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


Query : 2014A&A...571A..37S

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 - 2023
#notes
1 HD 10069b Pl 01 37 25.0335097438 -45 40 40.376513381           ~ 323 1
2 HAT-P-32 * 02 04 10.2774374568 +46 41 16.212315084   11.79 11.44 11.23   ~ 60 1
3 HAT-P-32b Pl 02 04 10.2775457769 +46 41 16.210382751           ~ 127 1
4 HD 32147 PM* 05 00 48.9993452248 -05 45 13.224327192 8.27 7.27 6.21 5.36 4.87 K3+V 436 1
5 HD 41248 PM* 06 00 32.7813939624 -56 09 42.597168768   9.42 8.81     G2V 67 1
6 HAT-P-20b Pl 07 27 39.9487418539 +24 20 11.518276475           ~ 71 1
7 HD 80606 PM* 09 22 37.5768032712 +50 36 13.435326684   9.78 9.00     G8V 312 2
8 HD 80606b Pl 09 22 37.5769478105 +50 36 13.434928660           ~ 303 1
9 HD 80607 PM* 09 22 39.7366541424 +50 36 13.952919312   9.937 9.070     G5 92 2
10 HD 100777 * 11 35 51.5232197976 -04 45 20.504631564   9.19 8.42     G8V 72 1
11 CD-27 10695b Pl 15 59 50.9489706053 -28 03 42.309432433           ~ 236 1
12 HD 147506b Pl 16 20 36.3579144486 +41 02 53.109043943           ~ 240 1
13 HD 156384C PM* 17 18 58.8272997802 -34 59 48.612673382 12.96 11.79 10.22 10.05 8.82 M1.5V 197 1
14 CoRoT-16b Pl 18 34 05.9188253411 -06 00 09.244766297           ~ 24 2
15 CoRoT-9b Pl 18 43 08.8101080314 +06 12 14.912939950           ~ 65 1
16 Kepler-94 Ro* 18 44 46.7440377288 +47 29 49.749482616           M0V 59 0
17 Kepler-102 PM* 18 45 55.8559851072 +47 12 28.845259020   12.58 12.07     K3V 96 0
18 HD 175289 PM* 18 52 36.1604006928 +45 08 23.345639700   9.95 9.50 9.44   F6IV 93 0
19 Kepler-132 Ro* 18 52 56.5641599064 +41 20 34.997513460   12.49 11.92     ~ 80 0
20 Kepler-30c Pl 19 01 08.0746750853 +38 56 50.218666290           ~ 64 1
21 Kepler-407 Ro* 19 04 08.7180702936 +49 36 52.219314504           ~ 61 0
22 Kepler-296 ** 19 06 09.6025302984 +49 26 14.396852760           M2V 78 0
23 Kepler-25 Ro* 19 06 33.2141354736 +39 29 16.358725104   11.32 10.77 10.598   ~ 138 1
24 BD+46 2629 ** 19 07 53.104944 +46 52 06.00420   10.12 9.70 9.80   kA2hA5mA7(IV)m: 149 0
25 Kepler-97 Ro* 19 09 18.3874144296 +48 40 24.368309184           G0V 56 0
26 Kepler-14 Ro* 19 10 50.110176 +47 19 58.87632   12.36 12.09 12.08 11.65 ~ 80 1
27 Kepler-113 Ro* 19 11 59.4990081336 +50 56 39.668230356           ~ 56 0
28 BD+48 2893 Ro* 19 24 07.7659706688 +49 02 24.928348272   10.73 10.08     G1V 117 1
29 Kepler-75b Pl 19 24 33.0185863758 +36 34 38.477482370           ~ 44 1
30 Kepler-420 Ro* 19 24 54.0364030656 +44 55 38.524017504   15.830 14.867     G5V 52 0
31 Kepler-420b Pl 19 24 54.0384866371 +44 55 38.518268700           ~ 37 0
32 Kepler-100 Ro* 19 25 32.6432787456 +41 59 24.945100548   11.86 11.06     ~ 99 0
33 BD+38 3583 Ro* 19 25 40.3885404552 +38 40 20.413186860   10.73 10.00     G5V 100 0
34 * sig Dra PM* 19 32 21.5902098601 +69 39 40.235805206 5.860 5.460 4.680 4.04 3.63 K0V 610 0
35 Kepler-74b Pl 19 32 22.2087182061 +41 21 19.907618268           ~ 40 1
36 Kepler-78b Pl 19 34 58.0139307295 +44 26 53.957326851           ~ 129 1
37 Kepler-87b Pl 19 51 40.0490992347 +46 57 54.427022288           ~ 32 1
38 Kepler-48 Ro* 19 56 33.4161659688 +40 56 56.496876216           K0V 92 1
39 Kepler-106 Ro* 20 03 27.3499329384 +44 20 15.191981988   13.68 12.98     ~ 70 0

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2023.01.27-08:48:05

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