to 0.01. The Matern 3/2 function was selected as it is capable of modeling the noise, stellar variations and instrumental systematics in the light curve using only two parameters, $\sigma$ and $\rho$.

We additionally incorporated a white noise term into our model. The purpose of this term is to ensure that our uncertainties are well estimated. Poorly estimated uncertainties lead to higher values for the jitter term (high in relation to the associated noise level) and the addition of white noise of the form:

$$\label{eqn:noise}
k(\tau_{n,m}) = \sigma^2\delta_{n,m},$$

where $\sigma$ is a tunable parameter.

Masses and Radii for two Example [*Kepler*]{} EBs\[solvedebs\]
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Here we describe the results of KIC 2445134 and KIC 3003991 to demonstrate the pipeline introduced in §\[analysis\]. These objects were selected as they are total eclipsers, have small [$\mathit{q}$]{}, and the data are adequate to derive precise masses and radii.

KIC 2445134
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KIC 2445134 is comprised of an F-type dwarf primary and an M-type secondary in an 8.4 day period, and has a flux ratio of $\sim0.01$ in the [*Kepler*]{} bandpass. It has a [*Kepler*]{} magnitude of 13.55 and an H-band magnitude of 12.40. We obtained six observations of KIC 2445134 with the HRS, which 