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We have measured the transmission spectrum of the extremely inflated hotJupiter WASP-52b using simultaneous photometric observations in SDSS u', g' anda filter centred on the sodium doublet (NaI) with the ULTRACAM instrumentmounted on the 4.2m William Herschel Telescope. We find that Rayleighscattering is not the dominant source of opacity within the planetaryatmosphere and find a transmission spectrum more consistent withwavelength-independent opacity such as from clouds. We detect an in-transitanomaly that we attribute to the presence of stellar activity and find thatthis feature can be more simply modelled as a bright region on the stellarsurface akin to Solar faculae rather than spots. A spot model requires asignificantly larger planet/star radius ratio than that found in previousstudies. Our results highlight the precision that can be achieved byground-based photometry with errors in the scaled planetary radii of less thanone atmospheric scale height, comparable to HST observations.

Transmission spectroscopy of the inflated exoplanet WASP-52b, and evidence for a bright region on the stellar surface