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Disentangling the Galactic Halo with APOGEE. II. Chemical and Star Formation Histories for the Two Distinct Populations

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dc.contributor.author Fernández-Alvar, E.
dc.contributor.author Carigi, L.
dc.contributor.author Schuster, W.J.
dc.contributor.author Hayes, C.R.
dc.contributor.author Ávila-Vergara, N.
dc.contributor.author Majewski, S.R.
dc.contributor.author Allende Prieto, C.
dc.contributor.author Beers, T.C.
dc.contributor.author Sánchez, S.F.
dc.contributor.author Zamora, O.
dc.contributor.author García-Hernández, D.A.
dc.contributor.author Tang, B.
dc.contributor.author Fernández-Trincado, J.G.
dc.contributor.author Tissera, P.
dc.contributor.author Geisler, D.
dc.contributor.author Villanova, S.
dc.date.accessioned 2018-07-23T21:08:30Z
dc.date.available 2018-07-23T21:08:30Z
dc.date.issued 2018
dc.identifier.citation Astrophysical Journal. Volume 852, Issue 1, 1 January 2018, Article number 50 es_ES
dc.identifier.issn 0000-4637X
dc.identifier.other DOI: 10.3847/1538-4357/aa9ced
dc.identifier.uri http://repositorio.unab.cl/xmlui/handle/ria/6361
dc.description Indexación: Scopus. es_ES
dc.description.abstract The formation processes that led to the current Galactic stellar halo are still under debate. Previous studies have provided evidence for different stellar populations in terms of elemental abundances and kinematics, pointing to different chemical and star formation histories (SFHs). In the present work, we explore, over a broader range in metallicity (-2.2 < [Fe H] < +0.5), the two stellar populations detected in the first paper of this series from metal-poor stars in DR13 of the Apache Point Observatory Galactic Evolution Experiment (APOGEE). We aim to infer signatures of the initial mass function (IMF) and the SFH from the two α-to-iron versus iron abundance chemical trends for the most APOGEE-reliable α-elements (O, Mg, Si, and Ca). Using simple chemical-evolution models, we infer the upper mass limit (M up) for the IMF and the star formation rate, and its duration for each population. Compared with the low-α population, we obtain a more intense and longer-lived SFH, and a top-heavier IMF for the high-α population. es_ES
dc.description.uri http://iopscience.iop.org/article/10.3847/1538-4357/aa9ced/meta
dc.language.iso en es_ES
dc.publisher Institute of Physics Publishing es_ES
dc.subject Galaxy: evolution es_ES
dc.subject Galaxy: halo es_ES
dc.subject Stars: abundances es_ES
dc.title Disentangling the Galactic Halo with APOGEE. II. Chemical and Star Formation Histories for the Two Distinct Populations es_ES
dc.type Article es_ES


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