Spectroscopic metallicities for planet-host stars: extending the samples

Astrophysics, abstract
astro-ph/0504154

From: Nuno C. Santos [view email]

Date (v1): Wed, 6 Apr 2005 18:21:04 GMT   (33kb)

Date (revised v2): Wed, 6 Apr 2005 22:08:55 GMT   (33kb)

Date (revised v3): Tue, 19 Apr 2005 10:31:24 GMT   (33kb)

Spectroscopic metallicities for planet-host stars: extending the samples

Authors:
N.C. Santos (1,2),
G. Israelian (3),
M. Mayor (2),
J.P. Bento (1),
P.C. Almeida (1),
S.G. Sousa (1),
A. Ecuvillon (3) ((1) Centro de Astronomia e Astrofisica da Universidade de Lisboa, (2) Observatoire de Geneve, (3) Instituto de Astrofisica de Canarias)

Comments: Accepted for publication in A&A; Replaced by new version on
19/04/2005: corrections in Tables 1 and 2

We present stellar parameters and metallicities for 29 planet-host stars, as
well as for a large volume-limited sample of 53 stars not known to be orbited
by any planetary-mass companion. These stars add to the results presented in
our previous series of papers, providing two large and uniform samples of 119
planet-hosts and 94 “single” stars with accurate stellar parameters and
[Fe/H] estimates. The analysis of the results further confirms that stars with
planets are metal-rich when compared with average field dwarfs. Important
biases that may compromise future studies are also discussed. Finally, we
compare the metallicity distributions for single planet-hosts and planet-hosts
in multiple stellar systems. The results show that a small difference cannot be
excluded, in the sense that the latter sample is slighly overmetallic. However,
more data are needed to confirm this correlation.

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