Abstract
Kepler-419 is a planetary system discovered by the Kepler photometry which is known to harbour two massive giant planets: an inner 3 M J transiting planet with a 69.8-day period, highly eccentric orbit, and an outer 7.5 M J 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 0.03 au. This suggests a mechanism for forming hot Jupiters in multiplanetary systems without the need of high mutual inclinations.
Original language | English |
---|---|
Article number | A90 |
Number of pages | 16 |
Journal | Astronomy & Astrophysics |
Volume | 615 |
DOIs | |
Publication status | Published - Jul 2018 |
Keywords
- Planetary systems
- Techniques: photometric
- Techniques: radial velocities
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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.; Díaz, R. F.; Hébrard, G. et al.
In: Astronomy & Astrophysics, Vol. 615, A90, 07.2018.Research output: Contribution to journal › Article › Research › peer-review
TY - JOUR
T1 - SOPHIE velocimetry of Kepler transit candidates XVIII. Radial velocity confirmation, absolute masses and radii, and origin of the Kepler-419 multiplanetary system
AU - Almenara, J. M.
AU - Díaz, R. F.
AU - Hébrard, G.
AU - Mardling, R.
AU - Damiani, C.
AU - Santerne, A.
AU - Bouchy, F.
AU - Barros, S. C.C.
AU - Boisse, I.
AU - Bonfils, X.
AU - Bonomo, A. S.
AU - Courcol, B.
AU - Demangeon, O.
AU - Deleuil, M.
AU - Rey, J.
AU - Udry, S.
AU - Wilson, P. A.
N1 - Funding Information: pDoíianz,tRa.tF.(,ϖAlm−enaϖra,J.=Mp.,i,Seante=rne0,.A8.3,)etwal.it2h01a4n,MaNvRerAaSg,e44p1e,9ri8a3stronafterA13410years,withthesystemremainingtrappednearthefixed TParokveednac,eGf.o,rKtihteai,rRs.u,p&poRrtaswioit,hFt.hAe.S2O0P0H8,IAEpinJ,st6r8u3m,e1n0t6a3nd the 1.93 m telescope Dotter,A.,Chaboyer,B.,Jevremovic´,D.,etal.2008,ApJS,178,89bcb Uanddr,y,inS.p,aMrtaicyuolra,r,Mfo.,r&thSeaenstosesn,tNia.lCw.o2r0k03o,fAth&eAn,ig4h0t7,as3s6i9stants. Financial sup- Doyle,L.R.,Carter,J.A.,Fabrycky,D.C.,etal.2011,Science,333,1602separationof0.06au.In contrast,CaseII initiallyachieves a Vpoorgtt,foSr.tShe.,SAOllPeHn,IES.oLb.s,eBrviagteiloonws,frBo.mCt.h, eetParol.g1ra9m94m, einNPartoiocn.aSlPdIeEP, lVaonlé.to2l1o9g8ie, maximumeccentricityof0.96duringashortperiodoflibration, (PNInPs)torufmCeNnRtaSti/oINnSinUA,Fsrtraonncoem,isygVraIItIe,fuedll.yDac.kLn.oCwrlaewdfgoerdd.W&eEa.lRso.Cacrkaninoew,l3e6d2ge Fabrycky, D. & Tremaine, S. 2007, ApJ, 669, 1298 Weiss, L. M., Marcy, G. W., Rowe, J. F., et al. 2013, ApJ, 768, 14 after which it escapes the librating region with a non-oscillatory support from the French National Research Agency (ANR-08-JCJC-0102-01). eFcocreemntarni-cMitayc,keayn,dD.t,hHuosgga,Dp.eWrm.,aLnanegn,tDly.,&lowGoopdemriaans,tJr.o2n01s3e,pPAarSaPt,i1o2n5.,Ford,E.B.,Ragozzine,D.,Rowe,J.F.,etal.2012,ApJ,756,185 WWerigthhta,nEk. LL.., EKirseeindhbaerrdgt,fPo.rRh.eMr .M, Manadinezl e&r, AA.gKo.l, ectoadle. 2a0n1d0,YA. JR, e1v4a0z, 1f8o6r8his 306 Zasescihstmanecisetewr,iMth.t&heKcüormstpeur,tiMng. 2c0lu0s9t,eAr &usAed, 4i9n6t,h5i7s7work. This paper includes Goldreich,P.&Schlichting,H.E.2014,AJ,147,32With an average periastronseparationof0.02 au, circularisa- data collected by the Kepler mission. Funding for the Kepler mission is pro-Goodman,J.&Weare,J.2010,Communicationsinappliedmathematicsandtionis rapid.Weemphasisethat the onlydifferencebetween vided by the NASA Science Mission directorate. Some of the data presented the two cases is the inital value of the difference in the apsidal in this paper were obtained from the Mikulski Archive for Space Telescopes lHonolgmiatun,dMes..J., Fabrycky, D. C., Ragozzine, D., et al. 2010, Science, 330, 51 (MAST). This research has made use of the Exoplanet Orbit Database and Panels e and f show the dependence of the values of eb and siblethroughtheuseof theAAVSOPhotometric All-SkySurvey(APASS),the ExoplanetDataExploreratexoplanets.org.Thisresearchwasmadepos- abIrwin, atJ.10B8.1952,yr, 10Ap9J,116,yr, a211nd 2.3 × 109 yr (the estimated age of funded by the Robert Martin Ayers Sciences Fund. This publication makes Kipping, D. M. 2010, MNRAS, 408, 1758 the system) on the initial difference in the apsidal longitudes, use of data products from the Two Micron All Sky Survey, which is a joint sKuogsgtoevs,tVin. gB.,thMactCtuhlleoulgohn, gP.