Precise masses for the transiting planetary system HD 106315 with HARPS

Autores
Barros, S. C. C.; Gosselin, H.; Lillo-Box, J.; Bayliss, D.; Delgado Mena, E.; Brugger, B.; Santerne, A.; Armstrong, D. J.; Adibekyan, V.; Armstrong, J. D.; Barrado, D.; Bento, J.; Boisse, I.; Bonomo, A. S.; Bouchy, F.; Brown, D. J. A.; Cochran, W. D.; Collier Cameron, A.; Deleuil, M.; Demangeon, O.; Diaz, Rodrigo Fernando; Doyle, A.; Dumusque, X.; Ehrenreich, D.; Espinoza, N.; Faedi, F.; Faria, J. P.; Figueira, P.; Foxell, E.; Hébrard, G.; Hojjatpanah, S.; Jackman, J.; Lendl, M.; Ligi, R.; Lovis, C.; Melo, C.; Mousis, O.; Neal, J. J.; Osborn, H. P.; Pollacco, D.; Santos, N. C.; Sefako, R.; Shporer, A.; Sousa, S. G.; Triaud, A. H. M. J.; Udry, S.; Vigan, A.; Wyttenbach, A.
Año de publicación
2017
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. The multi-planetary system HD 106315 was recently found in K2 data. The planets have periods of Pb ∼ 9.55 and Pc ∼ 21.06 days, and radii of rb = 2.44 ± 0.17 R⊕ and rc = 4.35 ± 0.23 R⊕. The brightness of the host star (V = 9.0 mag) makes it an excellent target for transmission spectroscopy. However, to interpret transmission spectra it is crucial to measure the planetary masses. Aims. We obtained high precision radial velocities for HD 106315 to determine the mass of the two transiting planets discovered with Kepler K2. Our successful observation strategy was carefully tailored to mitigate the effect of stellar variability. Methods. We modelled the new radial velocity data together with the K2 transit photometry and a new ground-based partial transit of HD 106315c to derive system parameters. Results. We estimate the mass of HD 106315b to be 12.6 ± 3.2 M⊕ and the density to be 4.7 ± 1.7 g cm-3, while for HD 106315c we estimate a mass of 15.2 ± 3.7 M⊕ and a density of 1.01 ± 0.29 g cm-3. Hence, despite planet c having a radius almost twice as large as planet b, their masses are consistent with one another. Conclusions. We conclude that HD 106315c has a thick hydrogen-helium gaseous envelope. A detailed investigation of HD 106315b using a planetary interior model constrains the core mass fraction to be 5-29%, and the water mass fraction to be 10-50%. An alternative, not considered by our model, is that HD 106315b is composed of a large rocky core with a thick H-He envelope. Transmission spectroscopy of these planets will give insight into their atmospheric compositions and also help constrain their core compositions.
