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Metal production in the early Universe: what chemical abundances in old stellar populations in the Milky Way tell us

Published online by Cambridge University Press:  13 February 2024

Miho N. Ishigaki Open the ORCID record for Miho N. Ishigaki [Opens in a new window]
Miho N. Ishigaki*
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan.
*
email: miho.ishigaki@nao.ac.jp
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Abstract

Old stellar populations in our Galaxy provide fossil records of the metal enrichment in the first few billion years of the cosmic history. Growing elemental abundance data of individual stars combined with stellar ages and kinematics allow us to make constraints on characteristic properties of the metal-enrichment sources in the early Universe, such as the first stars. In order to interpret observed chemical abundances in the oldest stellar populations in terms of metal-enrichment sources, stellar and supernova yield models are crucial. In this article, we review how we can interpret observed chemical abundances in old stars in terms of the nature of metal enrichment sources. We discuss the limitations and the prospects of empirically constraining supernova yield models based on a large sample of extremely metal-poor stars. At the same time, we emphasize the importance of hunting old stars beyond the Solar neighborhood, which can be achieved with the next-generation multi-object spectrographs at large telescopes.

Keywords

The Milky Way GalaxyMetal-poor starsChemical abundances
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S377: Early Disk-Galaxy Formation from JWST to the Milky Way , December 2022 , pp. 79 - 88
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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