Near-IR and optical radial velocities of the active M dwarf star Gl 388 (AD Leo) with SPIRou at CFHT and SOPHIE at OHP: A 2.23 day rotation period and no evidence for a corotating...

Autores
Carmona, A.; Delfosse, X.; Bellotti, S.; Cortés Zuleta, P.; Ould Elhkim, M.; Heidari, N.; Mignon, L.; Donati, J. F.; Cook, N.; Artigau, E.; Fouqué, P.; Martioli, E.; Cadieux, C.; Forveille, T.; Boisse, I.; Hébrard, G.; Diaz, Rodrigo Fernando; Lafrenière, D.; Kiefer, F.; Petit, P.; Doyon, R.; Acuña, L.; Arnold, L.; Santerne, A.; Mousis, O.; Ségrasan, D.; Stalport, M.; Udry, S.
Año de publicación
2023
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. The search for extrasolar planets around the nearest M dwarfs is a crucial step toward identifying the nearest Earth-like planets. One of the main challenges in this search is that M dwarfs can be magnetically active and stellar activity can produce radial velocity (RV) signals that could mimic those of a planet.Aims: We aim to investigate whether the 2.2-day period observed in optical RVs of the nearby active M dwarf star Gl 388 (AD Leo) is due to stellar activity or to a planet that corotates with the star as suggested in the past.Methods: We obtained quasi-simultaneous RVs of Gl 388 from 2019 to 2021 with SOPHIE, the optical échelle spectrograph (R ~75k) at the Observatoire de Haute-Provence in France, and RV and Stokes V measurements with SPIRou, the near-infrared spectropolarimeter at the Canada France Hawaii Telescope (R ~70k).Results: The SOPHIE RV time series (precision of 3-5 m s-1 per visit) displays a periodic signal with a 2.23 ± 0.01 day period and 23.6 ± 0.5 m s-1 amplitude, which is consistent with previous HARPS observations obtained in 2005-2006. The SPIRou RV time series (precision of 2 ms-1 per visit) is flat at 5 ms-1 rms and displays no periodic signals. RV signals of amplitude higher than 5.3 m s-1 at a period of 2.23 days can be excluded with a confidence level higher than 99%. Using the modulation of the longitudinal magnetic field (Bℓ) measured with SPIRou as a proxy of stellar rotation, we measure a rotation period of 2.2305 ± 0.0016 days.Conclusions: SPIRou RV measurements provide solid evidence that the periodic variability of the optical RVs of Gl 388 is due to stellar activity rather than to a corotating planet. The magnetic activity nature of the optical RV signal is further confirmed by the modulation of Bℓ with the same period. The SPIRou campaign on Gl 388 demonstrates the power of near-infrared RV to confirm or infirm planet candidates discovered in the optical around active stars. Our SPIRou observations additionally reiterate how effective spectropolarimetry is at determining the stellar rotation period from the variations of Bℓ.
Fil: Carmona, A.. Centre National de la Recherche Scientifique; Francia. Universite Grenoble Alpes; Francia
Fil: Delfosse, X.. Centre National de la Recherche Scientifique; Francia. Universite Grenoble Alpes; Francia
Fil: Bellotti, S.. Université Paul Sabatier; Francia. Université de Toulouse; Francia. Centro Europeo de Investigación y Tecnología Espacial; Países Bajos
Fil: Cortés Zuleta, P.. Aix Marseille Université; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Ould Elhkim, M.. Université Paul Sabatier; Francia. Université de Toulouse; Francia
Fil: Heidari, N.. Consejo Nacional de Investigaciones Cientificas y Tecnicas. Instituto de Ciencias Fisicas. - Universidad Nacional de San Martin. Instituto de Ciencias Fisicas.; Argentina. Aix Marseille Université; Francia
Fil: Mignon, L.. l’Université de Genève; Suiza
Fil: Donati, J. F.. Université de Toulouse; Francia
Fil: Cook, N.. University of Montreal; Canadá
Fil: Artigau, E.. University of Montreal; Canadá. Université de Montpellier; Suiza
Fil: Fouqué, P.. Université de Toulouse; Francia
Fil: Martioli, E.. Laboratório Nacional de Astrofísica; Brasil. Sorbonne University; Francia
Fil: Cadieux, C.. University of Montreal; Canadá
Fil: Forveille, T.. Universite Grenoble Alpes; Francia. Centre National de la Recherche Scientifique; Francia. Sorbonne University; Francia
Fil: Boisse, I.. Aix Marseille Université; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Hébrard, G.. Sorbonne University; Francia
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. Consejo Nacional de Investigaciones Científicas y Técnicas. Instituto de Ciencias Físicas. - Universidad Nacional de San Martín. Instituto de Ciencias Físicas; Argentina
Fil: Lafrenière, D.. University of Montreal; Canadá
