BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//Australia Telescope National Facility - ECPv6.16.2//NONSGML v1.0//EN
CALSCALE:GREGORIAN
METHOD:PUBLISH
X-WR-CALNAME:Australia Telescope National Facility
X-ORIGINAL-URL:https://www.atnf.csiro.au
X-WR-CALDESC:Events for Australia Telescope National Facility
REFRESH-INTERVAL;VALUE=DURATION:PT1H
X-Robots-Tag:noindex
X-PUBLISHED-TTL:PT1H
BEGIN:VTIMEZONE
TZID:Australia/Sydney
BEGIN:STANDARD
TZOFFSETFROM:+1100
TZOFFSETTO:+1000
TZNAME:AEST
DTSTART:20220402T160000
END:STANDARD
BEGIN:DAYLIGHT
TZOFFSETFROM:+1000
TZOFFSETTO:+1100
TZNAME:AEDT
DTSTART:20221001T160000
END:DAYLIGHT
BEGIN:STANDARD
TZOFFSETFROM:+1100
TZOFFSETTO:+1000
TZNAME:AEST
DTSTART:20230401T160000
END:STANDARD
BEGIN:DAYLIGHT
TZOFFSETFROM:+1000
TZOFFSETTO:+1100
TZNAME:AEDT
DTSTART:20230930T160000
END:DAYLIGHT
BEGIN:STANDARD
TZOFFSETFROM:+1100
TZOFFSETTO:+1000
TZNAME:AEST
DTSTART:20240406T160000
END:STANDARD
BEGIN:DAYLIGHT
TZOFFSETFROM:+1000
TZOFFSETTO:+1100
TZNAME:AEDT
DTSTART:20241005T160000
END:DAYLIGHT
BEGIN:STANDARD
TZOFFSETFROM:+1100
TZOFFSETTO:+1000
TZNAME:AEST
DTSTART:20250405T160000
END:STANDARD
BEGIN:DAYLIGHT
TZOFFSETFROM:+1000
TZOFFSETTO:+1100
TZNAME:AEDT
DTSTART:20251004T160000
END:DAYLIGHT
END:VTIMEZONE
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230830T150000
DTEND;TZID=Australia/Sydney:20230830T160000
DTSTAMP:20260527T084738
CREATED:20250819T072010Z
LAST-MODIFIED:20250819T072011Z
UID:14942-1693407600-1693411200@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Sarah Pearce (SKAO)
DESCRIPTION:The next generation of radio astronomy: progress on construction of the SKA Observatory\n\nAbstract\n\nThe SKA Observatory is now starting construction of its two telescopes\, SKA-Low and SKA-Mid\, on site in Western Australia and South Africa. This talk will provide the latest status on construction\, exploring the current and planned work at each site. It will also look at establishment of the Observatory worldwide\, with a particular focus on Australia and the partnerships with CSIRO. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-sarah-pearce-skao/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-30082023.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230906T150000
DTEND;TZID=Australia/Sydney:20230906T160000
DTSTAMP:20260527T084738
CREATED:20250819T071944Z
LAST-MODIFIED:20250819T071945Z
UID:14943-1694012400-1694016000@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Hyein Yoon (University of Sydney)
DESCRIPTION:FLASH – New searches for Extragalactic HI 21-cm absorption at 0.4 < z < 1.0\n\nAbstract\n\nFLASH (the First Large Absorption Survey in HI) is a wide-field radio survey searching for 21-cm line absorption at 0.4 < z < 1.0. The goal of the survey is to understand the evolution of the neutral gas in galaxies and its role in AGN accretion and feedback. In this talk\, I will highlight a set of new HI 21-cm absorption lines detected in the ASKAP Pilot Survey Phase 1 and 2. Both associated systems (where the HI gas is at the same redshift as the background radio source) and intervening systems (where the HI gas is in the foreground along the line-of-sight) will be discussed. Additionally\, I will report an update on the FLASH Full Survey\, which will continue for the next five years. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-hyein-yoon-university-of-sydney/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/png:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-06092023.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230913T150000
DTEND;TZID=Australia/Sydney:20230913T160000
DTSTAMP:20260527T084738
CREATED:20250819T071831Z
LAST-MODIFIED:20250819T071831Z
UID:14944-1694617200-1694620800@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Luke Davies (UWA)
DESCRIPTION:A Universal Murder Mystery – What is killing galaxies?\n\nAbstract\n\nThe Universe is dying. All across the cosmos for the last 10 billion years galaxies have been continuously killed\, and we still don’t know why. Today the Universe is littered with dead galaxies\, and their distribution is correlated with location (environment). This suggests that location is one of the prime suspects in this galactic whodunit. However\, previous observations and techniques have restricted us to only measuring galaxy environments in the nearby Universe\, inhibiting our ability to identify when\, where and why they are killed. In addition\, galaxy location might not be the only suspect in town. Monsters are hiding at the centres of the most massive galaxies\, ready to lead to their untimely demise. In this talk I will discuss various programs using large multi-wavelength surveys\, such as GAMA and DEVILS\, to explore the smoking gun factors that have led to the death of galaxies over the last 10billion years. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-luke-davies-uwa/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-13092023.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230920T150000
DTEND;TZID=Australia/Sydney:20230920T160000
DTSTAMP:20260527T084738
CREATED:20250819T071725Z
LAST-MODIFIED:20250819T071726Z
UID:14945-1695222000-1695225600@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Anais Moller (Swinburne)
DESCRIPTION:Transients in the era of large scale surveys\n\nAbstract\n\nVera C. Rubin Observatory will open a new era for optical astronomy by imaging the Southern Sky at unprecedented depths. I will introduce Fink\, which will process Rubin’s millions transient detections every night. Fink not only processes immense datasets in real-time\, but selects the most promising candidates for a breadth of science using machine learning and multi-wavelength and messenger survey data. n To make a leap to this new era\, I will review the contributions of machine learning classification for transient science and cosmology in the Dark Energy Survey. I will then present results from Fink’s processing of the Zwicky Transient Survey\, as a precursor of Rubin. These results include selection methods and analyses of supernovae\, kilonovae and satellite glints. I will conclude with the potential of connecting Rubin’s data with other observing facilities for multi-wavelength and messenger astronomy and our current efforts with Australian facilities. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-anais-moller-swinburne/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/png:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-20092023.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230927T150000
DTEND;TZID=Australia/Sydney:20230927T160000
DTSTAMP:20260527T084738
CREATED:20250819T071655Z
LAST-MODIFIED:20250819T071656Z
UID:14946-1695826800-1695830400@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Chayan Chatterjee (UWA)