-Rte.,rmCarstetra,tJe. Ao.f, eat asly. 2st0e1m4, AlipkJe, 7K84e, p14ler-419 project of the University of Massachusetts and the Infrared Processing and isLi,hG.,ighNaoz,ly dependentS., Kocsis, B.,on& Loeb,the vA.alu2014,e ofApJ,ϖb785,− ϖ116c at the time it Analysis Center/California Institute of Technology, funded by the National Aero- Mamajek, E. E., Prsa, A., Torres, G., et al. 2015, ArXiv e-prints nautics and Space Administration and the National Science Foundation. This [arXiv:1510.07674]wasbrought to thatstate (via collision or some other mecha- publication makes use of data products from the Wide-field Infrared Survey Mancini,L.,Lillo-Box,J.,Southworth,J.,etal.2016,A&A,590,A112nism).FortheadoptedQ-valuethesystemhascircularisedafter Explorer, which is a joint project of the University of California, Los Ange- 2M.3an×de1l,0K9. &yrA, gsoul,gEg.e2s0t0in2g, AtphJa, t58t0h,eL1t7ru1e Q-value is higher or has les, and the Jet Propulsion Laboratory/California Institute of Technology, funded Funding Information: by the National Aeronautics and Space Administration. Simulations in this paper made use of the REBOUND code which can be downloaded freely at http://github.com/hannorein/rebound. These simulations have been run on the Regor cluster kindly provided by the Observatoire de Genève. This publication makes use of The Data & Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planets data visualisation, exchange, and analysis. DACE is a platform of the Swiss National Centre of Competence in Research (NCCR) PlanetS, federating the Swiss expertise in Exoplanet research. The DACE platform is available at https://dace.unige.ch. This work has been carried out within the framework of the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation. The authors acknowledge the financial support of the SNSF. S.C.C.B. acknowledges support by the Fundação para a Ciência e a Tecnologia (FCT) through the Investigador FCT Contract IF/01312/2014/CP1215/CT0004 and also acknowledges support from FCT through national funds and by FEDER through COMPETE2020 by these grants UID/FIS/04434/2013 & POCI-01-0145-FEDER-007672 and PTDC/FIS-AST/1526/2014 & POCI-01-0145-FEDER-016886. A.S.B. acknowledges funding from the European Union Seventh Framework programme (FP7/2007-2013) under grant agreement No. 313014 (ETAEARTH). Funding Information: We thank Rebekah I. Dawson and Geoffrey W. Marcy for helpful discussions. We thank the technical team at the Observatoire de Haute-Provence for their support with the SOPHIE instrument and the 1.93 m telescope and, in particular, for the essential work of the night assistants. Financial support for the SOPHIE observations from the Programme National de Planétologie (PNP) of CNRS/INSU, France, is gratefully acknowledged. We also acknowledge support from the French National Research Agency (ANR-08- JCJC-0102-01). We thank L. Kreidberg for her Mandel & Agol code and Y. Revaz for his assistance with the computing cluster used in this work. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org. This research was made possible through the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Ange-les, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Simulations in this paper made use of the REBOUND code which can be downloaded freely at http://github.com/hannorein/rebound. These simulations have been run on the Regor cluster kindly provided by the Observatoire de Genève. This publication makes use of The Data & Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planets data visualisation, exchange, and analysis. DACE is a platform of the Swiss National Centre of Competence in Research (NCCR) PlanetS, federating the Swiss expertise in Exoplanet research. The DACE platform is available at https://dace.unige.ch. This work has been carried out within the framework of the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation. The authors acknowledge the financial support of the SNSF. S.C.C.B. acknowledges support by the Fundação para a Ciência e a Tecnologia (FCT) through the Investigador FCT Contract IF/01312/2014/CP1215/CT0004 and also acknowledges support from FCT through national funds and by FEDER through COMPETE2020 by these grants UID/FIS/04434/2013 & POCI-01-0145-FEDER-007672 and PTDC/FIS-AST/1526/2014 & POCI-01-0145-FEDER-016886. A.S.B. acknowledges funding from the European Union Seventh Framework programme (FP7/2007-2013) under grant agreement No. 313014 (ETAEARTH). Publisher Copyright: © ESO 2018
PY - 2018/7
Y1 - 2018/7
N2 - Kepler-419 is a planetary system discovered by the Kepler photometry which is known to harbour two massive giant planets: an inner 3 M J transiting planet with a 69.8-day period, highly eccentric orbit, and an outer 7.5 M J 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 0.03 au. This suggests a mechanism for forming hot Jupiters in multiplanetary systems without the need of high mutual inclinations.
AB - Kepler-419 is a planetary system discovered by the Kepler photometry which is known to harbour two massive giant planets: an inner 3 M J transiting planet with a 69.8-day period, highly eccentric orbit, and an outer 7.5 M J 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 0.03 au. This suggests a mechanism for forming hot Jupiters in multiplanetary systems without the need of high mutual inclinations.
KW - Planetary systems
KW - Techniques: photometric
KW - Techniques: radial velocities
UR - http://www.scopus.com/inward/record.url?scp=85056719286&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/201732500
DO - 10.1051/0004-6361/201732500
M3 - Article
AN - SCOPUS:85056719286
VL - 615
JO - Astronomy & Astrophysics
JF - Astronomy & Astrophysics
SN - 0004-6361
M1 - A90
ER -