) is a unique transiting hot Jupiter. It is one of very few known shortperiod planets orbiting a hot A-type star, making it one of the hottest planets currently known. The availability of Kepler data allows us to measure the planet's occultation (secondary eclipse) and phase curve in the optical, which we combine with occultations observed by warm Spitzer at 4.5 µm and 3.6 µm and a ground-based occultation observation in the K s band (2.1 µm). We derive a day-side hemisphere temperature of 2,750±160 K as the effective temperature of a black body showing the same occultation depths. Comparing the occultation depths with one-dimensional planetary atmosphere models suggests the presence of an atmospheric temperature inversion. Our analysis shows evidence for a relatively high geometric albedo, A g = 0.33 +0.04 −0.06 . While measured with a simplistic method, a high A g is supported also by the fact that the one-dimensional atmosphere models underestimate the occultation depth in the optical. We use stellar spectra to determine the dilution, in the four wide bands where occultation was measured, due to the visual stellar binary companion 1. ′′ 15±0. ′′ 05 away. The revised stellar parameters measured using these spectra are combined with other measurements leading to revised planetary mass and radius estimates of M p = 4.94-8.09 M J and R p = 1.406±0.038 R J . Finally, we measure a Kepler mid-occultation time that is 34.0±6.9 s earlier than expected based on the mid-transit time and the delay due to light travel time, and discuss possible scenarios.

Aims. We examined which exo-systems contain moons that may be detected in transit. Methods. We numerically modeled transit light curves of Earth-like and giant planets that cointain moons with 0.005-0.4 Earth-mass. The orbital parameters were randomly selected, but the entire system fulfilled Hill-stability. Results. We conclude that the timing effect is caused by two scenarios: the motion of the planet and the moon around the barycenter. Which one dominates depends on the parameters of the system. Already planned missions (Kepler, COROT) may be able to detect the moon in transiting extrasolar Earth-Moon-like systems with a 20% probability. From our sample of 500 free-designed systems, 8 could be detected with the photometric accuracy of 0.1 mmag and a 1 min sampling, and one contains a stony planet. With ten times better accuracy, 51 detections are expected. All such systems orbit far from the central star, with the orbital periods at least 200 and 10 days for the planet and the moon, while they contain K-and M-dwarf stars. Finally we estimate that a few number of real detections can be expected by the end of the COROT and the Kepler missions.