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BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20221005T150000
DTEND;TZID=Australia/Sydney:20221005T160000
DTSTAMP:20260516T041944
CREATED:20250819T074007Z
LAST-MODIFIED:20250819T074007Z
UID:14964-1664982000-1664985600@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Meriem Beheri (SISSA)
DESCRIPTION:Radio Selected NIR-dark sources shedding light on the dark side of high redshift SFR\n\nAbstract\n\nAbout 12 billion years ago\, the Universe was first experiencing light again after the dark ages\, and galaxies filled the environment with stars\, metals\, and dust. How efficient was this process\, and how fast did these primordial galaxies form stars and dust? We can answer these questions by tracing galaxies star formation rate density (SFRD) back to its unexplored high redshift tail\, traditionally observed in the Near-InfraRed (NIR)\, Optical\, and UV-bands. This means that the dustiest objects were missing. Further\, most studies on dust obscured galaxies at high redshift have been conducted in the sub-millimetre\, possibly affected by dust temperature biases. In this talk\, I will introduce you to the characterisation of Radio Selected NIR-dark (RS-NIRdark) sources in different fields with a panchromatic approach and new SED-fitting techniques developed by the GOThA (Galaxy Observational and Theoretical Astrophysics) group in SISSA. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-meriem-beheri-sissa/
LOCATION:NSW
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-05102022.jpg
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BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20221012T150000
DTEND;TZID=Australia/Sydney:20221012T160000
DTSTAMP:20260516T041944
CREATED:20250819T073851Z
LAST-MODIFIED:20250819T073851Z
UID:14963-1665586800-1665590400@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Xiaojin Liu (Beijing Normal University\, China)
DESCRIPTION:A Bayesian study of the spin-up process of millisecond pulsars\n\nAbstract\n\nMillisecond pulsars (MSPs) are one of the fastest-spinning objects in the Universe. They are usually believed to attain their fast spin via an accretion process that transfers angular momentum from their companions to the neutron stars\, though the spin-up process remains mysterious and is usually not given with much detail in the literature. The accretion theories\, however\, do predict a simple relation constraining the spin period and its time derivative\, i.e. the so-called spin-up line. Studying the spin-up line will reveal some secrets of the accretion process and probably shed light on finding the fastest spinning pulsars\, including a sub-ms one. In this talk\, I will present our study of the spin-up line using an MSP population. I will show the hierarchical Bayesian method we used and discuss the interesting results we found. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-xiaojin-liu-beijing-normal-university-china/
LOCATION:NSW
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-12102022.jpg
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BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20221019T150000
DTEND;TZID=Australia/Sydney:20221019T160000
DTSTAMP:20260516T041944
CREATED:20250819T073718Z
LAST-MODIFIED:20250819T073718Z
UID:14962-1666191600-1666195200@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Bi-Qing For (UWA)
DESCRIPTION:ASKAP WALLABY: dwarf galaxies in the local universe\n\nAbstract\n\nLow-mass\, or dwarf\, galaxies are the primary source of ionising photons during the epoch of reionisation and they are the building blocks of galaxies in the early Universe. Thus\, they play an important role as the strongest test for the standard Cold Dark Matter model on the smallest scale. In this talk\, I will present the results and goals of two ongoing dwarf galaxies-related projects that utilise ASKAP WALLABY data in conjunction with other legacy multiwavelength data. The two main studies are (1) probing role of galaxy interactions in quenching at low-mass end and (2) probing the formation mechanisms of low-surface brightness ‘dwarf’ galaxies (ultra-diffuse galaxies) from the HI perspective. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-bi-qing-for-uwa/
LOCATION:NSW
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-19102022.jpg
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20221026T150000
DTEND;TZID=Australia/Sydney:20221026T160000
DTSTAMP:20260516T041944
CREATED:20250819T073652Z
LAST-MODIFIED:20250819T073653Z
UID:14961-1666796400-1666800000@www.atnf.csiro.au
SUMMARY:S&A Colloquium: Yik Ki Ma (ANU)
DESCRIPTION:ASKAP as the Magnetic Probe of the Small Magellanic Cloud?\n\nAbstract\n\nHigh spatial resolution observations of the diffuse atomic (HI) gas have led to the realisation that the HI filamentary structures in the solar neighbourhood are aligned with the ambient magnetic field. It remains unclear whether this is a general attribute of the ISM across a large Galactic volume\, as well as in other galaxies with vastly different astrophysical characteristics. Using the high quality data from the Australian Square Kilometre Array Pathfinder (ASKAP) radio telescope for the Galactic ASKAP HI (GASKAP-HI) survey\, I investigated whether the ~10 pc-scale HI filaments in the Small Magellanic Cloud (SMC) can act as compass needles tracing the galactic magnetic field structure. Furthermore\, I mapped the preferred orientation of these filamentary HI structures to reveal the astrophysical processes shaping the ISM in the SMC. In this talk\, I will present the results from this work\, as well as highlighting the potential synergies between the GASKAP-HI and the POSSUM surveys. \nWatch recording\nEvent details\nDownload iCal\nCategory\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-yik-ki-ma-anu/
LOCATION:NSW
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-26102022-scaled.jpg
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