-up I h ave completed for the Foundation Supernova Survey was used to demonstrate fundamental flaws in the canonical use of stellar mass as a tracer of host galaxy systematics\, instead proposing the use of the [O II] equivalent w idth as a more robust tracer. Finally I present an analysis of spectroscop ic and photometric host galaxy properties for both the Foundation and DEBA SS samples\, using a hierarchical Bayesian approach to determine the optim al approach to correcting host galaxy systematics in SN Ia standardisation . LAST-MODIFIED:20260728T040007Z LOCATION:Zoom or Duffield Lecture Theatre (host: Chris Lidman) \nZoom: http s://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Bailey Martin (RSAA) "A Spectroscopic Investigation of SNe Ia and t he Systematic Influence of their Host Galaxies (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180529T010000Z DTEND:20180529T020000Z DTSTAMP:20261011T152429Z UID:fk9ufard5k4b4q68ge6f49enjc@google.com CREATED:20180510T011610Z DESCRIPTION:Recent spectroscopic observations of a few thousand galaxies re vealed an extended galaxy overdensity on supercluster scales close to the Zone of Avoidance in Vela. Due to dust obscuration it had not been recogn ised as such. Moreover\, at a redshift distance of ~18000km/s it is locate d just beyond the boundaries and volumes of systematic whole-sky redshift and peculiar velocity survey. Interestingly\, the structure lies conspicuo usly close to the apex where residual bulk-flows suggest considerable mass excess. This discovery demonstrates that we still do not know our cosmolo gical neighborhood very well despite the numerous redshift surveys that ha ve been going on in the last decades: dynamically important large-scale st ructures still remain hidden by the Milky Way. I will present a first desc ription of what we have learned from the still sparsely-sampled Vela Super cluster\, as well as the potential implications of this overdensity on the bulk flows\, including predictions from flow fields. A first mass overden sity estimate from the to date still sparsely sampled survey implies the V ela SCL to contribute ~ 50 km/s to the motion of the Local Group despite i ts distance. This will be followed by forthcoming survey plans\, including Taipan (spectroscopic) and MeerKAT (HI) in the early science verification phase\, to get a more comprehensive census of the Vela SCL\, including th e most opaque part of the Zone of Avoidance. LAST-MODIFIED:20180529T035106Z LOCATION:Duffield Lecture Theatre (host: Oh) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Renee Kraan-Korteweg (University of Capetown) "The Vela Supercluste r: Discovery and Implications" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220323T000000Z DTEND:20220323T010000Z DTSTAMP:20261011T152429Z UID:iuvcr1inc4mvvjatjccud3mlt4@google.com CREATED:20220315T231609Z DESCRIPTION:Because they are dark-matter dominated\, dwarf galaxies provide some of the most stringent tests of our cold dark matter model. Specifica lly\, Lambda CDM makes predictions about the number\, shape\, and spatial distributions of the faint friends of massive galaxies. I will present res ults from the Exploration of Local VolumE Satellites (ELVES) survey\, that constructs the largest known sample of satellites around Milky Way-like h osts. I will discuss the radial profiles\, mass-size relations\, and quenc hed fractions of the ELVES satellites. For the second half\, I will turn t o what we know about black holes in dwarf galaxies\, and how their demogra phics sheds light on the formation of the seeds of supermassive black hole s. LAST-MODIFIED:20220315T231609Z LOCATION:DLT & ZOOM (host: Stefania) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jenny Greene (Princeton University\, USA) "Invited Colloquium: Dwar f Galaxies and their Black Holes" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190801T010000Z DTEND:20190801T020000Z DTSTAMP:20261011T152429Z UID:1d2qn032c2s0tcg75ejef23hss@google.com CREATED:20190703T014109Z DESCRIPTION:Jupiter and Saturn played an important role opening gaps and fo rming dust traps in the protosolar accretion disk. This is reflected in th e distribution of chondrules and calcium-aluminum-rich inclusions (CAIs) i n chondritic meteorites. CAIs are almost exclusively present in chondrites that accreted in the outer Solar System\, and isotopic fingerprints show that chondrules were transported to the outer Solar System\, but no outer Solar System chondrules returned to the inner Solar System. A dust trap ca n only stop particles above a certain size\, while small particles flow th rough the trap together with the gas. Using a suite of simulations of the protosolar disk including gas\, dust\, and planets advanced for up to 50\, 000 Jupiter orbits\, I investigate the efficiency of planetary dust traps for different physical conditions. These models are compared to cosmochemi cal evidence from a systematic search for CAIs using electron microscope s cans of the ordinary chondrite NWA5697. Combining models and data gives ne w insight into the architecture of the young Solar System\, and novel cons traints on the gas surface density in the protosolar disk. Furthermore\, I show having Jupiter and Saturn initially in a 3:2 resonance\, as expected in the Nice II model\, is difficult to reconcile with the CAI size cut-of f in NWA5697. LAST-MODIFIED:20190703T014109Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Troels Haugbølle (University of Copenhagen) "Probing the protosola r disk using dust filtering of the gas giants in the early Solar System" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250327T000000Z DTEND:20250327T010000Z DTSTAMP:20261011T152429Z UID:08dkbgn67g8me7mu9lk90g2gpo@google.com CREATED:20250319T224207Z DESCRIPTION:Hot subdwarf stars are compact\, high-temperature stars that se rve as key laboratories for studying stellar evolution\, asteroseismology\ , and binary interactions. In my PhD thesis\, I present both theoretical a nd observational work to study hot subdwarfs across their full mass range and their implications for explaining unusual stellar objects. Among these are the mysterious Blue Large-Amplitude Pulsators\, a newly discovered cl ass of pulsators. I show that Shell-Helium-Burning hot subdwarfs are stron g candidates to explain this class\, outperforming other models proposed s o far. I also present insights from the discovery and characterization of J0526\, a short-period hot subdwarf binary\, confirming it as the smallest known non-degenerate star in a detached binary system. Further\, I explor e white dwarf merger outcomes\, specifically various Helium\, CO and ONe w hite dwarf mergers\, and demonstrate success in explaining recently observ ed phenomena\, such as the Gaia Q Branch and the exceptionally massive ste llar remnant J005311 with unusual spectral properties. Finally\, I discuss my extension of the Infrared Flux Method to hot subdwarfs\, incorporating ultraviolet and optical photometry\, and its implications for GALEX photo metry. LAST-MODIFIED:20250320T005608Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Luca Casagrande) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Heran Xiong (RSAA) "Hot subdwarf stars and related stellar objects: modelling and empirical effective temperatures (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170831T010000Z DTEND:20170831T020000Z DTSTAMP:20261011T152429Z UID:klqlh5tt8qalet95h1giigk4qo@google.com CREATED:20170623T041616Z DESCRIPTION:The Magellanic Clouds are two interacting\, gas-rich\, star-for ming\, low-mass\, nearby satellite galaxies of the Milky Way that afford a unique view of low-metallicty star-forming regions\, providing the neares t laboratories to study the processes relevant to star formation in the ea rly universe. We use the dust emission from HERITAGE Herschel data (Meixne r et al. 2013) to map the molecular gas in the Magellanic Clouds\, avoidin g the known biases of CO emission as a tracer of H2\, and find that on lar ge scales the molecular gas depletion time is not a strong function of met allicity. We compare galaxy-scale analytic star formation models to our ob servations and find that successfully predicting the trends in the low met allicity environment needs the inclusion of a diffuse neutral medium. The averaging of the scatter in the molecular gas depletion time as a function of scale size suggests that the drivers of the star formation process in these galaxies operate on large scales. On small (~ few pc) scales in the Small Magellanic Cloud (SMC)\, we study the effect of metallicity on the s tructure of photodissociation regions in the outskirts of molecular clouds using [CII] and [OI] spectroscopy combined with new ALMA 7-m array maps o f 12CO and 13CO. We estimate the total amount of molecular gas using [CII] to trace H2 at low-Av and 12CO to trace H2 at high-Av. We find that most of the molecular gas is traced by [CII] emission and that metallicity only affects the relationship between CO emission and molecular gas through ch anges in Av. Using mid-infrared spectroscopy from Spitzer Space Telescope in the SMC (Sandstrom et al. 2012)\, we model the H2 rotational line emiss ion to estimate temperatures\, column densities\, and fractions of warm H2 gas (T>100 K). The temperatures and column densities of warm H2 gas are s imilar to nearby galaxies\, but the SMC shows somewhat high fractions of w arm H2. The properties of the warm H2 gas indicate that it is located in p hotodissociation regions that are more extended in the low metallicity env ironment of the SMC. Finally\, I will discuss our new ATCA survey of HI an d OH absorption in the Magellanic Clouds. LAST-MODIFIED:20170821T003107Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Katie Jameson (RSAA) "Gas and Star Formation at Low Metallicity in the Magellanic Clouds" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220331T000000Z DTEND:20220331T010000Z DTSTAMP:20261011T152429Z UID:csu13veln8f95stgjlv3nm1co8@google.com CREATED:20220313T235312Z DESCRIPTION:Exoplanet detection surveys over the last twenty years have rev ealed a surprising diversity of planets orbiting other stars - this revolu tion is fueled by fundamental questions about the place of the Earth and t he Solar System in the Universe. How do planets form? What range in archit ectures of planetary systems exist? How does our Solar System fit into thi s context? The study of exoplanet atmospheres is the next step in leveragi ng exoplanetary detections. This is because a planet's atmosphere provides a fossil record of its primordial origins and controls its fate\, size\, appearance\, and ultimately its habitability. In this context\, I present comparative exoplanetology programs that aim at characterising planetary s ystems transiting nearby stars through the observations of their atmospher es. Our findings on the atmospheric composition and physical properties pr ovide insights into the formation and evolution of planetary systems and e nhance our understanding of our own Solar System's formation. Finally\, I also present strategies for probing habitable exoplanet atmospheres in the quest for bio-signatures. LAST-MODIFIED:20220330T031106Z LOCATION:DLT & ZOOM (host: Shyam Menon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jean-Michel Desert (University of Amsterdam) "Characterizing Exopla nets' Atmospheres to Unveil Planetary Origins\, Climate and Habitability" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231121T000000Z DTEND:20231121T010000Z DTSTAMP:20261011T152429Z UID:gaomep6bm7o4e94fj8d4psbdi8@google.com CREATED:20231105T224952Z DESCRIPTION:What have we learnt about the formation of stars and planets by imaging young stars\, and in particular the circumstelllar discs of mater ial around them? Can you grow a star by accreting from a disc? How quickly does the material in the disc get converted into planets? Can we understa nd what causes the outburst events on young stars? Can we detect young pla nets directly? How does this relate to the formation of our own solar syst em? I will try to answer all of these questions\, and more\, in just 45 mi nutes of your life. LAST-MODIFIED:20231105T224952Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Trey Yang) \nZoom: https:/ /anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Daniel Price (Monash U.) "How (not) to make stars and planets" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170818T040000Z DTEND:20170818T042000Z DTSTAMP:20261011T152430Z UID:bd8048h94p52dc756pul8443ko@google.com CREATED:20170614T034110Z DESCRIPTION:As Chief Scientist of Double Negative\, Oliver was instrumental in the creation of the Gravitational Renderer which enabled us to produce Oscar and BAFTA-winning visual effects for Christopher Nolan’s Interste llar. In 2014\, Oliver\, Dneg VFX Supervisor Paul Franklin\, Dneg CG Super visor Eugénie von Tunzelmann and leading astrophysicist Professor Kip Tho rne\, co-authored and published two scientific papers based on this work. Oliver will talk about his work and how he merged physics with special ef fects. LAST-MODIFIED:20170815T012606Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Oliver James (Double Negative) "The Science Behind Interstellar (Th e Movie)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241107T220000Z DTEND:20241108T060000Z DTSTAMP:20261011T152429Z UID:r0da9n226p01q31mvf2f3uclf8@google.com CREATED:20240919T012126Z DESCRIPTION:End-of-thesis talks from the honours and masters students. LAST-MODIFIED:20240929T234624Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Honours and masters students (RSAA) "Honours and masters end-of-the sis talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190305T000000Z DTEND:20190305T010000Z DTSTAMP:20261011T152429Z UID:r856e2ud8png909ju2bahr254g@google.com CREATED:20190122T033121Z DESCRIPTION:PHANGS aims to understand the interplay of the small-scale phys ics of gas and star formation with galactic structure and galaxy evolution . Using high spatial resolution observations we can investigate how physic s at or near the cloud-scale are affected by galaxy-scale conditions\, how they affect still smaller scale processes\, and how these influence the e volution of whole galaxies. In this talk\, I will present the early scienc e results from the PHANGS-MUSE programme. By mosaicking across entire gala xies at high angular resolution (1"=50pc) we are able to resolve thousands of individual HII regions and measure properties such as flux\, line rati os\, and metallicity for each of them. This allows us to examine\, in unpr ecedented detail\, how stars are formed in different galaxy environments u sing a statistical sample. We then combine this MUSE data with ALMA data a t a matched resolution\, meaning we can trace the relative distribution an d evolution of the gas properties of these galaxies in multiple phases. Th is gives us insight into how star formation fuelling is connected to speci fic galactic environments and how nuclear activity\, even at low luminosit y\, can affect the ISM. LAST-MODIFIED:20190227T000107Z LOCATION:CSO Common Room (host: Monty) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rebecca McElroy (MPIA) "PHANGS: Physics at high angular resolution in nearby galaxies with MUSE and ALMA" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191029T000000Z DTEND:20191029T010000Z DTSTAMP:20261011T152429Z UID:gqj3gpm2i9l5kggtg53a8u1tn8@google.com CREATED:20191004T042612Z DESCRIPTION:Astrophotonics (the application of photonics technologies in As tronomy) has now been a research and development endeavour for over 15 yea rs. An overview of some of the more promising Astrophotonic principles\, f unctions and devices will be presented along with current/future astronomi cal applications. LAST-MODIFIED:20191024T031606Z LOCATION:Duffield Lecture Theatre (host: Monty) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Roger Haynes (RSAA/AITC) "Astrophotonics - An overview" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230214T000000Z DTEND:20230214T010000Z DTSTAMP:20261011T152429Z UID:td5rc0vi53hbgmpa1n8j9h3kis@google.com CREATED:20230201T134311Z DESCRIPTION:Ground-based optical telescopes are essential to astronomy and astrophysics research\, but they are severely impacted by dynamic aberrati ons caused by the atmosphere. The most important dynamic aberrations inclu de atmospheric turbulence\, dome turbulence and optical surface shape defo rmations. A complete dynamic aberrations profile needs to be ascertained t o accurately plan\, confirm\, or compensate for the loss in image quality. Optimising the achievable image quality is essential to maximising the te lescope's scientific impact. This thesis colloquium presents the results t hat address dynamic aberration knowledge gaps for the Anglo-Australian Tel escope (AAT)\, Siding Spring Observatory (SSO)\, and the Giant Magellan Te lescope (GMT). LAST-MODIFIED:20230209T034609Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Jesse Cranney) \nZoom: htt ps://anu.zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Josephine Munro (RSAA) "Characterising Dynamic Aberrations for Grou nd-based Optical Telescopes (End of Thesis Talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170716T230000Z DTEND:20170717T000000Z DTSTAMP:20261011T152429Z UID:no8bqn7pm40hf2mqv2ijn3trog@google.com CREATED:20170622T062607Z DESCRIPTION:Since the measurements with COBE/FIRAS in the mid-90's we know that the energy spectrum of the cosmic microwave background (CMB) is extre mely close to that of a perfect blackbody. However\, a number of early Uni verse processes should create spectral distortions at a level within reach of present day technology. I