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DTSTART:20220402T160000
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BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20231206T150000
DTEND;TZID=Australia/Sydney:20231206T160000
DTSTAMP:20260522T130126
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/
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:20231129T150000
DTEND;TZID=Australia/Sydney:20231129T160000
DTSTAMP:20260522T130126
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/
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:20231122T150000
DTEND;TZID=Australia/Sydney:20231122T160000
DTSTAMP:20260522T130126
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/
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:20231115T150000
DTEND;TZID=Australia/Sydney:20231115T160000
DTSTAMP:20260522T130126
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/
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:20231108T150000
DTEND;TZID=Australia/Sydney:20231108T160000
DTSTAMP:20260522T130126
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/
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:20231101T150000
DTEND;TZID=Australia/Sydney:20231101T160000
DTSTAMP:20260522T130126
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/
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:20231025T150000
DTEND;TZID=Australia/Sydney:20231025T160000
DTSTAMP:20260522T130126
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/
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:20230927T150000
DTEND;TZID=Australia/Sydney:20230927T160000
DTSTAMP:20260522T130126
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/
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:20230920T150000
DTEND;TZID=Australia/Sydney:20230920T160000
DTSTAMP:20260522T130126
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/
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:20230913T150000
DTEND;TZID=Australia/Sydney:20230913T160000
DTSTAMP:20260522T130126
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/
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:20230906T150000
DTEND;TZID=Australia/Sydney:20230906T160000
DTSTAMP:20260522T130126
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/
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:20230830T150000
DTEND;TZID=Australia/Sydney:20230830T160000
DTSTAMP:20260522T130126
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/
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:20230823T150000
DTEND;TZID=Australia/Sydney:20230823T160000
DTSTAMP:20260522T130126
CREATED:20250819T072036Z
LAST-MODIFIED:20250819T072036Z
UID:14941-1692802800-1692806400@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Jennifer West (NSCC)
DESCRIPTION:Progress on understanding the Galactic magnetic field\n\nAbstract\n\nThe pursuit of understanding the structure and origin of the Milky Way’s magnetic field is a central science question driving several radio polarization surveys\, including the Polarization Sky Survey of the Universe’s Magnetism (POSSUM) and The Global Magneto-Ionic Medium Survey (GMIMS). I will give a brief overview of the progress we have made towards unravelling the answers to these questions. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-jennifer-west-nscc/
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/png:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-23082023.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230816T150000
DTEND;TZID=Australia/Sydney:20230816T160000
DTSTAMP:20260522T130126
CREATED:20250819T072130Z
LAST-MODIFIED:20250819T072131Z
UID:14940-1692198000-1692201600@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Virginia Kilborn (Swinburne)
DESCRIPTION:HI surveys from next generation radio telescopes\n\nAbstract\n\nHydrogen is the most common element in the Universe. Powering star formation\, it plays a crucial role in the formation and evolution of galaxies. Observations of Neutral Hydrogen (HI) in the radio wavelength allow us to survey for galaxies in the nearby universe\, and next generation surveys from telescopes such as the Australian Square Kilometre Array Pathfinder (ASKAP)\, meerKAT and FAST are expected to provide redshifts\, kinematics and gas content of around hundreds of thousands of galaxies\, and probe the gaseous environment surrounding – and inbetween – galaxies. In this talk I’ll provide an overview of HI science\, what we’ve learnt to date\, and touch on some of the potential future results of these new telescopes. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-virginia-kilborn-swinburne/
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-16082023.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230809T150000
DTEND;TZID=Australia/Sydney:20230809T160000
DTSTAMP:20260522T130126
CREATED:20250819T072202Z
LAST-MODIFIED:20250819T072203Z
UID:14939-1691593200-1691596800@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Barnali Das (CSIRO)
