Radial-velocity fitting challenge. II. First results of the analysis of the data set
- Autores
- Dumusque, X.; Borsa, F.; Damasso, M.; Diaz, Rodrigo Fernando; Gregory, P. C.; Hara, N. C.; Hatzes, A.; Rajpaul, V.; Tuomi, M.; Aigrain, S.; Anglada Escudé, G.; Bonomo, A. S.; Boué, G.; Dauvergne, F.; Frustagli, G.; Giacobbe, P.; Haywood, R. D.; Jones, H. R. A.; Laskar, J.; Pinamonti, M.; Poretti, E.; Rainer, M.; Ségransan, D.; Sozzetti, A.; Udry, S.
- Año de publicación
- 2017
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Context. Radial-velocity (RV) signals arising from stellar photospheric phenomena are the main limitation for precise RV measurements. Those signals induce RV variations an order of magnitude larger than the signal created by the orbit of Earth-twins, thus preventing their detection. Aims. Different methods have been developed to mitigate the impact of stellar RV signals. The goal of this paper is to compare the efficiency of these different methods to recover extremely low-mass planets despite stellar RV signals. However, because observed RV variations at the meter-per-second precision level or below is a combination of signals induced by unresolved orbiting planets, by the star, and by the instrument, performing such a comparison using real data is extremely challenging. Methods. To circumvent this problem, we generated simulated RV measurements including realistic stellar and planetary signals. Different teams analyzed blindly those simulated RV measurements, using their own method to recover planetary signals despite stellar RV signals. By comparing the results obtained by the different teams with the planetary and stellar parameters used to generate the simulated RVs, it is therefore possible to compare the efficiency of these different methods. Results. The most efficient methods to recover planetary signals take into account the different activity indicators, use red-noise models to account for stellar RV signals and a Bayesian framework to provide model comparison in a robust statistical approach. Using the most efficient methodology, planets can be found down to with a threshold of K/N = 7.5 at the level of 80–90% recovery rate found for a number of methods. These recovery rates drop dramatically for K/N smaller than this threshold. In addition, for the best teams, no false positives with K/N > 7.5 were detected, while a non-negligible fraction of them appear for smaller K/N. A limit of K/N = 7.5 seems therefore a safe threshold to attest the veracity of planetary signals for RV measurements with similar properties to those of the different RV fitting challenge systems.
Fil: Dumusque, X.. Université de Genève; Suiza
Fil: Borsa, F.. Osservatorio Astronomico di Brera; Italia
Fil: Damasso, M.. Osservatorio Astrofisico di Torino; Italia
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. Université de Genève; Suiza
Fil: Gregory, P. C.. University Of British Columbia; Canadá
Fil: Hara, N. C.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Hatzes, A.. Thüringer Landessternwarte Tautenburg; Alemania
Fil: Rajpaul, V.. University of Oxford; Reino Unido
Fil: Tuomi, M.. University Of Hertfordshire; Reino Unido
Fil: Aigrain, S.. University of Oxford; Reino Unido
Fil: Anglada Escudé, G.. Queen Mary University of London; Reino Unido
Fil: Bonomo, A. S.. Osservatorio Astrofisico di Torino; Italia
Fil: Boué, G.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Dauvergne, F.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Frustagli, G.. Osservatorio Astronomico di Brera; Italia
Fil: Giacobbe, P.. Osservatorio Astrofisico di Torino; Italia
Fil: Haywood, R. D.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Jones, H. R. A.. University of Hertfordshire,; Reino Unido
Fil: Laskar, J.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Pinamonti, M.. Osservatorio Astronomico di Trieste; Italia
Fil: Poretti, E.. Osservatorio Astronomico di Brera; Italia
Fil: Rainer, M.. Osservatorio Astronomico di Brera; Italia
Fil: Ségransan, D.. Observatoire de Genève; Suiza
Fil: Sozzetti, A.. Osservatorio Astrofisico di Torino; Italia
Fil: Udry, S.. Observatoire de Genève; Suiza - Materia
-
Techniques: Radial Velocities
Planetary Systems
Stars: Oscillations
Stars: Activity
Methods: Data Analysis - 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:11336/18442
Ver los metadatos del registro completo
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oai:ri.conicet.gov.ar:11336/18442 |
