BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//Australia Telescope National Facility - ECPv6.16.2//NONSGML v1.0//EN
CALSCALE:GREGORIAN
METHOD:PUBLISH
X-WR-CALNAME:Australia Telescope National Facility
X-ORIGINAL-URL:https://www.atnf.csiro.au
X-WR-CALDESC:Events for Australia Telescope National Facility
REFRESH-INTERVAL;VALUE=DURATION:PT1H
X-Robots-Tag:noindex
X-PUBLISHED-TTL:PT1H
BEGIN:VTIMEZONE
TZID:Australia/Sydney
BEGIN:STANDARD
TZOFFSETFROM:+1100
TZOFFSETTO:+1000
TZNAME:AEST
DTSTART:20250405T160000
END:STANDARD
BEGIN:DAYLIGHT
TZOFFSETFROM:+1000
TZOFFSETTO:+1100
TZNAME:AEDT
DTSTART:20251004T160000
END:DAYLIGHT
BEGIN:STANDARD
TZOFFSETFROM:+1100
TZOFFSETTO:+1000
TZNAME:AEST
DTSTART:20260404T160000
END:STANDARD
BEGIN:DAYLIGHT
TZOFFSETFROM:+1000
TZOFFSETTO:+1100
TZNAME:AEDT
DTSTART:20261003T160000
END:DAYLIGHT
BEGIN:STANDARD
TZOFFSETFROM:+1100
TZOFFSETTO:+1000
TZNAME:AEST
DTSTART:20270403T160000
END:STANDARD
BEGIN:DAYLIGHT
TZOFFSETFROM:+1000
TZOFFSETTO:+1100
TZNAME:AEDT
DTSTART:20271002T160000
END:DAYLIGHT
END:VTIMEZONE
BEGIN:VTIMEZONE
TZID:Australia/Perth
BEGIN:STANDARD
TZOFFSETFROM:+0800
TZOFFSETTO:+0800
TZNAME:AWST
DTSTART:20250101T000000
END:STANDARD
END:VTIMEZONE
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20260305T120000
DTEND;TZID=Australia/Sydney:20260305T123000
DTSTAMP:20260515T094149
CREATED:20260303T012603Z
LAST-MODIFIED:20260303T012603Z
UID:17865-1772712000-1772713800@www.atnf.csiro.au
SUMMARY:Colearnium: Phil Edwards (CSIRO)
DESCRIPTION:What was the ATCA built for (and what has it actually done)?\n\nThis week Phil Edwards will tell us “What was the ATCA built for (and what has it actually done)?“. \n\n \n\n \n\n\n\nPlease let me know if you’re willing to present at a future co-learnium or have requests for specific talks\, thanks! \n\nKind regards\, \n\nStefan Duchesne \n\nTeams meeting link below: \nTeams Meeting\nOrganiser\n\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/colearnium-phil-edwards-csiro-2/
LOCATION:NSW
CATEGORIES:Colearnia
ORGANIZER;CN="Stefan Duchesne":MAILTO:Stefan.Duchesne@csiro.au
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20260312T120000
DTEND;TZID=Australia/Sydney:20260312T130000
DTSTAMP:20260515T094149
CREATED:20260306T042802Z
LAST-MODIFIED:20260306T042802Z
UID:17980-1773316800-1773320400@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Eric Burt (NASA/JPL\, 2025 IEEE Distinguished Lecturer on Frequency Control)
DESCRIPTION:Frequency Standard Contributions to Limitations on the Signal-to-Noise Ratio of Very Long Baseline Interferometry Observations\n\nAbstract: \n\nSince its observation in 2019\, the first image of a super-massive black hole using Very Long Baseline Interferometry (VLBI) between a network of Earth-based radio telescopes has generated much scientific and public interest\, including the possible extension to include one or more space-based radio antennas in order to obtain higher image resolution.  The VLBI technique assumes that each radio telescope has its own frequency standard or “clock\,” and a key requirement for that frequency standard is that it have sufficient stability and precision to enable the phase-coherent combination of signals from the independent radio telescopes.  For ground-based radio telescopes\, the state-of-practice is to have a hydrogen maser co-located.  The number of frequency standards that are both space-qualified and perform well enough for this type of VLBI is a small subset of those available on the ground.  Among these\, it will be necessary to determine what type of frequency standard performance is really required.  In addition\, given the high cost of launching instruments into space\, it may be necessary to make difficult trade-offs between instrument size\, and performance.  To facilitate this trade space\, we derive a metric that directly links frequency standard noise characteristics to the signal-to-noise (S/N) ratio as a function of averaging time for the central VLBI observable\, known as the “visibility.”  Using this metric\, we find that among the existing space clock candidates\, only an Ultra-Stable Oscillator (USO) and space hydrogen maser are potentially viable.  Furthermore\, a USO will only be effective for relatively short integration times for the high observational frequencies required\, which are typically of order 100 GHz or higher.  While a hydrogen maser can extend the averaging time\, it is likely to have prohibitive size and cost for a space VLBI node.  