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One of the main atmospheric features in exoplanet atmospheres, detectableboth from ground- and space-based facilities, is Rayleigh scattering. Inhydrogen-dominated planetary atmospheres, Rayleigh scattering causes themeasured planetary radius to increase toward blue wavelengths in the opticalrange. We obtained a spectrophotometric time series of one transit of theSaturn-mass planet WASP-69b using the OSIRIS instrument at the Gran TelescopioCanarias. From the data we constructed 19 spectroscopic transit light curvesrepresenting 20 nm wide wavelength bins spanning from 515 nm to 905 nm. Wederived the transit depth for each curve individually by fitting an analyticalmodel together with a Gaussian process to account for systematic noise in thelight curves. We find that the transit depth increases toward bluerwavelengths, indicative of a larger effective planet radius. Our results areconsistent with space-based measurements obtained in the near infrared usingthe Hubble Space Telescope, which show a compatible slope of the transmissionspectrum. We discuss the origin of the detected slope and argue between twopossible scenarios: a Rayleigh scattering detection originating in the planet'satmosphere or a stellar activity induced signal from the host star.

The GTC exoplanet transit spectroscopy survey XI. Possible detection of Rayleigh scattering in the atmosphere of the Saturn-mass planet WASP-69b