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Radial-velocity fitting challenge. II. First results of the analysis of the data setDumusque, X.Borsa, F.Damasso, M.Diaz, Rodrigo FernandoGregory, P. C.Hara, N. C.Hatzes, A.Rajpaul, V.Tuomi, M.Aigrain, S.Anglada Escudé, G.Bonomo, A. S.Boué, G.Dauvergne, F.Frustagli, G.Giacobbe, P.Haywood, R. D.Jones, H. R. A.Laskar, J.Pinamonti, M.Poretti, E.Rainer, M.Ségransan, D.Sozzetti, A.Udry, S.Techniques: Radial VelocitiesPlanetary SystemsStars: OscillationsStars: ActivityMethods: Data Analysishttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. Radial-velocity (RV) signals arising from stellar photospheric phenomena are the main limitation for precise RV measurements. Those signals induce RV variations an order of magnitude larger than the signal created by the orbit of Earth-twins, thus preventing their detection. Aims. Different methods have been developed to mitigate the impact of stellar RV signals. The goal of this paper is to compare the efficiency of these different methods to recover extremely low-mass planets despite stellar RV signals. However, because observed RV variations at the meter-per-second precision level or below is a combination of signals induced by unresolved orbiting planets, by the star, and by the instrument, performing such a comparison using real data is extremely challenging. Methods. To circumvent this problem, we generated simulated RV measurements including realistic stellar and planetary signals. Different teams analyzed blindly those simulated RV measurements, using their own method to recover planetary signals despite stellar RV signals. By comparing the results obtained by the different teams with the planetary and stellar parameters used to generate the simulated RVs, it is therefore possible to compare the efficiency of these different methods. Results. The most efficient methods to recover planetary signals take into account the different activity indicators, use red-noise models to account for stellar RV signals and a Bayesian framework to provide model comparison in a robust statistical approach. Using the most efficient methodology, planets can be found down to with a threshold of K/N = 7.5 at the level of 80–90% recovery rate found for a number of methods. These recovery rates drop dramatically for K/N smaller than this threshold. In addition, for the best teams, no false positives with K/N > 7.5 were detected, while a non-negligible fraction of them appear for smaller K/N. A limit of K/N = 7.5 seems therefore a safe threshold to attest the veracity of planetary signals for RV measurements with similar properties to those of the different RV fitting challenge systems.Fil: Dumusque, X.. Université de Genève; SuizaFil: Borsa, F.. Osservatorio Astronomico di Brera; ItaliaFil: Damasso, M.. Osservatorio Astrofisico di Torino; ItaliaFil: 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. Université de Genève; SuizaFil: Gregory, P. C.. University Of British Columbia; CanadáFil: Hara, N. C.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Hatzes, A.. Thüringer Landessternwarte Tautenburg; AlemaniaFil: Rajpaul, V.. University of Oxford; Reino UnidoFil: Tuomi, M.. University Of Hertfordshire; Reino UnidoFil: Aigrain, S.. University of Oxford; Reino UnidoFil: Anglada Escudé, G.. Queen Mary University of London; Reino UnidoFil: Bonomo, A. S.. Osservatorio Astrofisico di Torino; ItaliaFil: Boué, G.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Dauvergne, F.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Frustagli, G.. Osservatorio Astronomico di Brera; ItaliaFil: Giacobbe, P.. Osservatorio Astrofisico di Torino; ItaliaFil: Haywood, R. D.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Jones, H. R. A.. University of Hertfordshire,; Reino UnidoFil: Laskar, J.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Pinamonti, M.. Osservatorio Astronomico di Trieste; ItaliaFil: Poretti, E.. Osservatorio Astronomico di Brera; ItaliaFil: Rainer, M.. Osservatorio Astronomico di Brera; ItaliaFil: Ségransan, D.. Observatoire de Genève; SuizaFil: Sozzetti, A.. Osservatorio Astrofisico di Torino; ItaliaFil: Udry, S.. Observatoire de Genève; SuizaEdp Sciences2017-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/18442Dumusque, X.; Borsa, F.; Damasso, M.; Diaz, Rodrigo Fernando; Gregory, P. C.; et al.; Radial-velocity fitting challenge. II. First results of the analysis of the data set; Edp Sciences; Astronomy And Astrophysics; 598; A133; 2-2017; 1-350004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201628671info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1609.03674info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2017/02/aa28671-16/aa28671-16.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T15:11:24Zoai:ri.conicet.gov.ar:11336/18442instacron: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 15:11:24.725CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Radial-velocity fitting challenge. II. First results of the analysis of the data set |
