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SOPHIE velocimetry of Kepler transit candidates XIV. A joint
photometric, spectroscopic, and dynamical analysis of the Kepler-117 system
release_6og7qr2hwbdnzitnql4y3676we
by
G. Bruno,
J.-M. Almenara,
S. C. C. Barros,
A. Santerne,
R. F. Diaz,
M.
Deleuil,
C. Damiani,
A. S. Bonomo,
I. Boisse,
F. Bouchy,
G. Hebrard,
G.
Montagnier
Released
as a article
.
2015
Abstract
As part of our follow-up campaign of Kepler planets, we observed Kepler-117
with the SOPHIE spectrograph at the Observatoire de Haute-Provence. This
F8-type star hosts two transiting planets in non-resonant orbits. The planets,
Kepler-117 b and c, have orbital periods ≃ 18.8 and ≃ 50.8 days,
and show transit-timing variations (TTVs) of several minutes. We performed a
combined Markov chain Monte Carlo (MCMC) fit on transits, radial velocities,
and stellar parameters to constrain the characteristics of the system. We
included the fit of the TTVs in the MCMC by modeling them with dynamical
simulations. In this way, consistent posterior distributions were drawn for the
system parameters. According to our analysis, planets b and c have notably
different masses (0.094 ± 0.033 and 1.84 ± 0.18 M_ J) and low
orbital eccentricities (0.0493 ± 0.0062 and 0.0323 ± 0.0033). The
uncertainties on the derived parameters are strongly reduced if the fit of the
TTVs is included in the combined MCMC. The TTVs allow measuring the mass of
planet b, although its radial velocity amplitude is poorly constrained.
Finally, we checked that the best solution is dynamically stable.
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