SIMBAD references

2014A&A...571A..37S - Astronomy and Astrophysics, volume 571A, 37-37 (2014/11-1)

SOPHIE velocimetry of Kepler transit candidates. XII. KOI-1257 b: a highly eccentric three-month period transiting exoplanet.

SANTERNE A., HEBRARD G., DELEUIL M., HAVEL M., CORREIA A.C.M., ALMENARA J.-M., ALONSO R., ARNOLD L., BARROS S.C.C., BEHREND R., BERNASCONI L., BOISSE I., BONOMO A.S., BOUCHY F., BRUNO G., DAMIANI C., DIAZ R.F., GRAVALLON D., GUILLOT T., LABREVOIR O., MONTAGNIER G., MOUTOU C., RINNER C., SANTOS N.C., ABE L., AUDEJEAN M., BENDJOYA P., GILLIER C., GREGORIO J., MARTINEZ P., MICHELET J., MONTAIGUT R., PONCY R., RIVET J.-P., ROUSSEAU G., ROY R., SUAREZ O., VANHUYSSE M. and VERILHAC D.

Abstract (from CDS):

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±0.05Msun, and 0.70±0.07Msun, 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±0.35Mjup, and a radius of 0.94±0.12Rjup, and thus a bulk density of 2.1±1.2g/cm3. The planet has an equilibrium temperature of 511±50K, 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.

Abstract Copyright:

Journal keyword(s): planetary systems - techniques: photometric - techniques: radial velocities - techniques: spectroscopic - methods: data analysis - stars: individual: KOI-1257 Ab

VizieR on-line data: <Available at CDS (J/A+A/571/A37): phot.dat rvkoi.dat rvconst.dat>

Simbad objects: 39

goto Full paper

goto View the reference in ADS

To bookmark this query, right click on this link: simbad:2014A&A...571A..37S and select 'bookmark this link' or equivalent in the popup menu


2020.11.28-00:29:02

© Université de Strasbourg/CNRS

    • Contact