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BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240117T150000
DTEND;TZID=Australia/Sydney:20240117T160000
DTSTAMP:20260524T223352
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\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-kana-morokuma-matsui-university-of-tokyo/
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-17012024.jpg
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BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240124T150000
DTEND;TZID=Australia/Sydney:20240124T160000
DTSTAMP:20260524T223352
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\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-tomoki-morokuma/
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:20260524T223352
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\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-hamsa-padmanabhan-university-of-geneva/
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:20260524T223352
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\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-rudrani-chowdhury-university-of-hong-kong/
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:20260524T223352
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\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-stanley-owocki-university-of-delaware/
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:20260524T223352
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\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-nivedita-mahesh-california-institute-of-technology/
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:20260524T223352
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\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-magda-arnaboldi-eso/
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:20260524T223352
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\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-anthony-j-beasley-nrao/
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:20260524T223352
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\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-samuel-lai-csiro/
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-27032024.jpg
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BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240410T110000
DTEND;TZID=Australia/Sydney:20240411T170000
DTSTAMP:20260524T223352
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\nColearnia
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:20260524T223352
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\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-albert-zijlstra-university-of-manchester/
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:20260524T223352
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\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-jordan-collier-aussrc-cira/
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:20260524T223352
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\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-ophelia-renaud-insa-ietr-france/
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:20260524T223352
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\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-anna-scaife-uni-of-manchester-uk-jayaram-n-chengalur-tifr-india-scott-ransom-nrao-usa/
CATEGORIES:Colloquia
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BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240515T150000
DTEND;TZID=Australia/Sydney:20240515T160000
DTSTAMP:20260524T223352
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\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-kai-polsterer-hits-ggmbh-heidelberg/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240522T150000
DTEND;TZID=Australia/Sydney:20240522T160000
DTSTAMP:20260524T223352
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\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-aman-chokshi-university-of-melbourne/
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/gif:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-22052024.gif
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240529T150000
DTEND;TZID=Australia/Sydney:20240529T160000
DTSTAMP:20260524T223352
CREATED:20250819T054222Z
LAST-MODIFIED:20250819T054223Z
UID:14867-1716994800-1716998400@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Ellie Sansom (ICRAR/Curtin)