DESCRIPTION:Coherent radio emission from hot magnetic stars\n\nAbstract\n\nHot magnetic stars are the perfect laboratories for understanding stellar magnetospheric phenomena due to the fact that their fields are extremely stable throughout their lifetimes\, and also have very simple topologies (dipolar in most cases). Their strong stellar winds interact with the magnetic fields giving rise to co-rotating magnetospheres extending up to several tens of stellar radii. The magnetosphere manifests itself via emission over a wide range of the electromagnetic spectrum\, starting from radio to X-ray. These emissions convey different kinds of information\, and together\, they act as probes for wind-magnetic field interplay. Among the different emissions that these magnetospheres produce\, the latest discovered\, and consequently\, the least understood one is the coherent radio emission\, also referred to as auroral radio emission. This is produced by electron cyclotron maser emission (ECME\, the same mechanism that drives auroral radio emission from magnetic ultracool dwarfs and planets). In my talk\, I will take you on our journey towards demystifying this phenomenon\, starting with some serendipitous discoveries\, followed by a systematic sub-GHz survey\, which ironically led to the discoveries of many more unexplained characteristics\, including discovery of radio flares\, in addition to providing solutions to existing problems. I will present the results that we have obtained so far regarding ECME incidence\, wideband properties and stability\, and potential scenarios to explain the observations. I will end with my future plan to obtain more definitive insights about magnetospheric operation and the role that ATNF instruments can play in achieving that goal. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-barnali-das-csiro/
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-09082023.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230802T150000
DTEND;TZID=Australia/Sydney:20230802T160000
DTSTAMP:20260522T130126
CREATED:20250819T072235Z
LAST-MODIFIED:20250819T072235Z
UID:14938-1690988400-1690992000@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Shriharsh Tendulkar (NCRA\, India)
DESCRIPTION:Multi-scale and multi-wavelength searches for FRBs (and other wavelengths)\n\nAbstract\n\nFulfilling the true promise of fast radio bursts (FRBs) as cosmological probes\, understanding their origins\, and their association with other transients necessitates our understanding of the FRB emission mechanism\, their formation channel(s)\, and their local environments. Most emission mechanisms expect that the prompt radio emission represents a small fraction of the total energy released — a larger fraction of the energy should be released at higher frequency wavebands: optical\, UV\, X-ray and in some cases\, gravitational waves (GW) and neutrinos\, either as prompt emission or as a longer-lived afterglow. Given that the observed rates of FRBs are two to three orders of magnitude higher than the sky rates of any other extragalactic transient\, it is clear that most FRBs will not have detectable multi-wavelength counterparts. The X-ray bursts aligned with the FRB-like radio emission from SGR 1935+2154 highlight the need to be alert to the brightest and nearest FRBs since those will be the most likely to have detectable multi-wavelength counterparts. Theoretical expectations also highlight the need to search for radio transients not just in the millisecond timescale\, but also at second timescales\, an area of phase space that is badly ignored. In this talk\, I will discuss results from CHIME/FRB in trying to constrain counterparts of FRBs\, FRB-GRB connections\, and FRB-GW connections and our efforts to increase the phase space of radio transients by searching for not-so-fast radio bursts. For these science cases\, I will also discuss two new projects: The proposed All Sky Transient Radio Array (ASTRA)\, an ultra-wide field of view telescope to detect the brightest and nearest radio transients and Daksha\, a proposed all-sky X-ray mission with 2-satellites in antipodal orbits to increase the detection rate of GRBs and electromagnetic counterparts of GW events. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-shriharsh-tendulkar-ncra-india/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230719T150000
DTEND;TZID=Australia/Sydney:20230719T160000
DTSTAMP:20260522T130126
CREATED:20250819T072302Z
LAST-MODIFIED:20250819T072302Z
UID:14937-1689778800-1689782400@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Darren Croton (Swinburne)
DESCRIPTION:How to model the Universe in N easy steps\n\nAbstract\n\nMuch progress has been made in recent years in our understanding of the co-evolution of galaxies and supermassive black holes\, and their connection to the underlying large-scale dark matter structure. In this talk I will discuss simulation and modelling techniques that bridge theories of galaxy and black hole formation with the properties of observed galaxy populations. In addition\, I will discuss a number of open questions important for extra-galactic astronomy and cosmology\, and explain how future large-scale surveys and galaxy formation models may jointly address them. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-darren-croton-swinburne/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230712T150000
DTEND;TZID=Australia/Sydney:20230712T160000
DTSTAMP:20260522T130126
CREATED:20250819T072329Z
LAST-MODIFIED:20250819T072330Z
UID:14936-1689174000-1689177600@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Ophelie Renaud (IETR-INSA\, France)
