band.

This allows for the extraction of measured RVs from fainter secondary stars, and therefore extends the lower limit on [$\mathit{q}$]{} for which masses of dwarf stars can be derived. While optical spectra tend to lose sensitivity at $q \sim 0.5$, NIR spectra can push down to $q \sim 0.1$ [@Prato2002; @2003ApJ...599.1344M; @2008ApJ...689..416B].

Measurements of select bright binaries have achieved mass ratio precisions of 0.02-0.42% (in $M\sin{i}$) [@2010ApJ...719.1293K], but precisions of 1-3% are still sufficient to distinguish between model parameters [@2010ApJ...718..502M]. The high photometric precision of [*Kepler*]{} makes it possible to determine the masses of some EBs purely photometrically [@2011Sci...331..562C; @2012ApJ...746..185F] via Doppler boosting and ellipsoidal effects [@2011MNRAS.415.3921F]. While the technique is promising, @2011Sci...331..562C achieved only a 10% mass precision using the [*Kepler*]{} photometry alone (i.e., without including any spectroscopic RVs), while @2012ApJ...746..185F found that only 5 of their 7 binaries had RV semi-amplitudes in agreement with those predicted from their photometric analysis. In a large follow-up program, @talor2015 observed 281 targets, confirming 70 binary systems while finding many of their false positives were due to pulsating red giants. The use of spectroscopic RVs therefore remains an essential and reliable method for obtaining mass precisions at the 1-3% level, motivating 