Fil: Barros, S. C. C.. Universidade Do Porto, Centro de Astrofisica; Portugal
Fil: Gosselin, H.. Laboratoire D'astrophysique de Marseille; Francia. Universite de Toulouse; Francia
Fil: Lillo-Box, J.. European Southern Observatory Santiago; Chile
Fil: Bayliss, D.. Universidad de Ginebra; Suiza
Fil: Delgado Mena, E.. Universidade Do Porto, Centro de Astrofisica; Portugal
Fil: Brugger, B.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Santerne, A.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Armstrong, D. J.. University of Warwick; Reino Unido
Fil: Adibekyan, V.. Universidade Do Porto, Centro de Astrofisica; Portugal
Fil: Armstrong, J. D.. University Of Hawaii System; Estados Unidos
Fil: Barrado, D.. Csic-inta - Centro de Astrobiologia (cab);
Fil: Bento, J.. Australian National University; Australia
Fil: Boisse, I.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Bonomo, A. S.. Istituto Nazionale Di Astrofisica; Italia
Fil: Bouchy, F.. Universidad de Ginebra; Suiza
Fil: Brown, D. J. A.. University of Warwick; Reino Unido
Fil: Cochran, W. D.. University of Texas at Austin; Estados Unidos
Fil: Collier Cameron, A.. University of St. Andrews; Reino Unido
Fil: Deleuil, M.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Demangeon, O.. Universidade Do Porto, Centro de Astrofisica; Portugal
Fil: Diaz, Rodrigo Fernando. Universidad de Ginebra; Suiza. 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. Universidad de Buenos Aires; Argentina
Fil: Doyle, A.. University of Warwick; Reino Unido
Fil: Dumusque, X.. Universidad de Ginebra; Suiza
Fil: Ehrenreich, D.. Universidad de Ginebra; Suiza
Fil: Espinoza, N.. Pontificia Universidad Católica de Chile; Chile. Millennium Institute Of Astrophysics; Chile. Universidad Católica de Chile; Chile
Fil: Faedi, F.. University of Warwick; Reino Unido
Fil: Faria, J. P.. Universidad de Porto; Portugal. Universidade Do Porto, Centro de Astrofisica; Portugal
Fil: Figueira, P.. Universidade Do Porto, Centro de Astrofisica; Portugal
Fil: Foxell, E.. University of Warwick; Reino Unido
Fil: Hébrard, G.. Universite Pierre et Marie Curie; Francia. Aix Marseille Universite; Francia
Fil: Hojjatpanah, S.. Universidade Do Porto, Centro de Astrofisica; Portugal. Universidad de Porto; Portugal
Fil: Jackman, J.. University of Warwick; Reino Unido
Fil: Lendl, M.. Institut Fur Weltraumforschung; Austria
Fil: Ligi, R.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Lovis, C.. Universidad de Ginebra; Suiza
Fil: Melo, C.. European Southern Observatory Santiago; Chile
Fil: Mousis, O.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Neal, J. J.. Universidad de Porto; Portugal. Universidade Do Porto, Centro de Astrofisica; Portugal
Fil: Osborn, H. P.. University of Warwick; Reino Unido
Fil: Pollacco, D.. University of Warwick; Reino Unido
Fil: Santos, N. C.. Universidad de Porto; Portugal. Universidade Do Porto, Centro de Astrofisica; Portugal
Fil: Sefako, R.. South African Astronomical Observatory; Sudáfrica
Fil: Shporer, A.. California Institute of Technology; Estados Unidos
Fil: Sousa, S. G.. Universidade Do Porto, Centro de Astrofisica; Portugal
Fil: Triaud, A. H. M. J.. University Of Cambridge Institute Of Astronomy; Reino Unido
Fil: Udry, S.. Universidad de Ginebra; Suiza
Fil: Vigan, A.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Wyttenbach, A.. Universidad de Ginebra; Suiza
Materia
PLANETS AND SATELLITES: COMPOSITION
PLANETS AND SATELLITES: DETECTION
PLANETS AND SATELLITES: FUNDAMENTAL PARAMETERS
STARS: INDIVIDUAL: HD 106315
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:11336/51858
Acceder
id CONICETDig_2d25114486c14e272378bb8b9b4598a6
oai_identifier_str oai:ri.conicet.gov.ar:11336/51858