We also investigate emerging frequency standards\, including optical clocks\, and find that the best option may be the optical local oscillator used in an optical clock by itself without the atomic reference.  This approach can greatly reduce size and complexity of the frequency standard by eliminating the atomic reference while providing a limit on VLBI visibility S/N significantly higher than what is possible with a hydrogen maser. \n\nPlease note that the event timezone is AEDT (UTC+11 hrs)\, and it will be held at Payne Scott room instead of the lecture theatre. \nJoin Event on Microsoft Teams\nLocation\n\nOrganiser\n\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-eric-burt-nasa-jpl-2025-ieee-distinguished-lecturer-on-frequency-control/
LOCATION:Marsfield Lecture Theatre\, 26 Pembroke Road\, Marsfield\, NSW\, 2122\, Australia
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/png:https://www.atnf.csiro.au/wp-content/uploads/2026/03/2025RS008476_fig_12-scaled.png
ORGANIZER;CN="Jishnu Thekkeppattu":MAILTO:Jishnunambissan.Thekkeppattu@csiro.au
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Perth:20260319T090000
DTEND;TZID=Australia/Perth:20260319T170000
DTSTAMP:20260515T094149
CREATED:20260129T061520Z
LAST-MODIFIED:20260204T030836Z
UID:16729-1773910800-1773939600@www.atnf.csiro.au
SUMMARY:ATUC Open Day
DESCRIPTION:Overview\n\nThe ATUC Open Day on 19 March 2026 will be held in the Auditorium at Kensington. Remote attendance will be made available via Teams. All are welcome to attend. \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\, you can do so via the ATUC Community Submission Form or by contacting any member of ATUC. \n\nTo participate in the ATUC Open Session\, please register in advance using the button below. The registration deadline is 17:00 AWST on 5 March 2026. \nRegister\nLocation\n\nOrganiser\n\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/atuc-meeting-19-and-20-march/
LOCATION:Kensington Auditorium\, 26 Dick Perry Avenue\, Kensington\, Western Australia\, 6151\, Australia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2026/01/ACherney_2250-scaled.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20260325T120000
DTEND;TZID=Australia/Sydney:20260325T130000
DTSTAMP:20260515T094149
CREATED:20260319T101801Z
LAST-MODIFIED:20260319T102254Z
UID:18378-1774440000-1774443600@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Luca Ighina (Harvard Center for Astrophysics)
DESCRIPTION:A New Radio Window on the Growth of the First Supermassive Black Holes\n\nAbstract: \n\nFrom reionizing the Universe to quenching star formation in massive galaxies\, accreting supermassive black holes (SMBHs)\, or active galactic nuclei (AGN)\, are thought to play a pivotal role in early galaxy evolution. Growing observational evidence\, including recent results from JWST\, suggests that accreting black holes are both more abundant and more massive at than predicted by current theoretical models. In this talk I will present recent observational results on accreting black holes in the early Universe\, with a particular focus on radio-powerful AGN. I will show how relativistic jets can play an important role in both the rapid assembly of very massive black holes and the regulation of star formation in their host galaxies in the early Universe.  \n\nWhile exciting\, current studies focus on optically luminous AGN\, which likely represent only the tip of the iceberg of the SMBH population at early cosmic times. Heavily obscured AGN\, whose accretion signatures are hidden at optical and near-infrared wavelengths\, are predicted to dominate the high-z AGN population\, yet these sources remain largely unconstrained from an observational point of view. The synergy between next-generation radio and near-infrared wide-area surveys will soon open a new window on this elusive population. In particular\, radio observations can reveal the presence of relativistic jets\, and therefore ongoing black hole accretion\, even in systems that are obscured at optical wavelengths. The combination of ASKAP/EMU and EUCLID-wide surveys will provide the deepest multi-wavelength view of the extra-Galactic southern sky\, enabling the construction of the first large\, unbiased census of accreting black holes at z>6. As an example of the power of this synergy\, I will present a preliminary cross-match of EMU and Euclid over the EUCLID deep field South (∼25 deg2). \n\nPlease note that the event timezone is AWST (UTC+8 hrs) \n\n \n\nLocation\n\nOrganiser\n\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-luca-ighina-harvard-center-for-astrophysics/
