also allowed for a larger, less dark spot.

![image](wasp52_fit_spot.pdf)

![image](stellar_surface_gband.pdf) ![image](filling_factor.pdf)

Fitting of bright region model {#sec:facula_model}
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As an alternative interpretation, the in-transit anomaly was also modelled as a bright feature analogous to Solar faculae. Solar faculae are bright regions on the solar photosphere which display limb brightening behaviour (e.g. @Unruh1999). They are often co-spatial with sunspots but not perfectly so (e.g. @Haywood2016).

The effects of occultations of bright regions in exoplanet transits have been discussed by [@Oshagh2014] and could lead to an observable anomaly in transit data. There has not yet been any conclusive evidence of a facula occultation in a transit light curve although [@Mohler2013] found evidence for a hot spot in GROND photometry of HATS-2b. They detected a bright feature in the Sloan-$g$ band, which covered the CaII lines, that was consistent with a chromospheric plage occultation.

<span style="font-variant:small-caps;">spotrod</span> was also used to model the facula scenario but instead of two individual spots with flux ratios $<1$, a single feature was modelled with a flux ratio of $>1$. This fitting method produced the fits seen in Fig. \[fig:plages\] with the results in Table \[tab:fit\_results\]. This model was able to reproduce the in-transit anomaly with an equally 