SOPHIE velocimetry of<i>Kepler</i>transit candidates

Santerne, A.; Díaz, R. F.; Moutou, C.; Bouchy, F.; Hébrard, G.; Almenara, J. M.; Bonomo, A. S.; Deleuil, M.; Santos, N. C.

doi:10.1051/0004-6361/201219608

Cited by 168 publications

(253 citation statements)

References 67 publications

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“…This object was part of the SOPHIE follow-up of Kepler candidates described by Santerne et al (2012). Like other objects followed-up with SOPHIE, shows that a significant fraction of the Kepler Objects of Interest are not transiting planets.…”

Section: Introductionmentioning

confidence: 68%

“…The spectra were reduced and extracted using the SOPHIE pipeline (Bouchy et al 2009), and the radial velocites were obtained from a Gaussian fit to the cross-correlation function with numerical masks corresponding to different spectral types. The charge transfer inefficiency (CTI) effect was corrected using the polynomial in Santerne et al (2012). For faint targets such as these, the spectral orders at the edge of the wavelength range are usually too noisy, and adding them in the average cross-1 http://archive.stsci.edu/kepler/kepler_fov/search.php …”

Section: Sophie Velocimetrymentioning

confidence: 99%

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SOPHIE velocimetry ofKeplertransit candidates

Díaz

Damiani

Deleuil

et al. 2013

A&A

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We report the discovery of a transiting brown dwarf companion to KOI-205, a K0 main-sequence star, in a 11.720125-day period orbit. The transits were detected by the Kepler space telescope, and the reflex motion of the star was measured using radial velocity observations obtained with the SOPHIE spectrograph. The atmospheric parameters of the host stars were determined from the analysis of high-resolution, high signal-to-noise ratio ESPaDOns spectra obtained for this purpose. Together with spectrophotometric measurements recovered from the literature, these spectra indicate that the star is a mildly metallic K0 dwarf with T eff 5237 ± 60 K. The mass of the companion is 39.9 ± 1.0 M Jup and its radius is 0.81 ± 0.02 R Jup , in agreement with current theoretical predictions. This is the first time a bona fide brown dwarf companion is detected in orbit around a star of this type. The formation and orbital evolution of brown dwarf companions is briefly discussed in the light of this new discovery.

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Section: Introductionmentioning

confidence: 68%

Section: Sophie Velocimetrymentioning

confidence: 99%

SOPHIE velocimetry ofKeplertransit candidates

Díaz

Damiani

Deleuil

et al. 2013

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“…1 and listed in Table B.1, together with their various ID, their main orbital and transit parameters (period, depth, and scaled distance to star), as well as their host properties as determined by Huber et al (2014). Santerne et al (2012b) used the same criteria in terms of magnitude limits and transit depths, but the candidate periods were limited to 25 days. The new sample extends the sample for periods up to 400 days and contains three times more candidates than the previous study.…”

Section: The Giant-planet Candidate Samplementioning

confidence: 99%

“…Brown 2003;Torres et al 2005;Cameron 2012), making it difficult to interpret the candidates without establishing their nature. Spectroscopic follow-up can easily reveal blended multiple stellar systems (Santerne et al 2012b;Kolbl et al 2015), and high-resolution imaging (e.g. Lillo-Box et al 2014) can unveil close-by companions.…”

Section: Introductionmentioning

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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“…Santos et al 2006;Ammler-von Eiff et al 2009, see also Mortier et al, in prep. ) or in planet discovery papers where the spectroscopic analysis was done by our team (see Santerne et al 2012, for a recent example). This guarantees the best possible uniformity of the results.…”

Section: Fgk Stars With Transiting Planetsmentioning

confidence: 99%

SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs

Santos

Sousa

Mortier

et al. 2013

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Context. Thanks to the importance that the star-planet relation has to our understanding of the planet formation process, the precise determination of stellar parameters for the ever increasing number of discovered extra-solar planets is of great relevance. Furthermore, precise stellar parameters are needed to fully characterize the planet properties. It is thus important to continue the efforts to determine, in the most uniform way possible, the parameters for stars with planets as new discoveries are announced. Aims. In this paper we present new precise atmospheric parameters for a sample of 48 stars with planets. We then take the opportunity to present a new catalogue of stellar parameters for FGK and M stars with planets detected by radial velocity, transit, and astrometry programs. Methods. Stellar atmospheric parameters and masses for the 48 stars were derived assuming local thermodynamic equilibrium (LTE) and using high-resolution and high signal-to-noise spectra. The methodology used is based on the measurement of equivalent widths for a list of iron lines and making use of iron ionization and excitation equilibrium principles. For the catalogue, and whenever possible, we used parameters derived in previous works published by our team, using well-defined methodologies for the derivation of stellar atmospheric parameters. This set of parameters amounts to over 65% of all planet host stars known, including more than 90% of all stars with planets discovered through radial velocity surveys. For the remaining targets, stellar parameters were collected from the literature. Results. The stellar parameters for the 48 stars are presented and compared with previously determined literature values. For the catalogue, we compile values for the effective temperature, surface gravity, metallicity, and stellar mass for almost all the planet host stars listed in the Extrasolar Planets Encyclopaedia. This data will be updated on a continuous basis. The compiled catalogue is available online. The data can be used for statistical studies of the star-planet correlation, as well as for the derivation of consistent properties for known planets.

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SOPHIE velocimetry ofKeplertransit candidates

Cited by 168 publications

References 67 publications

SOPHIE velocimetry ofKeplertransit candidates

SOPHIE velocimetry ofKeplertransit candidates

SOPHIE velocimetry ofKeplertransit candidates

SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs

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