LOCATION:CSIRO – Kensington\, Australian Resources Research Centre (ARRC)\, 26 Dick Perry Ave\, Kensington\, WA\, 6101\, Australia
CATEGORIES:Colloquia
ORGANIZER;CN="Gemma Anderson":MAILTO:gemma.anderson@csiro.au
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20260326T120000
DTEND;TZID=Australia/Sydney:20260326T130000
DTSTAMP:20260515T094149
CREATED:20260325T234550Z
LAST-MODIFIED:20260325T234550Z
UID:18546-1774526400-1774530000@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Matt Miles (Vanderbilt University)
DESCRIPTION:All Models Are Wrong: Noise Modelling in Pulsar Timing\n\nAbstract: \n\nPulsar timing arrays are only as good as the timing residuals they produce — and those residuals are only as clean as the method used to extract them. Traditional template-matching approaches measure pulse time-of-arrival (TOA) by fitting a single fixed or radio-frequency dependent template to observed profiles\, but this leaves a critical vulnerability: any stochastic variation in pulse shape is silently absorbed into the TOA as a systematic bias\, quietly corrupting the signals we are trying to extract. \n\nSCULPT is a new technique built of old ideas that fixes this at its source. By constructing a basis directly from observed profiles via SVD\, SCULPT learns the true structure of pulse shape variability from the data itself — no analytic assumptions\, no oracle knowledge required. Stochastic shape changes are absorbed into nuisance amplitude coefficients within this basis\, keeping them out of the timing solution. The result is a variational profile basis that is optimally adapted to the actual pulse morphology: expressive where it needs to be\, simple everywhere else. \n\nI will present the methodology behind this process and explore with the audience what it is we’re trying to achieve and why it’s an important goal. \n\nPlease note that the event timezone is AEDT (UTC+11 hrs) and will be held in the Faraday room \nJoin Event on Microsoft Teams\nLocation\n\nOrganiser\n\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-matt-miles-vanderbilt-university/
LOCATION:Marsfield Lecture Theatre\, 26 Pembroke Road\, Marsfield\, NSW\, 2122\, Australia
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/png:https://www.atnf.csiro.au/wp-content/uploads/2026/03/SCULPTGraphic_ManimCE_v0.20.1.png
ORGANIZER;CN="Jishnu Thekkeppattu":MAILTO:Jishnunambissan.Thekkeppattu@csiro.au
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20260331T150000
DTEND;TZID=Australia/Sydney:20260331T160000
DTSTAMP:20260515T094149
CREATED:20260325T234343Z
LAST-MODIFIED:20260325T234343Z
UID:18544-1774969200-1774972800@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Valentina Di Marco (University of Melbourne)
DESCRIPTION:All Models Are Wrong: Noise Modelling in Pulsar Timing\n\nAbstract: \n\nPulsar timing arrays\, like any experiment\, depend on accurate noise modelling to detect nanohertz gravitational waves. But the noise itself is much more complex than in some other experiments. It is multi-component and\, due to the astrophysical origin of several noise processes\, often uncertain and difficult to model accurately. In this talk\, I explore what happens when our noise models are wrong. \n\nI show that misspecified noise can bias gravitational-wave inference and distort spectral estimates. While these effects are sometimes conservative\, they can also lead to systematically incorrect conclusions\, highlighting the need to account for model uncertainty properly. \n\nI then present a transdimensional Bayesian approach for noise analysis that lets the data decide which noise processes are present in the signal. By jointly performing model selection and parameter estimation\, this framework provides a more robust and statistically consistent way to analyse pulsar timing data. \n\nPlease note that the event timezone is AEDT (UTC+11 hrs) \nJoin Event on Microsoft Teams\nLocation\n\nOrganiser\n\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-valentina-di-marco-university-of-melbourne/
LOCATION:Marsfield Lecture Theatre\, 26 Pembroke Road\, Marsfield\, NSW\, 2122\, Australia
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/png:https://www.atnf.csiro.au/wp-content/uploads/2026/03/Valentina_DiMarco.png
ORGANIZER;CN="Jishnu Thekkeppattu":MAILTO:Jishnunambissan.Thekkeppattu@csiro.au
END:VEVENT
END:VCALENDAR