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Precise masses for the transiting planetary system HD 106315 with HARPSBarros, S. C. C.Gosselin, H.Lillo-Box, J.Bayliss, D.Delgado Mena, E.Brugger, B.Santerne, A.Armstrong, D. J.Adibekyan, V.Armstrong, J. D.Barrado, D.Bento, J.Boisse, I.Bonomo, A. S.Bouchy, F.Brown, D. J. A.Cochran, W. D.Collier Cameron, A.Deleuil, M.Demangeon, O.Diaz, Rodrigo FernandoDoyle, A.Dumusque, X.Ehrenreich, D.Espinoza, N.Faedi, F.Faria, J. P.Figueira, P.Foxell, E.Hébrard, G.Hojjatpanah, S.Jackman, J.Lendl, M.Ligi, R.Lovis, C.Melo, C.Mousis, O.Neal, J. J.Osborn, H. P.Pollacco, D.Santos, N. C.Sefako, R.Shporer, A.Sousa, S. G.Triaud, A. H. M. J.Udry, S.Vigan, A.Wyttenbach, A.PLANETS AND SATELLITES: COMPOSITIONPLANETS AND SATELLITES: DETECTIONPLANETS AND SATELLITES: FUNDAMENTAL PARAMETERSSTARS: INDIVIDUAL: HD 106315TECHNIQUES: PHOTOMETRICTECHNIQUES: RADIAL VELOCITIEShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. The multi-planetary system HD 106315 was recently found in K2 data. The planets have periods of Pb ∼ 9.55 and Pc ∼ 21.06 days, and radii of rb = 2.44 ± 0.17 R⊕ and rc = 4.35 ± 0.23 R⊕. The brightness of the host star (V = 9.0 mag) makes it an excellent target for transmission spectroscopy. However, to interpret transmission spectra it is crucial to measure the planetary masses. Aims. We obtained high precision radial velocities for HD 106315 to determine the mass of the two transiting planets discovered with Kepler K2. Our successful observation strategy was carefully tailored to mitigate the effect of stellar variability. Methods. We modelled the new radial velocity data together with the K2 transit photometry and a new ground-based partial transit of HD 106315c to derive system parameters. Results. We estimate the mass of HD 106315b to be 12.6 ± 3.2 M⊕ and the density to be 4.7 ± 1.7 g cm-3, while for HD 106315c we estimate a mass of 15.2 ± 3.7 M⊕ and a density of 1.01 ± 0.29 g cm-3. Hence, despite planet c having a radius almost twice as large as planet b, their masses are consistent with one another. Conclusions. We conclude that HD 106315c has a thick hydrogen-helium gaseous envelope. A detailed investigation of HD 106315b using a planetary interior model constrains the core mass fraction to be 5-29%, and the water mass fraction to be 10-50%. An alternative, not considered by our model, is that HD 106315b is composed of a large rocky core with a thick H-He envelope. Transmission spectroscopy of these planets will give insight into their atmospheric compositions and also help constrain their core compositions.Fil: Barros, S. C. C.. Universidade Do Porto, Centro de Astrofisica; PortugalFil: Gosselin, H.. Laboratoire D'astrophysique de Marseille; Francia. Universite de Toulouse; FranciaFil: Lillo-Box, J.. European Southern Observatory Santiago; ChileFil: Bayliss, D.. Universidad de Ginebra; SuizaFil: Delgado Mena, E.. Universidade Do Porto, Centro de Astrofisica; PortugalFil: Brugger, B.. Laboratoire D'astrophysique de Marseille; FranciaFil: Santerne, A.. Laboratoire D'astrophysique de Marseille; FranciaFil: Armstrong, D. J.. University of Warwick; Reino UnidoFil: Adibekyan, V.. Universidade Do Porto, Centro de Astrofisica; PortugalFil: Armstrong, J. D.. University Of Hawaii System; Estados UnidosFil: Barrado, D.. Csic-inta - Centro de Astrobiologia (cab);Fil: Bento, J.. Australian National University; AustraliaFil: Boisse, I.. Laboratoire D'astrophysique de Marseille; FranciaFil: Bonomo, A. S.. Istituto Nazionale Di Astrofisica; ItaliaFil: Bouchy, F.. Universidad de Ginebra; SuizaFil: Brown, D. J. A.. University of Warwick; Reino UnidoFil: Cochran, W. D.. University of Texas at Austin; Estados UnidosFil: Collier Cameron, A.. University of St. Andrews; Reino UnidoFil: Deleuil, M.. Laboratoire D'astrophysique de Marseille; FranciaFil: Demangeon, O.. Universidade Do Porto, Centro de Astrofisica; PortugalFil: Diaz, Rodrigo Fernando. Universidad de Ginebra; Suiza. 