across channels fixed to the results from the first run ($a/R_{*}$, $b$, $T_{0}$ and the spot sizes and positions). Correlations with these parameters cause $R_{P}/R_{*}$ to move up and down together across the three wavelengths, contributing to the uncertainty in the absolute planetary radius in each of the bands. Since we are concerned with the shape of the transmission spectrum, we are interested in the relative radii between the bands and not the absolute planetary radius, thus motivating the second run of the MCMC with fixed system parameters.

We present the best fitting spot model in Fig. \[fig:spots\], after the second MCMC run, with the results in Table \[tab:fit\_results\] and transmission spectrum in Fig. \[fig:trans\_spec\] (blue squares).

With the sizes and contrasts calculated from <span style="font-variant:small-caps;">spotrod</span>, we were able to create a schematic of the stellar surface (Fig. \[fig:stellar\_surface\], left panel) and consider what filling factor would reproduce the derived contrasts (section \[sec:spot\_properties\] and Fig. \[fig:stellar\_surface\], right panel). This figure displays the large regions of stellar activity along the transit chord. The second spot crossing event comprises of a smaller region of higher contrast (0.2 in the $g'$ band, Table \[tab:fit\_results\]). The error in the contrast of this dark spot 