Abundance analysis of APOGEE spectra for 58 metal-poor stars from the bulge spheroid

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dc.contributor.authorRazera, R.
dc.contributor.authorBarbuy, B.
dc.contributor.authorMoura, T.C.
dc.contributor.authorErnandes, H.
dc.contributor.authorPérez Villegas, A.
dc.contributor.authorSouza, S.O.
dc.contributor.authorChiappini, C.
dc.contributor.authorQueiroz, A.B.A.
dc.contributor.authorAnders, F.
dc.contributor.authorFernández Trincado, J.G.
dc.contributor.authorFriaça, A.C.S.
dc.contributor.authorCunha, K.
dc.contributor.authorSmith, V.V.
dc.contributor.authorSantiago, B.X.
dc.contributor.authorSchiavon, R.P.
dc.contributor.authorValentini, M.
dc.contributor.authorMinniti, D.
dc.contributor.authorSchultheis, M.
dc.contributor.authorGeisler, D.
dc.contributor.authorSobeck, J.
dc.contributor.authorPlacco, V.M.
dc.contributor.authorZoccali, M.
dc.date.accessioned2023-04-10T22:50:32Z
dc.date.available2023-04-10T22:50:32Z
dc.date.issued2022-12-01
dc.descriptionIndexación: Scopus.es
dc.description.abstractThe central part of the Galaxy hosts a multitude of stellar populations, including the spheroidal bulge stars, stars moved to the bulge through secular evolution of the bar, inner halo, inner thick disc, inner thin disc, as well as debris from past accretion events. We identified a sample of 58 candidate stars belonging to the stellar population of the spheroidal bulge, and analyse their abundances. The present calculations of Mg, Ca, and Si lines are in agreement with the ASPCAP abundances, whereas abundances of C, N, O, and Ce are re-examined. We find normal α-element enhancements in oxygen, similar to magnesium, Si, and Ca abundances, which are typical of other bulge stars surveyed in the optical in Baade's Window. The enhancement of [O/Fe] in these stars suggests that they do not belong to accreted debris. No spread in N abundances is found, and none of the sample stars is N-rich, indicating that these stars are not second generation stars originated in globular clusters. Ce instead is enhanced in the sample stars, which points to an s-process origin such as due to enrichment from early generations of massive fast rotating stars, the so-called spinstars. © 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.es
dc.description.urihttps://academic-oup-com.recursosbiblioteca.unab.cl/mnras/article/517/3/4590/6653110
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, Volume 517, Issue 3, Pages 4590 - 46061 December 2022es
dc.identifier.doi10.1093/mnras/stac2136
dc.identifier.issn0035-8711
dc.identifier.urihttps://repositorio.unab.cl/xmlui/handle/ria/48420
dc.language.isoenes
dc.publisherOxford University Presses
dc.rights.licenseAtribución 4.0 Internacional (CC BY 4.0)
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/deed.es
dc.subjectGalaxy: bulgees
dc.subjectStars: abundanceses
dc.subjectStars: atmosphereses
dc.subjectDebrises
dc.subjectGalaxieses
dc.subjectAbundance analysises
dc.subjectMetal-poor stares
dc.subjectSecular evolutiones
dc.subjectSpectra'ses
dc.subjectStars - starses
dc.subjectStars: Bees
dc.subjectStellar populationses
dc.subjectStarses
dc.titleAbundance analysis of APOGEE spectra for 58 metal-poor stars from the bulge spheroides
dc.typeArtículoes
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