SOPHIE velocimetry of Kepler transit candidates - XII. KOI-1257 b: a highly eccentric three-month period transiting exoplanet
SOPHIE velocimetry of Kepler transit candidates - XII. KOI-1257 b: a highly eccentric three-month period transiting exoplanet
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DOI：
10.1051/0004-6361/201424158
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发表时间：
2014-06
影响因子：
6.5
通讯作者：
A. Santerne;A. Santerne;G. Hébrard;G. Hébrard;M. Deleuil;M. Havel;M. Havel;A. Correia;A. Correia;J. Almenara;R. Alonso;R. Alonso;L. Arnold;S. Barros;R. Behrend;L. Bernasconi;I. Boisse;I. Boisse;A. Bonomo;F. Bouchy;F. Bouchy;G. Bruno;C. Damiani;R. F. Díaz;R. F. Díaz;D. Gravallon;T. Guillot;O. Labrevoir;G. Montagnier;G. Montagnier;C. Moutou;C. Moutou;C. Rinner;N. Santos;L. Abe;M. Audejean;P. Bendjoya;C. Gillier;J. Gregorio;P. Martinez;J. Michelet;R. Montaigut;R. Poncy;J. Rivet;G. Rousseau;R. Roy;O. Suárez;M. Vanhuysse;D. Vérilhac
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文献类型：
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作者：
A. Santerne;A. Santerne;G. Hébrard;G. Hébrard;M. Deleuil;M. Havel;M. Havel;A. Correia;A. Correia;J. Almenara;R. Alonso;R. Alonso;L. Arnold;S. Barros;R. Behrend;L. Bernasconi;I. Boisse;I. Boisse;A. Bonomo;F. Bouchy;F. Bouchy;G. Bruno;C. Damiani;R. F. Díaz;R. F. Díaz;D. Gravallon;T. Guillot;O. Labrevoir;G. Montagnier;G. Montagnier;C. Moutou;C. Moutou;C. Rinner;N. Santos;L. Abe;M. Audejean;P. Bendjoya;C. Gillier;J. Gregorio;P. Martinez;J. Michelet;R. Montaigut;R. Poncy;J. Rivet;G. Rousseau;R. Roy;O. Suárez;M. Vanhuysse;D. Vérilhac
在本文中，我们报告了一颗新的凌日温暖巨行星：KOI-1257 b。它首先被开普勒太空望远镜在光度测量中发现为行星候选者，然后通过径向速度进行验证：后续使用 SOPHIE 摄谱仪。它绕主恒星运行的周期为 86,647661 d +/- 3 s，偏心率为 0.772 +/- 0.045。该行星经过一个富含金属、相对古老的双星系统的主恒星，主恒星和次恒星的质量分别为 0.99 +/- 0.05 M 圆点和 0.70 +/- 0.07 M 圆点。由于开普勒凌日光曲线的自洽模型，这个双星系统受到了限制； SOPHIE 径向速度；线平分线和半峰全宽 (FWHM) 变化，以及光谱能量分布。然而，还需要未来的观察来证实这一点。 PASTIS 全贝叶斯软件用于验证行星的性质并确定双星系统中的哪颗恒星是凌日宿主。通过考虑双星光度和径向速度的稀释，我们发现该行星的质量为 1.45 +/- 0.35 M-4，半径为 0.94(4) +/- 0.12 R-4，因此体积密度为 2.1 +/- 1.2 g cm(-3)。这颗行星的平衡温度为 511 +/- 50K，使其成为少数已知的暖木星群体之一。 HARPS-N 摄谱仪还用于观测 KOI-1257 b 的凌日，同时进行业余和专业光度测量联合跟踪，目的是限制该行星的轨道倾角。然而，罗西特-麦克劳克林效应并未被明确探测到，导致对行星轨道倾角的约束较差。
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-circle dot and 0.70 +/- 0.07 M-circle dot 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-4, and a radius of 0.94(4) +/- 0.12 R-4 and thus a bulk density of 2.1 +/- 1.2 g cm(-3). 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.