when fitting. The parameters that were fit individually in each of the channels were the ratio of planet to star radius $R_{P}/R_{*}$, the second limb darkening coefficient $u2$, and the parameters defining the long time scale trend. The first limb darkening coefficient, $u1$, was held fixed in the fitting as there is a degeneracy between the limb darkening parameters which can affect the light curve solution [@Southworth2008]. The limb darkening coefficients and priors were chosen from the tables of [@Claret2011]. Uniform priors were adopted for all the model parameters, with the MCMC walkers started at the values from [@Hebrard2013].

The resulting fits of the analytic limb-darkened transit light curves are shown in Fig. \[fig:mandel\_agol\]. The strongest residual across the whole light curve in all three wavelengths is seen during transit and is consistent across the three bands. This residual is akin to the planet occulting areas of stellar activity. We considered the possibility that this anomaly could have been associated with the use of incorrect limb darkening coefficients but no choice of coefficients could replicate this feature.

Fitting of star spot model {#sec:spot_model}
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The presence of the in-transit anomaly after the fitting of limb-darkened analytic light curves motivated the 