DESCRIPTION:Designing and Programming Astronomy Computing Systems for Optimal Power Efficiency and Performance\n\nAbstract\n\nIn this presentation\, we address the challenging problem of deploying complex astronomical applications on efficient target architectures. The allocation of resources in such scenarios significantly impacts performance outcomes. To automate and expedite this process\, we propose a method that leverages the Synchronous Dataflow (SDF) model and the Scaling up of Cluster of Actor on the Processing Element (SCAPE) technique. Our approach\, implemented in the PREESM rapid prototyping tool\, facilitates automated deployment on CPU\, GPU\, and FPGA architectures. We showcase the advanced implementation of CPU-based resource allocation in our tool\, which serves as a foundation for other target architectures. By providing a fast and easy resolution to this NP-hard problem\, our method greatly enhances the efficiency of deploying astronomical applications. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-ophelie-renaud-ietr-insa-france/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230628T150000
DTEND;TZID=Australia/Sydney:20230628T160000
DTSTAMP:20260522T130126
CREATED:20250819T072429Z
LAST-MODIFIED:20250819T072430Z
UID:14935-1687964400-1687968000@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Ashley Ruiter (UNSW\, Canberra)
DESCRIPTION:Mergers of white dwarfs and the transients they make\n\nAbstract\n\nFor the last decade\, mergers of double white dwarfs have been considered to be a likely\, possibly even favoured\, progenitor scenario for Type Ia supernovae. Though the Milky Way harbours ~100 million double white dwarf binaries\, only a small fraction of these will actually merge in a Hubble time\, let alone possess the “right” physical properties to lead to a Type Ia supernova if they do even merge. A different outcome of a white dwarf merger is the creation of another type of stellar transient: a hydrogen-deficient carbon (HdC) star. We know of ~130 of such ‘dusty’ HdC stars in the Galaxy – these are the R Coronae Borealis (RCB) stars\, and they are thought to be the end result of a merger of a carbon-oxygen white dwarf and a helium-rich white dwarf\, though their formation is not completely understood. In 2021\, another type of hydrogen-deficient carbon star was found in great numbers: 27 ‘dustless’ HdC stars were spectroscopically confirmed in our own Milky Way\, increasing the known number of this class from 4 (discovered >50 yrs ago) to 31. In 2022 we were granted time on the high-resolution (R~80\,000) Veloce echelle spectrograph with the aim of disentangling the difference in evolutionary history between the long-known ‘dusty’ RCB stars and the newly-discovered plethora of ‘dustless’ HdC stars – both classes of objects presumed to be the result of double white dwarf mergers. Though we were mostly fully clouded out and we await new opportunities for obtaining and analysing observational data\, I will discuss how different formation channels of white dwarf mergers may be plausibly linked to various transient phenomena such as Type Ia supernovae\, dusty RCB stars\, and dustless HdC stars. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-ashley-ruiter-unsw-canberra/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230621T150000
DTEND;TZID=Australia/Sydney:20230621T160000
DTSTAMP:20260522T130126
CREATED:20250819T072520Z
LAST-MODIFIED:20250819T072520Z
UID:14934-1687359600-1687363200@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Jean Francois Nezan (IETR – INSA\, France)
DESCRIPTION:Dataflow models for the design and programming of computing systems in astronomy\n\nAbstract\n\nProjects in astronomy like the Square Kilometer Array (SKA) or the European Extremely Large Telescope are among the world’s largest Big Data projects and the largest international computing collaborations\, with unique computing challenges in Signal Processing and Machine Learning (SPML) still to be solved. The challenge in terms of computing\, data transport and storage capacity is to design a processing chain ranging from the acquisition of raw data from the sensors to the production and the analysis of multidimensional images of the sky with Worldwide Distributed Calculations. In that context\, a new generation of Low-Power High-Performance Computing Systems has to replace general-purpose High-Performance Computing (HPC) systems to meet the challenge of climate change\, including the reuse and upgrades of computing systems already operational in a recycling approach. State of the art Programming Models and their Development Frameworks are lagging behind in offering support for efficient use of resources\, high service availability and quality and cost competitiveness. This presentation will discuss how dataflow models associated with platform- and component-based designs can help to tame complexity during the design and the operating phases of big projects in astronomy\, assessing the performance both in time and energy of a complex scientific workflow on a not-yet-existing computing infrastructure. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-jean-francois-nezan-ietr-insa-france/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230608T150000
