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ABSTRACT  As part of the long‐term radial velocity monitoring of known transiting planets, we have acquired new radial velocity data for the two transiting systems WASP‐12 and WASP‐14, each harbouring a gas giant on a close orbit (orbital period of 1.09 and 2.24 d, respectively). In both cases, the initial orbital solution suggested a significant orbital eccentricity, 0.049 ± 0.015 for WASP‐12b and 0.091 ± 0.003 for WASP‐14b. Since then, measurements of the occultation of WASP‐12 in the infrared have indicated that one projection of the eccentricity (  e  cos ω ) was close to zero, casting doubt on the eccentricity from the initial radial velocity orbit. Our measurements show that the radial velocity data are compatible with a circular orbit. A MCMC analysis taking into account the presence of correlated systematic noise in both the radial velocity and photometric data gives   e = 0.017 +0.015  −0.010  . In contrast, we confirm the orbital eccentricity of WASP‐14b, and refine its value to   e = 0.0877 ± 0.0030 , a 10σ detection. WASP‐14b is thus the closest presently known planet with a confirmed eccentric orbit.

Orbital eccentricity of WASP‐12 and WASP‐14 from new radial velocity monitoring with SOPHIE ★