2014A&A...571A..37S


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.21CET06:52:00

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

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Number of rows : 39

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 HD 10069b Pl 01 37 25.0335097438 -45 40 40.376513381           ~ 239 1
2 HAT-P-32b Pl 02 04 10.2775457769 +46 41 16.210382751           ~ 95 1
3 HAT-P-32 * 02 04 10.2775457769 +46 41 16.210382751   11.79 11.44 11.23   ~ 52 1
4 HD 32147 PM* 05 00 48.9991346145 -05 45 13.220341956 8.27 7.27 6.21 5.36 4.87 K3+V 419 1
5 HD 41248 PM* 06 00 32.7815442690 -56 09 42.597177626   9.42 8.81     G2V 55 1
6 HAT-P-20b Pl 07 27 39.9487418539 +24 20 11.518276475           ~ 58 1
7 HD 80606b Pl 09 22 37.5769478105 +50 36 13.434928660           ~ 281 1
8 HD 80606 PM* 09 22 37.5769478105 +50 36 13.434928660   9.78 9.00     G5 290 2
9 HD 80607 PM* 09 22 39.7367015092 +50 36 13.952617706   9.937 9.070     G5 83 2
10 HD 100777 * 11 35 51.5230327145 -04 45 20.501221342   9.19 8.42     G8V 54 1
11 CD-27 10695b Pl 15 59 50.9489706053 -28 03 42.309432433           ~ 205 1
12 HD 147506b Pl 16 20 36.3579144486 +41 02 53.109043943           ~ 218 1
13 HD 156384C PM* 17 18 58.8271844065 -34 59 48.612934284 12.96 11.79 10.22 10.05 8.82 M1.5V 169 1
14 CoRoT-16b Pl 18 34 05.9188253411 -06 00 09.244766297           ~ 22 2
15 CoRoT-9b Pl 18 43 08.8101080314 +06 12 14.912939950           ~ 61 1
16 Kepler-94 Ro* 18 44 46.7441195652 +47 29 49.746742707           M0V 51 0
17 Kepler-102 Ro* 18 45 55.8561241973 +47 12 28.843506748   12.58 12.07     K3V 83 0
18 HD 175289 Ro* 18 52 36.1606413704 +45 08 23.343183125   9.95 9.50 9.44   F6IV 84 0
19 Kepler-132 ** 18 52 56.5602135537 +41 20 34.904661489   12.49 11.92     ~ 77 0
20 Kepler-30c Pl 19 01 08.0746750853 +38 56 50.218666290           ~ 56 1
21 Kepler-407 Ro* 19 04 08.7182403634 +49 36 52.217637834           ~ 50 0
22 Kepler-296 ** 19 06 09.572976 +49 26 14.54424           M2V 69 0
23 Kepler-25 Ro* 19 06 33.2143323702 +39 29 16.357969502   11.32 10.77 10.598   ~ 118 1
24 BD+46 2629 Er* 19 07 53.104944 +46 52 06.00420   10.12 9.70 9.80   A0 133 0
25 Kepler-97 Ro* 19 09 18.3876122413 +48 40 24.365472961           G0V 48 0
26 Kepler-14 ** 19 10 50.110176 +47 19 58.87632   12.36 12.09 12.08 11.65 ~ 74 1
27 Kepler-113 Ro* 19 11 59.4989980119 +50 56 39.667591092           ~ 50 0
28 BD+48 2893 * 19 24 07.7660110490 +49 02 24.928201112   10.73 10.08     ~ 101 1
29 Kepler-75b Pl 19 24 33.0185863758 +36 34 38.477482370           ~ 35 1
30 Kepler-420b Pl 19 24 54.0384866371 +44 55 38.518268700           ~ 26 0
31 Kepler-420 Ro* 19 24 54.0384866371 +44 55 38.518268700   15.830 14.867     G5V 48 0
32 Kepler-100 Ro* 19 25 32.6433770205 +41 59 24.944182797   11.86 11.06     ~ 88 0
33 BD+38 3583 Ro* 19 25 40.3886092719 +38 40 20.411344230   10.73 10.00     ~ 79 0
34 * sig Dra PM* 19 32 21.5902990 +69 39 40.234737 5.860 5.460 4.680 4.04 3.63 K0V 588 0
35 Kepler-74b Pl 19 32 22.2087182061 +41 21 19.907618268           ~ 33 1
36 Kepler-78b Pl 19 34 58.0139307295 +44 26 53.957326851           ~ 110 1
37 Kepler-87b Pl 19 51 40.0490992347 +46 57 54.427022288           ~ 26 1
38 Kepler-48 Ro* 19 56 33.4161532347 +40 56 56.496048906           K0V 82 1
39 Kepler-106 Ro* 20 03 27.3499849021 +44 20 15.190864304   13.68 12.98     ~ 63 0

    Equat.    Gal    SGal    Ecl

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2021.01.21-06:52:00

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