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DTSTART;TZID=Australia/Sydney:20240306T150000
DTEND;TZID=Australia/Sydney:20240306T160000
DTSTAMP:20260516T144830
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\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-nivedita-mahesh-california-institute-of-technology/
LOCATION:NSW
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-06032024.jpg
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BEGIN:VEVENT
DTSTART;TZID=Australia/Sydney:20240313T150000
DTEND;TZID=Australia/Sydney:20240313T160000
DTSTAMP:20260516T144830
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\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-magda-arnaboldi-eso/
LOCATION:NSW
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-13032024.jpg
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DTSTART;TZID=Australia/Sydney:20240320T150000
DTEND;TZID=Australia/Sydney:20240320T160000
DTSTAMP:20260516T144830
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\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-anthony-j-beasley-nrao/
LOCATION:NSW
CATEGORIES:Colloquia
ATTACH;FMTTYPE=image/jpeg:https://www.atnf.csiro.au/wp-content/uploads/2024/12/Colloq-20032024.jpg
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DTSTART;TZID=Australia/Sydney:20240327T150000
DTEND;TZID=Australia/Sydney:20240327T160000
DTSTAMP:20260516T144830
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\nColloquia
URL:https://www.atnf.csiro.au/event/sa-colloquium-samuel-lai-csiro/
LOCATION:NSW
CATEGORIES:Colloquia
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