DESCRIPTION:A Global Fireball Observatory for planetary defence: a multidisciplinary approach\n\nAbstract\n\nWhen asteroids hit the Earth’s atmosphere\, they produce light\, heat and shock waves. Observing these phenomena\, from the fireball to the seismic and infrasound\, gives us a huge amount of information about the impacting object. We can calculate where they came from (their orbit)\, what they’re made of (geochemistry)\, size of the object\, and even where any meteorites might land. Large\, hazardous asteroid impacts are rare\, and civilisation-ending events from km-sized asteroids are relatively well constrained. But\, metre sized objects are still capable of posing a threat to people and property. Understanding these larger (>1 m diameters) events is fundamental to understanding the numbers of hazardous objects in the inner solar system; a key component to planetary defence. The Global Fireball Observatory is a planetary-scale observational facility for rare\, fireball events occurring when asteroids hit our atmosphere. Multi-sensor observations allows us to characterise these objects and inform the size frequency distribution of near Earth objects\, underlying planetary defence efforts. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-ellie-sansom-icrar-curtin/
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-29052024.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240605T150000
DTEND;TZID=Australia/Sydney:20240605T160000
DTSTAMP:20260524T223352
CREATED:20250819T053804Z
LAST-MODIFIED:20250819T053822Z
UID:14868-1717599600-1717603200@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Evgeni Grishin (Monash)
DESCRIPTION:Stellar Death and Compact Object mergers in Galactic nuclei\n\nAbstract\n\nThe dynamical and hydrodynamical evolution of stars and stellar remnants is greatly affected by the dense galactic nuclei (GN) environment. We explore the complex interplay of several physical processes that shape the properties\, rates and environments of nuclear transients and black hole (BH) mergers and gravitational-wave (GW) events: i) We show how stellar dynamics shape the rate and properties of stellar BH and NS dynamical evolution and mergers ii) For active galactic nuclei (AGN)\, we study how the presence of an accretion disc modifies the light curves of exploding supernovae and their relation to other nuclear transients. iii) We examine the gravitational torques in AGN discs that drive BH’s radial migration. We find that thermal diffusion greatly alters the existence and nature of migration traps in AGN discs\, which are believed to be responsible for massive hierarchical GW mergers. We find that GW mergers predominantly occur in low-luminosity AGNs. We use detailed recoil kicks and AGN models to study the efficiency of BH mergers for different generations. iv) If time permits\, we show how exotic axion dark-matter theories could be constrained via pulsar timing of pulsar binaries in galactic cores. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-evgeni-grishin/
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-05062024.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240612T150000
DTEND;TZID=Australia/Sydney:20240612T160000
DTSTAMP:20260524T223352
CREATED:20250819T053726Z
LAST-MODIFIED:20250819T053727Z
UID:14869-1718204400-1718208000@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Susmita Sett (Curtin)
DESCRIPTION:Imaging pulsar census of the Galactic Plane using MWA VCS data\n\nAbstract\n\nPulsars play a crucial role in exploring a wide range of physics and astrophysics\, such as probing dense-matter physics and testing strong-field gravity. Traditional pulsar surveys have mostly used time-domain periodicity searches\, but these methods can be hindered by scattering\, eclipses\, and orbital motion\, especially at low radio frequencies (<300 MHz). In contrast\, image domain searches for pulsars are more effective against these effects\, enabling new discoveries in the parameter space unreachable by traditional methods. To exploit the capability of image-based pulsar searches\, a pipeline has been developed to form 1-second full Stokes images from high-time-resolution data (Voltage Capture System\, VCS) from the Murchison Widefield Array (MWA). This led to the exploration of image-based techniques for identifying new pulsar candidates. In this talk\, I will describe a low-frequency image-based pulsar census of the Galactic Plane (GP) with the MWA focused on detecting the known pulsars in the observed region of the sky using both image-based and beamformed methods. This effort led to our detection of known pulsars\, with some being detected for the first time at low-frequency (150 MHz). The continuum flux densities of the pulsars detected in our image-based GP survey are significantly more reliable than the timing flux densities and therefore offer an additional benefit as flux densities are not readily available or are unreliable for many known pulsars at low frequencies. Therefore\, imaging is an effective approach for discovering new pulsars in less-explored regions of the DM space and improving the spectral modelling of the known detected pulsars. Upcoming facilities like SKA-Low will enhance the success of such image-based pulsar searches and aid in identifying new pulsar candidates. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-susmita-sett-curtin/
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-12062024.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240626T150000
DTEND;TZID=Australia/Sydney:20240626T160000
DTSTAMP:20260524T223352
CREATED:20250819T053632Z
LAST-MODIFIED:20250819T053633Z
UID:14870-1719414000-1719417600@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Benjamin Roberts (University of Queensland)