DESCRIPTION:Enabling rapid discovery of gravitational waves using machine learning\n\nAbstract\n\nGravitational waves are ripples in spacetime curvature created by some of the most energetic events in the universe like the collisions of compact astrophysical objects like black holes and neutron stars. These ripples propagate through space at the speed of light and are detected by several km long laser interferometers called LIGO and Virgo\, located in the US and Italy. The simultaneous observation of gravitational waves and prompt electromagnetic emissions from the compact object mergers can help reveal properties of extreme matter and gravity during and immediately after the coalescence. However\, such simultaneous observations rely on rapid detection and sky localization of gravitational waves\, often requiring alerts to be sent out before merger. \n\n In this seminar\, I will describe different machine learning models that I have developed to solve challenging problems in rapid gravitational wave discovery – pre- and post-merger sky localization\, and waveform extraction from real detector data. I will demonstrate the accuracy and feasibility of these methods on simulated data as well as on real gravitational wave events detected during the first three observation runs of LIGO and Virgo. Finally\, I will talk about the future scope of this research work and highlight some of the other areas in gravitational wave astronomy where these deep learning techniques can be applied. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-chayan-chatterjee-uwa/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-27092023.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20231025T150000
DTEND;TZID=Australia/Sydney:20231025T160000
DTSTAMP:20260527T084738
CREATED:20250819T071627Z
LAST-MODIFIED:20250819T071628Z
UID:14947-1698246000-1698249600@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Chris M. Moeckel (UC Berkeley)
DESCRIPTION:Radio observations of the giant planets: from the ground and up-close\n\nAbstract\n\nThe vertical distribution and evolution of trace gases in planetary atmospheres are key observables for understanding the dynamics of the atmosphere. Radio observations\, such as observations from the Microwave Radiometer (MWR) on board of Juno and observations from the earth-based telescopes such as the Very Large Array (VLA) are our current best tools to understand the sub-cloud structure on the giant planets. However\, inverting radio observations to recover the atmospheric structure is non-trivia. Based on the commonalities between different atmospheric model frameworks\, we show surprising results of what we learned about Jupiter’s atmosphere and address the implications for the atmosphere of giant planets in general. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-chris-m-moeckel-uc-berkeley/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-25102023-scaled.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20231101T150000
DTEND;TZID=Australia/Sydney:20231101T160000
DTSTAMP:20260527T084738
CREATED:20250819T071458Z
LAST-MODIFIED:20250819T071458Z
UID:14948-1698850800-1698854400@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Fernando Camilo (SARAO)
DESCRIPTION:MeerKAT at 5\n\nAbstract\n\nThe MeerKAT radio telescope in South Africa was inaugurated 5 years ago. In this talk I’ll provide a broad overview of science results to date. Among other examples\, I’ll show: how an exquisitely sensitive continuum image is constraining the star formation history of the universe\, putting it into tension with UV+IR-derived evolution; the discovery of OH megamasers at redshift > 0.5; how the study of neutral hydrogen down to column densities of ~5e17/cm^2 is enabling Local Group science outside the Local Group\, and revealing how gas is shaped and removed from galaxies in cluster environments. Come see how MeerKAT combined with a pulsar timing backend developed in Australia is enabling unprecedented tomographic mapping of the Local Bubble and constraints on a stochastic background of gravitational waves. I’ll also cover the discovery and study of numerous extragalactic and Galactic transients – including still mysterious sources with rotation periods up to tens of minutes – done in part jointly with the MWA and ASKAP. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-fernando-camilo-sarao/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-01112023-scaled.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20231108T150000
DTEND;TZID=Australia/Sydney:20231108T160000
DTSTAMP:20260527T084738
CREATED:20250819T071428Z
LAST-MODIFIED:20250819T071429Z
UID:14949-1699455600-1699459200@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Yuzhe (Robert) Song (Swinburne)
DESCRIPTION:Gamma-ray Emission from Nearby Stellar Flares and Undetected Pulsars\n\nAbstract\n\nThe continuing survey of the gamma-ray sky by the Large Area Telescope (LAT) onboard the Fermi Gamma-ray Space Telescope enables us to carry out population studies in gamma-rays. We developed novel stacking techniques to analyse Fermi-LAT data beyond the limit of point source sensitivity\, which subsequently have been applied to various types of astrophysical sources. \n\n So far\, less than 10% of known pulsars are detected in gamma-rays. Stacking analysis of pulsars off the Galactic plane shows a significant detection\, with a pulsar-like spectral index and a characteristic flux well below the Fermi-LAT point source sensitivity. Using COMPAS\, a rapid binary population synthesis code\, we provide a best fit model of distributions of pulsar properties at birth that can describe our observations. \n\n Young ultra-cool dwarfs are extremely magnetically active and produce highly energetic flares\, yet the Sun is the only isolated main sequence star detected in gamma-rays. We present a temporal analysis of red dwarf TVLM 513-46546 and reported periodicity in gamma-rays. Stacking Fermi-LAT data during flare events identified from optical and X-ray flare surveys reports an upper limit of flare gamma-ray emission. It likely originates from decay of neutral pions generated from the relativistic protons interacting within the stellar atmosphere. If confirmed\, this could be catastrophic on exoplanet atmospheres and significantly reduces the habitability on these worlds. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-yuzhe-robert-song-swinburne/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-08112023.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20231115T150000
DTEND;TZID=Australia/Sydney:20231115T160000
DTSTAMP:20260527T084738
CREATED:20250819T071310Z
LAST-MODIFIED:20250819T071311Z
UID:14950-1700060400-1700064000@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Joshua Pritchard (University of Sydney)