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. Universidad de Buenos Aires; ArgentinaFil: Doyle, A.. University of Warwick; Reino UnidoFil: Dumusque, X.. Universidad de Ginebra; SuizaFil: Ehrenreich, D.. Universidad de Ginebra; SuizaFil: Espinoza, N.. Pontificia Universidad Católica de Chile; Chile. Millennium Institute Of Astrophysics; Chile. Universidad Católica de Chile; ChileFil: Faedi, F.. University of Warwick; Reino UnidoFil: Faria, J. P.. Universidad de Porto; Portugal. Universidade Do Porto, Centro de Astrofisica; PortugalFil: Figueira, P.. Universidade Do Porto, Centro de Astrofisica; PortugalFil: Foxell, E.. University of Warwick; Reino UnidoFil: Hébrard, G.. Universite Pierre et Marie Curie; Francia. Aix Marseille Universite; FranciaFil: Hojjatpanah, S.. Universidade Do Porto, Centro de Astrofisica; Portugal. Universidad de Porto; PortugalFil: Jackman, J.. University of Warwick; Reino UnidoFil: Lendl, M.. Institut Fur Weltraumforschung; AustriaFil: Ligi, R.. Laboratoire D'astrophysique de Marseille; FranciaFil: Lovis, C.. Universidad de Ginebra; SuizaFil: Melo, C.. European Southern Observatory Santiago; ChileFil: Mousis, O.. Laboratoire D'astrophysique de Marseille; FranciaFil: Neal, J. J.. Universidad de Porto; Portugal. Universidade Do Porto, Centro de Astrofisica; PortugalFil: Osborn, H. P.. University of Warwick; Reino UnidoFil: Pollacco, D.. University of Warwick; Reino UnidoFil: Santos, N. C.. Universidad de Porto; Portugal. Universidade Do Porto, Centro de Astrofisica; PortugalFil: Sefako, R.. South African Astronomical Observatory; SudáfricaFil: Shporer, A.. California Institute of Technology; Estados UnidosFil: Sousa, S. G.. Universidade Do Porto, Centro de Astrofisica; PortugalFil: Triaud, A. H. M. J.. University Of Cambridge Institute Of Astronomy; Reino UnidoFil: Udry, S.. Universidad de Ginebra; SuizaFil: Vigan, A.. Laboratoire D'astrophysique de Marseille; FranciaFil: Wyttenbach, A.. Universidad de Ginebra; SuizaEDP Sciences2017-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/51858Barros, S. C. C.; Gosselin, H.; Lillo-Box, J.; Bayliss, D.; Delgado Mena, E.; et al.; Precise masses for the transiting planetary system HD 106315 with HARPS; EDP Sciences; Astronomy and Astrophysics; 608; A25; 12-2017; 1-140004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/10.1051/0004-6361/201731276info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201731276info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:55:23Zoai:ri.conicet.gov.ar:11336/51858instacron: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:34982025-09-29 09:55:23.776CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Precise masses for the transiting planetary system HD 106315 with HARPS
title Precise masses for the transiting planetary system HD 106315 with HARPS
spellingShingle Precise masses for the transiting planetary system HD 106315 with HARPS
Barros, S. C. C.
PLANETS AND SATELLITES: COMPOSITION
PLANETS AND SATELLITES: DETECTION
PLANETS AND SATELLITES: FUNDAMENTAL PARAMETERS
STARS: INDIVIDUAL: HD 106315
TECHNIQUES: PHOTOMETRIC
TECHNIQUES: RADIAL VELOCITIES
title_short Precise masses for the transiting planetary system HD 106315 with HARPS
title_full Precise masses for the transiting planetary system HD 106315 with HARPS
title_fullStr Precise masses for the transiting planetary system HD 106315 with HARPS
title_full_unstemmed Precise masses for the transiting planetary system HD 106315 with HARPS
title_sort Precise masses for the transiting planetary system HD 106315 with HARPS
dc.creator.none.fl_str_mv Barros, S. C. C.
Gosselin, H.
Lillo-Box, J.
Bayliss, D.
