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The Gaia-ESO Survey: Metallicity of the Chamaeleon I star-forming region

Spina, L.; Randich, S.; Palla, E.; Biazzo, K.; Sacco, G. G.; Alfaro, E. J.; Franciosini, E.; Magrini, L.; Morbidelli, L. and Frasca, A., et al. (2014) In Astronomy & Astrophysics 568.
Abstract
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. The 48 candidate members of Chamaeleon I have been observed with the... (More)
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. The 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 Hertzsprimg-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 nine 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 agrees 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. (Less)
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@article{e6ec8a3a-84ec-4a64-b741-b47333f851e3,
  abstract     = {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. The 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 Hertzsprimg-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 nine 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 agrees 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.},
  articleno    = {A2},
  author       = {Spina, L. and Randich, S. and Palla, E. and Biazzo, K. and Sacco, G. G. and Alfaro, E. J. and Franciosini, E. and Magrini, L. and Morbidelli, L. and Frasca, A. and Adibekyan, V. and Delgado-Mena, E. and Sousa, S. G. and Gonzalez Hernandez, J. I. and Montes, D. and Tabernero, H. and Tautvaisiene, G. and Bonito, R. and Lanzafame, A. C. and Gilmore, G. and Jeffries, R. D. and Vallenari, A. and Bensby, Thomas and Bragaglia, A. and Flaccomio, E. and Korn, A. J. and Pancino, F. and Recio-Blanco, A. and Smiljanic, R. and Bergemann, M. and Costado, M. T. and Damiani, F. and Hill, V. and Hourihane, A. and Jofre, P. and de Laverny, P. and Lardo, C. and Masseron, T. and Prisinzano, L. and Worley, C. C.},
  issn         = {0004-6361},
  keyword      = {open clusters and associations: individual: Chamaeleon I,stars:,pre-main sequence,stars: abundances,techniques: spectroscopic},
  language     = {eng},
  publisher    = {EDP Sciences},
  series       = {Astronomy & Astrophysics},
  title        = {The Gaia-ESO Survey: Metallicity of the Chamaeleon I star-forming region},
  url          = {http://dx.doi.org/10.1051/0004-6361/201424135},
  volume       = {568},
  year         = {2014},
}