$R$ $<$ 3% in , and 198 stars with $M$, $R$ $<$2% in DEBCat[^1], an updated version of .

Despite this steady growth in sample size, low-mass stars (defined here as $M < 0.8\,M_{\odot}$) remain a relatively small fraction of the overall sample. For example, DEBCat contains only 54 stars with $M
< 0.8\,M_{\odot}$, while the sample has only 10 such stars, none of which have orbital periods longer than five days. More recent results are starting to expand the low-mass sample [e.g., @Schwamb2013; @Gomez2014; @Zhou2015; @Dittmann2017; @Lubin2017; @Casewell2018], but a significant increase in sample size is still lacking, predominantly due to the resource expense associated with obtaining high-precision RVs (the method used to derive most of the EB dynamical masses in the current compilations), and because the poor flux ratio of a low-mass K/M dwarf orbiting a larger primary makes it difficult to detect in the optical.

Observations in the near-infrared (NIR) result in the tangible benefit of improving the flux contrast for EBs with a small mass-ratio (${\ensuremath{\mathit{q}}}={\ensuremath{\mathit{M}_B}}/{\ensuremath{\mathit{M}_A}}$). For example, the flux ratio of an M5 dwarf, with $T_{\rm{eff}}\sim3300$K to a G2 dwarf, with $T_{\rm{eff}}\sim5800$K, is $\sim10$ times more favorable in the $H$ band compared to the $V$ 