DESCRIPTION:Searches for Stellar Radio Activity in Circular Polarisation\n\nAbstract\n\nTransient radio bursts produced in the coronae of stellar atmospheres and within planetary magnetospheres often feature a high degree of circular polarisation. These events reveal the presence of strong magnetic fields\, and trace particle acceleration driven by magnetic reconnection\, space weather\, and auroral current systems. The detection of stellar radio emission has historically been challenged by the overwhelmingly higher surface density of extra-Galactic sources that dominate the radio sky\, which produce a large number of false positive associations to optically identified stars. Our knowledge of the radio star population has therefore been primarily driven by targeted studies of the most active\, nearby systems\, impacting the inference of population statistics and discovery of new regimes of stellar radio activity. \n\n In this talk I will present a body of work that exploits the circular polarisation of magnetically driven stellar radio emission to identify large samples of radio stars in widefield surveys. I will describe the application of this technique to two widefield surveys with the Australian Square Kilometre Array Pathfinder (ASKAP—the Rapid ASKAP Continuum Survey (RACS) and the Variables and Slow Transients (VAST) Pilot Survey—which resulted in 229 detections of a sample of 76 radio stars. Through repeat sampling of this group our observations place constraints on the statistical fraction of the M-dwarf population that produce radio bursts and provide a forecast of expected detection rates in future surveys with ASKAP and the Square Kilometre Array. Finally\, I will discuss the utility of circular polarisation searches to uncover novel regimes of stellar radio activity. I will highlight the discovery of rotationally modulated auroral radio pulses from an old\, slowly rotating M9.5 ultracool dwarf in a two year monitoring campaign with ASKAP and the Australia Telescope Compact Array. This object is the oldest and slowest rotator among known aurorally active ultracool dwarfs and displays a rich variety of radio burst features\, forming an important probe of the dynamo mechanism responsible for strong magnetism in ageing cool stars. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-joshua-pritchard-university-of-sydney/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/png:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-15112023.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20231122T150000
DTEND;TZID=Australia/Sydney:20231122T160000
DTSTAMP:20260527T084738
CREATED:20250819T071240Z
LAST-MODIFIED:20250820T032535Z
UID:14951-1700665200-1700668800@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Prajval Shastri (ICRAR / RRI)
DESCRIPTION:Different Angles on Accreting Supermassive Black Holes\n\nAbstract\n\nSupermassive black holes appear to inhabit the centres of most galaxies and co-evolve with them\, thus playing a significant role in regulating galaxy assembly. We are able to spot these black holes to very high redshifts when they accrete matter\, which is also what causes them to impact their environments out to spatial scales that are well beyond their gravitational sphere of influence. In this talk I will discuss the understanding that has emerged from multiple-frequencies studies of the systematics of accreting supermassive black holes. \n\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-prajval-shastri-icrar-rri/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-22112023.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20231129T150000
DTEND;TZID=Australia/Sydney:20231129T160000
DTSTAMP:20260527T084738
CREATED:20250819T071214Z
LAST-MODIFIED:20250819T071215Z
UID:14952-1701270000-1701273600@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Amit Seta (ANU)
DESCRIPTION:Magnetic fields in the Milky Way from pulsar observations\n\nAbstract\n\nPulsars can act as an excellent probe of the Milky Way magnetic field. The average strength of the Galactic magnetic field component parallel to the line of sight can be estimated as 1.232 RM/DM\, where RM and DM are the rotation and dispersion measure. However\, this assumes that the thermal electron density and magnetic field of the interstellar medium are uncorrelated. Using numerical simulations and observations\, we test the validity of this assumption. Based on magnetohydrodynamical simulations of driven turbulence\, we show that the correlation between the thermal electron density and the small-scale magnetic field increases with increasing Mach number of the turbulence. We find that the assumption of uncorrelated thermal electron density and magnetic fields is valid only for subsonic and transsonic flows\, but for supersonic turbulence\, the field strength can be severely overestimated. We then correlate existing pulsar observations from the Australia Telescope National Facility with regions of enhanced thermal electron density probed by CO\, Zeeman\, neutral hydrogen and Halpha observations. Using these observational data\, we show that the thermal electron density and magnetic fields are largely uncorrelated over kpc scales. Thus\, we conclude that the relation provides a good estimate of the magnetic field on Galactic scales\, but might break down on sub-kpc scales. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-amit-seta-anu/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/png:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-29112023.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20231206T150000
DTEND;TZID=Australia/Sydney:20231206T160000
DTSTAMP:20260527T084738
CREATED:20250819T071153Z
LAST-MODIFIED:20250819T071154Z
UID:14953-1701874800-1701878400@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Dipanjan Mitra (NCRA\, TIFR)
DESCRIPTION:Rotating vector model of pulsars\n\nAbstract\n\nMore than Fifty years have passed since the discovery of pulsars\, yet the physical mechanism of their coherent radio emission is unclear. The linear polarization position angle (PPA) tracks observed in normal pulsars (periods > 0.1 sec) can be explained by the rotating vector model (RVM)\, which forms the basis for understanding pulsar coherent radio emission physics. In several pulsars only one RVM like PPA track is seen while in other pulsars two parallel orthogonal tracks are seen\, and this variation can be understood as radiation coming out from the pulsar magnetosphere to mainly consist of extraordinary or ordinary waves polarized perpendicular or parallel to the planes of pulsar dipolar magnetic field. However there also exists an equally large sample of pulsars where the PPA traverses shows a complex non-RVM pattern. This diverse behaviour is in conflict with applying a unique emission mechanism to the pulsar population\, and hence the fundamental question of whether the outgoing waves are excited by maser or curvature radiation (also known as antenna mechanism) had remained unresolved. In this talk I will argue that high quality single pulse polarimetric observations can be used to distinguish the emission mechanism. I will showcase examples of how highly linearly polarized signals can unravel the underlying RVM\, particularly in pulsars with PPAs showing complex patterns. This feature strongly favours the coherent curvature radiation mechanism to be universally applicable in the normal pulsar population. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-dipanjan-mitra-ncra-tifr/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-06122023.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20231213T150000
