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Centro de Astrofísica da Universidade do Porto

Metallicity of M dwarfs
II. A comparative study of photometric metallicity scales

V. Neves, X. Bonfils, N. C. Santos, X. Delfosse, T. Forveille, F. Allard, C. Natário, C. S. Fernandes, S. Udry

Stellar parameters are not easily derived from M dwarf spectra, which are dominated by complex bands of diatomic and triatomic molecules and do not agree well with the individual line predictions of atmospheric models. M dwarf metallicities are therefore most commonly derived through less direct techniques. Several recent publications propose calibrations that provide the metallicity of an M dwarf from its Ks band absolute magnitude and its V - Ks color, but disagree at the ±0.1 dex level. We compared these calibrations using a sample of 23 M dwarfs, which we selected as wide (> 5 arcsec) companions of F-, G-, or K- dwarfs with metallicities measured on a homogeneous scale and which we require to have V band photometry measured to better than ∼0.03 magnitude. We find that the Schlaufman & Laughlin (2010, A&A, 519, A105) calibration has the lowest offsets and residuals against our sample, and used our improved statistics to marginally refine that calibration. With more strictly selected photometry than in previous studies, the dispersion around the calibration is well in excess of the [Fe/H] and photometric uncertainties. This suggests that the origin of the remaining dispersion is astrophysical rather than observational.

stars: late-type – stars: fundamental parameters – binaries: general – planetary systems – stars: atmospheres

Based on observations collected with the FEROS spectrograph at la Silla observatory under ESO programs 073.D-0802(A), 074.D-0670(A), 078.D-0760(A), and with the ELODIE and SOPHIE spectrographs at the Observatoire de Haute Provence.

Astronomy and Astrophysics
Volume 538, Page A25_1
February 2012

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