Volume 446, Number 3, February II 2006
|Page(s)||971 - 983|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||20 January 2006|
Fundamental properties of pre-main sequence stars in young, southern star forming regions: metallicities
The weak-lined T-Tauri stars
Laboratoire d'Astrophysique, Observatoire de Grenoble, BP 53, 38041 Grenoble, France e-mail: firstname.lastname@example.org;Jerome.Bouvier@obs.ujf-grenoble.fr
2 Dept. of Physics & Astronomy, Box 1807 Station B, Vanderbilt University, Nashville, TN 37235, USA
3 European Southern Observatory, Casilla 19001, Santiago 19, Chile e-mail: email@example.com
4 Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
5 Centro de Astronomia e Astrofísica da Universidade de Lisboa, Observatório Astrónomico de Lisboa, Tapada da Ajuda, 1349-018 Lisboa, Portugal e-mail: firstname.lastname@example.org
6 Observatoire de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland
Accepted: 5 October 2005
Aims. The primary motivation for this project is to search for metal-rich star forming regions, in which, stars of super-solar metallicity will be created, as hopefully, will be extra-solar planets orbiting them! The two aims of this project are: 1) to show that our sample stars are young, lithium rich, magnetically active and non-accreting kinematic members of their respective regions. 2) To measure the metallicity for such members. Methods. The feros échelle spectrograph together with eso's 2.2 m telescope, was used to obtain high resolution (R = 32 000) spectra for each of our weak-lined T-Tauri target stars. The wavelength range of the spectra is Å. Results. We find (pre-main sequence) model-dependent isochronal ages of the Lupus, Chamaeleon and CrA targets to be 9.1 ± 2.1 Myr, 4.5 ± 1.6 Myr and 9.0 ± 3.9 Myr respectively. The majority of the stars have Li i 6707.8 Å equivalent widths similar to, or above those of, their similar mass Pleiades counterparts, confirming their youthfulness. Most stars are kinematic members, either single or binary, of their regions. We find a mean radial velocity for objects in the Lupus cloud to be ± 1.8 km s-1, for the Chamaeleon i & ii clouds, ± 3.6 km s-1 whereas for the CrA cloud, we find ± 0.5 km s-1. All stars are coronally and chromospherically active, exhibiting X-ray and Hα emission levels marginally less, approximately equal or superior to that of their older IC 2602/2391 and/or Pleiades counterparts. All bar three of the targets show little or no signature of accretion from a circumstellar environment, according to their positions in a diagram. For the higher quality spectra, we have performed an iron-line metallicity analysis for five (5) stars in Chamaeleon, four (4) stars in Lupus and three (3) stars in the CrA star forming regions. These results show that all three regions are slightly metal-poor, with marginally sub-solar metallicities, with [Fe/H] = -0.11 ± 0.14, -0.10 ± 0.04 and -0.04 ± 0.05 respectively. Conclusions. A sample of stars in several nearby, young star-forming regions has been established, the majority of which is young, lithium rich, magnetically active and are non-accreting kinematic members of their respective clouds. Within the errors, each region is essentially of solar metallicity.
Key words: stars: fundamental parameters / stars: pre-main sequence / stars: abundances / ISM: individual objects: Lupus / ISM: individual objects: Chamaeleon i & ii / ISM: individual objects: Corona Australis (CrA)
© ESO, 2006
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