curve to be computed in a relatively short amount of time, but fit the model of the light curve combined with the instrumental and stellar trends to the complete data set.

The light curve and radial velocity data were fit simultaneously. Within our models, we fit the following parameters: inclination, $i$; eccentricity, $e$; argument of periastron, the angle from the ascending node to periastron, measured in the direction of motion, $\omega$; the primary and secondary potentials, proportional to the inverse radius, $\Omega_1$ and $\Omega_2$, respectively; third light $l3$; gamma velocity, the motion of the center of mass of the binary, $\gamma$; mass ratio, $q$; and semi-major axis, $sma$. We further set the albedos (reflective properties of the stars) and gravity darkening exponents (which relate to the change in temperature of the stars due to their obliquity), to the theoretical values of $A$=0.6 [@Rucinski1969b] and $\beta$=0.32 [@Lucy1967] for stars with convective envelopes ($T_\mathrm{eff} < 7000$K) and $A$=1.0 [@Rucinski1969a] and $\beta$=1.0 [@vonZeipel1924] for stars with radiative envelopes ($T_\mathrm{eff} > 7000$K). As @Diaz-Cordoves1992 showed that the square-root limb darkening model is preferable for objects that radiate towards the IR, we applied the square-root limb darkening law to our models and updated the limb-darkening 