chose to use <span style="font-variant:small-caps;">spotrod</span> due to the speed of its integration, which uses polar coordinates in the projection plane. The integration with respect to the polar coordinate is done analytically so that only the integration with respect to the radial coordinate needs to be performed numerically. To calculate the projection of the planet on the stellar surface, <span style="font-variant:small-caps;">spotrod</span> calculates the arrays of planar orbital elements $\xi$ and $\eta$, using the formalism of [@Pal2009], and assumes the same limb darkening law for the spot as for the star.

The system parameters were again fit across the three light curves simultaneously (although this time fitting for impact parameter, $b$, rather than the inclination, as required by <span style="font-variant:small-caps;">spotrod</span>) and with the addition of the parameters defining the spots. The fitting of one spot was tested but was unable to fit both bumps on either side of the transit mid-point, therefore two spots were used in further analysis. The parameters defining each spot were the longitude, latitude, radius ratio of spot to star, and ratio of the spot flux to stellar flux (with 1 being a spot with the same flux as the pristine photosphere and 0 being a spot with 