will give a broad-brush overview of recent t heoretical and experimental developments\, explaining why future measureme nts of the CMB spectrum will open an unexplored new window to early-univer se and particle physics. This provides an exciting new path forward in CMB cosmology which is complementary to planned and ongoing searches for prim ordial B-mode polarization signals. LAST-MODIFIED:20170708T065604Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jens Chluba (University of Manchester) "The Future of Cosmology wit h CMB Spectral Distortions" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220429T040000Z DTEND:20220429T043000Z DTSTAMP:20261011T152429Z UID:fla59um4sdlhkj3su2q9h8a240@google.com CREATED:20220426T033708Z DESCRIPTION:Sophie would share her experience at her internship in Sitael. LAST-MODIFIED:20220426T233109Z LOCATION:DLT & ZOOM (host: Marcus Birch) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sophie Hagley (RSAA) "Feast-of-Facts: Internship experience at Sita el" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250401T000000Z DTEND:20250401T010000Z DTSTAMP:20261011T152430Z UID:9qk2jajokrf95ttsmllr5c11f0@google.com CREATED:20250106T230123Z DESCRIPTION:The James Webb Space Telescope (JWST) has uncovered a mysteriou s population of extremely compact\, red sources at high redshift - so-call ed ''Little Red Dots'' (LRDs). Found ubiquitously across JWST fields\, the se objects exhibit broad Balmer lines\, peculiar V-shaped spectral energy distributions (SEDs)\, and a diversity of properties that challenge conven tional classification. Are LRDs the earliest growing black holes with unpr ecedented gas densities? Or could they be massive\, extremely compact gala xies whose stellar kinematics mimic broad-line emission? Despite extensive studies\, a consensus has yet to emerge. I will discuss the current state and future directions of one of JWST's most intriguing and debated discov eries. LAST-MODIFIED:20250331T235605Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ivo Labbe (Swinburne U.) "Little Red Dots\, Big Open Questions" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20141113T030000Z DTEND:20141113T040000Z DTSTAMP:20261011T152430Z UID:48n3bkkr4cikb8gj82i1ms96i4@google.com CREATED:20141117T132841Z DESCRIPTION:JWST is now approaching a crucial phase in its development. The thermal-vacuum testing is ramping up over the next year. I would like to give an overview of the mission and how one of the largest scientific proj ects ever undertaken is going as we enter the final years of its developme nt. Particularly since the ICRP report (will explain on Thursday!). This w ill be informal in style and questions/discussion will be encouraged... LAST-MODIFIED:20250925T231017Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Garth D. Illingworth (UCO/Lick Observatory) "A Post-ICRP Update on JWST: Just Four Years to Launch" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190808T010000Z DTEND:20190808T020000Z DTSTAMP:20261011T152429Z UID:pllp7oprfngurbg6b7pkot8c8o@google.com CREATED:20190619T035609Z DESCRIPTION:The Small Magellanic Cloud (SMC) provides the only laboratory t o study the detailed physics of star formation and the interstellar medium relevant to the high redshift universe. Not only is the transition from w arm to cold neutral gas a rate limiting step to the formation of molecular gas\, but it appears to influence star formation efficiency globally and we still do not understand how metallicity affects this transition. We pre sent first results from a new HI and OH absorption line study using the AT CA to measure the warm-to-cold atomic fraction and the atomic-to-molecular transition in the SMC. The survey includes 55 sources in the SMC\, which doubles the number of existing observations with up to 5x greater sensitiv ity and 4x higher spectral resolution than previous absorption line studie s. From these observations\, we are able to measure the optical depth\, av erage spin temperature\, individual cloud temperatures\, and cold atomic g as fraction. These measurements of the optical depth allow us to constrain the amount of 'CO-faint' gas that is optically thick HI. We find very col d (~20 K) temperatures for individual cold gas clouds and an average cold HI cloud temperature of 30 K\, lower than in the Milk Way\, and a cold ato mic gas fraction of 25% for the SMC\, which is similar to the Milky Way an d the Local Group. ALMA ACA CO observations of a subset of sources have on ly revealed detectable CO emission near one source with cold HI indicating that many regions with cold atomic gas have little CO emission and possib ly no molecular gas. I will also present preliminary results from a new la rge (1 deg x 0.5 deg) ALMA ACA CO map of the Southwest Bar of the SMC\, wh ich shows previously undetectable small (~ 2 pc) molecular gas clumps are found throughout the region. LAST-MODIFIED:20190802T031105Z LOCATION:Duffield Lecture Theatre (host: Pingel) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Katie Jameson (RSAA) "End of Postdoc Talk: Cold Neutral Gas and Mol ecular Gas at Low Metallicity in the Small Magellanic Cloud" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180319T000000Z DTEND:20180319T010000Z DTSTAMP:20261011T152429Z UID:64paaqd1g2ejbcf7ua25ol9jog@google.com CREATED:20180305T235605Z DESCRIPTION:[Multi-channel Photometric Survey Telescope - Mephisto] - Large -scale astronomical surveys play a key in modern astrophysical studies\, l eading to new discoveries and revolutionizing our understanding of the ori gin and evolution of the universe. The fast technological advances are cha nging the ways we view the sky\, from snapshot taking in surveys such as S DSS and XSTPS-GAC\, to movie shooting by observing the same sky thousands of times in surveys such as ZTF\, Skymapper\, WFST and LSST. The developme nts open up the possibility to probe the universe in multi-dimensions\, in particular in time domain. Build upon the experiences of those surveys an d to make a step forward\, we plan to build a wide-field multi-channel sur vey telescope - the Multi-channel Photometric Survey Telescope (Mephisto)\ , the first of this type in the world. Mephisto has a 1.6m primary and is equipped with three CCD cameras of a field-of-view 3.14 deg^2\, capable of simultaneously imaging the same patch of sky in three bands (ugi or vrz). The three cameras boast a total of 1.4 Giga pixels. Mephisto will yield r eal-time colours of astronomical objects with unprecedented accuracies\, a nd deliver for the first time a coloured documentary of our evolving unive rse. The development of Mephisto is expected to take four years (2018-2021 )\, and is expected to be operational in 2022. The Mephisto surveys will h ave two components: the Mephisto-W covering the whole northern sky of ~26\ ,000 deg^2 and the Mephisto-D\, Mephisto-H and Mephisto-M covering sky are as of respectively thousands\, hundreds and tens of square degrees with a corresponding cadence of days\, hours and minutes\, targeting specifically fast variables and transients. The unique capability of recording high-pr ecision real-time colours\, thus allowing quick and robust classification of fast transients\, makes Mephisto particularly powerful in time domain a strophysics. Celestial objects and forefront problems that Mephisto will t arget and tackle include\, for example\, astrophysical transients and the underlying physics\, galaxies and cosmology\, extreme metal-poor stars and Galactic archeology\, stars and planetary systems including the Solar Sys tem. Mephisto data products will be publicly available to the domestic and international communities. / [Optical design for Mephisto] - Multiple cha nnel Photometric Survey Telescope (Mephisto) is an ambitious project aimed at efficient survey the northern sky with three multiple band simultaneou sly. Mephisto\, with 1.6meter aperture 2 degrees FOV\, was design as Ritch ey-Chretien type\, similar with SKYMAPPER. Equipped with a field corrector \, the optics can delivered an ideal image quality of 0.3arcsec (80% encir cled energy circle diameter)\, an observation image quality of 0.6arcsec w ithout ADC. The optical splitting system was tricky. For avoiding the asti gmatism introduced by the dichroic mirrors\, 300mm beam splitting prisms w ere used for splitting the convergent beam to 0.31-0.41\, 0.41-0.70\, and 0.70-1 micrometer. Preliminary results show that the splitter is feasible and qualified. / [Galactic disk chemistry and kinematics from LAMOST] - On e of the fundamental tasks of modern astrophysics is to understand how gal axies form and evolve. Generally\, the quest can be pursed in two ways: st atistical analyses of large samples of distant galaxies (deep-field cosmol ogy) and detailed studies of large samples of member stars in the Local Gr oup of galaxies including our own\, the Milky Way (near-field cosmology). Initiated and aimed to make a major contribution to this latter\, 'near-fi eld cosmology' quest for understanding the galaxy formation and evolution\ , the LAMOST Galactic Spectroscopic Surveys have hitherto collected qualit y spectra of over 7M Galactic stars\, and this number is still increasing at a rate of 1M per annum. Combining with data from other available photom etric\, astrometric and spectroscopic surveys (e.g. Gaia\, APOGEE\, GALAH) \, the Surveys have yielded a unique dataset to help us draw an exquisite picture of unprecedented detail of our Galaxy\, in particular of the Galac tic disk. In this talk\, I will present the scope and motivation\, data re duction and release\, as well as scientific results of the surveys. LAST-MODIFIED:20180314T233606Z LOCATION:Duffield Lecture Theatre (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Bingqiu Chen\, Zhengyang Li\, and Yang Huang (Yunnan University / N anjing Institute of Astronomical Optics and Technology) "Multi-channel Pho tometric Survey Telescope - Mephisto (Bingqiu Chen & Zhengyang Li\; 35min) / Galactic disk chemistry and kinematics from LAMOST (Yang Huang\; 25min) " TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171027T030000Z DTEND:20171027T032000Z DTSTAMP:20261011T152429Z UID:897ia0kibktljjnn9t6sms7pic@google.com CREATED:20171018T071607Z DESCRIPTION:In half a year Gaia is expected to largely solve the problem of inaccurate distances within the Galaxy\, with a billion+ stars having tr igonometric parallax errors at a level of a few per-cent. Similarly\, thei r proper motions will reach exquisite accuracy by the standards we used s o far. But radial velocities could be measured only for a rather smaller s ample by Gaia. I will discuss important physical applications of accurate radial velocities and how to obtain them with ground-based spectroscopic s urveys where Galah is the primary asset. I will argue that while accuracy of a few km/s is needed for studies of Galactic kinematics a measurement a t a 100 m/s level opens up statistical studies of kinematics within the st ellar atmosphere and kinematics of stars within a cluster or a stream. And Galah is getting there. LAST-MODIFIED:20171020T080107Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tomaz Zwitter (University of Ljubljana) "Accurate stellar radial ve locities with Gaia and ground-based surveys" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160226T030000Z DTEND:20160226T032000Z DTSTAMP:20261011T152430Z UID:qj6drksk6o0iohcduvscs1soo8@google.com CREATED:20160129T011613Z DESCRIPTION:The briefing on the Defence Trade Control Act will be about the Act itself and how it may potentially impact research activity in RSAA (2 0 mins). Following this discussion\, researchers who consider their work h as no exposure to Act are free to leave. The second 40 minutes will explo re more closely those areas where researchers believe their work may have potential exposure. LAST-MODIFIED:20160223T040605Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Central Research Management Division (ANU) "Defence Trade Control A ct Briefing" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171117T033000Z DTEND:20171117T035000Z DTSTAMP:20261011T152429Z UID:kjpgjkjp6diqdvpitjhqg27o5k@google.com CREATED:20171024T175115Z DESCRIPTION:TBD LAST-MODIFIED:20171117T011107Z LOCATION:Duffield Lecture Theatre (host: Trans 101: experiencing both sides of the gender binary) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Henry Zovaro and Joel Wilson (ANU) "In recent years\, transgender p eople have become more and more prominent in mainstream media\, with some notable transgender individuals such as Chelsea Manning\, Caitlyn Jenner a nd Laverne Cox becoming household names. Nonetheless\, many people are una ware of the unique issues and struggles that transgender people face in th eir day-to-day existence. In this Feast of Facts\, we hope to give the aud ience a better understanding of what it means to be transgender\, how to b e a good ally\, and to dispel common misconceptions. Joel Wilson\, a trans gender man\, will talk about his experiences being perceived as both a wom an and a man\, with a focus on his experiences in STEM fields." TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160823T010000Z DTEND:20160823T020000Z DTSTAMP:20261011T152430Z UID:340ht4km975mtrqt7tqgm5i3dg@google.com CREATED:20160704T074111Z DESCRIPTION:As part of my PhD thesis I have performed some of the first eve r non-LTE spectral line formation calculations\, highlighting serious syst ematic errors in traditional 1D LTE analyses. In this talk I present resul ts for two of the most important metals in astronomy: oxygen and iron. For the OI 777nm triplet\, we found severe 3D non-LTE effects in solar-metall icity turn-off stars\, where the abundance corrections can reach around -0 .7 dex. In disagreement with several previous studies based on 1D non-LTE calculations\, we found the effects become monotonically smaller towards l ower metallicities. For FeI and FeII lines\, we found the 3D non-LTE effec ts to grow towards lower metallicities\, which has a large impact on the F eI excitation balance and FeI/FeII ionization balance in metal-poor stars. I discuss the implications of these results on spectroscopic stellar para meter determinations and on the [O/Fe] vs [Fe/H] relationship\, one of the key tracers of the Galactic Chemical Evolution. LAST-MODIFIED:20160805T044109Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anish Amarsi (RSAA) "Three dimensional non-local thermodynamic equi librium (3D non-LTE) spectral line formation in late-type stars" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250717T010000Z DTEND:20250717T020000Z DTSTAMP:20261011T152429Z UID:cfkmio090mn8pk9us4b4ul67i0@google.com CREATED:20250708T064106Z DESCRIPTION:The vast astronomical data archives hold an enormous amount of potential for discovery. With new analysis tools we can search these archi ves for new phenomena\, extend the scientific capacity of existing instrum ents\, and recover degraded observations. In this seminar I will present r esults from a range projects such as: an all-sky time domain survey with N ASA's TESS space telescope\; a novel approach to explore the rapid infrare d time domain with JWST\; and a method for analysing and removing satellit e streaks from MUSE IFU data. LAST-MODIFIED:20250714T235706Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ryan Ridden (U Canterbury) "Searching a Universe of Data" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240223T030000Z DTEND:20240223T040000Z DTSTAMP:20261011T152429Z UID:tsfnu1b1028iv4jiugpm2s2s84@google.com CREATED:20231120T224124Z DESCRIPTION:TBC LAST-MODIFIED:20231120T224124Z LOCATION:Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.zoom.us/j /83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Luca Casagrande (RSAA) "RSAA IDEA Town Hall Meeting" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241010T000000Z DTEND:20241010T010000Z DTSTAMP:20261011T152429Z UID:bv4cbda82j25ubnll3pc76av1s@google.com CREATED:20240417T012655Z DESCRIPTION:Advances in radio telescope technology have greatly improved ou r ability to explore the radio sky\, including its polarization which we u se to explore cosmic magnetism in diffuse environments. Large survey proje cts with new radio telescopes are going to produce more data than has exis ted in all prior radio observations combined\, but dealing with these data requires significant effort in technical development -- new pipelines\, a lgorithms\, and ideas. In this seminar I'll offer a behind-the-scenes look at the technical development for large radio polarization surveys\, with an eye to discussing similarities and differences to large optical data pr ojects. I'll also talk about some of the challenges that can happen when d oing software development in an astronomy context -- hopefully with some n uggets of wisdom for students who are embarking on software adventures. An d if time permits\, I'll talk about the unforeseen problems that can come with executing a big survey project. LAST-MODIFIED:20240930T020111Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Cameron Van Eck (RSAA) "Bringing radio polarization surveys into th e 21st century" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171110T040000Z DTEND:20171110T042000Z DTSTAMP:20261011T152429Z UID:c1m2erkdc8ta93ic5n76evd4dk@google.com CREATED:20171018T071613Z DESCRIPTION:Current cosmological simulations studying galaxy evolution incl ude a model for AGN feedback that seeds black holes with mass >10^5 h^-1 M _sun when the dark matter halo exceeds a given threshold mass. Taylor & Ko bayashi (2014) introduced a new model\, which seeds black holes at a lower mass based on gas properties. Under the same dark matter halo