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The relativley large spread in the derived metallicities ([Fe/H]) of M dwarfsshows that various approaches have not yet converged to consistency. Thepresence of strong molecular features, and incomplete line lists for thecorresponding molecules have made metallicity determinations of M dwarfsdifficult. Furthermore, the faint M dwarfs require long exposure times for asignal-to-noise ratio sufficient for a detailed spectroscopic abundanceanalysis. We present a high-resolution (R~50,000) spectroscopic study of asample of eight single M dwarfs and three wide-binary systems observed in theinfrared J-band. The absence of large molecular contributions allow for aprecise continuum placement. We derive metallicities based on the best fitsynthetic spectra to the observed spectra. To verify the accuracy of theapplied atmospheric models and test our synthetic spectrum approach, threebinary systems with a K-dwarf primary and an M-dwarf companion were observedand analysed along with the single M dwarfs. We obtain a good agreement betweenthe metallicities derived for the primaries and secondaries of our testbinaries and thereby confirm the reliability of our method of analysing Mdwarfs. Our metallicities agree well with certain earlier determinations, anddeviate from others. We conclude that spectroscopic abundance analysis in the Jband is a reliable method for establishing the metallicity scale for M dwarfs.We recommend its application to a larger sample covering lower as well ashigher metallicities. Further prospects of the method include abundancedeterminations for individual elements.

M-dwarf metallicities - A high-resolution spectroscopic study in the near infrared