points. To ensure we did not underestimate the noise in the light curve data, we included a Gaussian noise term in our fitting procedure, which is discussed in more detail in §\[sec:gp\].

### The PHOEBE Model {#sec:ph_model}

The  modeling software combines the complete treatment of the Roche potential with the detailed treatment of surface and horizon effects such as limb darkening, reflection and gravity brightening to derive an accurate model of the binary parameters. The current implementation uses the WD method of summing over the discrete trapezoidal surface elements, which cover the distorted stellar surfaces, to determine an accurate representation of the total observed flux and, consequently, a complete set of stellar and orbital parameters.  incorporates all the functionality of the WD code, but also provides an intuitive graphical user interface alongside many other improvements, including updated filters, PHOENIX model atmospheres [@Husser2013] and bindings that enable interfacing between  and .

To decrease the computational cost of using  with , for each iteration we created the light curve model containing 2000 data points in phase space. We then unfolded this model light curve into time space prior to adding the noise model and determining the log likelihood. This allowed the light 