期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 518, 期 3, 页码 4557-4578出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stac3332
关键词
stars: kinematics and dynamics; stars: Population II; Galaxy: abundances; Galaxy: bulge; Galaxy: evolution; Galaxy: formation
资金
- Dr. Margaret 'Marmie' Perkins Hess postdoctoral fellowship
- National Sciences and Engineering Research Council of Canada
- French National Research Agency (ANR) [ANR-18-CE31-0017]
- European Research Council (ERC) under the European Unions Horizon 2020 research and innovation programme [834148]
- ERC Starting Grant NEFERTITI [H2020/808240]
- Spanish Ministry of Science and Innovation (MICINN) [PID2020-117493GB-I00]
- Dutch Research Council (NWO) [VI.Vidi.193.093]
- International Space Science Institute (ISSI) in Bern, Switzerland
- GRACES, as part of the Gemini Large and Long Program [GN-X-LP-102]
- France (CNRS)
- France (MENESR)
- France (OMP)
- France (LATT)
- Canada (NSERC)
- CFHT
- ESA
- WestGrid
- Compute Canada
The investigation of metal-poor stars in the Galactic bulge provides insights into the early assembly and evolution of the Milky Way. The study suggests the presence of metal-poor stars similar to those in the Galactic halo in the bulge, as well as hints at the existence of ancient dissolved globular clusters in the inner Galaxy.
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 and 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]similar to-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.
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