pastis: Bayesian extrasolar planet validation – I. General framework, models, and performance

Díaz, R. F.; Almenara, J. M.; Santerne, A.; Moutou, C.; Lethuillier, Anthony; Deleuil, M.

doi:10.1093/mnras/stu601

Cited by 195 publications

(204 citation statements)

References 88 publications

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“…For that, we analysed the data with the MCMC algorithm of the PASTIS software (Díaz et al 2014a). We used a uniform prior for the RV amplitudes (between 0 and 100 km s −1 ) for the systemic RV (between −100 km s −1 and +100 km s −1 ) and for the argument of periastron (between 0 • and 360 • ).…”

Section: No Variation Casesmentioning

confidence: 99%

SOPHIE velocimetry ofKeplertransit candidates

Santerne

Moutou

Tsantaki

et al. 2016

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While giant extrasolar planets have been studied for more than two decades now, there are still some open questions as to their dominant formation and migration processes, as well as to their atmospheric evolution in different stellar environments. In this paper, we study a sample of giant transiting exoplanets detected by the Kepler telescope with orbital periods up to 400 days. We first defined a sample of 129 giant-planet candidates that we followed up with the SOPHIE spectrograph (OHP, France) in a 6-year radial velocity campaign. This allowed us to unveil the nature of these candidates and to measure a false-positive rate of 54.6 ± 6.5% for giant-planet candidates orbiting within 400 days of period. Based on a sample of confirmed or likely planets, we then derived the occurrence rates of giant planets in different ranges of orbital periods. The overall occurrence rate of giant planets within 400 days is 4.6 ± 0.6%. We recovered, for the first time in the Kepler data, the different populations of giant planets reported by radial velocity surveys. Comparing these rates with other yields, we find that the occurrence rate of giant planets is lower only for hot Jupiters but not for the longer-period planets. We also derive a first measurement of the occurrence rate of brown dwarfs in the brown-dwarf desert with a value of 0.29 ± 0.17%. Finally, we discuss the physical properties of the giant planets in our sample. We confirm that giant planets receiving moderate irradiation are not inflated, but we find that they are on average smaller than predicted by formation and evolution models. In this regime of low-irradiated giant planets, we find a possible correlation between their bulk density and the iron abundance of the host star, which needs more detections to be confirmed.

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Section: No Variation Casesmentioning

confidence: 99%

SOPHIE velocimetry ofKeplertransit candidates

Santerne

Moutou

Tsantaki

et al. 2016

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“…The normalized Kepler light curves were fitted by a transit model using the PASTIS code (Díaz et al 2014). The analysis also includes the fit of the SED and stellar evolution tracks to determine coherent stellar parameters.…”

Section: Photometry Analysismentioning

confidence: 99%

SOPHIE velocimetry ofKeplertransit candidates

Bourrier

Étangs

Hébrard

et al. 2015

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We present the detection and characterization of the transiting warm Jupiter KOI-12b, first identified with Kepler with an orbital period of 17.86 days. We combine the analysis of Kepler photometry with Doppler spectroscopy and line-profile tomography of timeseries spectra obtained with the SOPHIE spectrograph to establish its planetary nature and derive its properties. To derive reliable estimates for the uncertainties on the tomographic model parameters, we devised an empirical method of calculating statistically independent error bars on the time-series spectra. KOI-12b has a radius of 1.43 ± 0.13 R Jup and a 3σ upper mass limit of 10 M Jup . It orbits a fast-rotating star (v sin i = 60.0 ± 0.9 km s −1 ) with mass and radius of 1.45 ± 0.09 M and 1.63 ± 0.15 R , located at 426 ± 40 pc from the Earth. Doppler tomography allowed higher precision on the obliquity to be reached by comparison with analysis of the Rossiter-McLaughlin radial velocity anomaly, and we find that KOI-12b lies on a prograde, slightly misaligned orbit with low sky-projected obliquity λ = 12.6 +3.0 −2.9• . The properties of this planetary system, with a 11.4 mag host star, make of KOI-12b a precious target for future atmospheric characterization.

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“…We used the planet analysis and small transit investigation software (PASTIS; Díaz et al 2014), which is a Bayesian analysis software, for fitting a two-planet model. HD 190360b orbit was not fixed but subjected to strong priors for the Bayesian analysis.…”

Section: Validation Of the Correctionmentioning

confidence: 99%

The SOPHIE search for northern extrasolar planets

Courcol

Bouchy

Pepe

et al. 2015

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High-precision radial velocity surveys explore the population of low-mass exoplanets orbiting bright stars. This allows accurately deriving their orbital parameters such as their occurrence rate and the statistical distribution of their properties. Based on this, models of planetary formation and evolution can be constrained. The SOPHIE spectrograph has been continuously improved in past years, and thanks to an appropriate correction of systematic instrumental drift, it is now reaching 2 m s −1 precision in radial velocity measurements on all timescales. As part of a dedicated radial velocity survey devoted to search for low-mass planets around a sample of 190 bright solar-type stars in the northern hemisphere, we report the detection of a warm Neptune with a minimum mass of 16.1 ± 2.7 M ⊕ orbiting the solar analog HD 164595 in 40 ± 0.24 days. We also revised the parameters of the multiplanetary system around HD 190360. We discuss this new detection in the context of the upcoming space mission CHEOPS, which is devoted to a transit search of bright stars harboring known exoplanets.

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pastis: Bayesian extrasolar planet validation – I. General framework, models, and performance

Cited by 195 publications

References 88 publications

SOPHIE velocimetry ofKeplertransit candidates

SOPHIE velocimetry ofKeplertransit candidates

SOPHIE velocimetry ofKeplertransit candidates

The SOPHIE search for northern extrasolar planets

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