SOPHIE velocimetry ofKeplertransit candidates

Abstract

We report the discovery of a new hot-Jupiter, , transiting a solar-type star with an orbital period of 1.855558 days ± 0.6 s thanks to public photometric data from the Kepler space mission and new radial velocity observations obtained by the SOPHIE spectrograph mounted on the 1.93-m telescope at the Observatoire de Haute-Provence, France. The planet , with a radius of 0.89 ± 0.05 R Jup and a mass of 0.55 ± 0.09 M Jup , orbits a G6V star with R = 1.02 ± 0.03 R , M = 1.12 ± 0.07 M , [Fe/H] = 0.29 ± 0.16 dex, T eff = 5620 ± 140 K, and an age of 650 +2500 −300 Myr. KOI-196b is one of the rare close-in hot Jupiters with a radius smaller than Jupiter suggesting that it is a non-inflated planet. The high precision of the Kepler photometry permits us to detect the secondary transit with a depth of 64 +10 −12 ppm as well as the optical phase variation. We find a geometric albedo of A g = 0.30 ± 0.08, which is higher than most of the transiting hot Jupiters with a measured A g . Assuming no heat recirculation, we find a day-side temperature of T day = 1730 ± 400 K. The planet KOI-196b seems to be one of the rare hot Jupiters located in the short-period hot-Jupiter desert.

SOPHIE velocimetry ofKeplertransit candidates

“…Such precision is the minimum needed to significantly detect the RV signal of a Jupitermass planet with orbital periods of up to a few tens of days (e.g. Santerne et al 2011bSanterne et al , 2014.…”

“…Following Santerne et al (2014), we also corrected instrumental drifts in the RV using the ones measured on the constant star HD 185144 on the same nights. The RV we used for this correction are listed in Table D.1.…”

“…Comparison between the two on some targets have shown no significant differences (e.g. Santerne et al 2014). These stellar parameters are also available in SWEET-Cat 5 .…”

“…Lillo-Box et al 2014) can unveil close-by companions. However, to firmly establish their planetary nature, one has to detect their Doppler signature or use statistical methods (also known as planet-validation, see Santerne et al 2014, for an illustration of both methods). To correctly interpret the transit detections, follow-up observations are therefore needed, especially for the population of giant exoplanets.…”

SOPHIE velocimetry ofKeplertransit candidates XI. Kepler-412 system: probing the properties of a new inflated hot Jupiter

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