DTEND;TZID=Australia/Sydney:20231213T160000
DTSTAMP:20260527T084738
CREATED:20250819T071111Z
LAST-MODIFIED:20250819T071112Z
UID:14954-1702479600-1702483200@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Ron Ekers (CSIRO)
DESCRIPTION:History of radio astronomy\n\nAbstract\n\nIt was 90 years ago when Karl Jansky announced his discovery of radio noise from the Milky Way Galaxy at the April 1933 meeting of URSI in Washington and Radio Astronomy was born. I was asked to give a General Lecture on the entire history of radio astronomy at the URSI General Assembly in Sapporo\, Japan on 23 Aug 2023. I will give a slightly abbreviated version of this lecture as a S&A colloquium. \n\n Instead of just presenting a historical review of all the discoveries I will explore some of the circumstances leading up to the discoveries\, including some stories not generally known\, but which provide the background and context. These details are often excised from the standard scientific narrative but are essential to understand the roles played by serendipity\, prediction\, and technology. There is “nothing fortuitous” in so-called serendipitous discoveries. As Pasteur famously quoted “In the field of observation\, chance favors only the prepared mind.” \n\n While many discoveries are serendipitous\, they depend on the development of new technology. So\, it is the telescopes\, the instruments connected to the telescopes\, and the data analysis that leads to most new discoveries. The scientific discoveries for which facilities become famous are rarely those predicted from the science goals for which the telescopes were built. Building the next generation of radio telescopes to continue our 90 years of innovation and discovery will set new challenges. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-ron-ekers-csiro/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-13122023.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20231220T150000
DTEND;TZID=Australia/Sydney:20231220T160000
DTSTAMP:20260527T084738
CREATED:20250819T071043Z
LAST-MODIFIED:20250819T071044Z
UID:14955-1703084400-1703088000@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Joe Callingham (ASTRON/Leiden University)
DESCRIPTION:Radio stars and Exoplanets\n\nAbstract\n\nOne key question that astronomy is attempting to answer is whether there are habitable planets around stars other than our Sun. While we have entered an era where identifying nearby exoplanets has become standard\, discerning whether the environmental conditions dictated by the host stars are suitable for life has proved far more elusive. The detection of low-frequency radio emission from an M dwarf or an exoplanet provides a direct probe of extrasolar space weather and the planet’s magnetic field – information crucial for assessing the potential habitability of the planet. In this talk\, I will outline our LOFAR survey of stellar systems\, with a focus on our recent detection of strong\, highly circularly polarised low-frequency radio emission associated with nearby stars – the expected signpost of star-exoplanet interactions. I will discuss how our survey represents the most comprehensive observations of stellar systems at low frequencies\, and the implications of this new population in understanding the magnetosphere of M dwarfs and exoplanetary magnetic fields. \n\n \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-joe-callingham-astron-leiden-university/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-20122023.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240117T150000
DTEND;TZID=Australia/Sydney:20240117T160000
DTSTAMP:20260527T084738
CREATED:20250819T061409Z
LAST-MODIFIED:20250819T061409Z
UID:14852-1705503600-1705507200@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Kana Morokuma-Matsui (University of Tokyo)
DESCRIPTION:ALMA CO surveys of the Fornax cluster and the Eridanus supergroup\n\nAbstract\n\nThe evolution of galaxies is affected by their surrounding environment. The star formation (SF) in galaxies in galaxy clusters is known to be less active compared to those in the normal field. In order to understand the SF quenching processes in cluster galaxies\, we conducted CO(J=1-0) mapping survey of 64 Fornax cluster galaxies and 103 Eridanus supergroup galaxies using the Morita array of ALMA in cycles 5 and 7\, respectively. The Fornax cluster is the 2nd nearest galaxy cluster from the Milky Way at a distance of 20 Mpc. The Eridanus supergroup is located near the Fornax cluster and is an ensemble of galaxy groups that are expected to be a single cluster in the future. For the Fornax cluster\, the achieved beam size and sensitivity are 15′′ × 8′′ and ~12 mJy/beam1 at the velocity resolution of ∼10 km/s\, respectively. CO emission is detected from 23 out of the 64 galaxies. We find the low SF activity in the cluster galaxies is attributed to the low molecular gas contents of galaxies. The SF efficiency from molecular gas\, a ratio of SF rate over molecular gas mass\, in the Fornax galaxies is comparable to that of field galaxies. Combined with archival HI data\, we also find that the atomic-gas reservoirs are more heavily reduced than the molecular-gas reservoirs in the Fornax galaxies with low SF activity. In this colloquium\, I will present the preliminary results for the Eridanus supergroup galaxies. \n\n \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-kana-morokuma-matsui-university-of-tokyo/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-17012024.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240124T150000
DTEND;TZID=Australia/Sydney:20240124T160000
DTSTAMP:20260527T084738
CREATED:20250819T061337Z
LAST-MODIFIED:20250819T061337Z
UID:14853-1706108400-1706112000@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Tomoki Morokuma
DESCRIPTION:Time Domain Astronomy with Subaru Hyper Suprime-Cam and A Serendipitously Discovered Active Galactic Nucleus with Large Brightness Decline\n\nAbstract\n\nTime Domain Astronomy has been getting popular especially in optical astronomy\, mainly using wide-field imaging instruments. Hyper Suprime-Cam (HSC) on the 8.2-m Subaru telescope currently has the best survey capability in terms of survey speed. We have been conducting transient surveys with Subaru/HSC in various time scales from minutes to years since its first light in 2014. I will summarize several main results from our transient surveys. In the latter part of my talk\, I focus on one distant active galactic nucleus (AGN) showing a very large decline in brightness over 20 years. This object is interpreted as a rare phenomena in an AGN where its accretion activity has been almost shut down. \n\n \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-tomoki-morokuma/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-24012024.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240207T150000
DTEND;TZID=Australia/Sydney:20240207T160000
DTSTAMP:20260527T084738
CREATED:20250819T061235Z