DESCRIPTION:A brief history of time(keeping): atomic clocks at the precision frontier of fundamental physics\n\nAbstract\n\nAtomic clocks are the most precise instrucments ever constructed. The best atomic clocks today have a precision that corresponds to losing no more than a second over the lifetime of the universe. In this talk\, I’ll discuss the role of atomic clocks at the forefront of fundamental physics\, with a particular focus on dark matter\, and how precision atomic physics allows us to extend the search for dark matter (and other exotic physics) to lower and lower masses. (Image credit: N. Hanacek\, NIST) \nWatch recording\nEvent details\nDownload iCal\nCategory\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-benjamin-roberts-university-of-queensland/
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-26062024-scaled.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240703T150000
DTEND;TZID=Australia/Sydney:20240703T160000
DTSTAMP:20260524T223352
CREATED:20250819T053558Z
LAST-MODIFIED:20250819T053558Z
UID:14871-1720018800-1720022400@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Monserrat Martinez (Swinburne)
DESCRIPTION:The role of AGN in regulating galaxy evolution in massive z~3-4 galaxies\n\nAbstract\n\nAn excess of massive quiescent galaxies (MQGs) is found at the early universe (z~3-4). MQGs at this epoch suggest their stellar content was already in place in the first 1.5 Gyr of the Universe. These findings indicate that MQGs must have experienced an event that caused rapid quenching. Although observational evidence is scarce\, AGNs are the most suitable candidate for quenching these galaxies. In this talk\, we present a sample of massive galaxies (10 < log(𝑀★/𝑀⊙ ) < 11) at 3 < z < 4 from JWST NIRSpec and the ZFOURGE survey with K–band spectra of the Keck/MOSFIRE\, VLT/KMOS. We find that a large fraction have strong [OIII]5007 and H𝛽 emission lines with large line widths (𝜎 100 – 450 km/s). These results show a significantly high AGN fraction in massive galaxies\, ranging from 60–70%\, pointing to the period between 3 < z < 4 being a time of heightened activity for the development of supermassive black holes in the massive end of the galaxy population and provide evidence for their role in the emergence of the first massive quenched galaxies at this epoch. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-monserrat-martinez-swinburne/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240710T150000
DTEND;TZID=Australia/Sydney:20240710T160000
DTSTAMP:20260524T223352
CREATED:20250819T053450Z
LAST-MODIFIED:20250819T053450Z
UID:14872-1720623600-1720627200@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Patricia Forster
DESCRIPTION:Western Australia Aboriginal Astronomy\n\nAbstract\n\nTraditionally\, Aboriginal people used objects in the sky to establish direction\, guide navigation\, predict seasons and as calendars for planning social life. Their narratives linked objects in the sky to life and landforms on earth and frequently included a moral element. This talk will draw on less publicized aspects of WA Aboriginal Astronomy from my review of the topic published by Cambridge University Press for the Astronomical Society of Australia. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-patricia-forster/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240717T150000
DTEND;TZID=Australia/Sydney:20240717T160000
DTSTAMP:20260524T223352
CREATED:20250819T053315Z
LAST-MODIFIED:20250819T053315Z
UID:14873-1721228400-1721232000@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Apurba Bera (ICRAR/Curtin)
DESCRIPTION:The curious case of twin fast radio bursts detected in the ASKAP-CRAFT survey\n\nAbstract\n\nFast radio bursts (FRBs) are brilliant short-duration flashes of radio emission originating at cosmological distances. Vast diversity in the properties of currently known FRBs\, complex spectro-temporal structures and the fleeting nature of these events make it difficult to understand their progenitors and emission mechanism. The Commensal Real-time ASKAP Fast Transients (CRAFT) survey\, with the Australian Square Kilometre Array Pathfinder (ASKAP) radio telescope\, enables high time resolution spectro-polarimetric study of FRBs that helps us probe the physics of the emission source and its surrounding medium. In the currently available CRAFT FRB sample we identified two apparently unrelated FRBs that show remarkable resemblance in pulse shape\, rest-frame emission time-scales and polarization properties — which indicates that these two events are likely to have very similar progenitors. In this talk I will describe the observed properties of these two FRBs and discuss their possible interpretations. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-apurba-bera-icrar-curtin/
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-17072024.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240731T150000
DTEND;TZID=Australia/Sydney:20240731T160000
DTSTAMP:20260524T223352
CREATED:20250819T053237Z
LAST-MODIFIED:20250819T053238Z
