SOPHIE velocimetry of Kepler transit candidates XVIII. Radial velocity confirmation, absolute masses and radii, and origin of the Kepler-419 multiplanetary system

Autores
Almenara, J. M.; Diaz, Rodrigo Fernando; Hébrard, 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.
Año de publicación
2018
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
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.
Fil: Almenara, J. M.. Universidad de Ginebra; Suiza
Fil: Diaz, Rodrigo Fernando. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Hébrard, G.. Observatoire de Haute-provence; Francia
Fil: Mardling, R.. Universidad de Ginebra; Suiza. Monash University; Australia
Fil: Damiani, C.. Universite Paris-sud Xi; Francia
Fil: Santerne, A.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Bouchy, F.. Universidad de Ginebra; Suiza
Fil: Barros, S.C.C.. Universidade Do Porto, Centro de Astrofísica; Portugal
Fil: Boisse, I.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Bonfils, X.. Universite Grenoble Alpes; Francia
Fil: Bonomo, A.S.. Istituto Nazionale di Astrofisica; Italia
Fil: Courcol, B.. Universite Grenoble Alpes; Francia
Fil: Demangeon, O.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Deleuil, M.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Rey, J.. Universidad de Ginebra; Suiza
Fil: Udry, S.. Universidad de Ginebra; Suiza
Fil: Wilson, P.A.. Institut D 'astrophysique de Paris; Francia
Materia
PLANETARY SYSTEMS
TECHNIQUES: PHOTOMETRIC
TECHNIQUES: RADIAL VELOCITIES
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/81812

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network_name_str CONICET Digital (CONICET)
spelling SOPHIE velocimetry of Kepler transit candidates XVIII. Radial velocity confirmation, absolute masses and radii, and origin of the Kepler-419 multiplanetary systemAlmenara, J. M.Diaz, Rodrigo FernandoHébrard, 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.PLANETARY SYSTEMSTECHNIQUES: PHOTOMETRICTECHNIQUES: RADIAL VELOCITIEShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Kepler-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.Fil: Almenara, J. M.. Universidad de Ginebra; SuizaFil: Diaz, Rodrigo Fernando. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Hébrard, G.. Observatoire de Haute-provence; FranciaFil: Mardling, R.. Universidad de Ginebra; Suiza. Monash University; AustraliaFil: Damiani, C.. Universite Paris-sud Xi; FranciaFil: Santerne, A.. Laboratoire D'astrophysique de Marseille; FranciaFil: Bouchy, F.. Universidad de Ginebra; SuizaFil: Barros, S.C.C.. Universidade Do Porto, Centro de Astrofísica; PortugalFil: Boisse, I.. Laboratoire D'astrophysique de Marseille; FranciaFil: Bonfils, X.. Universite Grenoble Alpes; FranciaFil: Bonomo, A.S.. Istituto Nazionale di Astrofisica; ItaliaFil: Courcol, B.. Universite Grenoble Alpes; FranciaFil: Demangeon, O.. Laboratoire D'astrophysique de Marseille; FranciaFil: Deleuil, M.. Laboratoire D'astrophysique de Marseille; FranciaFil: Rey, J.. Universidad de Ginebra; SuizaFil: Udry, S.. Universidad de Ginebra; SuizaFil: Wilson, P.A.. Institut D 'astrophysique de Paris; FranciaEDP Sciences2018-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/81812Almenara, J. M.; Diaz, Rodrigo Fernando; Hébrard, G.; Mardling, R.; Damiani, C.; et al.; SOPHIE velocimetry of Kepler transit candidates XVIII. Radial velocity confirmation, absolute masses and radii, and origin of the Kepler-419 multiplanetary system; EDP Sciences; Astronomy and Astrophysics; 615; A90; 7-2018; 1-160004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201732500info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T15:20:41Zoai:ri.conicet.gov.ar:11336/81812instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-15 15:20:42.034CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv SOPHIE velocimetry of Kepler transit candidates XVIII. Radial velocity confirmation, absolute masses and radii, and origin of the Kepler-419 multiplanetary system
title SOPHIE velocimetry of Kepler transit candidates XVIII. Radial velocity confirmation, absolute masses and radii, and origin of the Kepler-419 multiplanetary system
spellingShingle 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.