DTEND;TZID=Australia/Sydney:20230608T160000
DTSTAMP:20260522T130126
CREATED:20250819T072550Z
LAST-MODIFIED:20250819T072550Z
UID:14933-1686236400-1686240000@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Amit Seta (ANU)
DESCRIPTION:Rotation measure structure functions with higher-order stencils as a probe of small-scale magnetic fluctuations and its application to Magellanic Clouds\n\nAbstract\n\nMagnetic fields and turbulence are important components of the interstellar medium (ISM) of star-forming galaxies. It is challenging to measure the properties of the small-scale ISM magnetic fields (magnetic fields at scales smaller than the turbulence driving scale). Using numerical simulations\, we demonstrate how the second-order rotation measure (RM\, which depends on thermal electron density and magnetic field) structure function can probe the properties of small-scale random magnetic fields. Particularly\, we show that computing the RM structure function with a higher-order stencil (more than the commonly-used two-point stencil) is necessary to accurately estimate the slope of the structure function. We then apply our results to radio polarisation observations of the Small and Large Magellanic Clouds and determine the strength and scale of their small-scale magnetic fields. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-amit-seta-anu-2/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230524T150000
DTEND;TZID=Australia/Sydney:20230524T160000
DTSTAMP:20260522T130126
CREATED:20250819T072715Z
LAST-MODIFIED:20250819T072715Z
UID:14932-1684940400-1684944000@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Nick Lomb (University of South Queensland) & Toner Stevenson (University of Sydney)
DESCRIPTION:Eclipse Chasers: Solar eclipses in Australia\n\nAbstract\n\nIn this presentation\, we give a few extracts from our book Eclipse Chasers\, recently published by CSIRO Publishing. Toner will focus on the 1922 eclipse experiment to confirm Einstein’s general theory of relativity\, while Nick will discuss the 1974 and 1976 total solar eclipses\, highlighting the involvement of CSIRO scientists. He will also mention the various mixed government and media messages that influenced public viewing of these events. Toner will conclude the presentation by showing her spectacular images of the recent eclipse in Exmouth and will leave you anticipating the next total solar eclipse to be visible in Australia. Eclipse Chasers by Nick Lomb and Toner Stevenson\, together with expert collaborators\, is a complete guide to past and future Australian eclipses. Past total solar eclipse campaigns described include the Far North Queensland eclipse of 1871 that is significant in the history of Australian science\, the famous 1922 “Einstein” eclipse in which the previously hidden role of women and First Nations people is emphasised and the eclipses of 1974 and 1976 in which CSIRO scientists had a major role. The book also explores the great significance of solar eclipses for First Nations peoples\, and their observations and cultural meanings. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-nick-lomb-university-of-south-queensland-toner-stevenson-university-of-sydney/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230510T150000
DTEND;TZID=Australia/Sydney:20230510T160000
DTSTAMP:20260522T130126
CREATED:20250819T072940Z
LAST-MODIFIED:20250819T072940Z
UID:14931-1683730800-1683734400@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Dale E. Gary (NJIT)
DESCRIPTION:Recent Advances in Solar Radio Imaging Spectroscopy\n\nAbstract\n\nAn impressive number of new radio instruments have appeared on the scene\, or are in the planning stages\, that perform high-resolution imaging at many closely spaced frequencies over a broad frequency range. In the case of imaging of the Sun\, this has ushered in a revolution in our understanding by providing radio imaging spectroscopy\, i.e.\, spatially resolved brightness temperature spectra. Such spectra can be connected directly to basic physical parameters of the radiating particles and their environment\, leading to a breakthrough in our understanding of solar flares and bursts as well as the structure and processes of the non-flaring solar atmosphere. This talk will cover the instruments and advances fueling this revolution\, and present some of the recent results for the Sun and also (briefly) stars. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-dale-e-gary-njit/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230503T150000
DTEND;TZID=Australia/Sydney:20230503T160000
DTSTAMP:20260522T130126
CREATED:20250819T073023Z
LAST-MODIFIED:20250819T073024Z
UID:14930-1683126000-1683129600@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Travis Rector (University of Alaska)