LAST-MODIFIED:20250819T061235Z
UID:14854-1707318000-1707321600@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Hamsa Padmanabhan (University of Geneva)
DESCRIPTION:Deciphering Cosmic Dawn: A Conquest of the Final Frontier\n\nAbstract\n\nI will begin with a broad-based introduction to some of the big open questions in cosmology\, and illustrate how upcoming experiments are well-poised to help answer them\, especially at the Cosmic Dawn — the birth of the first galaxies in our Universe — widely believed to be the ‘final frontier’ of cosmological surveys today. This period — about a hundred million years after the Big Bang — is primarily accessible due to radiation from hydrogen\, the most abundant element in the Universe\, which emits at a wavelength of 21 cm\, in the radio band. An exquisite investigation of the Cosmic Dawn will soon become possible with an emerging technique called intensity mapping (IM)\, which measures the integrated 21 cm emission from all sources\, using large arrays of radio telescopes. A particular advantage of IM is that it provides a tomographic\, or three-dimensional picture of the Universe\, unlocking significantly more information than we presently have from galaxy surveys. I will overview the latest advances in research related to the evolution of hydrogen over 12 billion years of cosmic time\, involving a novel data-driven framework to interpret current and future observations. This allows us to fully utilize our present knowledge of astrophysics in order to develop cosmological forecasts from IM. Apart from offering key insights into the nature of the first galaxies\, this opens up the exciting possibility of testing theories of fundamental physics from the Cosmic Dawn. \n\n \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-hamsa-padmanabhan-university-of-geneva/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-07022024.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240214T150000
DTEND;TZID=Australia/Sydney:20240214T160000
DTSTAMP:20260527T084738
CREATED:20250819T061157Z
LAST-MODIFIED:20250819T061157Z
UID:14855-1707922800-1707926400@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Rudrani Chowdhury (University of Hong Kong)
DESCRIPTION:Detecting last light from first stars\n\nAbstract\n\nFirst generation metal-free stars\, referred to as population III (Pop III) stars\, are believed to be the first objects to form out of the pristine gas in the very early Universe. Pop III stars have different structures from the current generation of stars and are important for generating heavy elements and shaping subsequent star formation. However\, it is very challenging to directly detect Pop III stars given their high redshifts and short life-times. In this work\, we propose a novel signature for detecting Pop III stars through their tidal disruption events (TDEs) by massive black holes. We model the emission properties and calculate the expected rates for these unique TDEs in the early Universe at z ~10. We find that Pop III star TDEs have much higher mass fallback rates compared to normal TDEs in the local universe and are therefore rather luminous\, rendering them feasible for detection. They also have very long observed flare evolution timescale\, making it more likely to detect such TDEs during their rising phase. We further demonstrate that a large fraction of the TDE emissions are redshifted to infrared wavelengths and can be detected by the James Webb Space Telescope and the Nancy Grace Roman Space Telescope. Lastly\, the TDE rate sensitively depends on the black hole mass function in the early Universe. We find a promising Pop III star TDE detection rate of up to a few tens per year using the Nancy Grace Roman Space Telescope. \n\n \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-rudrani-chowdhury-university-of-hong-kong/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-14022024.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240228T150000
DTEND;TZID=Australia/Sydney:20240228T160000
DTSTAMP:20260527T084738
CREATED:20250819T061124Z
LAST-MODIFIED:20250819T061124Z
UID:14856-1709132400-1709136000@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Stanley Owocki (University of Delaware)
DESCRIPTION:Stellar-wind-fed magnetospheres of magnetic massive stars\n\nAbstract\n\nA sub-population (~9%) of hot (OB) stars exhibit strong (B~100-10\,000 G)\, large-scale (often predominantly dipolar) magnetic fields that channel their stellar wind outflows into circumstellar magnetospheres. For young\, rapidly rotating B-stars that have not yet been spun down by wind-magnetic braking\, wind material can be trapped between the Kepler co-rotation radius (RK) and the Alfven radius (RA)\, forming then a “Centrifugal Magnetosphere” (CM)\, with density set at the critical level for “Centrifugal Breakout” (CBO) against the confining magnetic tension. This talk discusses how such CBO controls both the onset and strength of observed H-alpha emission\, while the energetics of the associated CBO-driven magnetic reconnection match well the observed scalings of a non-thermal\, circularly polarized radio emission from such stars . \n\n \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-stanley-owocki-university-of-delaware/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/png:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-28022024.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240306T150000
DTEND;TZID=Australia/Sydney:20240306T160000
DTSTAMP:20260527T084738
CREATED:20250819T061058Z
LAST-MODIFIED:20250819T061058Z
UID:14857-1709737200-1709740800@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Nivedita Mahesh (California Institute of Technology)
DESCRIPTION:The Frontier in Low Frequency Radio Astrophysics from the Farside of the Moon\n\nAbstract\n\nThe Farside Array for Radio Science Investigations of the Dark ages and Exoplanets (FARSIDE) is a NASA Probe-class concept to place a low-frequency radio interferometric array on the far side of the Moon. FARSIDE will look for radio emissions from magnetospheres of stars and exoplanets\, which affect exoplanet habitability and serve as a pathfinder for studying the Dark Ages of the Universe. The FARSIDE architecture employs a novel design consisting of 128 pairs of antennas and receiver nodes distributed over a 10 km × 10 km area in a four-arm spiral configuration that will operate from 200 kHz to 40 MHz. I will present the planned mission architecture\, array layout\, antenna packaging\, and deployment trade study. In addition\, this talk will cover the projected performance and sensitivity of the array for the two primary sciences cases. Given the novel deployment strategy for the FARSIDE array\, we have developed a forward modeling pipeline to simulate its polarization performance. This lunar array concept is developed a lot on the heritage of a similar low frequency telescope on ground – the OVRO Long Wavelength Array. And I will briefly discuss the current status and pipeline development efforts of the newly upgraded OVRO-LWA. The talk will end with an overview of one of humanities’ next “great” observatories – FarView – a NASA Innovative Advanced Concepts. Farview will be an observatory built in-situ on the lunar farside using materials from regolith. \n\n \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-nivedita-mahesh-california-institute-of-technology/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-06032024.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240313T150000