mass\, blac k holes in Taylor & Kobayashi reach 10^5.21 h^-1 M_sun\, whilst black hole s in other simulations have just been seeded with mass 10^5 h^-1 M_sun. Th is implies that black holes with a smaller seed mass exhibit a higher accr etion rate and produce more feedback energy than black holes with a larger seed mass under the same conditions. Seeding black holes with seed mass 1 0^5.21 h^-1 M_sun\, under the same dark matter halo mass\, could inform mo re physically motivated results for cosmological simulations. LAST-MODIFIED:20171106T003107Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ella Wang (ANU) "Black Hole Seeding in Cosmological Simulations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200619T040000Z DTEND:20200619T043000Z DTSTAMP:20261011T152429Z UID:iegglrefk7idg4i3isr7mdm12c@google.com CREATED:20200604T005106Z DESCRIPTION:Aspiring females in Science\, Technology\, Engineering and Math ematics (STEM) fields need to be shown potential careers are achievable an d given visible role models. However\, currently in NSW\, all students und ertaking a year 11 or year 12 Science course as part of their HSC are only shown a sexist representation of scientists. After this discovery in 2018 \, the #IncludeHer movement was started to see this biased representation in NSW fixed. Since then\, it has grown to a national campaign and sparked conversations with the NSW Education Standards Authority\, Sarah Mitchell \, the Minister for Early Education and Childhood Learning and over 1\,800 signatures in a worldwide petition. In this talk\, I will outline my jour ney running this campaign and the outcomes it is working towards. This tal k is to start the conversation about how we represent scientists to young students and discuss plausible solutions we can begin implementing immedia tely. LAST-MODIFIED:20200604T005106Z LOCATION:ZOOM (host: ) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Kat Ross (ICRAR) "Balancing the Equation: The #IncludeHer Movement" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261124T000000Z DTEND:20261124T010000Z DTSTAMP:20261011T152430Z UID:35ptpd398ogs8cighrbbi9lc64@google.com CREATED:20260615T020030Z DESCRIPTION:TBC LAST-MODIFIED:20260716T070028Z LOCATION:Zoom or Duffield Lecture Theatre (host: TBC) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:1 STATUS:CONFIRMED SUMMARY:Elena Pinetti (CCA\, Flatiron Institute) "TBC" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250812T010000Z DTEND:20250812T020000Z DTSTAMP:20261011T152429Z UID:mkrhnuhrbsqq386cuh6u0ed4l4@google.com CREATED:20250623T121110Z DESCRIPTION:Radio astronomy at centimeter to meter wavelengths has experien ced a technological revolution in the past decade\, enabling transformatio nal combinations of sensitivity\, field of view\, and time resolution. The recent discoveries are headlined by fast radio bursts (FRBs): energetic ( >10^39 erg)\, millisecond-duration impulses observed across the Universe. Although FRBs are likely associated with neutron stars\, they appear to oc cur in a remarkable diversity of environments. Understanding the formation of FRB sources is thus intertwined with problems in neutron-star formatio n. Regardless of their origins\, FRBs form exquisite tracers of the conten ts and physical conditions of the otherwise ''missing'' baryons along thei r sightlines. My group and I have built the Deep Synoptic Array (DSA-110) radio telescope\, which is discovering and pinpointing FRBs to host galaxi es at a world-leading rate. The results from our program shed new and deci sive light on the origins of FRBs. Further\, DSA-110 discoveries have\, fo r the first time\, sensitively determined the split between the cosmic bar yon contents around and in between galaxies. Our results favor scenarios w here moderately strong feedback from galaxy formation processes evacuate g alaxy halos\, and pave the way for the role of FRBs in precision cosmology . LAST-MODIFIED:20250807T012207Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Ashley Tan) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Vikram Ravi (Caltech) "Fast Radio Bursts" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151029T000000Z DTEND:20151029T010000Z DTSTAMP:20261011T152429Z UID:j4da3gi8l63gd9mrslkg3a39es@google.com CREATED:20150827T082115Z DESCRIPTION:Aboriginal and Torres Strait Islander people developed complex knowledge systems around the sun\, moon\, and stars. Stellar positions and properties (such as declination\, colour\, brightness\, and scintillation ) were important for navigation\, calendars\, economics\, and time-keeping . Transient astronomical phenomena (including comets\, meteors\, eclipses\ , and aurorae) reinforced sacred law and cultural practices and served as a moral charter. This talk will explore the various ways in which scientif ic astronomical knowledge was encoded in Indigenous oral and material trad itions. Videos of dances and songs recently recorded during ethnographic f ieldwork in the Torres Strait will be presented for the first time. LAST-MODIFIED:20151027T001105Z LOCATION:Duffield Lecture Theatre (host: David Nataf) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Duane Hamacher (UNSW) "The Science of Australian Indigenous Astrono my" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180925T010000Z DTEND:20180925T020000Z DTSTAMP:20261011T152429Z UID:9ou3iqk6c9p31aba3afjdmetho@google.com CREATED:20180920T014606Z DESCRIPTION:Diffuse Interstellar Bands (DIBs) are enigmatic absorption feat ures that are found in the spectra of reddened stars or other objects. Ide ntifying the carriers of DIBs has been a longstanding challenge and is sti ll very much a work in progress. Among of the proposed carriers are polyat omic molecules\, such as fullerenes. Despite their unknown carriers\, DIBs can be a potential tracer of ISM because (1) DIBs are numerous (around 50 0 bands are known at optical and IR wavelengths)\, (2) DIBs are not easily saturated\, and (3) DIBs are correlated with interstellar extinction. To perform automated DIB fitting to be applied to extensive data from stellar surveys and to build DIB databases\, different approaches are needed to e xtract DIBs from early and late type star spectra. The DIB databases can b e used as a complementary tool for locating interstellar clouds and to con struct 3D ISM map in the Galaxy. LAST-MODIFIED:20180921T002606Z LOCATION:Duffield Lecture Theatre (host: Zerjal) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Lucky Puspitarini (Institut Teknologi Bandung) "Extracting Diffuse Interstellar Bands from Stellar Spectra" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190307T000000Z DTEND:20190307T010000Z DTSTAMP:20261011T152430Z UID:s59uhi40ppkq6fbgupl0598h1o@google.com CREATED:20181214T080117Z DESCRIPTION:Two sample return missions are currently at their target astero ids. The JAXA Hayabusa2 mission is at asteroid Ryugu while NASA Osiris-RE x is at asteroid Bennu. These are C-type asteroids with a spectrum that i s flat and of low albedo. They are the first of a new type of object now termed “spinning top” asteroids because of their diamond shaped profil e. The asteroids have rubbly surfaces with numerous boulders and craters. Hayabusa2 has just completed a successful sampling touchdown while Osiri s-REx is scheduled to take a sample in December. These sample return miss ions are important because they take samples of the very surface of the as teroids. As such they give a different view of the parent bodies compared to meteorites which are ablated on their entry through Earth’s atmosphe re. LAST-MODIFIED:20190305T011107Z LOCATION:CSO Common Room (host: Pingel) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Trevor Ireland (RSES) "Sampling Spinning-top asteroids" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20250307T030000Z DTEND:20250307T040000Z DTSTAMP:20261011T152429Z UID:ns7ema98tfergdon5h9ln6ccso@google.com CREATED:20250131T012123Z DESCRIPTION:Thanks to high-sensitivity\, wide-band polarization observation s by the Square Kilometre Array and its pathfinders such as ASKAP\, the st udy of cosmic magnetic fields is expected to make significant progress thr ough the use of Faraday tomography\, which enables the tomographic imaging of magnetic field structure along the line of sight (LOS). The Faraday to mography provides information on parallel and perpendicular components of the magnetic field structure along the LOS\, but the distance to the struc tures cannot be obtained in principle. On the other hand\, by using star- light polarization with known distances\, it is possible to obtain informa tion about the perpendicular component of the magnetic field structure alo ng the LOS and the distance to the structure. By combining these two data\ , it is expected to obtain three-dimensional information on the physical d istance to and the perpendicular and parallel components of the magnetic f ield structures along the LOS\, which could lead to a detailed understandi ng of the three-dimensional magnetic field structure of the Milky Way. I w ill overview the Faraday tomography technique and introduce the ideas and some results of this research. LAST-MODIFIED:20250226T045108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Amit Seta) \nZoom: https:/ /anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Shinsuke Ideguchi (NAOJ) "Probing 3D structure of the Milky Way mag netic field using Faraday tomography and star-light polarization" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20211207T000000Z DTEND:20211207T010000Z DTSTAMP:20261011T152429Z UID:aqptmpgck2h4vjnboftuim7n3s@google.com CREATED:20210927T081613Z DESCRIPTION:Nowadays\, with current and future astronomical facilities and large-scale sky surveys\, hundreds of millions of galaxies are imaged. Con ventional techniques for galaxy morphology become challenging\, even impos sible to apply and analyse numerous datasets generated in the coming era. Hence\, machine learning techniques are of paramount importance in future galaxy studies. In this talk\, I will start with how supervised machine le arning techniques assist in the task of galaxy morphological classificatio n. I will discuss a variety of issues from two perspectives: machine learn ing and the definition of galaxy morphological types. After this\, I will introduce unsupervised machine learning applications to explore galaxy mor phology which provides a new insight towards galaxy morphological classifi cation. In particular\, machines decide a classification system to describ e the variation shown in galaxy morphology in the dataset. The methodology results in 27 machine-defined classes which are physically distinctive fr om each other. When we merge these machine classes into two main classes f or binary classification\, the unsupervised method provides an accuracy of 87% for separating early-type (ETG) and late-type galaxies (LTG) using a dataset with the morphology distribution of nearby galaxies (i.e.\, 22.7% ETG and 77.3% LTG). LAST-MODIFIED:20211206T114107Z LOCATION:ZOOM only (host: Lyla Jung) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ting-Yun (Sunny) Cheng (Durham University\, UK) "Invited Colloquium : Beyond the Hubble Sequence - What can a machine tell us?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220517T010000Z DTEND:20220517T020000Z DTSTAMP:20261011T152429Z UID:4nlkdg9e0bkonr7ce89rkf64bs@google.com CREATED:20220414T042115Z DESCRIPTION:HII regions are not simple objects. Turbulent flows that may be supersonic\, Herbig-Haro jets often crisscross sections of the nebula\, s tellar winds from the massive stars are some of the processes at work. A p articular observation has been nagging astrophysicists for some 70 years\, called the abundance discrepancy problem (ADP). Essentially\, the abundan ce measured from collisionnally excited lines is quite different from the one measured via recombination lines. Factors from 3-5 were measured\, it is even worst for planetary nebulae. A number of physical processes have b een proposed but none reproduce the observations. We proposed a new system atic approach using the SITELLE Fourier transform spectrometer at the Cana da-France-Hawaii Telescope and Fabry-Perot observations from the Observato ire du mont Megantic and Observatoire de Haute-Provence. We targeted the H II region Sh2-158 and a section of the Orion nebula. I will discuss mainly the CFHT results from Sh2-158 LAST-MODIFIED:20220510T025608Z LOCATION:DLT & ZOOM (host: Jackie) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Gilles Joncas (Laval University) "Invited Colloquium: Thermodynamic s of HII regions: Sh2-158" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230427T010000Z DTEND:20230427T020000Z DTSTAMP:20261011T152429Z UID:l083bc4c1ahkflng1j3vlq44m8@google.com CREATED:20230407T093108Z DESCRIPTION:Next generation experiments such as the Vera Rubin Observatory Legacy Survey of Space and Time (LSST) will provide a rich source of infor mation for multi-messenger astronomy tasks. To fully harness the power of these surveys\, we require analysis methods capable of dealing with large streams\, and which can identify promising transients within minutes for f ollow-up coordination. In this talk I will present Fink\, an astronomy bro ker specifically designed for LSST. Fink is based on high-end technology a nd designed for fast and efficient analysis of big data streams. It has be en chosen as one of the official LSST brokers who will receive the full da ta stream. I will highlight the state-of-the-art machine learning techniq ues used to generate early classification scores for a variety of time-dom ain phenomena\, including kilonovae. I will also describe the current effo rts being developed in Australia (https://www.ozgrav.org/ozfink-workshop-2 023.html) that will enable easy access to LSST the data stream through Fin k\, and discuss the possibility to develop tailored filters and science mo dules for other applications. In combination with other efforts already de veloped within the Fink community\, this collaboration has the potential t o boost scientific outcomes from searches for electromagnetic counterparts of gravitational waves. LAST-MODIFIED:20230416T231209Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Emille Ishida (Universite Clermont-Auvergne) "Fink: enabling multi- messenger astronomy in the Rubin era" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200722T031000Z DTEND:20200722T055000Z DTSTAMP:20261011T152429Z UID:608dv8vfpabmer7j16euqunhks@google.com CREATED:20200708T235207Z DESCRIPTION:Nicholas Killerby-Smith (13:10-13:30)\, Matt Roth (Proposal Tal k 13:30-14:00)\, Rajsekhar Mohapatra (14:00-14:20)\, Markus Dirnberger (14 :20-14:40)\, Afternoon Tea (14:40-15:00)\, Zefeng Li (Proposal Talk 15:00- 15:30)\, Jamie Soon (15:30-15:50) LAST-MODIFIED:20200708T235207Z LOCATION:ZOOM 997 8534 1005 (host: Travouillon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA HDR Students "HDR Student Annual Reviews" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20161110T000000Z DTEND:20161110T010000Z DTSTAMP:20261011T152429Z UID:ioj3gli1qk3cr9r7mk5eb7qrs4@google.com CREATED:20161014T024605Z DESCRIPTION:I will discuss the conditions for disk galaxies to produce supe rbubbles that can break out of the disk and produce galactic winds. With t he help of 2D hydrodynamic simulations\, we study superbubbles created by multiple supernova explosions. I will present our results which show that energy injection rate (surface density) needs to be ∼ 0.1 M_solar yr^− 1 kpc^−2 to create superbubbles that break out of the disk with sufficie nt speed for producing galactic winds. We also calculate the escape fracti on of ionizing photons through the dynamically evolving superbubble. We fi nd that the ionizing photons escape within a narrow cone angle of approxim ately 40 degrees \, consistent with observations of nearby galaxies. We sh ow how the escape fraction depends on the disk parameters (density\, scale height). Recent observations of nearby starburst galaxies have found mole cular outflows with molecular mass of 10^7 – 10^8 M_solar and with speed s of a few 10s of km/s at distances around 500 pc. We outline a scenario i n which molecules can form in dense superbubble shells of starburst nuclei . LAST-MODIFIED:20161109T002105Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Arpita Roy (RSAA) "Superbubble: energetics\, feedback to ISM\, esca pe path for ionizing photons\, and molecule formation" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150220T030000Z DTEND:20150220T032000Z DTSTAMP:20261011T152430Z UID:l3mdl5e5445775j840aejfl354@google.com CREATED:20150119T064111Z DESCRIPTION:Many intermediate-age star clusters in the Magellanic Clouds ex hibit very unusual features in their colour-magnitude diagrams that sugges t they may have formed their stars over periods spanning hundreds of milli ons of years per cluster. This poses a major challenge for theoretical mod els and is at odds with what we think we observe for very young systems th at are forming right now. Nonetheless\, this interpretation is enticing in the context of the formation of ancient globular clusters\, which almost always exhibit puzzling abundance patterns that apparently require multipl e episodes of star formation to explain. I will review some recent develop ments in this field - can individual star clusters really form over such e xtended intervals\, and are the Magellanic Cloud objects good stepping sto nes for understanding the formation of globular clusters? LAST-MODIFIED:20150216T223205Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dougal Mackey (RSAA) "Slowly-forming star clusters - fact or fictio n?