the facilities and data products we are using, and in §3 we discuss the analysis techniques applied to the spectroscopy and photometry, as well as probabilistic analysis that we use to derive realistic parameter uncertainties. In §4 we present two low-mass EBs from our sample, and provide our derived orbits, masses, and radii for these systems. In §5 we discuss these systems in the context of the pre-existing population of precisely measured low-mass EBs, and describe our plans for analyzing the remainder of our [*Kepler*]{} EB sample. As part of this program, we constructed a semi-automated reduction pipeline for the HET High-Resolution Spectrograph, which we describe in Appendix A.

Facilities and Datasets\[facilities\]
=====================================

The [*Kepler*]{} Mission\[kepler\]
----------------------------------

[*Kepler*]{} is a space-borne, 0.95-m, high-precision photometer equipped with a broadband filter covering 420 nm – 865 nm. From 2009 – 2013, [*Kepler*]{} monitored a single field located $13.5^{\circ}$ above the galactic plane in the direction of Cygnus, with a mission to detect transiting, habitable-zone exoplanets [@2010Sci...327..977B]. Its ability to conduct photometry with high precision [$\sim80$ ppm for $K_p = 12$; @2010ApJ...713L..92C] and to observe with a nearly continuous cadence facilitated numerous ancillary stellar astrophysics programs, including the detection of EBs over a 