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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/81812
Ver los metadatos del registro completo
id |
CONICETDig_5c773738d63733b065fd2983099bdad6 |
---|---|
oai_identifier_str |
oai:ri.conicet.gov.ar:11336/81812 |
network_acronym_str |
CONICETDig |
repository_id_str |
3498 |
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 |
_version_ |
1846083355715567616 |
score |
13.22299 |