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

Moutou, C.; Bonomo, A. S.; Bruno, G.; Montagnier, G.; Bouchy, F.; Almenara, J. M.; Barros, S. C. C.; Deleuil, M.; Díaz, R. F.; Hébrard, G.; Santerne, A.

doi:10.1051/0004-6361/201322201

Cited by 42 publications

(42 citation statements)

References 35 publications

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“…5.3. The other two massive substellar companions in our sample (KOI-205 b (∼40 M ) and KOI-415 b (∼62 M ): Díaz et al 2013;Moutou et al 2013a) are very likely to be brown dwarfs. Finally, the case of the 78 Mcompanion to KOI-189 has been classified as a very-low-mass star by Díaz et al (2014b).…”

Section: Bona Fide Planets and Brown Dwarfsmentioning

confidence: 81%

SOPHIE velocimetry ofKeplertransit candidates

Santerne

Moutou

Tsantaki

et al. 2016

A&A

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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: Bona Fide Planets and Brown Dwarfsmentioning

confidence: 81%

SOPHIE velocimetry ofKeplertransit candidates

Santerne

Moutou

Tsantaki

et al. 2016

A&A

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269

263

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“…Several are eclipsing binaries (KOIs 113, 134, 1032, 1463, and 3419) and one is a brown dwarf (KOI-415) as determined with radial velocity measurements by Moutou et al (2013). The transit signal detected in KOI-1546 was shown to arise from the variations of a different star in the field.…”

Section: False Positive Identificationmentioning

confidence: 91%

The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets^*

et al. 2017

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The California-Kepler Survey (CKS) is an observational program developed to improve our knowledge of the properties of stars found to host transiting planets by NASA's Kepler Mission. The improvement stems from new high-resolution optical spectra obtained using HIRES at the W. M. Keck Observatory. The CKS stellar sample comprises 1305 stars classified as Kepler objects of interest, hosting a total of 2075 transiting planets. The primary sample is magnitude-limited ( < Kp 14.2) and contains 960 stars with 1385 planets. The sample was extended to include some fainter stars that host multiple planets, ultra-short period planets, or habitable zone planets. The spectroscopic parameters were determined with two different codes, one based on template matching and the other on direct spectral synthesis using radiative transfer. We demonstrate a precision of 60K in T eff , 0.10dex in g log , 0.04dex in [ ] Fe H , and 1.0 -km s 1 in V i sin . In this paper, we describe the CKS project and present a uniform catalog of spectroscopic parameters. Subsequent papers in this series present catalogs of derived stellar properties such as mass, radius, and age; revised planet properties; and statistical explorations of the ensemble. CKS is the largest survey to determine the properties of Kepler stars using a uniform set of high-resolution, high signal-tonoise ratio spectra. The HIRES spectra are available to the community for independent analyses.

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“…The space-based CoRoT mission (Rouan et al 1999) discovered three transiting brown dwarfs: CoRoT3b (Deleuil et al 2008), CoRoT-15b (Bouchy et al 2011b), and CoRoT-33b (Csizmadia et al 2015). The Kepler mission uncovered another four transiting brown dwarfs: Kepler-39b (Bouchy et al 2011a), KOI-205b (Díaz et al 2013), KOI-415b (Moutou et al 2013), and KOI-189b (Díaz et al 2014b). Additionally KOI-554b and KOI-3728b have masses, measured via light curve modulations, just above 80 M J , putting them very close to the brown dwarf regime (Lillo-Box et al 2016).…”

Section: Introductionmentioning

confidence: 99%

EPIC 201702477b: A TRANSITING BROWN DWARF FROM K2 IN A 41 DAY ORBIT

Hojjatpanah¹,

Santerne²,

Dragomir³

et al. 2016

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We report the discovery of EPIC 201702477b, a transiting brown dwarf in a long period (40.73691±0.00037 day) and eccentric (e = 0.2281±0.0026) orbit. This system was initially reported as a planetary candidate based on two transit events seen in K2 Campaign 1 photometry and later validated as an exoplanet candidate. We confirm the transit and refine the ephemeris with two subsequent ground-based detections of the transit using the Las Cumbres Observatory Global Telescope 1 m telescope network. We rule out any transit timing variations above the level of ∼30 s. Using high precision radial velocity measurements from HARPS and SOPHIE we identify the transiting companion as a brown dwarf with a mass, radius, and bulk density of 66.9±1.7 M J , 0.757±0.065 R J , and 191±51 g cm −3 respectively. EPIC 201702477b is the smallest radius brown dwarf yet discovered, with a mass just below the H-burning limit. It has the highest density of any planet, substellar mass object, or main-sequence star discovered so far. We find evidence in the set of known transiting brown dwarfs for two populations of objects-high mass brown dwarfs and low mass brown dwarfs. The highermass population have radii in very close agreement to theoretical models, and show a lower-mass limit around 60 M J . This may be the signature of mass-dependent ejection of systems during the formation process.

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SOPHIE velocimetry ofKeplertransit candidates

Cited by 42 publications

References 35 publications

SOPHIE velocimetry ofKeplertransit candidates

SOPHIE velocimetry ofKeplertransit candidates

The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets^*

EPIC 201702477b: A TRANSITING BROWN DWARF FROM K2 IN A 41 DAY ORBIT

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SOPHIE velocimetry ofKeplertransit candidates

Cited by 42 publications

References 35 publications

SOPHIE velocimetry ofKeplertransit candidates

SOPHIE velocimetry ofKeplertransit candidates

The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets*

EPIC 201702477b: A TRANSITING BROWN DWARF FROM K2 IN A 41 DAY ORBIT

Contact Info

Product

Resources

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The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets^*