radii – $k = R_2/R_1$; the surface brightness ratio in the Kepler band – $S_{\rm Kp}$; the orbital inclination, $i$; the time of primary eclipse – $T_0$; the orbital period – $P$; $f_s = \sqrt{e}\sin(\omega)$ and $f_c = \sqrt{e}\cos(\omega)$, where $e$ is the orbital eccentricity and $\omega$ is the longitude of periastron; and “third light” – $\ell_3$.

We use $f_s$ and $f_c$ as parameters because a uniform prior probability distribution for these parameters corresponds to a uniform prior probability distribution for $e$. We use a quadratic limb-darkening law for both stars with priors on the coefficients calculated using [ldtk]{} [@2015MNRAS.453.3821P] based on the spherical model atmospheres by . To calculate these priors we assume $\log g =4.3
\pm 0.3$ and \[Fe/H\]$ = 0.0 \pm 0.2$ for all stars and effective temperature estimates from a preliminary analysis very similar to those derived in below in Section \[TeffSection\]. The standard error estimates on the coefficients inherited from the assumed errors on T$_{\rm eff}$, $\log g$ and \[Fe/H\] are likely to be underestimates of the true uncertainties since they do not account for systematic errors in the models and other issues with estimating limb darkening coefficients from models [@2011MNRAS.418.1165H]. To allow for this 