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While the planet-metallicity correlation for FGK main-sequence stars hostinggiant planets is well established, the results are not so clear for M-dwarfstars, for which precise metallicity measurements are not straightforward.However, new techniques using near infrared spectra show promising results.Using these, we determine stellar parameters and metallicities for a sample of16 M-dwarf stars, 11 of which host planets, with near-infrared spectra from theGemini Near-Infrared Spectrograph (GNIRS). We find that M-dwarfs with planetsare preferentially metal-rich compared to those without planets. This result,based on GNIRS spectra, is supported by the analysis of a relatively largersample of M stars with planets (18 in total) and a control sample of 213 Mstars without known planets, obtained from the catalogue of Terrien et al.(2015). This, on the one hand, coincides with the trend (not only for M- butalso for solar-type stars) reported in the literature and, on the other hand,demonstrates the utility of GNIRS spectra to obtain reliable stellar parametersof M stars. We also find that M dwarfs that harbor giant planets arepreferentially more metallic than those associated with low-mass planets(Neptune or super-Earth type). This trend also agrees with that previouslyreported for solar-type stars. These results would favor the core accretionmodel for planetary formation.

Testing the Planet-Metallicity Correlation in M-dwarfs with Gemini GNIRS Spectra