Show simple item record

dc.contributor.authorHayes, C.R.
dc.contributor.authorMajewski, S.R.
dc.contributor.authorShetrone, M.
dc.contributor.authorFernández-Alvar, E.
dc.contributor.authorPrieto, C.A.
dc.contributor.authorSchuster, W.J.
dc.contributor.authorCarigi, L.
dc.contributor.authorCunha, K.
dc.contributor.authorSmith, V.V.
dc.contributor.authorSobeck, J.
dc.contributor.authorAlmeida, A.
dc.contributor.authorBeers, T.C.
dc.contributor.authorCarrera, R.
dc.contributor.authorFernández-Trincado, J.G.
dc.contributor.authorGarcía-Hernández, D.A.
dc.contributor.authorGeisler, D.
dc.contributor.authorLane, R.R.
dc.contributor.authorLucatello, S.
dc.contributor.authorMatthews, A.M.
dc.contributor.authorMinniti, D.
dc.contributor.authorNitschelm, C.
dc.contributor.authorTang, B.
dc.contributor.authorTissera, P.B.
dc.contributor.authorZamora, O.
dc.date.accessioned2018-07-23T21:43:00Z
dc.date.available2018-07-23T21:43:00Z
dc.date.issued2018
dc.identifier.citationAstrophysical Journal. Volume 852, Issue 1, 1 January 2018, Article number 49es_ES
dc.identifier.issn0004-637X
dc.identifier.otherDOI: 10.3847/1538-4357/aa9cec
dc.identifier.urihttp://repositorio.unab.cl/xmlui/handle/ria/6362
dc.descriptionIndexación: Scopus.es_ES
dc.description.abstractWe 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.urihttp://iopscience.iop.org/article/10.3847/1538-4357/aa9cec/meta
dc.language.isoenes_ES
dc.publisherInstitute of Physics Publishinges_ES
dc.subjectGalaxy: diskes_ES
dc.subjectGalaxy: evolutiones_ES
dc.subjectGalaxy: formationes_ES
dc.subjectGalaxy: haloes_ES
dc.subjectStars: abundanceses_ES
dc.titleDisentangling the Galactic Halo with APOGEE. I. Chemical and Kinematical Investigation of Distinct Metal-poor Populationses_ES
dc.typeArticlees_ES


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record