Ages and Heavy Element Abundances from Very Metal-poor Stars in the Sagittarius Dwarf Galaxy

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dc.contributor.authorHansen, C.J.
dc.contributor.authorEl-Souri, M.
dc.contributor.authorMonaco, L.
dc.contributor.authorVillanova, S.
dc.contributor.authorBonifacio, P.
dc.contributor.authorCaffau, E.
dc.contributor.authorSbordone, L.
dc.date.accessioned2018-09-25T13:16:50Z
dc.date.available2018-09-25T13:16:50Z
dc.date.issued2018-03
dc.descriptionIndexación: Scopus.es_ES
dc.description.abstractSagittarius (Sgr) is a massive disrupted dwarf spheroidal galaxy in the Milky Way halo that has undergone several stripping events. Previous chemical studies were restricted mainly to a few, metal-rich ([Fe/H] ) stars that suggested a top-light initial mass function (IMF). Here we present the first high-resolution, very metal-poor ([Fe/H] =-1 to -3) sample of 13 giant stars in the main body of Sgr. We derive abundances of 13 elements, namely C, Ca, Co, Fe, Sr, Ba, La, Ce, Nd, Eu, Dy, Pb, and Th, that challenge the interpretation based on previous studies. Our abundances from Sgr mimic those of the metal-poor halo, and our most metal-poor star ([Fe/H] ) indicates a pure r-process pollution. Abundances of Sr, Pb, and Th are presented for the first time in Sgr, allowing for age determination using nuclear cosmochronology. We calculate ages of . Most of the sample stars have been enriched by a range of asymptotic giant branch (AGB) stars with masses between 1.3 and 5 M o. Sgr J190651.47-320147.23 shows a large overabundance of Pb (2.05 dex) and a peculiar abundance pattern best fit by a 3 M o AGB star. Based on star-to-star scatter and observed abundance patterns, a mixture of low- and high-mass AGB stars and supernovae (15-25 M o) is necessary to explain these patterns. The high level (0.29 0.05 dex) of Ca indicates that massive supernovae must have existed and polluted the early ISM of Sgr before it lost its gas. This result is in contrast with a top-light IMF with no massive stars polluting Sgr. © 2018. The American Astronomical Society. All rights reserved..es_ES
dc.description.urihttp://iopscience.iop.org/article/10.3847/1538-4357/aa978f/meta
dc.identifier.citationAstrophysical Journal, 855(2), art. no. 83.es_ES
dc.identifier.issn0004-637X
dc.identifier.otherDOI: 10.3847/1538-4357/aa978f
dc.identifier.urihttp://repositorio.unab.cl/xmlui/handle/ria/7050
dc.language.isoenes_ES
dc.publisherInstitute of Physics Publishinges_ES
dc.subjectGalaxies: dwarfes_ES
dc.subjectGalaxies: evolutiones_ES
dc.subjectGalaxy: haloes_ES
dc.subjectNuclear reactions, nucleosynthesis, abundanceses_ES
dc.subjectStars: abundanceses_ES
dc.subjectStars: chemically peculiares_ES
dc.titleAges and Heavy Element Abundances from Very Metal-poor Stars in the Sagittarius Dwarf Galaxyes_ES
dc.typeArtículoes_ES
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