DTEND;TZID=Australia/Sydney:20240313T160000
DTSTAMP:20260527T084738
CREATED:20250819T061017Z
LAST-MODIFIED:20250819T061018Z
UID:14858-1710342000-1710345600@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Magda Arnaboldi (ESO)
DESCRIPTION:The evolution of the Giant Andromeda galaxy mapped using planetary nebulae in its disc and inner halo\n\nAbstract\n\n \n\nIn 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 nearly radial orbit. This tumultuous recent past of Andromeda is very different from our own Milky Way galaxy\, that experienced a rather quiescent evolution in the last 8 Gyrs. I will present the evidence for a younger thin and older thicker disc component in M31 and present the age-velocity dispersion relation at the corresponding radial distance of the solar neighbourhood in M31. Then I explore the chemical composition of these discs using Oxygen and Argon element abundance. The two kinematically distinct discs in Andromeda are also chemically distinct\, 1) with the thin disc reaching higher Argon abundances than the thicker disc\, 2) the thicker disc having a positive Oxygen and null Argon radial gradient\, 3) while the thin disc presents a negative radial gradient in both Oxygen and Argon. The latter gradient is consistent with the negative Oxygen gradient previously measured for the HII regions. I then use the log(O/Ar) vs. (12 + log(Ar/H) ) distribution of stars with different ages to constraint the chemical evolution of the parent stellar populations in the thin and thicker M31 discs. The distributions in this plane show that the chemical and also the structural properties of the thin and thicker discs in M31 are remarkably different from those determined for the Milky Way. I then investigate the stellar populations and kinematics of the inner halo substructures – NE and W shelves\, Giant stellar stream and G1 clump – and compare them with the detailed predictions from simulations of a major merger event in Andromeda. The goal is to understand whether it is a wet or a dry merger\, and to further 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 information from the combined use of Oxygen and Argon to constrain the early phases of star formation in z>4.0 galaxies. \n\n \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-magda-arnaboldi-eso/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-13032024.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240320T150000
DTEND;TZID=Australia/Sydney:20240320T160000
DTSTAMP:20260527T084738
CREATED:20250819T060952Z
LAST-MODIFIED:20250819T060953Z
UID:14859-1710946800-1710950400@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Anthony J. Beasley (NRAO)
DESCRIPTION:Near and Long-term Trends and Opportunities in US Radio Astronomy\n\nAbstract\n\n \n\nIn this talk I will discuss the ambitious scientific program underway in the United States over the next decade to explore the radio Universe\, in concert with numerous powerful new instruments around the world\, and facilities at other wavelengths. The scientific opportunities and technical/operational challenges being faced by ground-based radio astronomy in the United States currently are significant; half a decade beyond the 2020 Decadal Survey process\, factors both internal and external to the astronomy community have slowed the development of many U.S. facilities. NRAO is exploring several new technologies and operational approaches to optimize the scientific return from our existing and planned instruments; these will be described. As the field of radio astronomy approaches its centenary\, we continue to seek new scientific horizons. \n\n \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-anthony-j-beasley-nrao/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-20032024.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240327T150000
DTEND;TZID=Australia/Sydney:20240327T160000
DTSTAMP:20260527T084738
CREATED:20250819T060923Z
LAST-MODIFIED:20250819T060924Z
UID:14860-1711551600-1711555200@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Samuel Lai (CSIRO)
DESCRIPTION:High-Redshift Ultraluminous Quasi-Stellar Objects\n\nAbstract\n\nOver the past century\, black holes transitioned from theoretical constructs to ubiquitous entities in the Universe. Extensive evidence supports the notion that supermassive black holes\, which reside in the nuclear region of most mature galaxies\, play an integral role in the assembly and dynamics of galactic material on cosmological timescales. However\, the rapid evolution of supermassive black holes and their immediate environments in the early Universe (< 1 Gyr) is still poorly understood due to the paucity of robust constraints on physical accretion mechanisms\, the limited statistical significance of available samples\, and the scarcity of independent methodologies of black hole characterisation. \n\n 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 for quasar spectra and apply it to a high-redshift quasar samples\, measuring emission-lines (e.g. Si IV λ1398\, O IV λ1402\, C IV λ1549\, Mg II λ2799\, Hβ λ4863Å) and inferring black hole properties from mass\, luminosity\, and metallicity-sensitive features. I also present an analysis of quasar demographics in a z ~ 5 sample\, measuring supermassive black hole growth. Furthermore\, I showcase how thermal accretion disc models can be used to describe quasar spectral energy distributions. This approach has potential as a physically-motivated independent method that can aid in constraining properties of black holes. In summary\, this research yields insights into the understanding of high-redshift supermassive black holes and their growth\, equipping us with the necessary tools for detailed studies of quasar spectra. \n\n \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-samuel-lai-csiro/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-27032024.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240410T110000
DTEND;TZID=Australia/Sydney:20240411T170000
DTSTAMP:20260527T084738
CREATED:20240516T024016Z
LAST-MODIFIED:20241030T234942Z
UID:333-1712746800-1712854800@www.atnf.csiro.au
SUMMARY:Australia Telescope User Committee Meeting 2024
