KOI-200 b and KOI-889 b: Two transiting exoplanets detected and characterized with<i>Kepler</i>, SOPHIE, and HARPS-N

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

doi:10.1051/0004-6361/201321394

Cited by 39 publications

(37 citation statements)

References 56 publications

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“…Kepler-74 b.-Kepler-74 b is a gas giant planet whose mass was determined from RV measurements (Hébrard et al 2013;Bonomo et al 2015). It has a relatively high equilibrium temperature of ∼1200 K. The star has a companion at a separation of 0 3, which is about 0.5 mag fainter in the optical (Ziegler et al 2017).…”

Section: Appendix a Notes On Individual Planetsmentioning

confidence: 99%

The Densities of Planets in Multiple Stellar Systems

Furlan

Howell

2017

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We analyze the effect of companion stars on the bulk density of 29 planets orbiting 15 stars in the Kepler field. These stars have at least one stellar companion within 2″, and the planets have measured masses and radii, allowing an estimate of their bulk density. The transit dilution by the companion star requires the planet radii to be revised upward, even if the planet orbits the primary star; as a consequence, the planetary bulk density decreases. We find that if planets orbited a faint companion star, they would be more volatile-rich, and in several cases their densities would become unrealistically low, requiring large, inflated atmospheres or unusually large mass fractions in an H/He envelope. In addition, for planets detected in radial velocity data, the primary star has to be the host. We can exclude 14 planets from orbiting the companion star; the remaining 15 planets in seven planetary systems could orbit either the primary or the secondary star, and for five of these planets the decrease in density would be substantial even if they orbited the primary, since the companion is of almost equal brightness as the primary. Substantial follow-up work is required in order to accurately determine the radii of transiting planets. Of particular interest are small, rocky planets that may be habitable; a lower mean density might imply a more volatile-rich composition. Reliable radii, masses, and thus bulk densities will allow us to identify which small planets are truly Earth-like.

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Section: Appendix a Notes On Individual Planetsmentioning

confidence: 99%

The Densities of Planets in Multiple Stellar Systems

Furlan

Howell

2017

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“…High-precision radial velocity follow-up has yielded ∼50 mass determinations from instruments scattered across the northern hemisphere, including the SOPHIE (Spectrographe pour l'Observation des Phénomènes des Intérieurs stellaires et des Exoplanètes) spectrograph at the Observatoire de HauteProvence (49-51), FIES (fiber-fed echelle spectrograph) on the Nordic Optical Telescope (52), HRS (high-resolution spectrograph) on the Hobby-Ebberly Telescope (53), HARPS-N (High Accuracy Radial velocity Planet Searcher-North) on the Telescopio Nazionale Galileo (54), and the HIRES (high-resolution Echelle spectrometer) spectrograph on Keck (55). Of special interest are the measurements for the subNeptune-size planets, particularly those that have densities indicative of a rocky composition: Kepler-10b (56) and Kepler-78b (57,58).…”

Section: Planet Confirmation and Characterizationmentioning

confidence: 99%

Exploring exoplanet populations with NASA’s Kepler Mission

Batalha

2014

Proc. Natl. Acad. Sci. U.S.A.

237

168

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The Kepler Mission is exploring the diversity of planets and planetary systems. Its legacy will be a catalog of discoveries sufficient for computing planet occurrence rates as a function of size, orbital period, star type, and insolation flux. The mission has made significant progress toward achieving that goal. Over 3,500 transiting exoplanets have been identified from the analysis of the first 3 y of data, 100 planets of which are in the habitable zone. The catalog has a high reliability rate (85-90% averaged over the period/radius plane), which is improving as follow-up observations continue. Dynamical (e.g., velocimetry and transit timing) and statistical methods have confirmed and characterized hundreds of planets over a large range of sizes and compositions for both single-and multiple-star systems. Population studies suggest that planets abound in our galaxy and that small planets are particularly frequent. Here, I report on the progress Kepler has made measuring the prevalence of exoplanets orbiting within one astronomical unit of their host stars in support of the National Aeronautics and Space Administration's long-term goal of finding habitable environments beyond the solar system. planet detection | transit photometry