UID:14874-1722438000-1722441600@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Hao Ding (NAOJ)
DESCRIPTION:Enhancing the studies of reference frame ties and millisecond pulsar formation channels with LBA astrometry of millisecond pulsars\n\nAbstract\n\nMillisecond pulsars (MSPs) are the fastest-spinning neutron stars. Thanks to their superbtime-keeping ability\, MSPs have provided sharp tests of gravitational theories\, and have been collectively used to constrain the stochastic gravitational-wave background (GWB). Precise astrometric studies of MSPs are desired in many ways. In this talk\, I will mainly focus on two scientific prospects promised by MSP astrometry. Firstly\, as I will explain in the talk\, the velocity distribution of MSPs is likely multi-modal. VLBI astrometry of MSPs holds the key to constraining the MSP velocity distribution\, which is directly linked to the formation channels of MSPs. Secondly\, VLBI and timing observations of MSPs can jointly refine the connection between the kinematic and dynamic reference frames\, which would betterquantify the systematics in pulsar timing array studies. As the major VLBI network in the southern hemisphere\, the Australian Long Baseline Array is crucial for significantly enriching the astrometrically studied MSP sample. I will introduce a new LBA program focusing on MSP astrometry\, and update its progress. Alongside the scientific discussions\, I will describe the main challenges the two studies are facing\, and outline some innovations in data reduction and analysis that may help us overcome the challenges. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-hao-ding-naoj/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240802T150000
DTEND;TZID=Australia/Sydney:20240802T160000
DTSTAMP:20260524T223352
CREATED:20250819T053148Z
LAST-MODIFIED:20250819T053149Z
UID:14875-1722610800-1722614400@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Tasso Tzioumis (CSIRO)
DESCRIPTION:34 years with CSIRO\n\nAbstract\n\nOn the occasion of his retirement from CSIRO\, Tasso Tzioumis will look back over his 34 year career in the Australia Telescope National Facility. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-tasso-tzioumis-csiro/
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-02082024-scaled.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240807T150000
DTEND;TZID=Australia/Sydney:20240807T160000
DTSTAMP:20260524T223352
CREATED:20250819T053112Z
LAST-MODIFIED:20250819T053112Z
UID:14876-1723042800-1723046400@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Laura Driessen (University of Sydney)
DESCRIPTION:The Sydney Radio Star Catalogue: a new catalogue of radio stars\n\nAbstract\n\nI will present a new catalogue of 839 radio stars detected < 3 GHz: the Sydney Radio Star Catalogue (SRSC). Most of these stars were identified using ASKAP. The ASKAP stars in the SRSC were found using a range of techniques: circular polarisation searches\, proper-motion searches\, variability searches and multiwavelength cross-matching. We have also included published radio stars from e.g. MeerKAT and V-LoTSS in the SRSC. The catalogue contains stars from across the Hertzsprung-Russell diagram\, from ultra-cool dwarfs to blue supergiants to Wolf Rayets. The previous best-known radio star catalogue\, the Wendker catalogue\, contained 228 radio stars detected < 3GHz. Hence the SRSC is a big leap forward in our understanding of the population and characteristics of radio stars. I will present an overview of the SRSC catalogue\, including the search methods\, the properties and types of stars\, the X-ray-radio characteristics using eROSITA_DE observations\, and the circular polarisation properties. I will also highlight some individual objects of particular interest. I will also present a short summary of ASKAP VAST\, with some recent updates. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-laura-driessen-university-of-sydney/
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-07082024.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240814T150000
DTEND;TZID=Australia/Sydney:20240814T160000
DTSTAMP:20260524T223352
CREATED:20250819T053020Z
LAST-MODIFIED:20250819T053020Z
UID:14877-1723647600-1723651200@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Orsola De Marco (AAL)
DESCRIPTION:AAL member update to CSIRO Space & Astronomy\n\nAbstract\n\nAAL is a not-for-profit organisation\, whose members are Australian universities and institutions with a significant astronomical research capability. CSIRO Space & Astronomy is one of our member institutions and we are so pleased to be delivering our member update to you all in person once more this year. During our presentation\, we will provide a quick introduction on who we are\, where our funding money comes from and where it goes. We will discuss some of our key projects\, the bid for full membership of ESO and AAL’s strategy moving forward over the next 12 to 24 months. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-orsola-de-marco-aal/
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-14082024.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240821T150000
