Contribution of reflected light to the total planetary flux for different grey geometric albedos as a function of wavelength. For the stellar emission spectrum a PHOENIX model (Husser et al. 2013) with the parameters T_eff = 5000 K, [M/H] = 0.0, and log g = 4.5 was used. To model the planetary atmosphere an irradiated atmosphere model provided by Mollière et al. (2015) with the parameters T_eff = 1250 K, [Fe/H] = 0.0, [C/O] = 0.70, planetary log g = 3.0, and stellar spectral type K5 was adopted. The thermal emission from the planet was extrapolated from the dayside temperature of 1192 ± 9 K, estimated with occultation measurements in the Spitzer 4.5 μm channel (Knutson et al. 2012).