DESCRIPTION:How astronomers can be part of the solution to climate change\n\nAbstract\n\nFrom a social\, environmental\, and political standpoint climate change is the most important scientific topic of our time. Fortunately we can still avoid the worst consequences\, but we need to take swift action. The good news is that climate change can be solved\, and astronomers are especially well suited to make a difference. Through the classes we teach and our public outreach we can\, and should\, take the opportunity to help people understand the causes and consequences of\, and solutions to\, climate change. \n\n We also need to address that astronomy as a profession is a contributor to climate change. From supercomputing\, air travel\, and operations we are responsible for an outsized carbon footprint. Astronomy is also being affected by climate change\, from the increased risk of forest fires to the stability of the atmospheric conditions at our observatories. How should astronomers change how we work in order to reduce our carbon footprint? How should we adapt to the impacts of climate change and proposed mitigation efforts? And how can we make changes that improve the equity and productivity of our profession? In my talk I will discuss the roles that astronomers can– and are– playing in addressing the climate crisis. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-travis-rector-university-of-alaska/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230426T150000
DTEND;TZID=Australia/Sydney:20230426T160000
DTSTAMP:20260522T130126
CREATED:20250819T073055Z
LAST-MODIFIED:20250819T073056Z
UID:14929-1682521200-1682524800@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Jayender Kumar (CSIRO)
DESCRIPTION:The dynamics and 3D structure of the Galactic long bar\n\nAbstract\n\nUnderstanding the 3D structure and associated dynamics of the inner 4-kpc of the Milky Way is very challenging because of high obscuration at optical wavelengths and our ability to accurately measure the distance and 3D motions of sources at these distances. \n\nIn this work\, we measured parallax and proper motions of three 22.2 GHz water masers\, each associated with a High-Mass Star-Forming Region (HMSFR) in the first quadrant of the Milky Way. With these measurements combined with other BeSSel projects’ published and un-published parallax and proper motion measurements of maser sources associated with HMSFRs within the 4 kpc region of the Galactic centre\, we present evidence that the young HMSFRs in the inner galaxy are located in the gases following ’quasi-elliptical’ orbits. These represent the first direct measurements of the dynamics of the Milky Way’s bar. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-jayender-kumar-csiro/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230419T150000
DTEND;TZID=Australia/Sydney:20230419T160000
DTSTAMP:20260522T130126
CREATED:20250819T103612Z
LAST-MODIFIED:20250819T103612Z
UID:15088-1681916400-1681920000@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Caroline Foster (UNSW)
DESCRIPTION:Challenges in understanding the dynamical evolution of galaxies\n\nAbstract\n\nIn this talk\, I will discuss the dynamical transformation of galaxies across cosmic time. I will explore common barriers to and possible solutions for the accurate measurement and determination of the dynamical evolution of galaxies. I will focus on the necessity of changing dynamical probes / baryonic phases (neutral gas\, ionised gas and stars) depending on the cosmic epoch or redshift. \n\n In the first instance\, I will discuss our attempt at quantifying and correcting for the impact of the progenitor bias with redshift using cosmological simulations. I will next address the implications of recent results on the dynamical coupling (or otherwise) of ionised gas and stars in galaxies on our ability to accurately infer dynamical evolution from observations at different epochs. Finally\, I will outline how the Middle-Ages Galaxy Properties with Integral field spectroscopy (MAGPI) Survey was designed to explicitly overcome some of these barriers and show a selection of initial results. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-caroline-foster-unsw/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230412T150000
DTEND;TZID=Australia/Sydney:20230412T160000
DTSTAMP:20260522T130126
CREATED:20250819T061431Z
LAST-MODIFIED:20250819T061432Z
UID:14889-1681311600-1681315200@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Chandra Murugesan (CSIRO)
DESCRIPTION:Resolved neutral atomic hydrogen (HI) gas studies to reveal the impact of intrinsic and environmental processes on Chandra Murugesan\n\nAbstract\n\nNeutral atomic Hydrogen (HI) gas is the fundamental reservoir from which stars in galaxies are eventually formed. As such\, studying the HI gas properties in galaxies give us important insights into how star formation proceeds. In addition\, the HI gas is affected by internal mechanisms/processes such as angular momentum (AM)\, star formation/AGN feedback\, disk instabilities\, as well as non-axisymmetric potentials such as bars. On the other hand\, the HI gas is also sensitive to (external) environmental processes such as tidal and ram-pressure stripping. Disentangling the degree of influence of these processes on the HI gas is paramount. In this talk I will show the importance of resolved HI studies in decoding the effects of both internal and external processes on galaxy evolution. By virtue of the extended nature of the HI disks in galaxies\, one can derive rotation curves out to many times their optical radii\, making high-resolution HI studies very important for tracing the total AM in galaxies. I will present the AM – Mass relation for local galaxies which is fundamental for constraining our cosmological models. In addition\, I will talk about the connection between AM\, disk stability and HI gas fraction in galaxies. Drawing from the results of a new HI survey of ring galaxies\, I will also highlight the effects of bars in redistributing the HI gas and star formation in galaxies. Finally\, I will present some new data is being delivered by the ASKAP WALLABY HI survey and the impact this is likely to have on HI and AM studies of galaxies in the local Universe as we venture into the SKA era. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-chandra-murugesan-csiro/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230331T150000
