components, $B_A$ and $B_B$, respectively, in Table \[orbpar2445134\]. Our measurement of the mass ratio, ${\ensuremath{\mathit{q}}}=0.411\pm0.001$, has a precision of better than 1%. Our derived masses (${\ensuremath{\mathit{M}_A}}=1.29\pm0.03\,{\ensuremath{\mathit{\,M_\odot}}}$, ${\ensuremath{\mathit{M}_B}}=0.53\pm0.01\,{\ensuremath{\mathit{\,M_\odot}}}$) and radii (${\ensuremath{\mathit{R}_A}}=1.42\pm0.01\,{\ensuremath{\mathit{\,R_\odot}}}$, ${\ensuremath{\mathit{R}_A}}=0.510\pm0.004\,{\ensuremath{\mathit{\,R_\odot}}}$) have measurement precisions of 1% or better, except for the primary mass which is constrained to 2%.

To assess the dependency of the parameter uncertainties on our light-curve per-point uncertainties, we ran our software in the same manner as outlined above, but with the uncertainties multiplied by 0.5 and 2 for KIC2445134. The outcome was that all fundamental parameters remained within the one sigma uncertainties quoted and the uncertainties were unchanged with the exception of the secondary radius uncertainty, which changed from 0.004${\ensuremath{\mathit{\,R_\odot}}}$ to 0.005${\ensuremath{\mathit{\,R_\odot}}}$ (still providing a 1% uncertainty) for the case of the increased per-point uncertainties.

KIC 3003991
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KIC 3003991 represents the faint end of our EB sample, with [*Kepler*]{} mag = 13.9, and is comprised of a late G-star and a mid M-star in a 7.2 day orbit with a [*Kepler*]{} flux ratio of $\sim$0.005. We obtained six observations with HRS and six observations with APOGEE. Once again, we were able to easily detect the low mass companion in the H-band spectra, with $\alpha\sim0.10$, and 