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Disentangling the Galactic Halo with APOGEE. I. Chemical and Kinematical Investigation of Distinct Metal-poor Populations

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dc.contributor.author Hayes, C.R.
dc.contributor.author Majewski, S.R.
dc.contributor.author Shetrone, M.
dc.contributor.author Fernández-Alvar, E.
dc.contributor.author Prieto, C.A.
dc.contributor.author Schuster, W.J.
dc.contributor.author Carigi, L.
dc.contributor.author Cunha, K.
dc.contributor.author Smith, V.V.
dc.contributor.author Sobeck, J.
dc.contributor.author Almeida, A.
dc.contributor.author Beers, T.C.
dc.contributor.author Carrera, R.
dc.contributor.author Fernández-Trincado, J.G.
dc.contributor.author García-Hernández, D.A.
dc.contributor.author Geisler, D.
dc.contributor.author Lane, R.R.
dc.contributor.author Lucatello, S.
dc.contributor.author Matthews, A.M.
dc.contributor.author Minniti, D.
dc.contributor.author Nitschelm, C.
dc.contributor.author Tang, B.
dc.contributor.author Tissera, P.B.
dc.contributor.author Zamora, O.
dc.date.accessioned 2018-07-23T21:43:00Z
dc.date.available 2018-07-23T21:43:00Z
dc.date.issued 2018
dc.identifier.citation Astrophysical Journal. Volume 852, Issue 1, 1 January 2018, Article number 49 es_ES
dc.identifier.issn 0004-637X
dc.identifier.other DOI: 10.3847/1538-4357/aa9cec
dc.identifier.uri http://repositorio.unab.cl/xmlui/handle/ria/6362
dc.description Indexación: Scopus. es_ES
dc.description.abstract We find two chemically distinct populations separated relatively cleanly in the [Fe/H]-[Mg/Fe] plane, but also distinguished in other chemical planes, among metal-poor stars (primarily with metallicities [Fe H] < -0.9) observed by the Apache Point Observatory Galactic Evolution Experiment (APOGEE) and analyzed for Data Release 13 (DR13) of the Sloan Digital Sky Survey. These two stellar populations show the most significant differences in their [X/Fe] ratios for the α-elements, C+N, Al, and Ni. In addition to these populations having differing chemistry, the low metallicity high-Mg population (which we denote "the HMg population") exhibits a significant net Galactic rotation, whereas the low-Mg population (or "the LMg population") has halo-like kinematics with little to no net rotation. Based on its properties, the origin of the LMg population is likely an accreted population of stars. The HMg population shows chemistry (and to an extent kinematics) similar to the thick disk, and is likely associated with in situ formation. The distinction between the LMg and HMg populations mimics the differences between the populations of low- and high-α halo stars found in previous studies, suggesting that these are samples of the same two populations. es_ES
dc.description.uri http://iopscience.iop.org/article/10.3847/1538-4357/aa9cec/meta
dc.language.iso en es_ES
dc.publisher Institute of Physics Publishing es_ES
dc.subject Galaxy: disk es_ES
dc.subject Galaxy: evolution es_ES
dc.subject Galaxy: formation es_ES
dc.subject Galaxy: halo es_ES
dc.subject Stars: abundances es_ES
dc.title Disentangling the Galactic Halo with APOGEE. I. Chemical and Kinematical Investigation of Distinct Metal-poor Populations es_ES
dc.type Article es_ES


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