DESCRIPTION:Overview\n\nThe next ATUC meeting will be held in hybrid format (including an in-person mode at the Lecture Theatre at Marsfield\, NSW) on 10-11 April 2024. \n\nOn 10 April\, an Open Session will be held that consists of updates and discussions on the various aspects of ATNF facilities. All are welcome to register to attend the Open Session\, using this registration form accessible by clicking the button below. General registration for ATUC will close at 17:00 AWST on 29 March 2024. \n\nAn agenda\, with details for hybrid participation\, will be made available to registered attendees closer to the event. \n\nIf you\, as a user (or potential user) of the ATNF\, are aware of any issues that need to be raised at the next ATUC meeting\, or would like to offer feedback on ATNF activities and facilities\, please contact any member of ATUC over the next few weeks. \n\nInformation on ATUC and how to contact its members can be found on the ATUC webpage. \n\nFor questions about this form or ATUC in general\, please contact Vanessa Moss. \nRegister now\nLocation\n\nAnother location\n\nOrganiser\n\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/atuc-2024/
LOCATION:Kensington Lecture Theatre\, WA\, Australia
CATEGORIES:Meeting
ORGANIZER;CN="Vanessa Moss":MAILTO:vanessa.moss@csiro.au
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240411T150000
DTEND;TZID=Australia/Sydney:20240411T160000
DTSTAMP:20260527T084738
CREATED:20250819T060853Z
LAST-MODIFIED:20250819T060854Z
UID:14861-1712847600-1712851200@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Albert Zijlstra (University of Manchester)
DESCRIPTION:Stars that merge in the Milky Way\n\nAbstract\n\n Stellar explosions come in two main varieties. At the top end are the supernovae\, visible to cosmological distances but which may be missed when occurring in our own Milky Way. The second group are the novae\, frequent events but much fainter. But some transients fall in between\, too bright and long-lasting for novae but too faint for supernovae. Although rare\, there are some historical observations of such events in the Milky Way. This talk will discuss two such eruptions. The first is CK Vul\, which exploded in 1670 as a 3rd magnitude nova\, re-appeared in 1671 and again in 1672. The second event is the supernova of 1181 which was (only) as bright as Saturn but remained visible for 180 days. Both objects are understood as stellar merger events; SN1181 is a possible Type Iax supernova\, the least understood of the major supernovae. \n\n The image above shows the Pa 30 nebula\, which we identify as the remnant of the supernova explosion of the year 1181. The left panel shows a false colour image of Pa 30 where red stands for an image taken with the WISE satellite at 11 micron\, green for WISE 22 micron\, and blue for ultraviolet emission mapped by the GALEX satellite; the contours show X-ray emission mapped with the XMM-Newton satellite. The majority of the X-ray emission originates from the core of the nebula while WISE sees the larger nebula. The panel on the right shows an image of the [O IIII] emission from the nebula\, taken with the 2.1-m telescope at Kitt Peak [O III] image. The green cross in the center of the image marks the location of the central star. Both panels are to the same scale. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-albert-zijlstra-university-of-manchester/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-11042024.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240417T150000
DTEND;TZID=Australia/Sydney:20240417T160000
DTSTAMP:20260527T084738
CREATED:20250819T060608Z
LAST-MODIFIED:20250819T060609Z
UID:14862-1713366000-1713369600@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Jordan Collier (AusSRC/CIRA)
DESCRIPTION:Clouds over middle-earth: using ilifu to combine the MeerKAT and the EMU for ORCs\n\nAbstract\n\n Combining ASKAP’s EMU survey and MeerKAT enables complementary science; ASKAP’s large FoV enables the discovery of new/rare types of objects\, like Odd Radio Circles (ORCs)\, while MeerKAT’s sensitivity enables deep follow up of such objects. I will speak about both instruments and how they are being used to open up new phase spaces of discovery\, with a particular focus on the spectral indices and polarisation of ORCs\, and my experience using these telescopes within the clouds across the continents of middle-earth! As an essential part of this research\, I will speak about a number of tools and systems that have been developed or adopted to deal with the PB scale of MeerKAT data at the Inter-University Institute for Data Intensive Astronomy (IDIA). I will present a number of these tools and underlying systems\, deployed on IDIA’s ilifu facility\, including those for storage\, processing\, visualisation\, and data transfers. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-jordan-collier-aussrc-cira/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-17042024.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240424T150000
DTEND;TZID=Australia/Sydney:20240424T160000
DTSTAMP:20260527T084738
CREATED:20250819T060316Z
LAST-MODIFIED:20250819T060316Z
UID:14863-1713970800-1713974400@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Ophelia Renaud (INSA-IETR\, France)
DESCRIPTION:Design and programming of heterogeneous and high-performance computing systems in astronomy\n\nAbstract\n\n In this presentation\, I address the difficult problem inherent in SKA of deploying complex astronomical applications under development on efficient target architectures that have not yet been built. Resource allocation in such scenarios has a significant impact on multiple factors such as latency\, memory\, energy\, and cost among others. Solutions such as rapid prototyping make it possible to reliably simulate and generate efficient code for this purpose. At INSA-IETR\, we are developing the PREESM rapid prototyping tool to automate and accelerate this process. The tool is based on numerous thesis and internship projects as well as numerous collaborations such as Rising Stars\, which is the subject of my presentation. This presentation will give an overview of the project’s progress in our team. I propose methods based on the SDF (Synchronous Dataflow) model and clustering techniques to facilitate the deployment of applications on complex architectures such as CPUs\, GPUs\, and FPGAs on one or more machines. By providing a quick and easy solution to this NP-hard problem\, our methods significantly improve the efficiency of astronomical application deployment. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-ophelia-renaud-insa-ietr-france/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/png:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-24042024.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240508T150000
DTEND;TZID=Australia/Sydney:20240508T160000
DTSTAMP:20260527T084738
CREATED:20250819T055031Z
LAST-MODIFIED:20250819T055031Z
UID:14864-1715180400-1715184000@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Anna Scaife  (Uni of Manchester\, UK); Jayaram N Chengalur (TIFR\, India); Scott Ransom (NRAO\, USA)