title |
Radial-velocity fitting challenge. II. First results of the analysis of the data set |
spellingShingle |
Radial-velocity fitting challenge. II. First results of the analysis of the data set Dumusque, X. Techniques: Radial Velocities Planetary Systems Stars: Oscillations Stars: Activity Methods: Data Analysis |
title_short |
Radial-velocity fitting challenge. II. First results of the analysis of the data set |
title_full |
Radial-velocity fitting challenge. II. First results of the analysis of the data set |
title_fullStr |
Radial-velocity fitting challenge. II. First results of the analysis of the data set |
title_full_unstemmed |
Radial-velocity fitting challenge. II. First results of the analysis of the data set |
title_sort |
Radial-velocity fitting challenge. II. First results of the analysis of the data set |
dc.creator.none.fl_str_mv |
Dumusque, X. Borsa, F. Damasso, M. Diaz, Rodrigo Fernando Gregory, P. C. Hara, N. C. Hatzes, A. Rajpaul, V. Tuomi, M. Aigrain, S. Anglada Escudé, G. Bonomo, A. S. Boué, G. Dauvergne, F. Frustagli, G. Giacobbe, P. Haywood, R. D. Jones, H. R. A. Laskar, J. Pinamonti, M. Poretti, E. Rainer, M. Ségransan, D. Sozzetti, A. Udry, S. |
author |
Dumusque, X. |
author_facet |
Dumusque, X. Borsa, F. Damasso, M. Diaz, Rodrigo Fernando Gregory, P. C. Hara, N. C. Hatzes, A. Rajpaul, V. Tuomi, M. Aigrain, S. Anglada Escudé, G. Bonomo, A. S. Boué, G. Dauvergne, F. Frustagli, G. Giacobbe, P. Haywood, R. D. Jones, H. R. A. Laskar, J. Pinamonti, M. Poretti, E. Rainer, M. Ségransan, D. Sozzetti, A. Udry, S. |
author_role |
author |
author2 |
Borsa, F. Damasso, M. Diaz, Rodrigo Fernando Gregory, P. C. Hara, N. C. Hatzes, A. Rajpaul, V. Tuomi, M. Aigrain, S. Anglada Escudé, G. Bonomo, A. S. Boué, G. Dauvergne, F. Frustagli, G. Giacobbe, P. Haywood, R. D. Jones, H. R. A. Laskar, J. Pinamonti, M. Poretti, E. Rainer, M. Ségransan, D. Sozzetti, A. Udry, S. |
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 |
dc.subject.none.fl_str_mv |
Techniques: Radial Velocities Planetary Systems Stars: Oscillations Stars: Activity Methods: Data Analysis |
topic |
Techniques: Radial Velocities Planetary Systems Stars: Oscillations Stars: Activity Methods: Data Analysis |
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. Radial-velocity (RV) signals arising from stellar photospheric phenomena are the main limitation for precise RV measurements. Those signals induce RV variations an order of magnitude larger than the signal created by the orbit of Earth-twins, thus preventing their detection. Aims. Different methods have been developed to mitigate the impact of stellar RV signals. The goal of this paper is to compare the efficiency of these different methods to recover extremely low-mass planets despite stellar RV signals. However, because observed RV variations at the meter-per-second precision level or below is a combination of signals induced by unresolved orbiting planets, by the star, and by the instrument, performing such a comparison using real data is extremely challenging. Methods. To circumvent this problem, we generated simulated RV measurements including realistic stellar and planetary signals. Different teams analyzed blindly those simulated RV measurements, using their own method to recover planetary signals despite stellar RV signals. By comparing the results obtained by the different teams with the planetary and stellar parameters used to generate the simulated RVs, it is therefore possible to compare the efficiency of these different methods. Results. The most efficient methods to recover planetary signals take into account the different activity indicators, use red-noise models to account for stellar RV signals and a Bayesian framework to provide model comparison in a robust statistical approach. Using the most efficient methodology, planets can be found down to with a threshold of K/N = 7.5 at the level of 80–90% recovery rate found for a number of methods. These recovery rates drop dramatically for K/N smaller than this threshold. In addition, for the best teams, no false positives with K/N > 7.5 were detected, while a non-negligible fraction of them appear for smaller K/N. A limit of K/N = 7.5 seems therefore a safe threshold to attest the veracity of planetary signals for RV measurements with similar properties to those of the different RV fitting challenge systems. Fil: Dumusque, X.. Université de Genève; Suiza Fil: Borsa, F.. Osservatorio Astronomico di Brera; Italia Fil: Damasso, M.. Osservatorio Astrofisico di Torino; Italia 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. Université de Genève; Suiza Fil: Gregory, P. C.. University Of British Columbia; Canadá Fil: Hara, N. C.