SOPHIE velocimetry ofKeplertransit candidates

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.

HAT-P-67b: An Extremely Low Density Saturn Transiting an F-subgiant Confirmed via Doppler Tomography∗

“…A number of other inflated gas giants have been discovered around subgiants (KOI-680b, Almenara et al 2015;EPIC 206247743b, Van Eylen et al 2016;KELT-8b, Fulton et al 2015;KELT-11b, Pepper et al 2016; and HAT-P-65b and HAT-P-66b, Hartman et al 2016) and giants (e.g., EPIC 211351816b, Grunblatt et al 2016). One hypothesis is that these gas giants are reinflated by the evolved host star (Lopez & Fortney 2016).…”

SOPHIE velocimetry ofKeplertransit candidates

“…Almenara et al 2015;Bonomo et al 2015). These stellar parameters were derived using either the MOOG (as described above) or the VWA software.…”

“…Another example is the inflation of some giant, highly irradiated planets that could not be modelled with reasonable physical ingredients (e.g. Almenara et al 2015).…”

K2-60b and K2-107b. A Sub-Jovian and a Jovian Planet from the K2 Mission

“…The planet orbits an F9 star about to leave the main sequence. It is one of only a few transiting planets known to orbit sub-giants (e.g., Almenara et al 2015;Pepper et al 2016;Smith et al 2016;Van Eylen et al 2016). The planet's calculated effective temperature is 1780±90 K, its radius is 1.44±0.15R Jup , and its mass is 0.84±0.08M Jup .…”