BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//Australia Telescope National Facility - ECPv6.16.2//NONSGML v1.0//EN
CALSCALE:GREGORIAN
METHOD:PUBLISH
X-WR-CALNAME:Australia Telescope National Facility
X-ORIGINAL-URL:https://www.atnf.csiro.au
X-WR-CALDESC:Events for Australia Telescope National Facility
REFRESH-INTERVAL;VALUE=DURATION:PT1H
X-Robots-Tag:noindex
X-PUBLISHED-TTL:PT1H
BEGIN:VTIMEZONE
TZID:Australia/Sydney
BEGIN:STANDARD
TZOFFSETFROM:+1100
TZOFFSETTO:+1000
TZNAME:AEST
DTSTART:20220402T160000
END:STANDARD
BEGIN:DAYLIGHT
TZOFFSETFROM:+1000
TZOFFSETTO:+1100
TZNAME:AEDT
DTSTART:20221001T160000
END:DAYLIGHT
BEGIN:STANDARD
TZOFFSETFROM:+1100
TZOFFSETTO:+1000
TZNAME:AEST
DTSTART:20230401T160000
END:STANDARD
BEGIN:DAYLIGHT
TZOFFSETFROM:+1000
TZOFFSETTO:+1100
TZNAME:AEDT
DTSTART:20230930T160000
END:DAYLIGHT
BEGIN:STANDARD
TZOFFSETFROM:+1100
TZOFFSETTO:+1000
TZNAME:AEST
DTSTART:20240406T160000
END:STANDARD
BEGIN:DAYLIGHT
TZOFFSETFROM:+1000
TZOFFSETTO:+1100
TZNAME:AEDT
DTSTART:20241005T160000
END:DAYLIGHT
END:VTIMEZONE
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230608T150000
DTEND;TZID=Australia/Sydney:20230608T160000
DTSTAMP:20260515T155503
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/
LOCATION:NSW
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/png:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-08062023.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230621T150000
DTEND;TZID=Australia/Sydney:20230621T160000
DTSTAMP:20260515T155503
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/
LOCATION:NSW
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-21062023.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20230628T150000
DTEND;TZID=Australia/Sydney:20230628T160000
DTSTAMP:20260515T155503
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/
LOCATION:NSW
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/png:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-28062023.png
END:VEVENT
END:VCALENDAR