PLANETARY SYSTEMS
TECHNIQUES: PHOTOMETRIC
TECHNIQUES: RADIAL VELOCITIES
title_short SOPHIE velocimetry of Kepler transit candidates XVIII. Radial velocity confirmation, absolute masses and radii, and origin of the Kepler-419 multiplanetary system
title_full SOPHIE velocimetry of Kepler transit candidates XVIII. Radial velocity confirmation, absolute masses and radii, and origin of the Kepler-419 multiplanetary system
title_fullStr SOPHIE velocimetry of Kepler transit candidates XVIII. Radial velocity confirmation, absolute masses and radii, and origin of the Kepler-419 multiplanetary system
title_full_unstemmed SOPHIE velocimetry of Kepler transit candidates XVIII. Radial velocity confirmation, absolute masses and radii, and origin of the Kepler-419 multiplanetary system
title_sort SOPHIE velocimetry of Kepler transit candidates XVIII. Radial velocity confirmation, absolute masses and radii, and origin of the Kepler-419 multiplanetary system
dc.creator.none.fl_str_mv Almenara, J. M.
Diaz, Rodrigo Fernando
Hébrard, 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.
author Almenara, J. M.
author_facet Almenara, J. M.
Diaz, Rodrigo Fernando
Hébrard, 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.
author_role author
author2 Diaz, Rodrigo Fernando
Hébrard, 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.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv PLANETARY SYSTEMS
TECHNIQUES: PHOTOMETRIC
TECHNIQUES: RADIAL VELOCITIES
topic PLANETARY SYSTEMS
TECHNIQUES: PHOTOMETRIC
TECHNIQUES: RADIAL VELOCITIES
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv 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.
Fil: Almenara, J. M.. Universidad de Ginebra; Suiza
Fil: Diaz, Rodrigo Fernando. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Hébrard, G.. Observatoire de Haute-provence; Francia
Fil: Mardling, R.. Universidad de Ginebra; Suiza. Monash University; Australia
Fil: Damiani, C.. Universite Paris-sud Xi; Francia
Fil: Santerne, A.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Bouchy, F.. Universidad de Ginebra; Suiza
Fil: Barros, S.C.C.. Universidade Do Porto, Centro de Astrofísica; Portugal
Fil: Boisse, I.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Bonfils, X.. Universite Grenoble Alpes; Francia
Fil: Bonomo, A.S.. Istituto Nazionale di Astrofisica; Italia
Fil: Courcol, B.. Universite Grenoble Alpes; Francia
Fil: Demangeon, O.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Deleuil, M.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Rey, J.. Universidad de Ginebra; Suiza
Fil: Udry, S.. Universidad de Ginebra; Suiza
Fil: Wilson, P.A.. Institut D 'astrophysique de Paris; Francia
description 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.
publishDate 2018
dc.date.none.fl_str_mv 2018-07
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/81812
Almenara, J. M.; Diaz, Rodrigo Fernando; Hébrard, G.; Mardling, R.; Damiani, C.; et al.; SOPHIE velocimetry of Kepler transit candidates XVIII. Radial velocity confirmation, absolute masses and radii, and origin of the Kepler-419 multiplanetary system; EDP Sciences; Astronomy and Astrophysics; 615; A90; 7-2018; 1-16
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/81812
identifier_str_mv Almenara, J. M.; Diaz, Rodrigo Fernando; Hébrard, G.; Mardling, R.; Damiani, C.; et al.; SOPHIE velocimetry of Kepler transit candidates XVIII. Radial velocity confirmation, absolute masses and radii, and origin of the Kepler-419 multiplanetary system; EDP Sciences; Astronomy and Astrophysics; 615; A90; 7-2018; 1-16
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201732500
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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