Delgado Mena, E.
Brugger, B.
Santerne, A.
Armstrong, D. J.
Adibekyan, V.
Armstrong, J. D.
Barrado, D.
Bento, J.
Boisse, I.
Bonomo, A. S.
Bouchy, F.
Brown, D. J. A.
Cochran, W. D.
Collier Cameron, A.
Deleuil, M.
Demangeon, O.
Diaz, Rodrigo Fernando
Doyle, A.
Dumusque, X.
Ehrenreich, D.
Espinoza, N.
Faedi, F.
Faria, J. P.
Figueira, P.
Foxell, E.
Hébrard, G.
Hojjatpanah, S.
Jackman, J.
Lendl, M.
Ligi, R.
Lovis, C.
Melo, C.
Mousis, O.
Neal, J. J.
Osborn, H. P.
Pollacco, D.
Santos, N. C.
Sefako, R.
Shporer, A.
Sousa, S. G.
Triaud, A. H. M. J.
Udry, S.
Vigan, A.
Wyttenbach, A.
author Barros, S. C. C.
author_facet Barros, S. C. C.
Gosselin, H.
Lillo-Box, J.
Bayliss, D.
Delgado Mena, E.
Brugger, B.
Santerne, A.
Armstrong, D. J.
Adibekyan, V.
Armstrong, J. D.
Barrado, D.
Bento, J.
Boisse, I.
Bonomo, A. S.
Bouchy, F.
Brown, D. J. A.
Cochran, W. D.
Collier Cameron, A.
Deleuil, M.
Demangeon, O.
Diaz, Rodrigo Fernando
Doyle, A.
Dumusque, X.
Ehrenreich, D.
Espinoza, N.
Faedi, F.
Faria, J. P.
Figueira, P.
Foxell, E.
Hébrard, G.
Hojjatpanah, S.
Jackman, J.
Lendl, M.
Ligi, R.
Lovis, C.
Melo, C.
Mousis, O.
Neal, J. J.
Osborn, H. P.
Pollacco, D.
Santos, N. C.
Sefako, R.
Shporer, A.
Sousa, S. G.
Triaud, A. H. M. J.
Udry, S.
Vigan, A.
Wyttenbach, A.
author_role author
author2 Gosselin, H.
Lillo-Box, J.
Bayliss, D.
Delgado Mena, E.
Brugger, B.
Santerne, A.
Armstrong, D. J.
Adibekyan, V.
Armstrong, J. D.
Barrado, D.
Bento, J.
Boisse, I.
Bonomo, A. S.
Bouchy, F.
Brown, D. J. A.
Cochran, W. D.
Collier Cameron, A.
Deleuil, M.
Demangeon, O.
Diaz, Rodrigo Fernando
Doyle, A.
Dumusque, X.
Ehrenreich, D.
Espinoza, N.
Faedi, F.
Faria, J. P.
Figueira, P.
Foxell, E.
Hébrard, G.
Hojjatpanah, S.
Jackman, J.
Lendl, M.
Ligi, R.
Lovis, C.
Melo, C.
Mousis, O.
Neal, J. J.
Osborn, H. P.
Pollacco, D.
Santos, N. C.
Sefako, R.
Shporer, A.
Sousa, S. G.
Triaud, A. H. M. J.
Udry, S.
Vigan, A.
