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J/A+A/615/A90         Kepler-419 radial velocities             (Almenara+, 2018)

SOPHIE velocimetry of Kepler transit candidates. XVIII. Radial velocity confirmation, absolute masses and radii, and origin of the Kepler-419 multiplanetary system. Almenara J.M., Diaz R.F., Hebrard G., Mardling R., Damiani C., Santerne A., Bouchy F., Barros S.C.C., Boisse I., Bonfils X., Bonomo A.S., Courcol B., Demangeon O., Deleuil M., Rey J., Udry S., Wilson P.A. <Astron. Astrophys. 615, A90 (2018)> =2018A&A...615A..90A (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Exoplanets ; Radial velocities Keywords: planetary systems - techniques: photometric - techniques: radial velocities - Abstract: Kepler-419 is a planetary system discovered by the Kepler photometry which is known to harbour two massive giant planets: an inner 3MJ transiting planet with a 69.8-day period, highly eccentric orbit, and an outer 7.5MJ non-transiting planet predicted from the transit-timing variations (TTVs) of the inner planet b to have a 675-day period, moderately eccentric orbit. Here we present new radial velocity (RV) measurements secured over more than two years with the SOPHIE spectrograph, where both planets are clearly detected. The RV data is modelled together with the Kepler photometry using a photodynamical model. The inclusion of velocity information breaks the MR-3 degeneracy inherent in timing data alone, allowing us to measure the absolute stellar and planetary radii and masses. With uncertainties of 12 and 13% for the stellar and inner planet radii, and 35, 24, and 35% for the masses of the star, planet b, and planet c, respectively, these measurements are the most precise to date for a single host star system using this technique. The transiting planet mass is determined at better precision than the star mass. This shows that modelling the radial velocities and the light curve together in systems of dynamically interacting planets provides a way of characterising both the star and the planets without being limited by knowledge of the star. On the other hand, the period ratio and eccentricities place the Kepler-419 system in a sweet spot; had around twice as many transits been observed, the mass of the transiting planet could have been measured using its own TTVs. Finally, the origin of the Kepler-419 system is discussed. We show that the system is near a coplanar high-eccentricity secular fixed point, related to the alignment of the orbits, which has prevented the inner orbit from circularising. For most other relative apsidal orientations, planet b's orbit would be circular with a semi-major axis of 0.03au. This suggests a mechanism for forming hot Jupiters in multiplanetary systems without the need of high mutual inclinations. Description: File tablea1 contains the radial velocities of Kepler-419 obtained with the SOPHIE spectrograph installed at the 1.93-m telescope of the Observatoire de Haute-Provence (France). Objects: ----------------------------------------------------------------- RA (2000) DE Designation(s) ----------------------------------------------------------------- 19 41 40.30 +51 11 05.2 Kepler-419 = KIC 12365184 = KOI-1474 ----------------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 27 45 SOPHIE radial velocities of Kepler-419
See also: J/A+A/528/A63 : Velocitometry transit of KOI-428b (Santerne+, 2011) J/A+A/544/L12 : Velocitometry transit of KOI-13 (Santerne+, 2012) J/A+A/571/A37 : KOI-1257 photometric and velocimetric data (Santerne+, 2014) J/A+A/573/A124 : Kepler-117 (KOI-209) transit-timing variations (Bruno+, 2015) J/A+A/587/A64 : Physical properties of giant exoplanets (Santerne+, 2016) Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1- 13 F13.5 d BJD Barycentric Julian Date of observation 15- 21 F7.3 km/s RV Radial velocity 23- 27 F5.3 km/s e_RV Radial velocity uncertainty
Acknowledgements: Jose Manuel Almenara, Jose.Almenara(at)unige.ch References: Ehrenreich et al., Paper I 2011A&A...525A..85E Santerne et al., Paper II 2011A&A...528A..63S, Cat. J/A+A/528/A63 Bouchy et al., Paper III 2011A&A...533A..83B Santerne et al., Paper IV 2011A&A...536A..70S Bonomo et al., Paper V 2012A&A...538A..96B Santerne et al., Paper VI 2012A&A...544L..12S, Cat. J/A+A/544/L12 Santerne et al., Paper VII 2012A&A...545A..76S Diaz et al., Paper VIII 2013A&A...551L...9D Moutou et al., Paper IX 2013A&A...558L...6M Barros et al., Paper X 2014A&A...561L...1B Deleuil et al., Paper XI 2014A&A...564A..56D Santerne et al., Paper XII 2014A&A...571A..37S, Cat. J/A+A/571/A37 Diaz et al., Paper XIII 2014A&A...572A.109D Bruno et al., Paper XIV 2015A&A...573A.124B, Cat. J/A+A/573/A124 Almenara et al., Paper XV 2015A&A...575A..71A Bourrier et al., Paper XVI 2015A&A...579A..55B Santerne et al., Paper XVII 2016A&A...587A..64S, Cat. J/A+A/587/A64
(End) Patricia Vannier [CDS] 07-Apr-2018
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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