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

Spina, L. ; Randich, S. ; Palla, F. ; Sacco, G. G. ; Magrini, L. ; Franciosini, E. ; Morbidelli, L. ; Prisirizano, L. ; Alfaro, E. J. and Biazzo, K. , et al. (2014) In Astronomy & Astrophysics 567.
Abstract
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... (More)
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 similar to 60 M-circle plus hydrogen-depleted material from the circumstellar disk. (Less)
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subject
keywords
stars: abundances, stars: pre-main sequence, open clusters and, associations: individual: gamma Velorum, techniques: spectroscopic
in
Astronomy & Astrophysics
volume
567
article number
A55
publisher
EDP Sciences
external identifiers
  • wos:000341185300078
  • scopus:84903996443
ISSN
0004-6361
DOI
10.1051/0004-6361/201423527
project
Gaia-ESO Survey
language
English
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yes
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7c303d64-ae13-4b12-b345-cb9d557e8916 (old id 4709887)
date added to LUP
2016-04-01 14:44:35
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2020-05-24 04:52:55
@article{7c303d64-ae13-4b12-b345-cb9d557e8916,
  abstract     = {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 similar to 60 M-circle plus hydrogen-depleted material from the circumstellar disk.},
  author       = {Spina, L. and Randich, S. and Palla, F. and Sacco, G. G. and Magrini, L. and Franciosini, E. and Morbidelli, L. and Prisirizano, L. and Alfaro, E. J. and Biazzo, K. and Frasca, A. and Gonzalez-Hernandez, J. I. and Sousa, S. G. and Adibekyan, V. and Degado-Mena, E. and Montes, D. and Tabernero, H. and Klutsch, A. and Gilmore, G. and Feltzing, Sofia and Jeffries, R. D. and Micela, G. and Vallenari, A. and Bensby, T. and Bragaglia, A. and Flaccomio, E. and Koposov, S. and Lanzafame, A. C. and Pancino, E. and Recio-Banco, A. and Smiljanie, R. and Costado, M. T. and Damiani, F. and Hill, V. and Hourihane, A. and Jofre, P. and de Laverny, P. and Masseron, T. and Worley, C.},
  issn         = {0004-6361},
  language     = {eng},
  publisher    = {EDP Sciences},
  series       = {Astronomy & Astrophysics},
  title        = {The Gaia-ESO Survey: the first abundance determination of the pre-main-sequence cluster gamma Velorum},
  url          = {http://dx.doi.org/10.1051/0004-6361/201423527},
  doi          = {10.1051/0004-6361/201423527},
  volume       = {567},
  year         = {2014},
}