Improved parameters of seven Kepler giant companions characterized with SOPHIE and HARPS-N

被引:51
作者
Bonomo, A. S. [1 ]
Sozzetti, A. [1 ]
Santerne, A. [2 ]
Deleuil, M. [3 ]
Almenara, J. -M. [3 ]
Bruno, G. [3 ]
Diaz, R. F. [4 ]
Hebrard, G. [5 ,6 ,7 ]
Moutou, C. [3 ]
机构
[1] INAF Osservatorio Astron Torino, I-10025 Pino Torinese, Italy
[2] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, P-4150762 Oporto, Portugal
[3] Aix Marseille Univ, CNRS, LAM Lab Astrophys Marseille UMR 7326, F-13388 Marseille, France
[4] Univ Geneva, Observ Astron, CH-1290 Versoix, Switzerland
[5] Univ Aix Marseille, Observ Haute Provence, F-04870 St Michel lObservatoire, France
[6] CNRS, F-04870 St Michel lObservatoire, France
[7] Univ Paris 06, CNRS UMR7095, Inst Astrophys Paris, F-75014 Paris, France
关键词
planetary systems; stars: fundamental parameters; techniques: photometric; techniques: spectroscopic; techniques: radial velocities; LIMB-DARKENING COEFFICIENTS; TRANSITING EXOPLANETS; PLANETARY CANDIDATES; EXTRASOLAR PLANETS; LIGHT CURVES; HOT JUPITER; B; VELOCIMETRY; COROT; STELLAR;
D O I
10.1051/0004-6361/201323042
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Radial velocity observations of Kepler candidates obtained with the SOPHIE and HARPS-N spectrographs have permitted unveiling the nature of the the giant planets Kepler-41b, Kepler-43b, Kepler-44b. Kepler-74b, and Kepler-75b, the massive companion Kepler-39b, and the brown dwarf KOI-205b. These companions were previously characterized with long-cadence (LC) Kepler data. Here we aim at refining the parameters of these transiting systems by i) modelling the published radial velocities and Kepler short cadence (SC) data that provide a much better sampling of the transits; ii) performing new spectral analyses of the SOPHIE and ESPaDOnS spectra, after improving our procedure for selecting and co-adding the SOPHIE spectra of faint stars (K-p greater than or similar to 14); and iii) improving stellar rotation periods hence stellar age estimates through gyrochronology, when possible, by using all the available LC data up to quarter Q17. Posterior distributions of the system parameters were derived with a differential evolution Markov chain Monte Carlo approach, Our main results are as follows: a) Kepler -41b is significantly larger and less dense than previously found because a lower orbital inclination is favoured by SC data. This also affects the determination of the geometric albedo that is lower than previously derived: A(g) < 0.135; b) Kepler-44b is moderately smaller and denser than reported in the discovery paper, as a consequence of the slightly shorter transit duration found with SC data; good agreement was achieved with published Kepler-43, Kepler 75, and KOI-205 system parameters, although the host stars Kepler 75 and KOI-205 were found to be slightly richer in metals and hotter, respectively; d) the previously reported non-zero eccentricities of Kepler-39b and Kepler-74b might be spurious. If their orbits were circular, the two companions would be smaller and denser than in the eccentric case. The radius of Kepler-39b is still larger than predicted by theoretical isochrones. Its parent star is hotter and richer in metals than previously determined.
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