from the spot model but find this would require a total dimming of the star of 12%, which we consider unlikely. This is discussed in more detail in section \[sec:unocculted\].

We conclude that the comparison of our planet/star radius ratios with independent studies strongly favours the presence of a facula in our observed transit. Nevertheless, in sections \[sec:spot\_properties\] and \[sec:facula\_properties\] we discuss the implications of both models.

### Spot properties {#sec:spot_properties}

The best fitting spot model indicates two large regions of stellar activity (Fig. \[fig:stellar\_surface\], left panel) which are consistent with the majority of the in-transit data being activity affected (Fig. \[fig:spots\]).

Although spot modelling codes, including <span style="font-variant:small-caps;">spotrod</span>, fit spots as circular areas on the stellar surface, in reality these may be areas of several small spots which may be arranged in more complex configurations on the stellar surface. If the features in our light curves really were single spots with temperatures consistent with those expected for K stars, we would expect to see large amplitude bumps and a strong colour dependence. When considering the spots resulting from our modelling however, we believe that the spots are more accurately interpreted as active regions, with spots and pristine photosphere contained 