The Gaia-ESO Survey: The first abundance determination of the pre-main-sequence cluster gamma velorum

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Tabernero, H.
Koposov, S.
Hourihane, A.
Jofré, P.
Masseron, T.
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Context. Knowledge of the abundance distribution of star forming regions and young clusters is critical to investigate a variety of issues, from triggered star formation and chemical enrichment by nearby supernova explosions to the ability to form planetary systems. In spite of this, detailed abundance studies are currently available for relatively few regions. Aims. In this context, we present the analysis of the metallicity of the Gamma Velorum cluster, based on the products distributed in the first internal release of the Gaia-ESO Survey. Methods. The Gamma Velorum candidate members have been observed with FLAMES, using both UVES and Giraffe, depending on the target brightness and spectral type. In order to derive a solid metallicity determination for the cluster, membership of the observed stars must be first assessed. To this aim, we use several membership criteria including radial velocities, surface gravity estimates, and the detection of the photospheric lithium line. Results. Out of the 80 targets observed with UVES, we identify 14 high-probability members. We find that the metallicity of the cluster is slightly subsolar, with a mean [Fe/H]=−0.057±0.018 dex. Although J08095427-4721419 is one of the high-probability members, its metallicity is significantly larger than the cluster average. We speculate about its origin as the result of recent accretion episodes of rocky bodies of ∼60 M_⊕ hydrogen-depleted material from the circumstellar disk.
© EDP Sciences. We acknowledge the support from INAF and Ministero dell’Istruzione, dell’Università e della Ricerca (MIUR) in the form of the grant “Premiale VLT 2012”. We also acknowledge the financial support from “Programme National de Cosmologie and Galaxies” (PNCG) of CNRS/INSU, France. The results presented here benefited from discussions in three GaiaESO workshops supported by the ESF (European Science Foundation) through the GREAT (Gaia Research for European Astronomy Training) Research Network Program (Science meetings 3855, 4127 and 4415). T.B. was funded by grant No. 621-2009-3911 from The Swedish Research Council. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. E.J.A. acknowledges financial support from the “Ministerio de Economía y Competitividad” of Spain through grant AYA2010-17631. S.G.S, EDM, and V.Zh.A. acknowledge support from the Fundac¸o para a Ciéncia e Tecnologia (Portugal) in the form of grants SFRH/BPD/47611/2008, SFRH/BPD/76606/2011, SFRH/BPD/70574/2010, respectively
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