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Centro de Astrofísica da Universidade do Porto

Transiting exoplanets from the CoRoT space mission
XXV. CoRoT-27b: a massive and dense planet on a short-period orbit

H. Parviainen, D. Gandolfi, M. Deleuil, C. Moutou, H. J. Deeg, S. Ferraz-Mello, B. Samuel, Sz. Csizmadia, T. Pasternacki, G. Wuchterl, M. Havel, M. Fridlund, R. Angus, B. Tingley, S. Grziwa, J. Korth, S. Aigrain, J.-M. Almenara, R. Alonso, A. Baglin, S. C. C. Barros, P. Bordé, F. Bouchy, J. Cabrera, R. F. Díaz, R. Dvorak, A. Erikson, T. Guillot, A. Hatzes, G. Hébrard, T. Mazeh, G. Montagnier, A. Ofir, M. Ollivier, M. Pätzold, H. Rauer, D. Rouan, A. Santerne, J. Schneider

Abstract
Aims. We report the discovery of a massive and dense transiting planet CoRoT-27b on a 3.58-day orbit around a 4.2 Gyr-old G2 star. The planet candidate was identified from the CoRoT photometry, and was confirmed as a planet with ground-based spectroscopy.
Methods.
The confirmation of the planet candidate is based on radial velocity observations combined with imaging to rule out blends. The characterisation of the planet and its host star was carried out using a Bayesian approach where all the data (CoRoT photometry, radial velocities, and spectroscopic characterisation of the star) are used jointly. The Bayesian analysis included a study whether the assumption of white normally distributed noise holds for the CoRoT photometry and whether the use of a non-normal noise distribution offers advantages in parameter estimation and model selection.
Results.
CoRoT-27b has a mass of 10.39 ± 0.55MJup, a radius of 1.01 ± 0.04RJup, a mean density of g   cm-3, and an effective temperature of 1500 ± 130 K. The planet orbits around its host star, a 4.2 Gyr-old G2-star with a mass M = 1.06M and a radius R = 1.05R, on a 0.048 ± 0.007 AU orbit of 3.58 days. The radial velocity observations allow us to exclude highly eccentric orbits, namely, e < 0.065 with 99% confidence. Given its high mass and density, theoretical modelling of CoRoT-27b is demanding. We identify two solutions with heavy element mass fractions of 0.11 ± 0.08M and 0.07 ± 0.06M, but even solutions void of heavy elements cannot be excluded. We carry out a secondary eclipse search from the CoRoT photometry using a method based on Bayesian model selection, but conclude that the noise level is too high to detect eclipses shallower than 9% of the transit depth. Using a non-normal noise model was shown not to affect the parameter estimation results, but led to significant improvement in the sensitivity of the model selection process.

Keywords
planets and satellites: detection – stars: individual: CoRoT-27 – techniques: photometric – techniques: radial velocities – techniques: spectroscopic – methods: statistical

Astronomy and Astrophysics
Volume 562, Page A140_1
February 2014

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