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170912T010000Z DTEND:20170912T020000Z DTSTAMP:20261011T152430Z UID:sgt3lcnliah0hpe7frhn0hbt60@google.com CREATED:20170808T043614Z DESCRIPTION:TBD LAST-MODIFIED:20170912T102606Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dary Alexandra Ruiz (ANU) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230316T000000Z DTEND:20230316T010000Z DTSTAMP:20261011T152430Z UID:chslc1vn8663sffe28sg6kj8o4@google.com CREATED:20230125T032111Z DESCRIPTION:My thesis will cover the Cosmology application of Fast Radio Bu rsts (FRBs) and the study of FRBs' origin. FRBs are mysterious millisecond radio signals. Using the scattering information from localized FRBs\, we can have a better estimation of the Dispersion Measure (DM) contributed by the host galaxy components (DMh)\, and thus the DM contributed by the int ergalactic medium (IGM)\, DM. Based on these results\, the Hubble constant and Cosmological parameters can be constrained more accurately than in pr evious works that did not account for scattering. Another project is about the future constraints on the dark matter with gravitational lensed FRBs. My home country\, Taiwan is building a new telescope\, the Bustling Unive rse Radio Survey Telescope in Taiwan (BURSTT) dedicated to FRB searches. I n this project\, I estimate the probability to find gravitationally lensed FRBs\, based on the scaled redshift distribution from the latest CHIME ca talog (Masui and Chime/Frb Collaboration\, 2021) and the lensing probabili ty function from (Munoz et al.\, 2016). Using this result\, we can constra in primordial black holes (PBHs) to form a part of dark matter in the low mass range (down to 10-4 solar mass). While doing this project\, I also ho pe to link the Australian and Taiwanese astronomy communities together and look forward to more future collaboration. Besides Cosmology\, I will pre dict the number of FRB detection from Globular Clusters (GCs). We will use MeerKAT data and CryoPAF-Parkes data for this project. A last possible si de project that I will be working on is the search for the optical counter parts of FRBs with the Tomo-e Gozen telescope and the Seimei telescope. Bo th of these projects will lead us to a better understanding of the FRB ori gin. LAST-MODIFIED:20230307T230611Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Simon Ho (RSAA) "A Pursuit of Fast Radio Bursts' Origin and their C osmological Applications (Thesis Proposal)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160623T230000Z DTEND:20160624T000000Z DTSTAMP:20261011T152429Z UID:15n2e6seq7mdqh0gv8psjvfpg4@google.com CREATED:20160504T030116Z DESCRIPTION:TBD LAST-MODIFIED:20160504T030116Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Annual Student Talks (RSAA) "Various" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20191119T000000Z DTEND:20191119T010000Z DTSTAMP:20261011T152430Z UID:aig4e9naj7mai83jlq0qigvs8s@google.com CREATED:20191029T102108Z DESCRIPTION:Cosmological simulations predict that early-type galaxies (ETGs ) are the results of extended mass accretion histories. The latter are cha racterized by different numbers of mergers\, mergers mass ratios and gas f ractions\, and timing. Depending on the sequence and nature of these merge rs that follow the first phase of the in-situ star formation\, these accr etion histories may lead to ETGs that have low or high mass halos\, and th at rotate fast or slow. Since the stellar halos maintain the fossil record s of the events that led to their formation\, a discontinuity may be in pl ace between the inner regions of ETGs and their outer halos\, because the time required for the halos stars to exchange their energies and momenta i s very long compared with the age of these systems. Exquisite deep photome try and extended spectroscopy for significant samples of ETGs are then use d to quantify the occurrence and significance of such a transition in the galaxies' structural and kinematical parameters. Once this transition radi us is measured\, its dependency with the effective radius of the galaxies light distribution and total stellar masses can be investigated. Such corr elations can then be compared with the predictions of accreted\, i.e. ex-s itu vs. in-situ components from cosmological simulations to validate such models. LAST-MODIFIED:20191110T175106Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Magda Arnaboldi (ESO) "Elliptical galaxies/stellar halos connection " TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170825T043000Z DTEND:20170825T045000Z DTSTAMP:20261011T152429Z UID:khmkrgjl85pb0q360tekf8svao@google.com CREATED:20170808T233112Z DESCRIPTION:Understanding physical processes responsible for the formation and evolution of galaxies like the Milky Way is a fundamental problem in a strophysics. However\, a key challenge is that the properties and orbits o f the stars can only be observed at present: to understand what happened i n the Milky Way at earlier epochs\, one must explore "archaeological" tech niques. One idea\, "chemical tagging"\, aims to probe the history of the M ilky Way via the unique imprint in chemical abundance space of long-disrup ted star forming associations. I will discuss the opportunities and challe nges associated with chemical tagging\, including a first constraint on th e disrupted cluster mass function in the Milky Way\, and how extragalactic IFU studies could be informative in the studies of chemical tagging. I wi ll also describe a new set of tools for efficient measuring multi-elementa l abundances from large quantities of low-resolution stellar spectra\, der iving the binary fraction of the Milky Way\, and inferring asteroseismic p arameters from spectra alone. LAST-MODIFIED:20170825T014106Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Yuan-Sen Ting (RSAA) "GALAH and FunnelWeb in the new era of Galacti c Archaeology" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160324T000000Z DTEND:20160324T010000Z DTSTAMP:20261011T152429Z UID:vgn8dhdged81h2ekt90kp2lng4@google.com CREATED:20160317T065105Z DESCRIPTION:TBD LAST-MODIFIED:20160323T125105Z LOCATION:Duffield Lecture Theatre (host: Helga Denes) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Douglas Scott (University of British Columbia) "The Universe accord ing to Planck" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200924T010000Z DTEND:20200924T013000Z DTSTAMP:20261011T152429Z UID:0m5vuug2h8uuft8cu65o5h9rso@google.com CREATED:20200907T041109Z DESCRIPTION:TBD LAST-MODIFIED:20200907T041110Z LOCATION:ZOOM 997 8534 1005 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dávid Guszejnov (UT Austin (USA)) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20231214T000000Z DTEND:20231214T010000Z DTSTAMP:20261011T152429Z UID:kha25e864uj5v1gvse01fk7bms@google.com CREATED:20231112T230119Z DESCRIPTION:Globular clusters (GCs) are among the most ancient objects in t he local Universe\, acting as tracers of galaxy formation across both spac e and time. With the recent JWST discovery of nitrogen-rich star formation in a redshift 11 galaxy\, and the discovery that over 50% of the in-situ stars in the Milky Way (MW) likely formed in clusters\, understanding the role of GCs in the context of galaxy evolution is becoming ever more impor tant. The MW hosts a large (~150) and diverse population of GCs. Among the se clusters\, a fraction are thought to have formed in-situ\, alongside th e MW\, while others were likely accreted alongside disrupted dwarf galaxie s. A small number of MW GCs may themselves be the sole remaining remnants of disrupted dwarf galaxies as stripped nuclear star clusters. In this tal k I will discuss ongoing work to identify the origins of accreted GCs\, hi ghlighting the strength of combining high resolution chemical abundances w ith dedicated dynamical simulations. I will present results for population s of accreted GCs as well as individuals\, presenting initial results as t o the origins of the MW's two most enigmatic GCs\, NGC 2419 and M 22. LAST-MODIFIED:20231211T001107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBC) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Stephanie Monty (Cambridge U.) "Galactic Archaeology with Globular Clusters" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190731T010000Z DTEND:20190731T020000Z DTSTAMP:20261011T152429Z UID:6vd9pmp2g4of4jl63jomdgf348@google.com CREATED:20190605T025608Z DESCRIPTION:One of the most obvious missing links in the emerging network o f international multi-wavelength astronomy is fully dedicated\, large aper ture\, highly multiplexed spectroscopy at a range of spectral resolutions in the optical and near infrared wavelength range. The Maunakea Spectrosco pic Explorer (MSE) is designed to fill this gap and is the only such facil ity currently at an advanced stage of development\, having recently compet ed a 3 year system conceptual design. Australian scientists and engineers have been a critical component of the collaboration since the beginning. M SE is completely dedicated to multi-object spectroscopy of samples of thou sands and millions of astrophysical objects. It will lead the world in thi s arena\, due to its unique design capabilities: it will boast a large (11 .25 m) aperture and wide (1.52 sq. degree) field of view\; it will have th e capabilities to observe at a wide range of spectral resolutions\, from R 2500 to R40\,000\, with massive multiplexing (4\,332 spectra per exposure\ , with all spectral resolutions available at all times). More than 10 mill ion fiber-hours of 10m-class spectrscopy is available per year with MSE\, and it will provide critical follow-up for multi-wavelength imaging surve ys\, such as those of the LSST\, Gaia\, WFIRST and the SKA. MSE enables a synergy between wide-field imaging surveys and pointed follow-up by the up coming generation of extremely large telescopes. In this presentation\, I will provide an overview of MSE\, describing the many science drivers that it will enable in a broad range of fields\, from exoplanetary systems thr ough to the Milky Way\, black holes\, cosmology and dark matter. I will re view the current design status\, as well as the international partnership\ , and I will focus on the important roles played by Australian colleagues in its development so far. I will describe the plan for completing MSE des ign and construction and will highlight the opportunities for Australia as we approach first light of this transformational facility. LAST-MODIFIED:20190725T163108Z LOCATION:Duffield Lecture Theatre (host: Monty) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Alan McConnachie (NRC Herzberg) "Massively multiplexed spectroscopy for the coming decades: the science" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260421T013000Z DTEND:20260421T023000Z DTSTAMP:20261011T152430Z UID:ikq8bh48s71rt66i876k7un8hs@google.com CREATED:20260323T234810Z DESCRIPTION:TBD LAST-MODIFIED:20260323T234811Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ben Pope (Macquarie U.) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20261105T000000Z DTEND:20261105T010000Z DTSTAMP:20261011T152430Z UID:nhbvel7818up0pe0njg1j85vds@google.com CREATED:20260615T020032Z DESCRIPTION:TBC LAST-MODIFIED:20261006T060010Z LOCATION:Zoom or Duffield Lecture Theatre (host: Naomi McClure-Griffiths) \ nZoom: https://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOnt d.1 SEQUENCE:3 STATUS:CONFIRMED SUMMARY:Hilay Shah (RSAA) "TBC (End-of-thesis talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160421T010000Z DTEND:20160421T020000Z DTSTAMP:20261011T152429Z UID:26ngjekucilehnifvc4m1kd858@google.com CREATED:20160228T234115Z DESCRIPTION:We present a series of our studies on how HI is accreted\, dist ributed and connected with the formation of optical structures in massive disk galaxies in the low redshift universe. First We introduce the Bluedis k project\, an HI imaging survey with the aim of searching for signs of ga s accretion in massive HI-excess disk galaxies. Major and minor merger eve nts are ruled out as the main source of gas accretion. We found an HI-rich environment around HI-rich galaxies\, out to a projected distance of 1 Mp c and systematic velocity difference of 500 km/s\, supporting a scenario w here the central galaxies are fuelled by an extended gas reservoir. We rev isit the remarkably tight HI size-mass relation of galaxies. We find that the scatter around the relation does not depend on mass or HI richness of galaxies. We discuss its constrain on galaxy formation models. We show tha t the cold gas is closely connected with the formation of central bulges\, bars\, disks and disk outskirts in massive disk galaxies. LAST-MODIFIED:20160418T043605Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jing Wang (CSIRO) "Gas accretion and the subsequent evolution of ma ssive disk galaxies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171026T000000Z DTEND:20171026T010000Z DTSTAMP:20261011T152429Z UID:p24ac9panis9c9t27rf1slgn8s@google.com CREATED:20170912T102611Z DESCRIPTION:Our current understanding of galaxy formation is based on the presence of an elusive matter component: the Cold Dark Matter (CDM). Such a component is extremely successful explaining and reproducing the large scale structure of the Universe\, on the other hand many have claimed that CDM is incompatible with observations on galactic and sub-galactic scales . In my talk I will first summarize the numerical techniques used to study structure formation and then revisit the problems of CDM on small scales within the galaxy formation framework. I will show that current data do no t disprove or challenge the CDM model\, and that claims in this direction are based on a poor comparison between data and theoretical predictions. I will conclude presenting some future tests that might tell us if CDM is i ndeed the right model for the unseen matter component of our Universe. LAST-MODIFIED:20171018T071606Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Andrea Maccio (NYU Abu Dhabi) "Cold Dark Matter dies hard" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190723T010000Z DTEND:20190723T020000Z DTSTAMP:20261011T152429Z UID:q6u6ede67dh08ulin6b8oolr2k@google.com CREATED:20190612T025106Z DESCRIPTION:The ionized interstellar medium (ISM) provides essential inform ation on the star-forming environments\, metal enrichment\, and underlying ionizing radiation field in galaxies. It is crucial to understand how the ionized ISM evolves with Cosmic time. In this talk\, I will present a sam ple of local galaxies that closely resemble the properties of high-redshif t galaxies at high redshift. These local analogs of high-redshift galaxies provide a unique local laboratory to study high-redshift galaxies. I will discuss how to use these analogs to improve our understanding of the high -redshift metallicity empirical calibrations and physical mechanism(s) to drive the evolution of optical diagnostics lines from high redshift to low redshift. LAST-MODIFIED:20190722T040604Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Fuyan Bian (ESO) "Evolution of Ionized Interstellar Medium from Hig h-redshift to Low-redshift." TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241126T000000Z DTEND:20241126T010000Z DTSTAMP:20261011T152429Z UID:kirc7mq3rqovgjlo073t14j20g@google.com CREATED:20240815T063639Z DESCRIPTION:The hunt for dark matter's true nature has led us to an unexpec ted cosmic signpost: the distribution of interstellar and intergalactic du st. Through high-resolution hydrodynamical simulations of Milky Way-type h aloes\, I'll demonstrate how dust could serve as an observational discrimi nator between cold dark matter (CDM) and warm dark matter (WDM). Our simul ations reveal how CDM's enhanced substructure necessitates higher supernov a efficiency\, compared to WDM\, to reproduce observed satellite galaxy po pulations. This creates distinct dust production rates and distributions a round host galaxies. I'll present our published results examining dust mas s and distribution across cosmological models\, before discussing broader implications for galaxy modelling with supercomputers and new applications of AI for understanding galactic evolution. LAST-MODIFIED:20241106T065614Z LOCATION:ZOOM and Duffield Lecture Theatre (host: Vanhiep Nguyen) \nZoom: h ttps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Darren Croton (Swinburne) "Cosmic dust as a dark matter discriminat or" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170504T010000Z DTEND:20170504T020000Z DTSTAMP:20261011T152429Z UID:nl213hkkqbpf7jp3knb4jp4sk0@google.com CREATED:20170409T233606Z DESCRIPTION:Find abstract at: https://physics.anu.edu.au/events/?EventID=63 7 LAST-MODIFIED:20170424T000104Z LOCATION:China in the World Auditorium\, building 188 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Chris McKee (UC Berkeley) "Baryons and Dark Matter in the Galaxy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160830T010000Z DTEND:20160830T020000Z DTSTAMP:20261011T152429Z UID:jv6javtprlt0nf7fphnd1q0cbg@google.com CREATED:20160725T002613Z DESCRIPTION:The Zwicky Transient Facility (ZTF) has been designed with a si ngular focus: a systematic exploration of the night sky at a magnitude lev el well suited for spectral classification and follow up with the existing class of 4-m to 10-m class telescopes. ZTF is a public-private partnershi p with equal contributions from a consortium of world-wide partners and an NSF MSIP grant. The discovery engine for ZTF is a 47 square degree camera (realized through 16 e2V monolithic CCDs) that fills the entire focal pla ne of the 48-inch Oschin telescope of the Palomar Observatory. This clarit y allows an exploration of different cadences and thus opens up the possib ility for a thorough exploration of the dynamic optical sky. In short\, ZT F is an experiment of Time Domain Astronomy (TDA) experiments. ZTF consis ts of a 47 square degree camera on the Palomar Oschin 48-inch telescope (P 48) and the Spectral Energy Distribution Machine (SEDM)\, a low resolution IFU spectrograph tuned for variability/transient classification\, on the Palomar 60-inch telescope. The SEDM is already commissioned and the camera on P48 is expected to see first light in January 2017. At the short caden ce end\, ZTF will detect one young supernova (<1 day) every day. For mid-c adence we expect a veritable explosion of cosmic explosions. For long cade nce\, ZTF will be a prodigious factory for Tidal Disruption Events and Sup er-Luminous Supernovae. Visiting the Galactic Plane 300 times a year ZTF w ill be prove to be a bonanza for stellar astronomers. Since ZTF is PI-led effort there is considerable room for innovation and rapid implementation. In short\, ZTF is a TDA pathfinder for LSST. LAST-MODIFIED:20160826T154106Z LOCATION:Duffield Lecture Theatre (host: Joao Bento) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Shri Kulkarni (Caltech) "The Zwicky Transient Facility" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20221028T030000Z DTEND:20221028T033000Z DTSTAMP:20261011T152429Z UID:2bvhjmis23l3u9slfa6m40t6f8@google.com CREATED:20221017T025111Z DESCRIPTION:Back in February I took an interest in celestial navigation (fi nding a ship's position from astronomical measurements). I knew almost not hing about it\, and learned some interesting things I wanted to share. An unexpected mashup of astronomy\, history\, and... computer games? LAST-MODIFIED:20221024T182109Z LOCATION:DLT & ZOOM (host: TBD) \nZoom: https://anu.zoom.us/j/99785341005?p wd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Cameron Van Eck (RSAA) "How Does Celestial Navigation Even Work\, A nyways?