EDP Sciences
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Volume 398, Number 3, February II 2003
Page(s) 1121 - 1135
Section Formation and evolution of planetary systems
DOI http://dx.doi.org/10.1051/0004-6361:20021711

A&A 398, 1121-1135 (2003)
DOI: 10.1051/0004-6361:20021711

Automated spectroscopic abundances of A and F-type stars using echelle spectrographs

II. Abundances of 140 A-F stars from ELODIE and CORALIE
D. Erspamer and P. North

Institut d'astronomie de l'Université de Lausanne, 1290 Chavannes-des-Bois, Switzerland
(Received 14 June 2002 / Accepted 26 August 2002)

Using the method presented in Erspamer & North (2002, hereafter Paper I), detailed abundances of 140 stars are presented. The uncertainties characteristic of this method are presented and discussed. In particular, we show that for a  S/N ratio higher than 200, the method is applicable to stars with a rotational velocity as high as 200  ${\rm km~s^{-1}}$. There is no correlation between abundances and $V\sin{i}$, except a spurious one for Sr, Sc and Na which we explain by the small number of lines of these elements combined with a locally biased continuum. Metallic giants (Hauck 1986) show larger abundances than normal giants for at least 8 elements: Al, Ca, Ti, Cr, Mn, Fe, Ni and Ba. The anticorrelation for Na, Mg, Si, Ca, Fe and Ni with $V\sin{i}$ suggested by Varenne & Monier (1999) is not confirmed. The predictions of the Montréal models (e.g. Richard et al. 2001) are not fulfilled in general. However, a correlation between $\left[\frac{{\rm Fe}}{{\rm H}}\right]$ and $\log{g}$is found for stars of 1.8 to 2.0  $M_\odot$. Various possible causes are discussed, but the physical reality of this correlation seems inescapable.

Key words: techniques: spectroscopic -- stars: abundances -- stars: chemically peculiar -- stars: fundamental parameters

Offprint request: P. North, Pierre.North@obs.unige.ch

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