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tokens: dwarf—M dwarf eclipsing binaries. We drew sample 1 from Henry McCarthy ( 1993 ), Delfosse et al. ( 2000 ), and Benedict et al. ( 2016 ), excluding those in our calibration sample (Section 2 ). We added one target, GJ 2005A, for which the BC pair was analyzed in this paper, but Seifahrt et al. ( 2008 ) provide a mass determination for the A component. For sample 2, we drew eclipsing binaries from the compilations of Hartman et al. ( 2011 ) and Parsons et al. ( 2018 ), restricting the sample to double-lined eclipsing binaries, those with individual mass estimates better than 5%, and systems with a parallax from the second Gaia data release passing the Gaia quality cuts given in Appendix C of Lindegren et al. ( 2018 ). We removed 19e-3-08413AB because the distance is too large (≫500 pc) to assume zero reddening and excluded systems from Kraus et al. ( 2011 ) because they have no reported flux or luminosity ratios, which are needed to estimate Δ K S (detailed below). Lastly, we removed PTFEB132+19AB (Kraus et al. 2017 ) because it is young (≃650 Myr). In total this gives us individual masses for 29 stars with which to test our – M * relation. A significant advantage of eclipsing binaries is that we could adopt the much more precise parallaxes from Gaia , as they all have orbits that are too tight to show detectable centroid motion. For the astrometric binaries/triples, we drew parallaxes either from Gaia DR2 parallaxes of nearby companions (e.g., for Gl 644ABC we used the Gaia parallax from the wider companion Gl 643) or from sources that accounted for the high-order nature of the system. As with binaries analyzed in this paper, unresolved K S values were taken from 2MASS. We used AO data from VLT/NaCo to derive Δ K for Gl 866AC-B and our own Keck/NIRC2 measurements for Gl 644A-BC and GJ 2005A-B-C (all three are resolved), just as was done for binaries analyzed in this paper. For other systems, including unresolved components of the triples (Gl 866A-C and Gl 644B-C), the literature only provided contrast ratios in optical bands. We converted these to Δ K S using the synthetic and observed magnitudes given in Mann et al. ( 2015 ), following a procedure analogous to that outlined in Kraus et al. ( 2017 ). To briefly summarize, we found the combination of two single-star spectral templates that reproduced both the unresolved spectral energy distribution ( Gaia and 2MASS photometry) and the measured contrast(s) from the literature reference (usually V , R , or Kepler ) and then computed a Δ K S value for the best-fit template combination. This is similar to our conversion of Δ K X to Δ K S detailed in Appendix A . Correction from optical to NIR contrasts depends on metallicity (e.g., Schlaufman Laughlin 2010 ), and precise metallicities of these systems were not known. Instead, we assumed that all systems were −0.6 [Fe/H] +0.4, and we adopted uncertainties that encompass the range of values due to unknown metallicity. Errors introduced from these