DESCRIPTION:CSIRO Space & Astronomy Special Mini-Symposium\n\nAbstract\n\n This week a special mini-symposium will be held in-person at Marsfield\, and on-line\, with the three international members of the ATNF Steering Committee each giving a short presentation. \n\nScaling laws and self-supervised learning in AI for astrophysics – Anna Scaife (University of Manchester)\n\n As the current trend in deep-learning tends towards more data\, more compute and more parameters\, we ask: how large can astrophysical deep-learning models get? Using the largest dataset of labelled astronomy data available\, we examine the scaling laws for supervised problems in astrophysics and conclude that self-supervised learning is a more promising direction for large-scale deep-learning in astronomy given the available label volumes; however\, we also conclude that using in-domain (astronomy) data for pre-training results in better performance for the down-stream tasks from these self-supervised representations. Finally\, I will show how we are building self-supervised foundation models for radio astronomy and a variety of the downstream tasks where we have applied them in practice. \n\nThe evolution of the HI content of galaxies – Jayaram Chengalur (TIFR)\n\n Over cosmic time\, galaxies grow by merger\, and/or by the accretion of matter via inflows. As galaxies evolve they also convert their gas into stars. On a cosmic scale\, it is well established that the star formation peaked about 10 billion years ago and that the average star formation rate per unit volume has declined sharply since then. Hydrogen is dominant baryonic component of galaxies\, and atomic hydrogen is also the primary fuel for star formation. Stars form as the gas cools to become molecular hydrogen\, and then cools further and collapses into stars under self gravity. Understanding the evolution of the atomic hydrogen content of galaxies is hence key to understanding the evolution of the star formation rate with cosmic time. The recent upgrade to the Giant Metrewave Radio Telescope (GMRT)\, has allowed significant progress to be made in observing HI in galaxies at redshifts around 1 using the stacking method. In this talk\, I will discuss some of the results from ongoing atomic hydrogen surveys of star forming galaxies using the upgraded GMRT. \n\nNew Exotic and Massive Pulsars in Globular Clusters – Scott Ransom (NRAO)\n\n In the past five years\, the number of known globular cluster pulsars\, most of them of the millisecond variety\, has blossomed by more than 130 to a total of over 300. The main reasons were the commissioning of the extremely sensitive FAST and MeerKAT radio telescopes\, and increased computing power applied to the searches themselves. In this talk I’ll mention some of the fascinating exotic systems that have been found\, discuss the importance of long-term timing of these systems\, and hint at the astrophysics and basic physics those systems will provide. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-anna-scaife-uni-of-manchester-uk-jayaram-n-chengalur-tifr-india-scott-ransom-nrao-usa/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-08052024a.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240515T150000
DTEND;TZID=Australia/Sydney:20240515T160000
DTSTAMP:20260527T084738
CREATED:20250819T054651Z
LAST-MODIFIED:20250819T054652Z
UID:14865-1715785200-1715788800@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Kai Polsterer (HITS gGmbH\, Heidelberg)
DESCRIPTION:From Supervised to Unsupervised ML: lessons learned from learning machines\n\nAbstract\n\nThe amount\, size\, and complexity of astronomical data-sets is growing rapidly in the last decades. Now\, with new technologies and dedicated survey telescopes\, the databases are even growing faster. Besides dealing with poly-structed and complex data\, sparse data has become a field of growing scientific interest. By applying technologies from the fields of computer sciences\, mathematics\, and statistics\, astronomical data can be accessed and analysed more efficiently. \n\n A specific field of research in astroinformatics is the estimation of the redshift of extra-galactic sources\, a measure of their distance\, by just using sparse photometric observations. Observing the full spectroscopic information that would be necessary to directly measure the redshift\, would be too time-consuming. Therefore\, building accurate statistical models is a mandatory step\, especially when it comes to reflecting the uncertainty of the estimates. Statistics and especially weather forecasting has introduced and utilized proper scoring rules and especially the continuous ranked probability score to characterize the calibration as well as the sharpness of predicted probability density functions. \n\n After presenting how this work led from well calibrated redshift estimates to an improvement in statistical post-processing of weather forecast simulations\, an example of interdisciplinarity in data-science\, we continue with unsupervised machine learning techniques. We start with the challenge of classifying morphologies of radio-galaxies\, talk about star-formation history in LMC\, discuss the difficulties in representing time-series\, and end with a discussion on novel explorative science platforms for e.g. spectral data. In this part of the talk\, we show-case how machine learning can be used as a machinery of discovery to access large data-sets. Several examples are presented to provide examples for the individual researchers in the audience. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-kai-polsterer-hits-ggmbh-heidelberg/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/png:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-15052024.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240522T150000
DTEND;TZID=Australia/Sydney:20240522T160000
DTSTAMP:20260527T084738
CREATED:20250819T054344Z
LAST-MODIFIED:20250819T054345Z
UID:14866-1716390000-1716393600@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Aman Chokshi (University of Melbourne)
DESCRIPTION:Instrumental Challenges of an Epoch of Reionization Detection\n\nAbstract\n\nAll-sky satellite measurements of Murchison Widefield Array beams reveal significant asymmetric sidelobe distortions at an ~10% level\, attributed to a range of environmental effects. In this talk I present the experiment used to carry out satellite beam measurements\, and the Bayesian MCMC framework developed to incorporate these satellite measurements into a simulation test-bed to understand and propagate the effects of distorted beams on Epoch of Reionization (EoR) Science. I demonstrate how mismatches between realistically deformed beams and the perfect beam assumed during calibration lead to unavoidable spectral contamination between 100-1000 times brighter than the expected EoR signal. I also outline methods which will enable next-generation telescopes such as the Square Kilometre Array to implement parallel and affordable beam monitoring systems\, facilitating the highest fidelity science outputs. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-aman-chokshi-university-of-melbourne/
LOCATION:WA
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/gif:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-22052024.gif
END:VEVENT
END:VCALENDAR