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DTSTART;TZID=Australia/Sydney:20240313T150000
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DTSTAMP:20260516T044731
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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