SOPHIE velocimetry of Kepler transit candidates

V. The three hot Jupiters KOI-135b, KOI-204b, and KOI-203b (alias Kepler-17b)^⋆

¹ Laboratoire d’Astrophysique de Marseille, Université Aix-Marseille & CNRS, 38 rue Frédéric Joliot-Curie, 13388 Marseille Cedex 13, France
e-mail: aldo.bonomo@oamp.fr
² Institut d’Astrophysique de Paris, UMR 7095 CNRS, Université Pierre & Marie Curie, 98bis boulevard Arago, 75014 Paris, France
³ Observatoire de Haute-Provence, Université Aix-Marseille & CNRS, 04870 St. Michel l’Observatoire, France
⁴ Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
⁵ Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Portugal
⁶ Oversky, 47 allée des Palanques, 33127 Saint Jean d’Illac, France

Received: 24 October 2011
Accepted: 17 November 2011

Abstract

We report the discovery of two new transiting hot Jupiters, KOI-135b and KOI-204b, which were previously identified as planetary candidates by the Kepler team, and independently confirm the planetary nature of Kepler-17b, recently announced by Désert et al. (2011, ApJS, 197, 14). Radial-velocity measurements, taken with the SOPHIE spectrograph at the Observatoire de Haute-Provence (France), and Kepler photometry (Q1 and Q2 data) were used to derive the orbital, stellar, and planetary parameters. KOI-135b and KOI-204b orbit their parent stars in  ~3.02 and 3.25 days, respectively. They have approximately the same radius, R_p = 1.20 ± 0.06 R_Jup and 1.24 ± 0.07 R_Jup, but different masses M_p  = 3.23 ± 0.19 M_Jup and 1.02 ± 0.07 M_Jup. As a consequence, their bulk densities differ by a factor of four, ρ_p = 2.33 ± 0.36   g   cm^-3 (KOI-135b) and 0.65 ± 0.12   g   cm^-3 (KOI-204b), meaning that their interior structures are different. All three planets orbit metal-rich stars with  [Fe/H]  ~ 0.3 dex. Our SOPHIE spectra of Kepler-17 were used both to measure the radial-velocity variations and to determine the stellar atmospheric parameters, allowing us to refine the characterisation of the planetary system. In particular we found the radial-velocity semi-amplitude and the stellar mass to be respectively slightly smaller and larger than in Désert et al. These two quantities, however, compensate and lead to a fully consistent planetary mass. Our analysis gives M_p  = 2.47 ± 0.10 M_Jup and R_p = 1.33 ± 0.04 R_Jup. We found evidence of a younger age for this planetary system, t < 1.8 Gyr, which is supported by both evolutionary tracks and gyrochronology. Finally, we confirm the detection of the optical secondary eclipse by Désert et al. and also find the brightness phase variation with the Q1 and Q2 Kepler data. The latter indicates a low redistribution of stellar heat to the night side (<16% at 1-σ), if the optical planetary occultation comes entirely from thermal flux. The geometric albedo is A_g < 0.12 (1-σ).