OGLE2-TR-L9b: an exoplanet transiting a rapidly rotating F3 star

Context. The photometric observations of the OGLE-II microlens monitoring campaign have been taken in the period 1997-2000. All light curves of this campaign have recently become public. Our analysis of these data has revealed 13 low-amplitude transiting objects among similar to 15700 stars in three Carina fields towards the Galactic disk. One of these objects, OGLE2-TR-L9 (P similar to 2.5 days), turned out to be an excellent transiting-planet candidate. Aims. We report on our investigation of the true nature of OGLE2-TR-L9. By re-observing the photometric transit, we attempt to determine the transit parameters to high precision, and, by spectroscopic observations, to estimate the properties of the host star and determine the mass of the transiting object by means of radial-velocity measurements. Methods. High precision photometric observations were obtained in g', r', i', and z' band simultaneously, using the new GROND detector, mounted on the MPI/ESO 2.2 m telescope at La Silla. Eight epochs of high-dispersion spectroscopic observations were obtained using the fiber-fed FLAMES/UVES Echelle spectrograph, mounted on ESO's Very Large Telescope at Paranal. Results. The photometric transit, now more than 7 years after the last OGLE-II observations, was re-discovered only similar to 8 min from its predicted time. The primary object is a rapidly rotating F3 star with v sin i = 39.33 +/- 0.38 km s(-1), T = 6933 +/- 58 K, log g = 4.25 +/- 0.01, and [Fe/H] = -0.05 +/- 0.20. The transiting object is an extrasolar planet with M(p) = 4.5 +/- 1.5 M(Jup) and R(p) = 1.61 +/- 0.04 R(Jup). Since this is the first planet detected orbiting a fast rotating star, the uncertainties in both the radial-velocity measurements and the planetary mass are larger than for most other planets discovered to date. The rejection of possible blend scenarios was based on a quantitative analysis of the multi-color photometric data. A stellar-blend scenario of an early F-star with a faint eclipsing-binary system is excluded, due to 1) the consistency between the spectroscopic parameters of the star and the mean density of the transited object as determined from the photometry, and 2) the excellent agreement between the transit signal as observed at four different wavelengths.