the continual use of spectra to measure the stellar masses of EBs.

Stellar models rely on the precision measurements that EBs afford for calibrating the physical parameters used in their calculations (leading to well-characterized EBs often being referred to as stellar “benchmarks”). Stars with $M > 0.8\,M_{\odot}$ generally agree with theoretical models to within observational uncertainties. Lower mass stars, however, are often observed to have radii that are 5-15% larger than model predictions . There is observational and theoretical evidence to suggest that magnetic fields could be the cause , due to interaction with the partially convective outer atmospheres and/or generation of cool starspots at polar latitudes. Unidentified opacity sources have also been suggested [@2006ApJ...644..475B], although a lack of metallicity measurements for many stars in the current EB sample has prevented an in-depth examination of that possible correlation. Models that use a different equation of state than previous works agree with observations of one low-mass [*Kepler*]{} EB [KOI-126; @2011ApJ...740L..25F], opening another regime of parameter space to explore.

In this paper we introduce the *SDSS-HET Survey of Kepler Eclipsing Binaries*, which is combining [*Kepler*]{} photometry with ground-based spectroscopy to precisely measure orbital parameters, dynamical masses and radii, and temperature ratios for 