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dc.contributor.author
Dumusque, X.
dc.contributor.author
Borsa, F.
dc.contributor.author
Damasso, M.
dc.contributor.author
Diaz, Rodrigo Fernando
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dc.contributor.author
Gregory, P. C.
dc.contributor.author
Hara, N. C.
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Hatzes, A.
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Rajpaul, V.
dc.contributor.author
Tuomi, M.
dc.contributor.author
Aigrain, S.
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Anglada Escudé, G.
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Bonomo, A. S.
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Boué, G.
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Dauvergne, F.
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Frustagli, G.
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Giacobbe, P.
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Haywood, R. D.
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Jones, H. R. A.
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Laskar, J.
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Pinamonti, M.
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Poretti, E.
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Rainer, M.
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Ségransan, D.
dc.contributor.author
Sozzetti, A.
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Udry, S.
dc.date.available
2017-09-04T19:52:19Z
dc.date.issued
2017-02
dc.identifier.citation
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
dc.identifier.issn
0004-6361
dc.identifier.uri
http://hdl.handle.net/11336/23613
dc.description.abstract
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 K/N = Kpl/RVrms × √Nobs = 5 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.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
EDP Sciences
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dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
Methods: Data Analysis
dc.subject
Planetary Systems
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Stars: Activity
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Stars: Oscillations
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Techniques: Radial Velocities
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Astronomía
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dc.subject.classification
Ciencias Físicas
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dc.subject.classification
CIENCIAS NATURALES Y EXACTAS
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dc.title
Radial-velocity fitting challenge: II. First results of the analysis of the data set
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2017-08-25T19:55:40Z
dc.journal.volume
598
dc.journal.number
A133
dc.journal.pagination
1-35
dc.journal.pais
Francia
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dc.journal.ciudad
Paris
dc.description.fil
Fil: Dumusque, X.. Universidad de Ginebra; Suiza. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
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Fil: Borsa, F.. Osservatorio Astronomico Di Brera; Italia
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Fil: Damasso, M.. Istituto Nazionale Di Astrofisica; Italia
dc.description.fil
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
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Fil: Gregory, P. C.. University of British Columbia; Canadá
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Fil: Hara, N. C.. Universite Pierre et Marie Curie; Francia
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Fil: Hatzes, A.. Thuringer Landessternwarte Tautenburg; Alemania
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Fil: Rajpaul, V.. University of Oxford; Reino Unido
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Fil: Tuomi, M.. University Of Hertfordshire; Reino Unido
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Fil: Aigrain, S.. University of Oxford; Reino Unido
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Fil: Anglada Escudé, G.. University Of Hertfordshire; Reino Unido
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Fil: Bonomo, A. S.. Istituto Nazionale Di Astrofisica; Italia
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Fil: Boué, G.. Universite Pierre et Marie Curie; Francia
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Fil: Dauvergne, F.. Universite Pierre et Marie Curie; Francia
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Fil: Frustagli, G.. Osservatorio Astronomico Di Brera; Italia
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Fil: Giacobbe, P.. Istituto Nazionale Di Astrofisica; Italia
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Fil: Haywood, R. D.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
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Fil: Jones, H. R. A.. University Of Hertfordshire; Reino Unido
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Fil: Laskar, J.. Universite Pierre et Marie Curie; Francia
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Fil: Pinamonti, M.. Università degli Studi di Trieste; Italia
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Fil: Poretti, E.. Osservatorio Astronomico Di Brera; Italia
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Fil: Rainer, M.. Osservatorio Astronomico Di Brera; Italia
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Fil: Ségransan, D.. Universidad de Ginebra; Suiza
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Fil: Sozzetti, A.. Istituto Nazionale Di Astrofisica; Italia
dc.description.fil
Fil: Udry, S.. Universidad de Ginebra; Suiza
dc.journal.title
Astronomy and Astrophysics
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dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1051/0004-6361/201628671
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2017/02/aa28671-16/aa28671-16.html
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