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Metallicity is a fundamental parameter that contributes to the physicalcharacteristics of a star. However, the low temperatures and complex moleculespresent in M dwarf atmospheres make it difficult to measure their metallicitiesusing techniques that have been commonly used for Sun-like stars. Althoughthere has been significant progress in developing empirical methods to measureM dwarf metallicities over the last few years, these techniques have beendeveloped primarily for early- to mid-M dwarfs. We present a method to measurethe metallicity of mid- to late-M dwarfs from moderate resolution (R~2000)K-band (2.2 microns) spectra. We calibrate our formula using 44 wide binariescontaining an F, G, K, or early M primary of known metallicity and a mid- tolate-M dwarf companion. We show that similar features and techniques used forearly M dwarfs are still effective for late-M dwarfs. Our revised calibrationis accurate to 0.07 dex for M4.5-M9.5 dwarfs with -0.58<[Fe/H]<+0.56 and showsno systematic trends with spectral type, metallicity, or the method used todetermine the primary star metallicity. We show that our method givesconsistent metallicities for the components of M+M wide binaries. We verifythat our new formula works for unresolved binaries by combining spectra ofsingle stars. Lastly, we show that our calibration gives consistentmetallicities with the Mann et al. (2013a) study for overlapping (M4-M5) stars,establishing that the two calibrations can be used in combination to determinemetallicities across the entire M dwarf sequence.

Prospecting in Ultracool Dwarfs: Measuring the Metallicities of Mid- and Late-M Dwarfs