Wyttenbach, A.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
author
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author
dc.subject.none.fl_str_mv PLANETS AND SATELLITES: COMPOSITION
PLANETS AND SATELLITES: DETECTION
PLANETS AND SATELLITES: FUNDAMENTAL PARAMETERS
STARS: INDIVIDUAL: HD 106315
TECHNIQUES: PHOTOMETRIC
TECHNIQUES: RADIAL VELOCITIES
topic PLANETS AND SATELLITES: COMPOSITION
PLANETS AND SATELLITES: DETECTION
PLANETS AND SATELLITES: FUNDAMENTAL PARAMETERS
STARS: INDIVIDUAL: HD 106315
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 Context. The multi-planetary system HD 106315 was recently found in K2 data. The planets have periods of Pb ∼ 9.55 and Pc ∼ 21.06 days, and radii of rb = 2.44 ± 0.17 R⊕ and rc = 4.35 ± 0.23 R⊕. The brightness of the host star (V = 9.0 mag) makes it an excellent target for transmission spectroscopy. However, to interpret transmission spectra it is crucial to measure the planetary masses. Aims. We obtained high precision radial velocities for HD 106315 to determine the mass of the two transiting planets discovered with Kepler K2. Our successful observation strategy was carefully tailored to mitigate the effect of stellar variability. Methods. We modelled the new radial velocity data together with the K2 transit photometry and a new ground-based partial transit of HD 106315c to derive system parameters. Results. We estimate the mass of HD 106315b to be 12.6 ± 3.2 M⊕ and the density to be 4.7 ± 1.7 g cm-3, while for HD 106315c we estimate a mass of 15.2 ± 3.7 M⊕ and a density of 1.01 ± 0.29 g cm-3. Hence, despite planet c having a radius almost twice as large as planet b, their masses are consistent with one another. Conclusions. We conclude that HD 106315c has a thick hydrogen-helium gaseous envelope. A detailed investigation of HD 106315b using a planetary interior model constrains the core mass fraction to be 5-29%, and the water mass fraction to be 10-50%. An alternative, not considered by our model, is that HD 106315b is composed of a large rocky core with a thick H-He envelope. Transmission spectroscopy of these planets will give insight into their atmospheric compositions and also help constrain their core compositions.
Fil: Barros, S. C. C.. Universidade Do Porto, Centro de Astrofisica; Portugal
Fil: Gosselin, H.. Laboratoire D'astrophysique de Marseille; Francia. Universite de Toulouse; Francia
Fil: Lillo-Box, J.. European Southern Observatory Santiago; Chile
Fil: Bayliss, D.. Universidad de Ginebra; Suiza
Fil: Delgado Mena, E.. Universidade Do Porto, Centro de Astrofisica; Portugal
Fil: Brugger, B.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Santerne, A.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Armstrong, D. J.. University of Warwick; Reino Unido
Fil: Adibekyan, V.. Universidade Do Porto, Centro de Astrofisica; Portugal
Fil: Armstrong, J. D.. University Of Hawaii System; Estados Unidos
Fil: Barrado, D.. Csic-inta - Centro de Astrobiologia (cab);
Fil: Bento, J.. Australian National University; Australia
Fil: Boisse, I.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Bonomo, A. S.. Istituto Nazionale Di Astrofisica; Italia
Fil: Bouchy, F.. Universidad de Ginebra; Suiza
Fil: Brown, D. J. A.. University of Warwick; Reino Unido
Fil: Cochran, W. D.. University of Texas at Austin; Estados Unidos
Fil: Collier Cameron, A.. University of St. Andrews; Reino Unido
Fil: Deleuil, M.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Demangeon, O.. Universidade Do Porto, Centro de Astrofisica; Portugal
Fil: Diaz, Rodrigo Fernando. Universidad de Ginebra; Suiza. 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. Universidad de Buenos Aires; Argentina
Fil: Doyle, A.. University of Warwick; Reino Unido
Fil: Dumusque, X.. Universidad de Ginebra; Suiza
Fil: Ehrenreich, D.. Universidad de Ginebra; Suiza
Fil: Espinoza, N.. Pontificia Universidad Católica de Chile; Chile. Millennium Institute Of Astrophysics; Chile. Universidad Católica de Chile; Chile
Fil: Faedi, F.. University of Warwick; Reino Unido
Fil: Faria, J. P.. Universidad de Porto; Portugal. Universidade Do Porto, Centro de Astrofisica; Portugal
