J. -M. Almenara, C. Damiani, F. Bouchy, M. Havel, G. Bruno, G. Hébrard, R. F. Díaz, M. Deleuil, S. C. C. Barros, I. Boisse, A. S. Bonomo, G. Montagnier, A. Santerne

Abstract
We report the validation and characterization of three new transiting exoplanets using SOPHIE radial velocities: KOI-614b, KOI-206b, and KOI-680b. KOI-614b has a mass of 2.86 ± 0.35 M_Jup and a radius of 1.13 ^+0.26_-0.18 R_Jup, and it orbits a G0, metallic ([ Fe/H ] = 0.35 ± 0.15) dwarf in 12.9 days. Its mass and radius are familiar and compatible with standard planetary evolution models, so it is one of the few known transiting planets in this mass range to have an orbital period over ten days. With an equilibrium temperature of T_eq = 1000 ± 45 K, this places KOI-614b at the transition between what is usually referred to as “hot” and “warm” Jupiters. KOI-206b has a mass of 2.82 ± 0.52 M_Jup and a radius of 1.45 ± 0.16 R_Jup, and it orbits a slightly evolved F7-type star in a 5.3-day orbit. It is a massive inflated hot Jupiter that is particularly challenging for planetary models because it requires unusually large amounts of additional dissipated energy in the planet. On the other hand, KOI-680b has a much lower mass of 0.84 ± 0.15 M_Jup and requires less extra-dissipation to explain its uncommonly large radius of 1.99 ± 0.18 R_Jup. It is one of the biggest transiting planets characterized so far, and it orbits a subgiant F9-star well on its way to the red giant stage, with an orbital period of 8.6 days. With host stars of masses of 1.46 ± 0.17 M_⊙ and 1.54 ± 0.09 M_⊙, respectively, KOI-206b, and KOI-680b are interesting objects for theories of formation and survival of short-period planets around stars more massive than the Sun. For those two targets, we also find signs of a possible distant additional companion in the system.

Keywords
planetary systems, techniques: photometric, techniques: radial velocities, techniques: spectroscopic

Astronomy & Astrophysics
Volume 575, Number of pages A71
2015 March

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