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160908T010000Z DTEND:20160908T020000Z DTSTAMP:20261011T152429Z UID:60uosjdcmh5viq9ks6lk7bp07c@google.com CREATED:20160725T044114Z DESCRIPTION:The development of sensitive Near Infra-Red instruments has mad e it possible to study the galaxy properties at z~2\, just 3Gy after the B ig Bang. This is expected to be the time period where galaxies are activel y star forming and evolving rapidly to form the massive galaxies that are observed in our local neighbourhood. ZFIRE is a survey\, which utilises th e MOSFIRE instrument on Keck telescope over 18 nights to study properties of ZFOURGE selected mass complete galaxies in rich environments at z~2. In my talk I will present results of our attempt to constrain the Initial Ma ss Function (IMF) of galaxies at these redshifts using a cluster and a fie ld sample. We have investigated the degeneracy between the star formation histories and the IMF to make strong constrains on the stellar mass distri bution of these galaxies using synthetic stellar spectra. I will focus on the role of dust\, star-bursts\, stellar rotation\, binaries\, and metalli city on determining observed galaxy properties at z~2 to address whether Z FIRE results favour the canonical concept of a universal IMF. LAST-MODIFIED:20160904T234604Z LOCATION:Duffield Lecture Theatre (host: Melanie Kaasinen) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Themiya Nanayakkara (Swinburne University) "In-situ IMF at z~2" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200128T000000Z DTEND:20200128T003000Z DTSTAMP:20261011T152429Z UID:gq1krs6ohuuvfcvbfb850ik438@google.com CREATED:20191128T031109Z DESCRIPTION:On average girls earn higher grades in maths than boys in schoo l\, yet fewer women than men are employed in maths-intensive careers in Sc ience\, Technology\, Engineering\, and Mathematics (STEM). According to th e 'variability hypothesis'\, this over-representation of males is driven b y gender differences in variance\; greater male variability leads to great er numbers of men who exceed the performance threshold\, particularly in c areers associated with innate talent or brilliance (e.g. 'rocket science') . In this talk I will present results from a meta-analysis suggesting grea ter variability is insufficient to explain male over-representation in STE M\, as gender differences in both mean and variance of student grades are smaller in STEM than non-STEM subjects. I will then discuss research more broadly on why gender gaps in STEM persist\, and what can be done to incre ase the participation of women in male-dominated fields. Link for registra tion: https://www.eventbrite.com/e/why-are-fewer-women-than-men-employed-i n-fields-associated-with-brilliance-tickets-90271888649 LAST-MODIFIED:20200122T021105Z LOCATION:Duffield Lecture Theatre (host: Rey) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Rose O'Dea (University of New South Wales) "Why are fewer women tha n men employed in fields associated with brilliance?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241011T030000Z DTEND:20241011T033000Z DTSTAMP:20261011T152429Z UID:3dhgvqffrgc6bsefmvs2tql03o@google.com CREATED:20240918T130617Z DESCRIPTION:I will be showing off a side project myself and Neco Kriel have been working on that we have dubbed "Chi-Scrapper"\, this handy bit of so ftware searches the ArXiv for articles matching keywords for your researc h interests and then uses a small LLM to rank them according to their rele vance to your research interests. It can run locally\, or on the cloud\, a nd outputs in markdown\, or into a pretty Web UI. LAST-MODIFIED:20241002T233611Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Cameron Jones (RSAA) "ArXiv curation tools" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260428T013000Z DTEND:20260428T023000Z DTSTAMP:20261011T152430Z UID:n01hpfjabmnu57dcqaaldgg43o@google.com CREATED:20260503T120049Z DESCRIPTION:The conventional approach in astronomical instruments is to sam ple the signal at more than twice the Nyquist frequency\; for example\, th e pixels in an imager are generally less than half the full-width half max imum of the point spread function\, and in spectroscopy spectral pixels ar e less than half the full-width half maximum of the line spread function. This leads to a requirement for very large numbers of pixels in order to sample a wide-field image or a broad-band spectrum. However\, recent dev elopments in data science have shown that for certain types of signal\, it is possible to significantly under-sample measurements and recover the fu ll signal at high fidelty using a technique called compressed sensing. In this talk I will describe this technique\, and its applicability to astro nomy. I will discuss potential applications to the design of astronomical instruments with optimised sampling\, including imaging\, spectroscopy\, and wavefront sensing\, with far fewer pixels than conventional instrument s. LAST-MODIFIED:20260503T120049Z LOCATION:Zoom or DLT (host: Hajime Ogane) \nZoom: https://anu.zoom.us/j/829 74980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Simon Ellis (Macquarie U.) "Beating Nyquist: Compressed Sensing in Astronomical Instrument Design" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210617T030000Z DTEND:20210617T040000Z DTSTAMP:20261011T152429Z UID:4ag7g58slsj4h233tre59gfcao@google.com CREATED:20210614T235606Z DESCRIPTION:In this thesis we analyse the observational relations between g alaxy structure and global stellar population properties to determine the dependencies between a galaxy's star formation and mass assembly histories . Stellar population parameters correlate with a range of galaxy propertie s\, but it is unclear which relations are causal and which are the result of another underlying trend. The well-established correlations between mas s and other galaxy properties are often considered evidence for mass drivi ng a galaxy's evolution. However\, we find that\, at fixed mass\, stellar population properties show significant dependence on size\, indicating tha t the size of a galaxy is also an important property tracing\, and possibl y influencing\, its evolution. The focus of the thesis is to quantitativel y compare trends between various stellar population properties and key gal axy structural parameters --- in particular the galaxy's mass\, gravitatio nal potential\, and surface density --- in order to determine which relati ons are intrinsically tighter and are therefore more likely to reflect a c ausal relation. We divide our work into three parts focusing on early-type galaxies\, star-forming galaxies and micro high-redshift galaxies\, respe ctively. This division reflects both the physical differences between thes e samples\, as well as technical differences in measuring their stellar po pulation properties. LAST-MODIFIED:20210615T021608Z LOCATION:ZOOM and DLT (host: Sven Buder) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tania Barone (RSAA) "End-of-Thesis Colloquium: Galaxy Evolution: Th e link between a galaxy's structure and its stellar population" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220412T010000Z DTEND:20220412T020000Z DTSTAMP:20261011T152429Z UID:0391snck26h832fdartthjgum8@google.com CREATED:20220405T001608Z DESCRIPTION:Vera C. Rubin Observatory will open a new era for optical astro nomy. For 10 years\, Rubin will image the Southern Sky at unprecedented de pths through the Legacy Survey of Space and Time (LSST). I will introduce Fink\, selected to process LSST time-domain data. Fink is designed to iden tify and communicate the most promising time-domain candidates for a bread th of science. LSST holds the keys to fundamental questions such as the na ture of Dark Energy and the characterisation of astrophysical events. To m ake this leap\, I will review recent results and advances in supernova cos mology from the Dark Energy Survey. I will also highlight the potential of studying new events such as kilonovae to characterise our Universe and it s extreme physics. Finally\, I'll discuss the potential of connecting Rubi n with Australian facilities through Fink to harness unique opportunities for cosmology and multi-wavelength and messenger astronomy. LAST-MODIFIED:20220411T011708Z LOCATION:DLT & ZOOM (host: Marcus Birch) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Anais Moller (Swinburne) "Invited Colloquium: The next generation f or supernova cosmology and time-domain astronomy" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200924T010000Z DTEND:20200924T013000Z DTSTAMP:20261011T152429Z UID:9olo412k70cfbha5in4gsfi3gs@google.com CREATED:20200911T060508Z DESCRIPTION:TBD LAST-MODIFIED:20200911T060509Z LOCATION:ZOOM 997 8534 1005 (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dávid Guszejnov (UT Austin (USA)) "TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150414T010000Z DTEND:20150414T020000Z DTSTAMP:20261011T152429Z UID:bjic51df74361fj11gr6kjqpoo@google.com CREATED:20141205T003614Z DESCRIPTION:Asteroseismology - the study of stellar oscillations - is a pow erful tool to probe the structure and evolution of stars. In addition to t he large number of newly discovered exoplanets\, space-based telescopes su ch as Kepler have revolutionized asteroseismology by detecting oscillation s in thousands of stars from the main sequence to the red-giant branch. In this talk I will highlight recent asteroseismic discoveries by Kepler\, f ocusing in particular on exoplanet host stars. I will furthermore discuss current efforts to improve fundamental properties of the Kepler parent sam ple and their importance for deriving accurate planet occurrence rates. Fi nally I will present first asteroseismic results by Kepler's follow-up mis sion\, K2\, and discuss its synergy with the GALAH survey for probing the chemo-dynamical evolution of stellar populations in our Galaxy (galactic a rcheology). LAST-MODIFIED:20150409T012107Z LOCATION:Duffield Lecture Theatre (host: Fang Yuan) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Daniel Huber (University of Sydney) "The Space Photometry Revolutio n of Asteroseismology & Exoplanets" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150508T040000Z DTEND:20150508T042000Z DTSTAMP:20261011T152429Z UID:ag6dm5021immpnm05etukmo1to@google.com CREATED:20150319T040623Z DESCRIPTION:It is possible to piece together the processes that have shaped the observed characteristics of a galaxy by studying its stars in detail. The Large Magellanic Cloud (LMC) is an excellent candidate for this type of study because of its favourable viewing angle and ongoing star formatio n. I present the results of high-resolution VLT/FLAMES observations of ~80 red giant stars around star cluster NGC 1846\, located in the disc of the LMC. I will compare our measured abundances of 18 elements with similar studies in the LMC and Milky Way to compare the chemical evolution of the two galaxies. LAST-MODIFIED:20150501T051106Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Shaheen Iqbal (RSAA) "Elemental Abundance Patterns in the LMC Field Population around NGC 1846" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251009T000000Z DTEND:20251009T010000Z DTSTAMP:20261011T152430Z UID:pkkn4sd3a94oi0dr623q2md6cc@google.com CREATED:20250925T231108Z DESCRIPTION:The main question shaping today's cosmology is the Hubble tensi on\, the apparent discrepancy between the measured near- and far-Universe Hubble constants\, H0\, potentially suggesting physics beyond Lambda-CDM. Most local measurements to date use the concept of the cosmic distance lad der\, the empirical path to H0. In this talk\, I will describe the use of Type II supernovae\, exploding red supergiant stars\, for distance estimat ion\, which provides an independent avenue here. The method we use is base d on the radiative transfer modeling of optical spectra\, yielding precise luminosity estimates. Beyond showcasing the method itself\, I will descri be a number of empirical tests we conducted in recent years\, along with a proof of principle H0 estimate based on a literature sample of objects. LAST-MODIFIED:20251009T113608Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Brian Schmidt) \nZoom: htt ps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Geza Csornyei (ESO) "SNe II the rescue: independent determination o f the Hubble constant through the modeling of Type II supernovae" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181214T030000Z DTEND:20181214T032000Z DTSTAMP:20261011T152429Z UID:ng5nu5l0ul8s71d4bjumgavftk@google.com CREATED:20181212T021105Z DESCRIPTION:As part of the development of an Adaptive Optics Tracking and P ushing (AOTP) system\, the U200-G ULTIMA® Gimbal Optical Mount ('old moun t') and OptoSigma BHAN-50S-N Gimbal Optical Mount ('new mount') were both tested for drift when resting\, ability to adhere to a prescribed circular path\, and for independence of the X and Y axes. It was found that there was a delay after any reversal in direction\, leading to skipped steps\, s o this was also tested in attempt to quantify the delay. It was found that the old mount exhibited signs of drift during supposedly stationary perio ds and a jitter in the undriven axis when the driven axis changed directio n\, leading to a maximum of a 1.2 arcsecond on sky movement. The new mount did not display the signs of drift\, and showed lesser signs of movement in the undriven axis\, with a maximal jitter of 0.6 arcseconds on sky move ment. Both mounts displayed evidence of skipped or missing steps when chan ging direction\, but the exact number was difficult to quantify as tests d id not display the same trends. The number of skipped steps varied between 49 to 105 steps. LAST-MODIFIED:20181213T061104Z LOCATION:CSO Common Room (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jae Boyd (RSAA) "Evaluation and Comparison of Gimbal Mounts for Ada ptive Optics Tracking and Pushing System" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171103T030000Z DTEND:20171103T032000Z DTSTAMP:20261011T152429Z UID:h3bl1lljqvkbc6atqdgb8s9s1c@google.com CREATED:20171011T230107Z DESCRIPTION:The MAGMO HI absorption processing project is a pilot study for moving processing from the manual techniques of the last generation of Ga lactic HI surveys (eg SGPS) to the automated approach needed for the GASKA P project. During the project I analysed the absorption spectra extracted from high spectral and angular resolution HI observations taken in 440 Gal actic plane fields using the Australia Telescope Compact Array. In this ta lk I will discuss the science findings of the project and the processing t echniques used. LAST-MODIFIED:20171101T231107Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:James Dempsey (ANU) "Cold HI in the Milky Way: The MAGMO Sample" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201106T030000Z DTEND:20201106T033000Z DTSTAMP:20261011T152429Z UID:ovjqq9jgnjek3h9igpu2p0dejg@google.com CREATED:20200826T024116Z DESCRIPTION:The new FoF format is like an Open Mic: Our speakers have 15 mi nutes each to talk about topics of their choice. The idea of the new FoF i s to get to know the many individuals that work under the same roof\, allo w newcomers to find friends easily\, and find new friends or colleagues wi th similar interests and hobbies. So feel free to talk about some of your most favourite adventures\, memorable Stromlo anecdotes\, your hobbies\, y our last COVID-DIY project\, your voluntary activities outside of Stromlo or whatever you are passionate about. Science talks (about a scientific to pic/question that you are interested in) are also welcome\, but be mindful of your audience (astronomers\, students\, engineers\, professional staff ). LAST-MODIFIED:20201011T050513Z LOCATION:ZOOM 997 8534 1005 (host: Seta) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tony Travouillon and Matthew Colless (RSAA) "FoF: Phantom Maps and the current status of Hubble constant discrepancies" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181120T030000Z DTEND:20181120T032000Z DTSTAMP:20261011T152429Z UID:nr02281s0k2q2eqkpbo9hlsfh8@google.com CREATED:20181101T050610Z DESCRIPTION:Born out of the 2015 dotAstro conference\, the 'Space Shark' is a small device that can be programmed to point and track objects in the s ky - the goal is to inspire children and adults alike to learn more about astronomy and engineering. For the past 3 months\, our team of six enginee ring students from ANU have been working on a new prototype for the Space Shark to make it more reliable\, more attractive\, and even more education al. In this presentation\, we will showcase the new Space Shark and presen t our work from the past few months. We invite anyone interested to come a long and you might just find out why sharks have anything to do with space . LAST-MODIFIED:20181117T102605Z LOCATION:CSO Common Room (host: Zerjal) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Space Shark Techlauncher Team (AITC) "Space Shark: An Awesome Astro nomical Outreach Device" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170907T010000Z DTEND:20170907T020000Z DTSTAMP:20261011T152430Z UID:4m15b92lctomg8ln1deahabk44@google.com CREATED:20170814T001111Z DESCRIPTION:During the Epoch of Reionization the first sources of energetic photons (stars and quasars) ionized the inter-galactic medium\, forever a ltering the conditions for future star formation and galaxy growth. Observ ing the 21cm emission from neutral hydrogen during this period (which is r edshifted to radio wavelengths here on Earth) and its evolution is a key s cience driver behind the Murchison Wide-field Array (MWA) and the SKA. Fut ure IR observations of high redshift galaxies with JWST and the Wide Field IR Survey Telescope (WFIRST) will further expand our knowledge about the sources driving reionization. In order to fully leverage the combined resu lts of these radio and IR observations\, we need to be able to simultaneou sly model high-redshift galaxy formation and large scale cosmic reionizati on. However\, this is a difficult task. In this talk I will give a brief overview of some of the associated challenges before moving on to discuss semi-analytics as a useful and powerful compliment to other simulation me thods. I will then introduce the Dark-ages Reionization And Galaxy Observ ables from Numerical Simulations (DRAGONS) programme\, and specifically Me raxes\, the first semi-analytic galaxy formation model to include a tempor ally and spatially coupled treatment of galaxy growth and reionization. F inally\, I’ll demonstrate the success of this model in reproducing a num ber of key observables across a broad range of redshifts\, as well as it ’s utility for investigating a number of important topics such as the io nizing photon budget\, 21cm power-spectra\, galaxy sizes and the relative importance of AGN for reionization. LAST-MODIFIED:20170829T011105Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Simon Mutch (University of Melbourne) "The Epoch of Reionization an d DRAGONS" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160707T010000Z DTEND:20160707T020000Z DTSTAMP:20261011T152429Z UID:a0pbo5hm9dhhjgg07rq0anahis@google.com CREATED:20160510T064616Z DESCRIPTION:Extragalactic jets originate from the immediate vicinity of sup ermassive black holes. They interact with their environment forming radio lobes with sufficient cross section to cause galaxy-wide effects. Studying the interaction of jets with their environment therefore promises insight s into the surroundings of black holes\, and effects on galaxy evolution. I will show simulation studies of the jet environment interaction. Compari son with observations allow us to constrain the conditions in the vicinity of the supermassive black holes. A particular\, long-standing question is what the jets are made of\, again related to processes in the immediate v icinity of black holes. For a Galactic jet source\, Mikroquasar V404\, we have detected positrons directly by their annihilation signature in MeV sp ectra with INTEGRAL\, with implications for all black-hole jet systems. Ou r simulations also provide some insight into heating of the intracluster m edium and effects of magnetic fields in and around radio lobes. In gas-ric h galaxies\, jets clear out gas in some parts of the galaxy\, but overall lead to enhanced star formation due to the high pressure applied by the ra dio lobes. A signature of jet-induced stars is their high velocity. Such s tars are observed in the Milky Way and may plausibly have been produced by a recent jet-outburst of SGR A*\, which might also have produced the FERM I bubbles and the excess of positrons currently annihilating in the bulge of the Milky Way. LAST-MODIFIED:20160627T233607Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Martin Krause (University of Tasmania) "Extragalactic Jets" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170421T040000Z DTEND:20170421T042000Z DTSTAMP:20261011T152429Z UID:com2ivrr712nkfp58114tjnpfg@google.com CREATED:20170419T013604Z DESCRIPTION:Molecular clouds show the earliest stages of stellar and planet ary evolution and provide an opportunity to understand how grains grow to form planetary bodies. In molecular clouds with a total visual extinction above a few magnitudes\, some components of the molecular gas freeze out on the surfaces of dust grains. These ice mantles around dust grains are t he sites of complex surface chemistry that leads to the formation of simpl e organic molecules in these mantles. The icy surfaces also facilitate the coagulation of the dust particles\, setting the stage for grain growth an d ultimately the formation of planetary bodies. As part of the JWST NIRCa m GTO program\, we will observe a selection of small molecular cores using the wide field grism spectroscopy mode of NIRCam. I will present the resu lts of a preliminary study of several candidate molecular cores using UKIR T\, Spitzer\, and IRTF. After the preliminary studies we have selected th ree molecular cores in different evolutionary stages for the GTO program: B68\, a quiescent molecular core\, LDN 694-2\, a collapsing pre-stellar co re\, and B335\, a protostellar core. All these cores are seen against a de nse background of stars in the inner Galaxy and offer the opportunity for spatially well-resolved mapping of the ice feature distribution. We will o btain slitless grism spectroscopy with NIRCam in six filters covering the features of H2O\, CO2\, CO\, CH3OH\, and the XCN feature. Simulations usi ng aXeSim have shown that spectrum overlap will occur in a fraction of the spectra\, but will not be a prohibitive problem. LAST-MODIFIED:20170419T032604Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Laurie Chu (University of Hawaii) "Ice Feature Spectroscopy in Near by Molecular Cores With JWST NIRCam" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170717T003000Z DTEND:20170717T013000Z DTSTAMP:20261011T152429Z UID:2edmqhbir0s91t1i8f7d9a3q2o@google.com CREATED:20170622T062607Z DESCRIPTION:Most of our understanding of the Universe stems one way or anot her from star-light. However\, only by building realistic models of convec tion and radiative transfer in the dynamic stellar atmospheres\, can we pr edict the detailed strengths and shapes of lines in the emitted light and accurately infer the properties of stars. Recently\, we reached the milest one of making 3D non-LTE line formation of highly complex species like Fe numerically feasible for late-type stars and can for the first time predic t their metallicities without invoking free parameters. I will demonstrat e how improved models affect our understanding of the origin of elements a nd chemical evolution in stars\, stellar populations\, and the Galaxy. The next challenge lies in incorporating physically more realistic models int o automated spectroscopic analysis pipelines for million-star spectroscopi c surveys\, e.g. the ongoing Gaia-ESO and GALAH. Looking ahead\, their suc cessors WEAVE and 4MOST will expand the stellar inventory by another order of magnitude: what questions about the history of our Galaxy can then be asked and answered? LAST-MODIFIED:20170710T001105Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Karin Lind (Max Planck Institute for Astronomy) "Galactic Archaeolo gy with the New Generation of Stellar Spectroscopic Models and Surveys" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220505T010000Z DTEND:20220505T013000Z DTSTAMP:20261011T152429Z UID:0b6esirji0qhq18is015de30jk@google.com CREATED:20220301T002619Z DESCRIPTION:The first billion years after the Big Bang represent the final frontier in assembling a complete picture of cosmic history. During this e arly period the first galaxies formed and the universe became bathed in li ght. Hydrogen clouds in the space inbetween galaxies were then transformed from an atomic gas to an ionised medium of detached protons and electrons . A key goal for JWST is to explore the emergence of the earliest galaxies in the redshift range z > 12\, beyond reach of current facilities. Recent studies of cosmic microwave background data provide some evidence for suc h early star formation. Since time is compressed at high redshift\, we ca n gain further insight via measures of dust\, metals and mature stellar po pulations seen in galaxies at redshifts z~8-10. I will review the evidence for early star formation from observations undertaken with HST/Spitzer an d ALMA\, and conclude with the prospects for direct detection of the impli ed progenitors with JWST. LAST-MODIFIED:20220425T042210Z LOCATION:DLT & ZOOM (host: Neco Kriel) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Richard Ellis (UCL) "Homing in on Cosmic Dawn: When Did the First G alaxies Emerge from Darkness?" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20241105T000000Z DTEND:20241105T010000Z DTSTAMP:20261011T152429Z UID:1kfepkdm92f26ncn8mbvft8uro@google.com CREATED:20240501T002201Z DESCRIPTION:The cold dark matter model has been extremely successful in exp laining several fundamental properties of galaxy formation and evolution\, as well as the large-scale structure of the Universe. However\, it exhibi ts some discrepancies at galactic scales\, which has sparked interest in a lternative dark matter models. The study of the low surface brightness uni verse has gained momentum over the last 20 years\, thanks to its potential to provide insights into the physics of our Universe. This is the univers e with the lowest density of stars\, where dark matter reigns. Consequentl y\, the structural properties of low surface brightness objects are determ ined by the nature of the dark matter\, and can be used to understand this elusive component. In this talk I will discuss how recent developments in ultra-deep imaging are accelerating our ability to understand the nature of dark matter. LAST-MODIFIED:20241007T075618Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Hilay Shah) \nZoom: https: //anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Mireia Montes (ICE-CSIC) "Unlocking the secrets of dark matter with low surface brightness observations" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230428T040000Z DTEND:20230428T050000Z DTSTAMP:20261011T152429Z UID:em8fsd45vsmrp2glo2m0j910pc@google.com CREATED:20230421T084107Z DESCRIPTION:The MAVIS adaptive optics imager and spectrograph for the VLT\, is being led by AITC\, working closely with Astralis-AAO at Macquarie Uni versity and international partners in Italy\, France and Germany. In March the MAVIS team completed the instrument Preliminary Design Review\, and h ave just now received the formal report from ESO's expert review panel. Th is overview presentation will briefly outline the MAVIS Science Case\, pro vide an overview of the instrument design\, report on the PDR outcomes and outline the team's next steps on the path from here to first light. LAST-MODIFIED:20230426T063108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Jesse Cranney) \nZoom: htt ps://anu.zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Francois Rigaut (RSAA) "MAVIS Preliminary Design Review and Onward to Phase C!" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20151124T000000Z DTEND:20151124T010000Z DTSTAMP:20261011T152429Z UID:1lv9t8otd2bbfj6n44musm2328@google.com CREATED:20151018T233612Z DESCRIPTION:We present spectral line images of [CI] 809 GHz\, CO J=1-0 110 & 115 GHz and HI 1.4 GHz line emission along a ~1° region in the l=328° direction of the Galactic plane. The [CI] data comes from the High Elevat ion Antarctic Terahertz (HEAT) telescope\, a new facility on the summit of the Antarctic plateau where the precipitable water vapour falls to the lo west values found on the surface of the Earth. Some terahertz windows are opened through the atmosphere from this site almost continuously during th e winter. The CO and HI datasets come from the Mopra and Parkes/ATCA Sout hern Galactic Plane Surveys\, respectively. Together\, these data cubes pr ovide wide-field (1° scale) panoramic imaging at good spatial and spectra l resolution (2' and 1 km/s) of the atomic and molecular gas of the inters tellar medium. We are able to calculate and compare the column densities in the carbon\, carbon-monoxide and hydrogen emitting regions. Carbon is found in neutral or singly-ionized form within the first optical depth fro m the surfaces of molecular cloud\, so that the [CI] emission provides a d irect probe of the amount of dark (i.e. CO-free) molecular gas that is pre sent. We also identify a filamentary molecular cloud\, ~75 x 5pc long with mass ~4 x 10E4 MSun and a narrow velocity emission range of just 4 km/s. The morphology and kinematics of this filament are similar in CO\, [CI] an d HI\, though in the latter appears as self-absorption. We calculate line fluxes and column densities for the three emitting species\, which are br oadly consistent with a PDR model for a GMC exposed to the average interst ellar radiation field. The [C/CO] abundance ratio averaged through the fi lament is found to be approximately unity. The G328 filament is constrain ed to be cold (TDust < 20K) by the lack of far-IR emission\, to show no cl ear signs of star formation\, and to only be mildly turbulent from the nar row line width. We suggest that it may represent a GMC shortly after form ation\, or perhaps still be in the process of formation. LAST-MODIFIED:20151018T233612Z LOCATION:Duffield Lecture Theatre (host: Christoph Federrath) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Michael Burton (UNSW) "Carbon in Molecular Clouds - probing the dar k molecular gas" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20181128T004000Z DTEND:20181128T010000Z DTSTAMP:20261011T152429Z UID:c19tngve5h1k0tr759vhd0j46k@google.com CREATED:20181125T215606Z DESCRIPTION:The Australian Dark Energy Survey is entering the final year of a 6-year Reverberation Mapping program\, to measure the mass of the centr al supermassive black holes of almost 800 Active Galactic Nuclei. Reverber ation Mapping measures the time taken for continuum emission radiated from the core of AGN to ionise clouds of gas orbiting the central black hole. The ultimate goal is to develop the AGN as new “standardisable candles ”\, allowing us to determine distances in the Universe far beyond what i s currently practical using supernovae. This would greatly improve our abi lity to understand dark energy and the evolution of the expansion of the U niverse. We find that the current OzDES spectroscopic cadence (approximate ly monthly) poorly samples the emission-line light curves of the lower lum inosity AGN at z < 1. This is a critical limitation as these sources ancho r the calibration of high-z AGN as cosmological distance standards\, and o verlap with the region where type Ia supernova measurements are abundant\, allowing cross-probe analysis.My analysis indicates that the window funct ion for observational data plays a critical role in lag recovery\, more so than the global number of data points\, or the duration of the survey. Th is classic observational “quality verses quantity” problem can be amel iorated through stacking of observations from physically similar sources t o recover statistical properties for this class of object. LAST-MODIFIED:20181125T215606Z LOCATION:CSO Common Room (host: Oh) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Umang Malik (RSAA) "Simulating Lag Recovery for Low-Luminosity AGN with Reverberation Mapping" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20200723T230000Z DTEND:20200724T065000Z DTSTAMP:20261011T152429Z UID:m3iqo509tnjeuh441vkijel7ak@google.com CREATED:20200708T235209Z DESCRIPTION:Abdu Abohalima (9:00-9:20)\, Break (9:20-9:40)\, Patrick Armstr ong (Proposal Talk 9:40-10:10)\, Morning Tea (10:10-11:00)\, Stephanie Mon ty (11:00-11:20)\, Yifei Jin (11:20-11:40)\, Aldo Mura (11:40-12:00)\, Sow mya Hassan Krishna (12:00-12:20)\, Lunch Break (12:20-13:00)\, Wei Shen (P roposal Talk 13:00-13:30)\, Richard Samuel (13:30-13:50)\, - (13:50-14:20) \, Isabella Gerrard (Proposal Talk 14:20-14:50)\, Afternoon Tea (14:50-15: 30)\, Hao Zhang (15:30-15:50)\, Ji-Jia Tang (15:50-16:10)\, Shyam Menon (P roposal Talk 16:10-16:40) LAST-MODIFIED:20200722T062107Z LOCATION:ZOOM 997 8534 1005 (host: Travouillon) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA HDR Students (RSAA) "HDR Student Annual Reviews" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260512T050000Z DTEND:20260512T060000Z DTSTAMP:20261011T152430Z UID:m40omb3pfj8jtkcso2eiqqs6r4@google.com CREATED:20260503T113002Z DESCRIPTION:Our monthly skillshare sessions offer a practical\, hands-on sp ace for students and postdocs to exchange research skills\, professional d evelopment tools\, and effective workflows in an informal and supportive s etting. Skillshare is run on the second Tuesday of each month\, 3:00-4:30i sh pm in the CSO Common Room\, with ~15-30 minutes of introduction followe d by ~30-60 minutes of panel discussions or open-ended hands-on activities . LAST-MODIFIED:20260503T113338Z LOCATION:CSO Common Room (host: Sven Buder) \n SEQUENCE:2 STATUS:CONFIRMED SUMMARY:Monthly Skillshare (RSAA) "Impactful Collaborating and Networking" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20201209T220000Z DTEND:20201209T230000Z DTSTAMP:20261011T152429Z UID:1a9ti1bgieu1ghpg5lfdarmprs@google.com CREATED:20200928T073122Z DESCRIPTION:The recent example of PDS 70 has shown that forming giant plane ts are relatively bright in the near-infrared\, with a planet to star cont rast of 1:1000. Nevertheless\, the detection yields of high-contrast imagi ng surveys for young planetary-mass companions (e.g.