| Issue |
A&A
Volume 551, March 2013
|
|
|---|---|---|
| Article Number | A36 | |
| Number of page(s) | 17 | |
| Section | Stellar atmospheres | |
| DOI | https://doi.org/10.1051/0004-6361/201220574 | |
| Published online | 15 February 2013 | |
Metallicity of M dwarfs
III. Planet-metallicity and planet-stellar mass correlations of the HARPS GTO M dwarf sample⋆,⋆⋆
1
Centro de Astrofísica, Universidade do Porto,
Rua das Estrelas,
4150-762
Porto,
Portugal
e-mail: vasco.neves@astro.ua.pt
2
UJF-Grenoble 1/CNRS-INSU, Institut de Planétologie et
d’Astrophysique de Grenoble (IPAG) UMR 5274, 38041
Grenoble,
France
3
Departamento de Física e Astronomia, Faculdade de Ciências,
Universidade do Porto, Rua do Campo
Alegre, 4169-007
Porto,
Portugal
4
Centre de Recherche Astrophysique de Lyon, UMR 5574: CNRS,
Université de Lyon, École Normale
Supérieure de Lyon, 46 allée d’Italie, 69364
Lyon Cedex 07,
France
5
Observatoire de Genève, Université de Genève,
51 chemin des
Maillettes, 1290
Sauverny,
Switzerland
Received: 15 October 2012
Accepted: 13 December 2012
Aims. The aim of this work is the study of the planet-metallicity and the planet-stellar mass correlations for M dwarfs from the HARPS GTO M dwarf subsample.
Methods. We use a new method that takes advantage of the HARPS high-resolution spectra to increase the precision of metallicity, using previous photometric calibrations of [Fe/H] and effective temperature as starting values.
Results. In this work we use our new calibration (rms = 0.08 dex) to study the planet-metallicity relation of our sample. The well-known correlation for giant planet FGKM hosts with metallicity is present. Regarding Neptunians and smaller hosts no correlation is found but there is a hint that an anti-correlation with [Fe/H] may exist. We combined our sample with the California Planet Survey late-K and M-type dwarf sample to increase our statistics but found no new trends.
We fitted a power law to the frequency histogram of the Jovian hosts for our sample and for the combined sample, fp = C10α [Fe/H] , using two different approaches: a direct bin fitting and a Bayesian fitting procedure. We obtained a value for C between 0.02 and 0.04 and for α between 1.26 and 2.94.
Regarding stellar mass, an hypothetical correlation with planets was discovered, but was found to be the result of a detection bias.
Key words: stars: fundamental parameters / stars: late-type / stars: low-mass / stars: atmospheres / planetary systems
Based on observations made with the HARPS instrument on the ESO 3.6-m telescope at La Silla Observatory under programme ID 072.C-0488.
Tables 2, 8, and Appendix A are available in electronic form at http://www.aanda.org
© ESO, 2013
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