Discovery of a nitrogen-enhanced mildly metal-poor binary system: Possible evidence for pollution from an extinct AGB star

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dc.contributor.authorFernández-Trincado, José G.
dc.contributor.authorMennickent, Ronald
dc.contributor.authorCabezas, Mauricio
dc.contributor.authorZamora, Olga
dc.contributor.authorMartell, Sarah L.
dc.contributor.authorBeers, Timothy C.
dc.contributor.authorPlacco, Vinicius M.
dc.contributor.authorNataf, David M.
dc.contributor.authorMészáros, Szabolcsk
dc.contributor.authorMinniti, Dantel
dc.contributor.authorSchleicher, Dominik R. G.
dc.contributor.authorTang, Baitian
dc.date.accessioned2023-03-27T22:08:42Z
dc.date.available2023-03-27T22:08:42Z
dc.date.issued2019
dc.descriptionIndexación Scopuses
dc.description.abstractWe report the serendipitous discovery of a nitrogen-rich, mildly metal-poor ([Fe/H] = -1.08) giant star in a single-lined spectroscopic binary system found in the SDSS-IV Apache Point Observatory Galactic Evolution Experiment (APOGEE-2) survey, Data Release 14 (DR14). Previous work has assumed that two percent of halo giants with unusual elemental abundances have been evaporated from globular clusters, but other origins for their abundance signatures, including binary mass transfer, must also be explored. We present the results of an abundance reanalysis of the APOGEE-2 high-resolution near-infrared spectrum of 2M12451043+1217401 with the Brussels Automatic Stellar Parameter (BACCHUS) automated spectral analysis code. We manually re-derive the main element families, namely light elements (C, N), elements (O, Mg, Si), the iron-peak element (Fe), s-process element (Ce), and light odd-Z element (Al). Our analysis confirms the N-rich nature of 2M12451043+1217401, which has a [N/Fe] ratio of +0.69, and shows that the abundances of C and Al are slightly discrepant from those of a typical mildly metal-poor red giant branch star, but exhibit Mg, Si, O and s-process abundances (Ce) of typical field stars. We also detect a particularly large variability in the radial velocity of this star over the period of the APOGEE-2 observations; the most likely orbit fit to the radial velocity data has a period of 730.89 ±106.86 days, a velocity semi-amplitude of 9.92 ±0.14 km s-1, and an eccentricity of ∼0.1276 ±0.1174. These data support the hypothesis of a binary companion, which has probably been polluted by a now-extinct asymptotic giant branch star.es
dc.identifier.citationAstronomy and Astrophysics Volume 6312019 Article number A97es
dc.identifier.doi10.1051/0004-6361/201935369en
dc.identifier.issn0004-6361
dc.identifier.urihttps://repositorio.unab.cl/xmlui/handle/ria/47951
dc.language.isoenes
dc.publisherAstronomy and Astrophysicses
dc.rights.licenseAttribution 4.0 International (CC BY 4.0)en
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/en
dc.subjectBinaries: generales
dc.subjectStars: abundanceses
dc.subjectStars: AGB and post-AGBes
dc.subjectStars: chemically peculiares
dc.subjectStars: evolutiones
dc.subjectTechniques: spectroscopices
dc.titleDiscovery of a nitrogen-enhanced mildly metal-poor binary system: Possible evidence for pollution from an extinct AGB stares
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