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“…HARPS-N was commissioned in early 2012 with one of its main goals being to follow up Kepler objects of interest. HARPS-N has already characterised two transiting giant exoplanets in synergy with SOPHIE (KOI-200 b and KOI-889 b: Hébrard et al 2013b), as well as the transiting rocky planet Kepler-78 b (Sanchis-Ojeda et al 2013;Pepe et al 2013).…”

Section: Harps-n Spectroscopic Follow-upmentioning

confidence: 99%

“…We adopted the parameters derived by the VWA analysis for homogeneity with our previous results (e.g. Santerne et al 2011a,b;Hébrard et al 2013b;Barros et al 2014;Deleuil et al 2014). …”

Section: Spectral Analysismentioning

confidence: 99%

“…We modelled the light curve using the EBOP code (Nelson & Davis 1972;Etzel 1981;Popper & Etzel 1981) extracted from the JKTEBOP package (Southworth 2008). The model is described with 23 free parameters: the orbital period P, the epoch of transit T 0 , the orbital inclination i p , the orbital eccentricity e p , the argument of periastron ω p , the radius ratio r p /R , the linear and quadratic limb darkening coefficients u a and u b (respectively), the stellar effective temperature T eff , the iron abundance [Fe/H], and the stellar density ρ , as well as the contamination, the flux out-of-transit, and an extra source of white noise (jitter) for each of the four seasons of the Kepler data as already done in Hébrard et al (2013b). We used the Dartmouth evolutionary tracks (Dotter et al 2008) to estimate the stellar parameters.…”

Section: Model A: Light-curve Analysismentioning

confidence: 99%

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SOPHIE velocimetry ofKeplertransit candidates

Santerne¹,

Hébrard²,

Deleuil³

et al. 2014

A&A

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In this paper we report a new transiting warm giant planet: KOI-1257 b. It was first detected in photometry as a planet-candidate by the Kepler space telescope and then validated thanks to a radial velocity follow-up with the SOPHIE spectrograph. It orbits its host star with a period of 86.647661 d ± 3 s and a high eccentricity of 0.772 ± 0.045. The planet transits the main star of a metal-rich, relatively old binary system with stars of mass of 0.99 ± 0.05 M and 0.70 ± 0.07 M for the primary and secondary, respectively. This binary system is constrained thanks to a self-consistent modelling of the Kepler transit light curve, the SOPHIE radial velocities, line bisector and full-width half maximum (FWHM) variations, and the spectral energy distribution. However, future observations are needed to confirm it. The PASTIS fully-Bayesian software was used to validate the nature of the planet and to determine which star of the binary system is the transit host. By accounting for the dilution from the binary both in photometry and in radial velocity, we find that the planet has a mass of 1.45 ± 0.35 M , and a radius of 0.94 ± 0.12 R , and thus a bulk density of 2.1 ± 1.2 g cm −3 . The planet has an equilibrium temperature of 511 ± 50 K, making it one of the few known members of the warm-Jupiter population. The HARPS-N spectrograph was also used to observe a transit of KOI-1257 b, simultaneously with a joint amateur and professional photometric follow-up, with the aim of constraining the orbital obliquity of the planet. However, the Rossiter-McLaughlin effect was not clearly detected, resulting in poor constraints on the orbital obliquity of the planet.

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KOI-200 b and KOI-889 b: Two transiting exoplanets detected and characterized withKepler, SOPHIE, and HARPS-N

Cited by 39 publications

References 56 publications

The Densities of Planets in Multiple Stellar Systems

The Densities of Planets in Multiple Stellar Systems

Exploring exoplanet populations with NASA’s Kepler Mission

SOPHIE velocimetry ofKeplertransit candidates

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