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The Pristine Inner Galaxy Survey (PIGS) V: a chemo-dynamical investigation of the early assembly of the Milky Way with the most metal-poor stars in the bulge

Published online by Cambridge University Press:  13 February 2024

Federico Sestito Open the ORCID record for Federico Sestito [Opens in a new window] ,
Kim A. Venn Open the ORCID record for Kim A. Venn [Opens in a new window] ,
Anke Arentsen  and
David Aguado
Federico Sestito*
Affiliation:
Department of Physics and Astronomy, University of Victoria, PO Box 3055, STN CSC, Victoria BC V8W 3P6, Canada.
Kim A. Venn
Affiliation:
Department of Physics and Astronomy, University of Victoria, PO Box 3055, STN CSC, Victoria BC V8W 3P6, Canada.
Anke Arentsen
Affiliation:
Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
David Aguado
Affiliation:
Instituto de Astrofísica de Canarias (IAC), Vía Láctea, E-38200 La Laguna, Tenerife, Spain Universidad de La Laguna, Dept. Astrofísica, E-38200 La Laguna, Tenerife, Spain
*
email: sestitof@uvic.ca
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Abstract

The investigation of the metal-poor tail in the Galactic bulge provides unique information on the early Milky Way assembly and evolution. A chemo-dynamical analysis of 17 very metal-poor stars (VMP, [Fe/H < – 2.0]) selected from the Pristine Inner Galaxy Survey was carried out based on Gemini/GRACES spectra. The chemistry suggests that the majority of our stars are very similar to metal-poor stars in the Galactic halo. Orbits calculated from Gaia EDR3 imply these stars are brought into the bulge during the earliest Galactic assembly. Most of our stars have large [Na,Ca/Mg] abundances, and thus show little evidence of enrichment by pair-instability supernovae. Two of our stars (P171457, P184700) have chemical abundances compatible with second-generation globular cluster stars, suggestive of the presence of ancient and now dissolved globular clusters in the inner Galaxy. One of them (P171457) is extremely metal-poor ([Fe/H < – 3.0]) and well below the metallicity floor of globular clusters, which supports the growing evidence for the existence of lower-metallicity globular clusters in the early Universe. A third star (P180956, [Fe/H]∼ – 2) has low [Na,Ca/Mg] and very low [Ba/Fe] for its metallicity, which are consistent with formation in a system polluted by only one or a few low-mass supernovae. Interestingly, its orbit is confined to the Galactic plane, like other very metal-poor stars found in the literature, which have been associated with the earliest building blocks of the Milky Way.

Keywords

Galaxy: formationGalaxy: evolutionGalaxy: bulgeGalaxy: abundancesstars: kinematics and dynamicsstars: Population II
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. 102 - 106
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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