Volume 526, February 2011
|Number of page(s)||8|
|Published online||06 January 2011|
Chemical composition of the Taurus-Auriga association ⋆
INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 3522
2 INAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
Received: 19 August 2010
Accepted: 17 November 2010
Context. The Taurus-Auriga association is perhaps the most famous prototype of a low-mass star forming region, surveyed at almost all wavelengths. Unfortunately, like several other young clusters/associations, this T association lacks an extensive abundance analysis determination.
Aims. We present a high-resolution spectroscopic study of seven low-mass members of Taurus-Auriga, including both weak-lined and classical T Tauri stars designed to help robustly determine their metallicity.
Methods. After correcting for spectral veiling, we performed equivalent width and spectral synthesis analyses using the GAIA set of model atmospheres and the 2002 version of the code MOOG.
Results. We find a solar metallicity, obtaining a mean value of [Fe/H] = −0.01 ± 0.05. The α-element Si and the Fe-peak one Ni confirm a solar composition. Our work shows that the dispersion among members is well within the observational errors at variance with previous claims. As in other star forming regions, no metal-rich members are found, reinforcing the idea that old planet-host stars form in the inner part of the Galactic disc and subsequently migrate.
Key words: stars: abundances / open clusters and associations: individual: Taurus-Auriga
© ESO, 2011
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