Fil: Figueira, P.. Universidade Do Porto, Centro de Astrofisica; Portugal
Fil: Foxell, E.. University of Warwick; Reino Unido
Fil: Hébrard, G.. Universite Pierre et Marie Curie; Francia. Aix Marseille Universite; Francia
Fil: Hojjatpanah, S.. Universidade Do Porto, Centro de Astrofisica; Portugal. Universidad de Porto; Portugal
Fil: Jackman, J.. University of Warwick; Reino Unido
Fil: Lendl, M.. Institut Fur Weltraumforschung; Austria
Fil: Ligi, R.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Lovis, C.. Universidad de Ginebra; Suiza
Fil: Melo, C.. European Southern Observatory Santiago; Chile
Fil: Mousis, O.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Neal, J. J.. Universidad de Porto; Portugal. Universidade Do Porto, Centro de Astrofisica; Portugal
Fil: Osborn, H. P.. University of Warwick; Reino Unido
Fil: Pollacco, D.. University of Warwick; Reino Unido
Fil: Santos, N. C.. Universidad de Porto; Portugal. Universidade Do Porto, Centro de Astrofisica; Portugal
Fil: Sefako, R.. South African Astronomical Observatory; Sudáfrica
Fil: Shporer, A.. California Institute of Technology; Estados Unidos
Fil: Sousa, S. G.. Universidade Do Porto, Centro de Astrofisica; Portugal
Fil: Triaud, A. H. M. J.. University Of Cambridge Institute Of Astronomy; Reino Unido
Fil: Udry, S.. Universidad de Ginebra; Suiza
Fil: Vigan, A.. Laboratoire D'astrophysique de Marseille; Francia
Fil: Wyttenbach, A.. Universidad de Ginebra; Suiza
description Context. The multi-planetary system HD 106315 was recently found in K2 data. The planets have periods of Pb ∼ 9.55 and Pc ∼ 21.06 days, and radii of rb = 2.44 ± 0.17 R⊕ and rc = 4.35 ± 0.23 R⊕. The brightness of the host star (V = 9.0 mag) makes it an excellent target for transmission spectroscopy. However, to interpret transmission spectra it is crucial to measure the planetary masses. Aims. We obtained high precision radial velocities for HD 106315 to determine the mass of the two transiting planets discovered with Kepler K2. Our successful observation strategy was carefully tailored to mitigate the effect of stellar variability. Methods. We modelled the new radial velocity data together with the K2 transit photometry and a new ground-based partial transit of HD 106315c to derive system parameters. Results. We estimate the mass of HD 106315b to be 12.6 ± 3.2 M⊕ and the density to be 4.7 ± 1.7 g cm-3, while for HD 106315c we estimate a mass of 15.2 ± 3.7 M⊕ and a density of 1.01 ± 0.29 g cm-3. Hence, despite planet c having a radius almost twice as large as planet b, their masses are consistent with one another. Conclusions. We conclude that HD 106315c has a thick hydrogen-helium gaseous envelope. A detailed investigation of HD 106315b using a planetary interior model constrains the core mass fraction to be 5-29%, and the water mass fraction to be 10-50%. An alternative, not considered by our model, is that HD 106315b is composed of a large rocky core with a thick H-He envelope. Transmission spectroscopy of these planets will give insight into their atmospheric compositions and also help constrain their core compositions.
publishDate 2017
dc.date.none.fl_str_mv 2017-12
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/11336/51858
Barros, S. C. C.; Gosselin, H.; Lillo-Box, J.; Bayliss, D.; Delgado Mena, E.; et al.; Precise masses for the transiting planetary system HD 106315 with HARPS; EDP Sciences; Astronomy and Astrophysics; 608; A25; 12-2017; 1-14
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/51858
identifier_str_mv Barros, S. C. C.; Gosselin, H.; Lillo-Box, J.; Bayliss, D.; Delgado Mena, E.; et al.; Precise masses for the transiting planetary system HD 106315 with HARPS; EDP Sciences; Astronomy and Astrophysics; 608; A25; 12-2017; 1-14
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/url/http://www.aanda.org/10.1051/0004-6361/201731276
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201731276
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_ 1844613670465699840
score 13.070432

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