\, SHINE\, GPIES) are small (2%). The reason for this is that wide-separation giant planets are intrinsically rare\, and their distribution peaks at semi-major axes of 2- 3 au. Classical high-contrast imaging can only probe this parameter space out to 25 pc. Interferometric techniques are the only ones reaching high e nough angular resolution to study planet formation in the nearest star-for ming regions (120-140 pc). In this talk\, I will show how we adapt single- dish kernel phase interferometry for surveying 40 young stars in the Tauru s star-forming region from the ground. We achieve detection limits compara ble to the protoplanet PDS 70 b at angular separations down to 0.5 lambda/ D\, proving the high-contrast and high-resolution capabilities of this tec hnique. At even smaller spatial scales\, long-baseline optical interferome try with GRAVITY and MATISSE now start to detect exoplanets and circumstel lar disks. These detections are still limited by poorly understood systema tic errors\, though\, which is why we develop a method to extract and mode l these correlated errors directly from the data. By accounting for them i n the model fitting process\, we find that the faint source detection limi ts improve by a factor of 2. A proper treatment of the uncertainties is a cornerstone for optical interferometry on its rising path towards studying planet formation and evolution. LAST-MODIFIED:20201201T012312Z LOCATION:ZOOM 997 8534 1005 (host: Cullinane) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Jens Kammerer (RSAA) "End-of-Thesis Talk: Interferometric technique s for high-contrast\, high-resolution imaging of giant protoplanets and ci rcumstellar disks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260310T040000Z DTEND:20260310T053000Z DTSTAMP:20261011T152430Z UID:ntng0lfu088vf961g7kqeq2c28@google.com CREATED:20251125T233110Z DESCRIPTION:Our monthly skillshare sessions offer a practical\, hands-on sp ace for students and postdocs to exchange research skills\, professional d evelopment tools\, and effective workflows in an informal and supportive s etting. Skillshare is run on the second Tuesday of each month\, 3:00-4:30 ish pm in the CSO Common Room\, with ~15-30 minutes of introduction follow ed by ~30-60 minutes of panel discussions or open-ended hands-on activitie s. LAST-MODIFIED:20260210T225215Z LOCATION:CSO Common Room (in-person only) (host: Sven Buder) \nZoom: https: //anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Monthly Skillshare (RSAA) "Supercomputing setup and proposals" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20230330T000000Z DTEND:20230330T010000Z DTSTAMP:20261011T152429Z UID:6rma53lc3c6os8lnnkvq4a8p0s@google.com CREATED:20230223T022109Z DESCRIPTION:Star formation in galaxies are governed by the complex interpla y of several nonlinear physical mechanisms operating in the interstellar m edium (ISM). However\, in spite of the underlying complexity\, there is ov erwhelming evidence for fundamental scaling relations and trends governing the conversion of gas to stars that seem to imply a self-regulating agent at play -- studies over the past decade have highlighted that stellar fee dback play the role of this self-regulating agent. Specifically\, the radi ation emitted by young massive stars have been shown to play a pivotal rol e in regulating the star formation efficiency in\, and controlling the evo lutionary cycle of\, GMCs in weakly star-forming galaxies in the local Uni verse. In this talk\, I will present work done in my thesis that extends a nd tests this picture on highly massive\, compact GMCs\, typical of high-p ressure environments such as rare infrared-bright merging galaxies (ULIRGs ) in the local universe\, and more commonly at earlier redshifts. These GM Cs form so-called super star clusters (SSCs\; e.g. in M82)\, whose highly compact\, bound nature have garnered interest in their potential role as p recursors of globular clusters. I will highlight novel numerical technique s we developed to model the radiation emitted by massive stars and their i nteraction with dusty gas (radiation hydrodynamics)\, which vastly improve s over earlier methods in the literature\, and alleviates the technical di fficulties involved in modelling the aforementioned regime. I will focus o n the similarities and differences of star formation and feedback in this regime with GMCs typical of Milky Way-like galaxies\, and explore their im plications on the evolution of SSCs and the larger-scale ISM. I will also discuss how radiation feedback sculpts the turbulent ISM locally in HII re gions\, modifies the dynamical properties of gas and magnetic fields in th em\, and contemplate what this might imply for the possibility that additi onal star formation may be triggered locally by feedback. LAST-MODIFIED:20230322T235112Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Neco) \nZoom: https://anu. zoom.us/j/84138346977?pwd=UElURkg3bjVsV1M3R0NnWVV1dGJTUT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Shyam Menon (RSAA) "The Interplay of Star Formation and Radiation F eedback in the ISM (End of Thesis Talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20210611T040000Z DTEND:20210611T043000Z DTSTAMP:20261011T152429Z UID:i7aqu76t86gjqmvoqhsirsbipo@google.com CREATED:20210427T010112Z DESCRIPTION:The Feast-of-Facts are an informal open-mic format from RSAA me mbers for RSAA members. LAST-MODIFIED:20210427T010112Z LOCATION:DLT and ZOOM (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Henry Zovaro and TBD (RSAA) "FoF: Formula 1 and TBD" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180419T010000Z DTEND:20180419T020000Z DTSTAMP:20261011T152429Z UID:mfpm7mtbmse97q0llfltr9ajjk@google.com CREATED:20180110T231110Z DESCRIPTION:Connecting planetary systems at different stages of stellar evo lution helps us understand their formation\, evolution and fate\, as well as provides us with crucial insights about their dynamics and chemistry. P ost-main-sequence stars -- white dwarfs\, giant branch stars and pulsars - - all host planetary systems\, which often include remnant debris discs. H ere I provide a review of our current knowledge of these systems. I show h ow this interdisciplinary field incorporates several facets of stellar phy sics and chemistry as well as solar system physics and chemistry\, and det ail simulation-based efforts to understand the big picture. LAST-MODIFIED:20180205T061614Z LOCATION:Duffield Lecture Theatre (host: McIntyre) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dimitri Veras (University of Warwick) "The growing field of post-ma in-sequence exoplanetary science" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160527T040000Z DTEND:20160527T042000Z DTSTAMP:20261011T152429Z UID:id43kcra4i2r0nknqv974hbu3o@google.com CREATED:20160418T000614Z DESCRIPTION:We report here on the discovery of faint extended wings of H ob served out to an apparent velocity of 7600 kms−1 in the Orion Nebula (M4 2) and in five H II regions in the Large and the Small Magellanic Clouds. We show that\, these wings are caused by Raman scattering of both the OI a nd Si II resonance lines and stellar continuum UV photons with HI followed by radiative decay to the HI n = 2 level. The broad wings also seen in H and in H result from Raman scattering of the UV continuum in the HI n = 4 and n = 5 levels respectively.The Raman scattering fluorescence is correla ted with the intensity of the narrow permitted lines of OI and Si II. In t he case of Si II\, this is explained by radiative pumping of the same 1023 .7°A resonance line involved in the Raman scattering by the Ly radiation field. The subsequent radiative cascade produces enhanced Si II 5978.9\, 6 347.1 and 6371.4°A permitted transitions. Finally we show that in OI\, ra diative pumping of the 1025.76°A resonance line by the Lyman series radia tion field is also the cause of the enhancement in the permitted lines of this species lying near H in wavelength\, but here the process is a little more complex. We argue that all these processes are active in the zone of the H II region near the ionisation front. LAST-MODIFIED:20160418T000614Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Michael Dopita (ANU) "The Discovery of Raman Scattering in HII Regi ons" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20150825T010000Z DTEND:20150825T020000Z DTSTAMP:20261011T152429Z UID:urpus59kl8l3llunt94ro7ulds@google.com CREATED:20150731T123112Z DESCRIPTION:The Siding Spring Southern Seyfert Spectroscopic Snapshot Surve y (S7) is providing integral field spectroscopy on ~140 nearby active gala xies in the wavelength region 3300-7000 Angstroms at resolutions as high a s 7000. In this talk\, I present the first results of this survey. I show how\, by combining data analysis with detailed photoionisation and shock m odelling\, we are gaining a new understanding of the physics of both Seyfe rt and LINER galaxies. LAST-MODIFIED:20150816T065608Z LOCATION:Duffield Lecture Theatre (host: Sarah Sweet) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Michael Dopita (RSAA) "S7: Probing the Physics of Active Nuclei" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20220711T232000Z DTEND:20220712T034000Z DTSTAMP:20261011T152429Z UID:38iu4aeg1ppod1ln1hibpjru64@google.com CREATED:20220705T051606Z DESCRIPTION:Schedule available at : https://anu365-my.sharepoint.com/:x:/g/ personal/u1057001_anu_edu_au/EX00_zlqLHdKpjR-rZiRGBABRC1a20hn3dM4wEmmIMyoT Q?e=DpJnwu LAST-MODIFIED:20220705T051606Z LOCATION:DLT & ZOOM (host: Tony Travouillon) \nZoom: https://anu.zoom.us/j/ 99785341005?pwd=ZzNXRUtGVlRQdzBqYjVJbytNUGhuZz09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA HDR Students (RSAA) "RSAA HDR Students Thesis Proposals and An nual Reviews" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20160804T010000Z DTEND:20160804T020000Z DTSTAMP:20261011T152429Z UID:i83lonaeuo7dc3ff5khrv3b4gg@google.com CREATED:20160510T064617Z DESCRIPTION:In interstellar and intergalactic space\, densities are far low er and shock speeds far higher than anything that can be produced in a ter restrial laboratory. Electrons and ions at these shock fronts are heated by plasma waves and magnetic turbulence rather than by direct collisions. The relative degree to which electrons and ions are heated at the shock tr ansition is one of the important unsolved problems in plasma astrophysics. Furthermore\, the lack of temperature equilibrium between electrons and persists far downstream from the shock\, strongly impacting the optical\, X-ray and UV emission from young supernova remnants (SNRs). Some SNRs in the non-radiative stage of evolution exhibit faint optical spectra domina ted by the Balmer emission lines of hydrogen (i.e.\, they are ‘Balmer-Do minated'). These Balmer lines\, which consist of broad and narrow compone nts\, arise in a very thin ionization layer immediately behind the shock\, and offer rare and valuable diagnostics of the poorly understood physics of the shock transition. I will describe some of the latest results in th e study of Balmer-dominated shocks\, including how the Balmer line spectra can provide a sensitive probe of the physics of electron-ion temperature equilibration. Recent work suggests that the mechanisms heating the ele ctrons and ions are also connected to cosmic ray acceleration in supernova remnants up to the knee in the cosmic ray spectrum at 1e15 eV. LAST-MODIFIED:20160725T043107Z LOCATION:Duffield Lecture Theatre (host: Helga Denes) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Parviz Ghavamian (Towson University) "Balmer-Dominated Supernova Re mnants and the Physics of Collisionless Shocks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190129T000000Z DTEND:20190129T010000Z DTSTAMP:20261011T152429Z UID:upsbciuqeap7qfdqbgeo25losc@google.com CREATED:20190108T041106Z DESCRIPTION:Feedback in the form of protostellar jets plays an important ro le in the process of star formation. These jets are launched from protost ellar disks at au scales via the interaction of magnetic fields with weakl y ionised disk material\, and extend up to cloud scales (~ 1-3 pc)\, drivi ng turbulence and influencing the star formation rate and the initial mass function. In this talk\, I present the results of my PhD work on jet feed back\, divided into two parts. In part one\, I present a novel approach t o modelling the jet-launching region in protostellar disks\, combining a s eries of 1.5D semi-analytic\, steady-state\, vertical disc-wind solutions into a radially extended 1+1.5D model\, incorporating all three magnetic d iffusion mechanisms (Ohm\, Hall and ambipolar). From this model I find th at the majority of mass outflow via disc winds occurs over a radial width of a fraction of an au\, with outflow rates attenuating rapidly on either side. I also find that the mass accretion rate\, midplane plasma beta\, su rface density profile and ionisation structure each have significant effec ts on both the location of the wind-launching region and the ejection/accr etion ratio. In part two\, I present new results characterising the densi ty variance - Mach number relation in interstellar medium (ISM) turbulence . This relation is important for understanding the properties of ISM turb ulence driven by feedback processes\, including the star formation rate an d initial mass function\, and is well-studied in the isothermal regime. I extend the analysis to the adiabatic regime\, modelling turbulence with di atomic molecular (gamma = 7/5) and monatomic (gamma = 5/3) adiabatic indic es. Stirring the gas solenoidally at low wavenumbers\, I find that as the gas heats in adiabatic compressions\, it evolves along the relationship i n the density variance-Mach number plane\, but deviates significantly from the isothermal form. I calculate new relations that take the adiabatic in dex into account and provide good fits for a range of Mach numbers. LAST-MODIFIED:20190123T055106Z LOCATION:CSO Common Room (host: Zerjal) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Christopher Nolan (RSAA) "Understanding protostellar jet feedback o n disk and cloud scales (End-of-Thesis colloquium)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240326T000000Z DTEND:20240326T013000Z DTSTAMP:20261011T152429Z UID:6kuv3erbt62fm7l089e31ej12g@google.com CREATED:20240220T233620Z DESCRIPTION:For the last decade\, mergers of double white dwarfs have been considered to be a likely\, possibly even favoured\, progenitor scenario f or Type Ia supernovae. Though the Milky Way harbours ~100 million double w hite dwarf binaries\, only a small fraction of these will actually merge i n a Hubble time and possess the "right" physical properties to produce a T ype Ia supernova even if a merger occurs. A different outcome of a white d warf merger is the creation of another type of stellar transient: a hydrog en-deficient carbon (HdC) star. We know of ~130 of such ‘dusty’\, HdC stars in the Galaxy - these are the R Coronae Borealis (RCB) supergiants\, and they are thought to be the end result of a merger of a carbon-oxygen white dwarf and a helium-rich white dwarf\, though their formation is not completely understood. In 2021\, another type of hydrogen-deficient carbon star was found in great numbers: 27 "dustless" HdC stars were spectroscop ically confirmed in our own Milky Way with WiFeS\, increasing the known nu mber of this class from 4 (discovered >50 yrs ago) to 31. We have been gra nted time on the high-resolution (R~80\,000) Veloce echelle spectrograph w ith the aim of disentangling the progenitor properties of the long-known ‘dusty’ RCB stars and the newly-discovered plethora of ‘dustless’ HdC stars - both classes of objects presumed to be the result of double wh ite dwarf mergers. I will discuss how different formation channels of merg ing white dwarfs may be plausibly linked to both Type Ia supernovae as wel l as these 'failed' Type Ia supernovae: the HdC stars. LAST-MODIFIED:20240315T062107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Mark Krumholz) \nZoom: htt ps://anu.zoom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ashley Ruiter (UNSW Canberra / ADFA) "Mergers of white dwarfs and t he transients they make" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260825T050000Z DTEND:20260825T061500Z DTSTAMP:20261011T152430Z UID:89j48e62ui5sghq7cnbntpit80@google.com CREATED:20260803T010012Z DESCRIPTION:Our monthly Skillshare sessions provide an informal\, supportiv e\, and practical space for students and postdoctoral researchers to devel op and exchange research skills\, professional-development tools\, and eff ective workflows. The format is primarily focused on students\, in particu lar those enrolled in the ASTR8030 course Astronomy and Astrophysics Resea rch Skills. However\, everyone is very warmly invited to join and contribu te.