DTEND;TZID=Australia/Sydney:20240821T160000
DTSTAMP:20260524T223352
CREATED:20250819T052823Z
LAST-MODIFIED:20250819T052823Z
UID:14878-1724252400-1724256000@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Pascal Keller (Leiden Observatory)
DESCRIPTION:Investigating the Epoch of Reionisation with Radio Interferometers\n\nAbstract\n\nThe Epoch of Reionisation (EoR) marks the cosmic period during which the neutral hydrogen that pervaded the Universe transitioned to an almost entirely ionised state. The most promising probe of the EoR is the redshifted 21 cm line\, which has the potential to characterise the 3-dimensional distribution of neutral hydrogen. The statistical detection of its spatial fluctuations is a prime objective of modern low-frequency radio interferometers\, though instrumental systematics and calibration errors pose an immense challenge. In this talk\, I will discuss a calibration-independent method of detecting the cosmological signal fluctuations using the interferometric closure phase. I discuss recent developments in the interpretation of the closure phase delay power spectrum and present constraints on it obtained from a full season of HERA observations. \n\n Additionally\, I present the results of a VLA L-Band survey of 138 optically confirmed reionisation-era quasars. The survey aimed at finding quasars suitable for measuring the cosmological 21 cm signal in absorption to their bright radio emissions. The survey was further used to constrain the statistical properties of the high-redshift quasar population and their cosmic evolution. \n\n Together\, these efforts extend the required groundwork for detecting the cosmological 21 cm signal from the EoR. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-pascal-keller-leiden-observatory/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240828T150000
DTEND;TZID=Australia/Sydney:20240828T160000
DTSTAMP:20260524T223352
CREATED:20250819T052729Z
LAST-MODIFIED:20250819T052730Z
UID:14879-1724857200-1724860800@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Oliver Oayda (University of Sydney)
DESCRIPTION:Probing the Cosmic Dipole in the Radio Sky using ASKAP for Cosmology\n\nAbstract\n\nThe dipole of the Cosmic Microwave Background (“CMB”) is conventionally understood to be due to our heliocentric motion through the Universe at a speed of about 370 km/s. It is therefore called the kinematic dipole. If this interpretation is correct\, this motion should impact other observables\, for example large-scale radio galaxy surveys surveyed up to some limiting flux density. Our motion is anticipated to induce a variation in galaxy source density described by a dipole — the “cosmic dipole”. Analysing the consistency between this dipole and the kinematic dipole functions as a test of the cosmological principle\, which is the assumption that our Universe is homogeneous and isotropic on large scales. We present a Bayesian analysis of two radio galaxy surveys — RACS-low and NVSS — and find that\, even after accounting for local sources\, the dipole points roughly in the same direction as the kinematic dipole but has an amplitude 2 to 3 times larger than anticipated. This accords with other studies in the literature and represents an ongoing challenge to the kinematic interpretation of the CMB\, and therefore the cosmological principle. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-oliver-oayda-university-of-sydney/
CATEGORIES:Colloquia
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DTSTART;TZID=Australia/Sydney:20240918T150000
DTEND;TZID=Australia/Sydney:20240918T160000
DTSTAMP:20260524T223352
CREATED:20250819T052601Z
LAST-MODIFIED:20250819T052602Z
UID:14880-1726671600-1726675200@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Dongjin Kim (CSIRO)
DESCRIPTION:Radio Jet and Obscuring Torus of Active Galactic Nuclei Revealed by VLBI\n\nAbstract\n\nActive Galactic Nuclei (AGNs) are believed to play a significant role in the formation and evolution of galaxies through their energetic jet outflows. However\, observational constraints are still limited when it comes to understanding how radio jets are triggered and how jet feedback operates in different types of AGNs. To gain insights into these processes\, it is crucial to study both the continuum radio jet and the circumnuclear gas in AGNs. This presentation will review high-angular-resolution VLBI studies on AGN radio jets and their immediate surroundings. Specifically\, I will emphasize spectroscopic studies of AGNs using molecular absorption and highlight promising scientific opportunities that can be achieved with current and future mm/sub-mm VLBI arrays. These studies provide valuable insights into the nuclear environments of AGNs\, offering a better understanding of the triggering and feedback mechanisms driving radio jet outflows. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColearnia
URL:https://www.atnf.csiro.au/event/sa-colloquium-dongjin-kim-csiro/
CATEGORIES:Colloquia
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