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 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:
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RA (2000) DE Designation(s)
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19 41 40.30 +51 11 05.2 Kepler-419 = KIC 12365184 = KOI-1474
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 27 45 SOPHIE radial velocities of Kepler-419
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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
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Bytes Format Units Label Explanations
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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
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Acknowledgements:
Jose Manuel Almenara, Jose.Almenara(at)unige.ch
References:
Ehrenreich et al., Paper I 2011A&A...525A..85E 2011A&A...525A..85E
Santerne et al., Paper II 2011A&A...528A..63S 2011A&A...528A..63S, Cat. J/A+A/528/A63
Bouchy et al., Paper III 2011A&A...533A..83B 2011A&A...533A..83B
Santerne et al., Paper IV 2011A&A...536A..70S 2011A&A...536A..70S
Bonomo et al., Paper V 2012A&A...538A..96B 2012A&A...538A..96B
Santerne et al., Paper VI 2012A&A...544L..12S 2012A&A...544L..12S, Cat. J/A+A/544/L12
Santerne et al., Paper VII 2012A&A...545A..76S 2012A&A...545A..76S
Diaz et al., Paper VIII 2013A&A...551L...9D 2013A&A...551L...9D
Moutou et al., Paper IX 2013A&A...558L...6M 2013A&A...558L...6M
Barros et al., Paper X 2014A&A...561L...1B 2014A&A...561L...1B
Deleuil et al., Paper XI 2014A&A...564A..56D 2014A&A...564A..56D
Santerne et al., Paper XII 2014A&A...571A..37S 2014A&A...571A..37S, Cat. J/A+A/571/A37
Diaz et al., Paper XIII 2014A&A...572A.109D 2014A&A...572A.109D
Bruno et al., Paper XIV 2015A&A...573A.124B 2015A&A...573A.124B, Cat. J/A+A/573/A124
Almenara et al., Paper XV 2015A&A...575A..71A 2015A&A...575A..71A
Bourrier et al., Paper XVI 2015A&A...579A..55B 2015A&A...579A..55B
Santerne et al., Paper XVII 2016A&A...587A..64S 2016A&A...587A..64S, Cat. J/A+A/587/A64
(End) Patricia Vannier [CDS] 07-Apr-2018