\n\nSessions are held on selected Tuesdays from approximately 3:00-4:15 ish pm in the CSO Common Room. Depending on the topic\, they may include s hort introductions\, demonstrations\, panel discussions\, interactive exer cises\, or open-ended hands-on activities. LAST-MODIFIED:20260803T020014Z LOCATION:Zoom or CSO Common Room (host: Sven Buder and Melanie Kaasinen) \n Zoom: https://anu.zoom.us/j/89544552112?pwd=Bdoo5fgMVS2Ls6e3Fs0NSNk9OMpaXn .1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:RSAA Skillshare (RSAA) "How to give a great presentation" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260310T000000Z DTEND:20260310T010000Z DTSTAMP:20261011T152430Z UID:hu2tmqjkrbj9f91q9lcpqjmo8k@google.com CREATED:20251203T021614Z DESCRIPTION:Fast radio bursts (FRBs) are intense pulses of radio emission t hat originate in distant galaxies. They are now delivering on their promis e as tools to understand extreme physical processes and environments\, and as powerful probes of the diffuse cosmic web of baryons\, nearly impossib le to study otherwise. It is of particular importance to pinpoint FRBs to host galaxies. In this presentation I will discuss what we have learned ab out FRBs from studies of their host galaxies\, and how we have used these localised FRBs to study the structure of the Universe. I will also show ho w we can use novel wide bandwidth observations to explain the extreme appa rent luminosity of FRB emission. I will then highlight some of the challe nges that will be faced as larger samples of FRBs are localised at larger distances. I will conclude by motivating a wide field local Universe FRB i nstrument concept that can answer the outstanding questions in FRB researc h. LAST-MODIFIED:20260301T233108Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Tomasz Rozanski) \nZoom: h ttps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ryan Shannon (Swinburne U.) "Fundamental astrophysics with fast rad io bursts" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260430T013000Z DTEND:20260430T023000Z DTSTAMP:20261011T152430Z UID:8sf0sskk32gdc273hl2uf9pf50@google.com CREATED:20260503T120321Z DESCRIPTION:The gravitational forces measured beyond the Solar System tell us that 85% of the matter in the Universe is invisible. But despite its ab undance\, dark matter has so-far avoided direct detection by laboratory ex periments on Earth. As a result\, particle physics theory has flourished t o develop dark matter candidates that span a wide range of masses and phen omenologies. In this talk\, I will discuss some consequences of dark matte r physics on galaxies including the predicted abundances of low-mass dark matter halos. In particular\, I will show that “mini” collisions with low-mass halos have an inconspicuously important role in driving diversity amongst large star-forming galaxies in cosmological simulations. These co llisions are ubiquitous for heavy\, weakly-interacting dark matter particl es but suppressed by warmer\, lighter candidates. LAST-MODIFIED:20260503T120321Z LOCATION:Zoom or Duffield Lecture Theatre (host: Trevor Mendel) \nZoom: htt ps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Connor Bottrell (UWA) "Mini mergers with major consequences in a co ld dark matter universe" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20211116T043000Z DTEND:20211116T055000Z DTSTAMP:20261011T152430Z UID:qkfi6jv5bq2afupda9ja5ikibs@google.com CREATED:20211109T022108Z DESCRIPTION:Schedule: 15:30 David Raithel 16:10 Vihan Patel LAST-MODIFIED:20211111T232609Z LOCATION:ZOOM and DLT (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Master students (RSAA) "RSAA Master Thesis Talks" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20171102T000000Z DTEND:20171102T010000Z DTSTAMP:20261011T152429Z UID:ottg80kn6tskmdr9dalecsf00g@google.com CREATED:20171018T071609Z DESCRIPTION:In April 2018\, the second Data Release of the ESA Gaia mission is expected and will once again broaden our astrometrical horizon. The we ek before\, the team of the stellar spectroscopic Galactic Archaeology wit h HERMES (GALAH) survey will also publish its second Data Release\, contai ning stellar parameters and up to 30 element abundances - in simple words: ’stellar DNA’ - for an unprecedented number of stars overlapping with Gaia\, hence broadening the chemo-dynamic horizon by several magnitudes a nd dimensions. To accomplish this\, the GALAH team is using a multi-step a pproach of a 'physics-driven' spectrum analysis for a representative set o f stars within the GALAH survey followed by the 'data-driven' analysis wit h The Cannon. We construct (’train’) a spectral model of GALAH spectra based on the training set and then propagate the information onto the who le sample of currently more than 500 000 spectra. I will explain the machi nery to achieve this in more detail and show first science results of the combination of GALAH and Gaia Data Release 1 - which can help you to get r eady for GALAH & Gaia DR2 - including a sneak peak of GALAH DR2 element ab undances covering various nucleosynthesis channels like alpha- and s-/r-pr ocess. LAST-MODIFIED:20171028T182607Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Sven Buder (MPIA) "The GALAH survey and Gaia" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20180119T030000Z DTEND:20180119T032000Z DTSTAMP:20261011T152429Z UID:hlsr6kfbs693cv6a9acdp96ie4@google.com CREATED:20180116T074106Z DESCRIPTION:Using data from the CFHTLenS survey\, we have recently made the first stacked image of the dark-matter dominated filaments of the cosmic web that connect galaxies. This opens up a new window to studying the non- linear Universe\, which will be fully exploited in upcoming weak lensing s urveys such as CFIS\, Euclid and WFIRST. LAST-MODIFIED:20180119T070106Z LOCATION:Duffield Lecture Theatre (host: Battisti) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Michael Hudson (University of Waterloo) "Mapping the Cosmic Web wit h Gravitational Lensing" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20260407T013000Z DTEND:20260407T023000Z DTSTAMP:20261011T152430Z UID:c51vnseqevbep9v4hpg092thgg@google.com CREATED:20260322T230607Z DESCRIPTION:Strong gravitational lensing provides a unique window into gala xy mass distributions\, but extracting this information requires solving a complex\, ill-posed inverse problem. To truly "sharpen the lens" in the e ra of multi-band and multi-resolution surveys\, we must rely on rigorous B ayesian forward-modeling to maximize the information extracted from these datasets. In this talk\, I will first present a novel\, lenstronomy-based modeling pipeline that performs robust joint inference on multi-band imagi ng\, demonstrating its application on four-band (z\, i\, r\, g) PISCO data for 16 lens candidates. By comparing this with single-band modeling\, I w ill show how a multi-wavelength approach significantly tightens the constr aints on the lens models. Building on this\, I will explore how we leverag e modern\, GPU-accelerated frameworks (e.g.\, herculens) to tackle high-re solution HST imaging from the AGEL survey. Employing a flexible\, pixelate d source reconstruction strategy allows us to more cleanly capture complex source morphologies and improve the fidelity of the inferred mass models. Finally\, I will highlight the ongoing challenges of modeling highly comp lex lensing configurations and discuss the critical next step: integrating stellar kinematic constraints to physically break mass degeneracies and f urther refine future dark matter studies. LAST-MODIFIED:20260323T234808Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Tim Gao) \nZoom: https://a nu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Huimin Qu (U. Sydney) "Sharpening the Lens: Robust Bayesian Forward -Modeling from Multi-Band Surveys to High-Resolution Space Imaging" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170310T033000Z DTEND:20170310T035000Z DTSTAMP:20261011T152429Z UID:ivg1fr3tmojnct7t5vembpn8uc@google.com CREATED:20170309T035605Z DESCRIPTION:It has recently been shown that active galactic nuclei (AGN) ma y be possible to use as standardisable candles utilising the method of rev erberation mapping. Their luminosity allows them to be seen at high redshi fts (z>2) using even medium-sized ground-based telescopes\, used by for in stance the Dark Energy Survey (DES) and the Australian Dark Energy Survey (OzDES)\, who are together targeting 771 AGN for reverberation mapping pur poses. Using their data I will perform analysis which will expand the fiel d of reverberation mapping\, and teach us more about the cosmology of our Universe. LAST-MODIFIED:20170309T035605Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Natalia Sommer (RSAA) "Reverberation Mapping: Studying the Universe by Studying Active Galactic Nuclei - Thesis proposal" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20251014T000000Z DTEND:20251014T010000Z DTSTAMP:20261011T152429Z UID:k913u1qjraqkj2jd4ecn5ru2ak@google.com CREATED:20250122T035141Z DESCRIPTION:NASA's Kepler and TESS space missions have revolutionised aster oseismology by providing long light curves with exquisite precision. Thes e allow us to measure the natural oscillation frequencies of stars\, which probe their interiors and provide accurate measurements of their fundamen tal properties (mass\, radius and age). I will review some of the recent h ighlights\, including applications to Sun-like stars\, metal-poor stars an d red giants. LAST-MODIFIED:20250923T021610Z LOCATION:ZOOM or Duffield Lecture Theatre (host: Tomasz Rozanski) \nZoom: h ttps://anu.zoom.us/j/82974980739?pwd=MJiiD4Rx5j7OrMaiVuAveyEIVsOntd.1 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tim Bedding (U Sydney) "Probing inside stars with asteroseismology" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190724T230000Z DTEND:20190725T000000Z DTSTAMP:20261011T152429Z UID:9fknr01o3ur13g5po4jkt92v6s@google.com CREATED:20190712T011106Z DESCRIPTION:[A colloquium by the shortlisted candidate for the new Centre f or Gravitational Astrophysics] The observation of gravitational waves from the compact binary coalescences (CBC) opens a new era of gravitational-wa ve physics and multi-messenger astronomy. What happens after the coalescen ce? What else can we learn from the remnants? In this talk\, I will introd uce two studies about the CBC remnants. One is to search for gravitational waves from the remnant of the binary neutron star merger\, GW170817. Alth ough no significant signal candidate is found for this particular event\, development and verification of new methods is of importance for future ap plications. Prospects will become good with future detectors and the combi nation of multiple channels. The other is to search for yet-undiscovered\, weakly interacting\, ultralight bosons by following up the newly born bla ck holes after the coalescences. The number of such particles around a rap idly rotating black hole can grow exponentially due to the phenomenon of s uperradiance\, forming a macroscopic cloud and generating continuous gravi tational waves. The theory of boson clouds around black holes and the grav itational-wave emission mechanism will be explained. The search challenges and the empirical estimates of the search sensitivity will be discussed. These gravitational-wave searches are closely connected to theoretical pre dictions and electromagnetic observations. One of the most exciting aspect s of gravitational-wave discovery is that pieces from different channels a re being brought together to study fundamental physics. LAST-MODIFIED:20190712T011106Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Ling (Lilli) Sun (Caltech) "After the coalescences - searches for t he binary neutron star post-merger remnants and ultralight bosons" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20240905T010000Z DTEND:20240905T020000Z DTSTAMP:20261011T152429Z UID:9adp06krc4lsagtcnndhonung8@google.com CREATED:20240417T012648Z DESCRIPTION:Stellar spectra emulators often reach a limit in accuracy\, lea ding to systematic errors in the estimation of stellar atmosphere paramete rs. I would like to introduce the TransformerPayne emulator and compare it s performance with The Payne emulator (a fully connected neural network)\, its large version\, and a convolutional-based emulator. When tested on sy nthetic spectra grids\, TransformerPayne demonstrated superior performance \, achieving a mean absolute error of approximately 0.15%\, which is sever al times better than the other methods considered. Additionally\, Transfor merPayne excels when using a fine-tuning approach\, allowing pretraining o n grids of stellar spectra with simplified physics and transferring this k nowledge to more complex grids\, which reduces the required training grid size by up to tenfold. Furthermore\, we show that an analysis of the emula tor's internal workings reveals interpretable features shared across spect ral lines\, offering a partial explanation for its enhanced accuracy and d ata efficiency. LAST-MODIFIED:20240820T040116Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Tomasz Rozanski (RSAA) "TransformerPayne: Precise and Data Efficien t Stellar Spectra Emulator for the Deep Learning Era" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20190308T033000Z DTEND:20190308T035000Z DTSTAMP:20261011T152429Z UID:7cpug653vkkjbfrm5s047be6tc@google.com CREATED:20190129T043118Z DESCRIPTION:We report our discovery of observational evidence for the coher ence between galaxy rotation and the average motion of neighbors. Using th e Calar Alto Legacy Integral Field Area (CALIFA) survey data and the NASA- Sloan Atlas (NSA) catalog\, we estimate the angular momentum vectors of 44 5 CALIFA galaxies and build composite maps of their neighbor galaxies on t he parameter space of velocity versus distance. The composite radial profi les of the luminosity-weighted mean velocity of neighbors show striking ev idence for dynamical coherence between the rotational direction of the CAL IFA galaxies and the average moving direction of their neighbor galaxies. The signal of such dynamical coherence is significant for the neighbors wi thin 800 kpc distance from the CALIFA galaxies with a confidence level of 3.5sigma\, when the angular momentum is measured at the outskirt (Re 2 sigma divergence from dark energy as a cosmological constant. This has been the prevailing theory of dark energy since its dis covery\, leading to the LCDM concordance model of our Universe. However\, with the improved constraints provided by the DES analysis\, this model is thrown into question for the first time. To achieve the constraining powe r required to get these results involved improving statistical and systema tic uncertainties throughout the entire DES cosmological pipeline. These i mprovements are a results of dozens of researchers around the globe. In th is talk\, I will focus on my contributions improving Pippin\, the overarch ing pipeline which enables the DES analysis\, and developing a new method for evaluating the consistency of the DES results. The results from the DE S analysis are far from conclusive\, so if we are to determine the legitim acy of the cosmological constant\, further improvements to the statistic a nd systematic uncertainties are required. Upcoming surveys\, such as the L egacy Survey of Space and Time (LSST) aim to observe orders of magnitudes more SNe Ia than DES\, however with these improvements to the sample size come a whole host of challenges which must be addressed. As part of this t alk I discuss these challenges\, and my efforts to develop new statistical techniques to address these challenges. In particular I investigate likel ihood free\, forward modelled techniques which provide significantly great er control over systematic uncertainties with fewer assumptions\, at the c ost of much greater computational complexity. LAST-MODIFIED:20240409T072107Z LOCATION:ZOOM or Duffield Lecture Theatre (host: TBD) \nZoom: https://anu.z oom.us/j/83410388355?pwd=Qm9CMWI4QStWSHI3UzJXRXFvL3FSQT09 SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Patrick Armstrong (RSAA) "The Path to Uncovering Dark Energy: Impro ving statistical and computational techniques for supernova cosmology (End of Thesis Talk)" TRANSP:OPAQUE END:VEVENT BEGIN:VEVENT DTSTART:20170413T010000Z DTEND:20170413T020000Z DTSTAMP:20261011T152429Z UID:06q4k62q3o73sf1ea79f29pmto@google.com CREATED:20170327T123611Z DESCRIPTION:The first direct detections of gravitational waves in late 2015 were made possible by a forty year experimental campaign to design\, buil d\, and operate LIGO\, the Laser Interferometer Gravitational-wave Observa tory. In this talk\, I’ll cover gravitational waves and what makes them so difficult to detect and at the same time such powerful and unique probe s of the universe. Much of the presentation will focus on the interferomet ers\, the LIGO detections during the O1 run and their astrophysical implic ations. Time permitting\, I’ll give a preview of where LIGO intends to g o in the next decade and beyond. LAST-MODIFIED:20170409T233604Z LOCATION:Duffield Lecture Theatre (host: TBD) SEQUENCE:0 STATUS:CONFIRMED SUMMARY:Dave Reitze (University of Florida & LIGO) "Black Holes' Last Tango : LIGO and the Dawn of Gravitational Wave Astronomy" TRANSP:OPAQUE END:VEVENT END:VCALENDAR