The Gaia-ESO survey: metallicity of the chamaeleon i star-forming region



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Montes Gutiérrez, David (2014) The Gaia-ESO survey: metallicity of the chamaeleon i star-forming region. Astronomy and astrophysics, 568 . ISSN 0004-6361

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Context. Recent metallicity determinations in young open clusters and star-forming regions suggest that the latter may be characterized by a slightly lower metallicity than the Sun and older clusters in the solar vicinity. However, these results are based on small statistics and inhomogeneous analyses. The Gaia-ESO Survey is observing and homogeneously analyzing large samples of stars in several young clusters and star-forming regions, hence allowing us to further investigate this issue.
Aims. We present a new metallicity determination of the Chamaeleon I star-forming region, based on the products distributed in the first internal release of the Gaia-ESO Survey.
Methods. 48 candidate members of Chamaeleon I have been observed with the high-resolution spectrograph UVES. We use the surface gravity, lithium line equivalent width and position in the Hertzsprung-Russell diagram to confirm the cluster members and we use the iron abundance to derive the mean metallicity of the region.
Results. Out of the 48 targets, we confirm 15 high probability members. Considering the metallicity measurements for 9 of them, we find that the iron abundance of Chamaeleon I is slightly subsolar with a mean value [Fe/H]= −0.08 ± 0.04 dex. This result is in agreement with the metallicity determination of other nearby star-forming regions and suggests that the chemical pattern of the youngest stars in the solar neighborhood is indeed more metal-poor than the Sun. We argue that this evidence may be related to the chemical distribution of the Gould Belt that contains most of the nearby star-forming regions and young clusters.

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© ESO 2014. Artículo firmado por 40 autores. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188.B- 3002. This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. 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”. The results presented here benefit from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. We acknowlodge the use of the ASURV astronomy survival analysis package (Lavalley et al. 1992) which is freely available from E.D.M., S.G.S. and V.Zh.A. acknowledge the support from the Fundação para a Ciência e Tecnologia, FCT (Portugal) in the form of the fellowships SFRH/BPD/76606/2011, SFRH/BPD/47611/2008 and SFRH/BPD/70574/2010 from the FCT (Portugal), respectively. We also acknowledge the support of the French Agence Nationale de la Recherche, under contract ANR-2010-BLAN-0508-01OTP, and the “Programme National de Cosmologie et Galaxies” (PNCG) of CNRS/INSU, France. J.I.G.H. acknowledges financial support from the Spanish Ministry project MINECO AYA2011-29060, and also from the Spanish Ministry of Economy and Competitiveness (MINECO) under the 2011 Severo Ochoa Program MINECO SEV-2011-0187. H.M.T. and D.M. acknowledges financial support from the Spanish Ministry of Economy and Competitiveness (MINECO) project AYA2011-30147-C03-02. T.B. was funded by grant No. 621-2009-3911 from The Swedish Research Council.

Uncontrolled Keywords:Astrophysics; Iodine; Surveys chemical distributions; Hertzsprung-russell diagrams; Open clusters and associations-individual; Solar neighborhood; Star-forming region; Stars-abundances; Stars-pre-main sequence; Techniques-spectroscopic.
Subjects:Sciences > Physics > Astrophysics
Sciences > Physics > Astronomy
ID Code:29776
Deposited On:29 Apr 2015 07:35
Last Modified:10 Dec 2018 15:05

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