DTEND;TZID=Australia/Sydney:20230331T160000
DTSTAMP:20260522T130126
CREATED:20250819T061501Z
LAST-MODIFIED:20250819T061501Z
UID:14888-1680274800-1680278400@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Michael Kramer (MPIfR\, Bonn)
DESCRIPTION:Probing relativistic gravity with radio astronomy\n\nAbstract\n\nWe experience a golden era in testing and exploring relativistic gravity. Whether it is results from gravitational wave detectors\, satellite or lab experiments\, radio astronomy plays an important complementary role. Here one can mention the cosmic microwave background\, black hole imaging and\, obviously\, binary pulsars. This talk will provide an overview how these methods relate to each other\, and will in particular focus on new results from the study of binary pulsars\, where we can test the behaviour of strongly self-gravitating bodies with unrivalled precision. The talk will also give an outlook of what we can expect from new experiments\, such as with MeerKAT or the SKA. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-michael-kramer-mpifr-bonn-2/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230322T150000
DTEND;TZID=Australia/Sydney:20230322T160000
DTSTAMP:20260522T130126
CREATED:20250819T061527Z
LAST-MODIFIED:20250819T061527Z
UID:14887-1679497200-1679500800@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Natasha Hurley Walker (ICRAR/Curtin)
DESCRIPTION:Long-period radio transients\n\nAbstract\n\nSKA pathfinder instruments are probing the radio sky in new ways\, probing the sky on timescales hitherto poorly-explored. Sensitive image-plane surveys are discovering new kinds of radio transients\, with unusual temporal\, spectral\, and polarisation properties. Two intriguing periodic transients were published last year: a pulsar-like object repeating every 76s that is growing fainter with time (Caleb et al. 2022)\, and a short-lived radio transient repeating every 18 minutes (Hurley-Walker et al. 2022a). Both are potential examples of “ultra-long period” (ULP) magnetars\, and their radio emission might be explained by a temporary twisting and/or reorganisation of their intense magnetic fields. \n\n These discoveries are spurring new searches for similar long-period sources. Last year we conducted a transient imaging survey of the Galactic plane with the MWA at 200 MHz. We were successful in detecting a further long-period transient\, which compared to previous examples shows different pulse morphology\, polarisation behaviour\, and a staggeringly different activity window. Timing estimates place the source below the conventional “death lines” of emission mechanisms that explain radio emission in neutron stars. These sources are just the tip of the iceberg of a new population\, the exploration of which will illuminate the behaviour of neutron stars and therefore physics in extreme environments. I will conclude the talk with future survey plans across a range of telescopes. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-natasha-hurley-walker-icrar-curtin/
CATEGORIES:Colloquia
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END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230315T150000
DTEND;TZID=Australia/Sydney:20230315T160000
DTSTAMP:20260522T130126
CREATED:20250819T061554Z
LAST-MODIFIED:20250819T061555Z
UID:14886-1678892400-1678896000@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Douglas Scott (University of British Columbia)
DESCRIPTION:The Standard Cosmological Model\n\nAbstract\n\nAll empirical data relating to our Universe are currently well fit by a basic model that contains only a few key ingredients: the background is described by homogeneous and isotropic solutions within General Relativity\, in which there is domination by vacuum energy and cold dark matter in a roughly flat expanding geometry; the density fluctuations appear to be nearly scale-invariant\, adiabatic and Gaussian (close to the simplest thing we could imagine); and all of today’s structure grew through gravitational instability. Within this picture the Universe is described by just a handful of numbers\, which are now known to quite high precision. So what is left to do in cosmology? How many digits of precision do we need? Where did these values come from? Are there more numbers that we haven’t thought of yet? Is this model anything like the Standard Model of Particle Physics? Are there signs that we need “physics beyond the standard model”? Did someone say “anomalies” and “tensions”? \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-douglas-scott-university-of-british-columbia/
CATEGORIES:Colloquia
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END:VEVENT
END:VCALENDAR