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Hatzes, A.. Thüringer Landessternwarte Tautenburg; Alemania Fil: Rajpaul, V.. University of Oxford; Reino Unido Fil: Tuomi, M.. University Of Hertfordshire; Reino Unido Fil: Aigrain, S.. University of Oxford; Reino Unido Fil: Anglada Escudé, G.. Queen Mary University of London; Reino Unido Fil: Bonomo, A. S.. Osservatorio Astrofisico di Torino; Italia Fil: Boué, G.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Dauvergne, F.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Frustagli, G.. Osservatorio Astronomico di Brera; Italia Fil: Giacobbe, P.. Osservatorio Astrofisico di Torino; Italia Fil: Haywood, R. D.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Jones, H. R. A.. University of Hertfordshire,; Reino Unido Fil: Laskar, J.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Pinamonti, M.. Osservatorio Astronomico di Trieste; Italia Fil: Poretti, E.. Osservatorio Astronomico di Brera; Italia Fil: Rainer, M.. Osservatorio Astronomico di Brera; Italia Fil: Ségransan, D.. Observatoire de Genève; Suiza Fil: Sozzetti, A.. Osservatorio Astrofisico di Torino; Italia Fil: Udry, S.. Observatoire de Genève; Suiza |
description |
Context. Radial-velocity (RV) signals arising from stellar photospheric phenomena are the main limitation for precise RV measurements. Those signals induce RV variations an order of magnitude larger than the signal created by the orbit of Earth-twins, thus preventing their detection. Aims. Different methods have been developed to mitigate the impact of stellar RV signals. The goal of this paper is to compare the efficiency of these different methods to recover extremely low-mass planets despite stellar RV signals. However, because observed RV variations at the meter-per-second precision level or below is a combination of signals induced by unresolved orbiting planets, by the star, and by the instrument, performing such a comparison using real data is extremely challenging. Methods. To circumvent this problem, we generated simulated RV measurements including realistic stellar and planetary signals. Different teams analyzed blindly those simulated RV measurements, using their own method to recover planetary signals despite stellar RV signals. By comparing the results obtained by the different teams with the planetary and stellar parameters used to generate the simulated RVs, it is therefore possible to compare the efficiency of these different methods. Results. The most efficient methods to recover planetary signals take into account the different activity indicators, use red-noise models to account for stellar RV signals and a Bayesian framework to provide model comparison in a robust statistical approach. Using the most efficient methodology, planets can be found down to with a threshold of K/N = 7.5 at the level of 80–90% recovery rate found for a number of methods. These recovery rates drop dramatically for K/N smaller than this threshold. In addition, for the best teams, no false positives with K/N > 7.5 were detected, while a non-negligible fraction of them appear for smaller K/N. A limit of K/N = 7.5 seems therefore a safe threshold to attest the veracity of planetary signals for RV measurements with similar properties to those of the different RV fitting challenge systems. |
publishDate |
2017 |
dc.date.none.fl_str_mv |
2017-02 |
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/11336/18442 Dumusque, X.; Borsa, F.; Damasso, M.; Diaz, Rodrigo Fernando; Gregory, P. C.; et al.; Radial-velocity fitting challenge. II. First results of the analysis of the data set; Edp Sciences; Astronomy And Astrophysics; 598; A133; 2-2017; 1-35 0004-6361 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/18442 |
identifier_str_mv |
Dumusque, X.; Borsa, F.; Damasso, M.; Diaz, Rodrigo Fernando; Gregory, P. C.; et al.; Radial-velocity fitting challenge. II. First results of the analysis of the data set; Edp Sciences; Astronomy And Astrophysics; 598; A133; 2-2017; 1-35 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/10.1051/0004-6361/201628671 info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1609.03674 info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2017/02/aa28671-16/aa28671-16.html |
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 |
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reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) |
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Consejo Nacional de Investigaciones Científicas y Técnicas |
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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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