Volume 568, August 2014
|Number of page(s)||22|
|Published online||04 September 2014|
Metallicity of M dwarfs
IV. A high-precision [Fe/H] and Teff technique from high-resolution optical spectra for M dwarfs ⋆,⋆⋆,⋆⋆⋆
1 Departamento de Física, Universidade Federal do Rio Grande do Norte, 59072-970 Natal, RN, Brazil
2 Centro de Astrofísica and Faculdade de Ciências, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
3 Univ. Grenoble Alpes, IPAG, 38000 Grenoble, France
4 CNRS, IPAG, 38000 Grenoble, France
5 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
6 Observatoire de Genève, Université de Genève, 51 chemin des Maillettes, 1290 Sauverny, Switzerland
Received: 6 May 2014
Accepted: 23 June 2014
Aims. In this work we develop a technique to obtain high precision determinations of both metallicity and effective temperature of M dwarfs in the optical.
Methods. A new method is presented that makes use of the information of 4104 lines in the 530–690 nm spectral region. It consists in the measurement of pseudo equivalent widths and their correlation with established scales of [Fe/H] and Teff.
Results. Our technique achieves a rms of 0.08 ± 0.01 for [Fe/H], 91 ± 13 K for Teff, and is valid in the (−0.85,0.26 dex), (2800, 4100 K), and (M0.0, M5.0) intervals for [Fe/H], Teff and spectral type respectively. We also calculated the RMSEV which estimates uncertainties of the order of 0.12 dex for the metallicity and of 293 K for the effective temperature. The technique has an activity limit and should only be used for stars with log LHα/Lbol< − 4.0.
Key words: stars: atmospheres / stars: fundamental parameters / stars: late-type / stars: low-mass / methods: data analysis
© ESO, 2014
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