The chemistry of stars in the bar of the Milky Way

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dc.contributor.authorWegg, C.
dc.contributor.authorRojas-Arriagada, A.
dc.contributor.authorSchultheis, M.
dc.contributor.authorGerhard, O.
dc.date.accessioned2025-01-23T21:09:01Z
dc.date.available2025-01-23T21:09:01Z
dc.date.issued2019
dc.description.abstractWe use a sample of 938 red clump giant stars located in the direction of the Galactic long bar to study the chemistry of Milky Way bar stars. Kinematically separating stars on bar orbits from stars with inner disc orbits, we find that stars on bar-like orbits are more metal rich with a mean iron abundance of ⟨[Fe/H]⟩=+0.30 compared to ⟨[Fe/H]⟩=+0.03 for the inner disc. Spatially selecting bar stars is complicated by a strong vertical metallicity gradient of -1.1 dex kpc(-1), but we find the metallicity distribution varies in a manner consistent with our orbital selection. Our results have two possible interpretations. The first is that the most metal rich stars in the inner Galaxy pre-existed the bar, but were kinematically cold at the time of bar formation and therefore more easily captured onto bar orbits when the bar formed. The second is that the most metal rich stars formed after the bar, either directly onto the bar following orbits or were captured by the bar after their formation.
dc.fuente.origenWOS
dc.identifier.doi10.1051/0004-6361/201936779
dc.identifier.eissn1432-0746
dc.identifier.issn0004-6361
dc.identifier.urihttps://doi.org/10.1051/0004-6361/201936779
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/100797
dc.identifier.wosidWOS:000502994500002
dc.language.isoen
dc.revistaAstronomy & astrophysics
dc.rightsacceso restringido
dc.subjectGalaxy
dc.subjectabundances
dc.subjectGalaxy
dc.subjectkinematics and dynamics
dc.subjectGalaxy
dc.subjectcenter
dc.titleThe chemistry of stars in the bar of the Milky Way
dc.typeartículo
dc.volumen632
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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