Fil: Kiefer, F.. Sorbonne University; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Petit, P.. Université de Toulouse; Francia
Fil: Doyon, R.. University of Montreal; Canadá
Fil: Acuña, L.. Centre National de la Recherche Scientifique; Francia
Fil: Arnold, L.. Centre National de la Recherche Scientifique; Francia
Fil: Santerne, A.. Centre National de la Recherche Scientifique; Francia. Canada France Hawaii Telescope; Estados Unidos
Fil: Mousis, O.. Université de Montpellier; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Ségrasan, D.. Université de Montpellier; Francia
Fil: Stalport, M.. l'Université de Genève; Suiza
Fil: Udry, S.. l'Université de Genève; Suiza
Materia
planetary systems
stars: low-mass
methods: observational
techniques: spectroscopic
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:11336/254133

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network_name_str CONICET Digital (CONICET)
spelling Near-IR and optical radial velocities of the active M dwarf star Gl 388 (AD Leo) with SPIRou at CFHT and SOPHIE at OHP: A 2.23 day rotation period and no evidence for a corotating planetCarmona, A.Delfosse, X.Bellotti, S.Cortés Zuleta, P.Ould Elhkim, M.Heidari, N.Mignon, L.Donati, J. F.Cook, N.Artigau, E.Fouqué, P.Martioli, E.Cadieux, C.Forveille, T.Boisse, I.Hébrard, G.Diaz, Rodrigo FernandoLafrenière, D.Kiefer, F.Petit, P.Doyon, R.Acuña, L.Arnold, L.Santerne, A.Mousis, O.Ségrasan, D.Stalport, M.Udry, S.planetary systemsstars: low-massmethods: observationaltechniques: spectroscopictechniques: radial velocitieshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. The search for extrasolar planets around the nearest M dwarfs is a crucial step toward identifying the nearest Earth-like planets. One of the main challenges in this search is that M dwarfs can be magnetically active and stellar activity can produce radial velocity (RV) signals that could mimic those of a planet.Aims: We aim to investigate whether the 2.2-day period observed in optical RVs of the nearby active M dwarf star Gl 388 (AD Leo) is due to stellar activity or to a planet that corotates with the star as suggested in the past.Methods: We obtained quasi-simultaneous RVs of Gl 388 from 2019 to 2021 with SOPHIE, the optical échelle spectrograph (R ~75k) at the Observatoire de Haute-Provence in France, and RV and Stokes V measurements with SPIRou, the near-infrared spectropolarimeter at the Canada France Hawaii Telescope (R ~70k).Results: The SOPHIE RV time series (precision of 3-5 m s-1 per visit) displays a periodic signal with a 2.23 ± 0.01 day period and 23.6 ± 0.5 m s-1 amplitude, which is consistent with previous HARPS observations obtained in 2005-2006. The SPIRou RV time series (precision of 2 ms-1 per visit) is flat at 5 ms-1 rms and displays no periodic signals. RV signals of amplitude higher than 5.3 m s-1 at a period of 2.23 days can be excluded with a confidence level higher than 99%. Using the modulation of the longitudinal magnetic field (Bℓ) measured with SPIRou as a proxy of stellar rotation, we measure a rotation period of 2.2305 ± 0.0016 days.Conclusions: SPIRou RV measurements provide solid evidence that the periodic variability of the optical RVs of Gl 388 is due to stellar activity rather than to a corotating planet. The magnetic activity nature of the optical RV signal is further confirmed by the modulation of Bℓ with the same period. The SPIRou campaign on Gl 388 demonstrates the power of near-infrared RV to confirm or infirm planet candidates discovered in the optical around active stars. Our SPIRou observations additionally reiterate how effective spectropolarimetry is at determining the stellar rotation period from the variations of Bℓ.Fil: Carmona, A.. Centre National de la Recherche Scientifique; Francia. Universite Grenoble Alpes; FranciaFil: Delfosse, X.. Centre National de la Recherche Scientifique; Francia. Universite Grenoble Alpes; FranciaFil: Bellotti, S.. Université Paul Sabatier; Francia. Université de Toulouse; Francia. Centro Europeo de Investigación y Tecnología Espacial; Países BajosFil: Cortés Zuleta, P.. Aix Marseille Université; Francia. Centre National de la Recherche Scientifique; FranciaFil: Ould Elhkim, M.. Université Paul Sabatier; Francia. Université de Toulouse; FranciaFil: Heidari, N.. Consejo Nacional de Investigaciones Cientificas y Tecnicas. Instituto de Ciencias Fisicas. - Universidad Nacional de San Martin. Instituto de Ciencias Fisicas.; Argentina. Aix Marseille Université; FranciaFil: Mignon, L.. l’Université de Genève; SuizaFil: Donati, J. F.. Université de Toulouse; FranciaFil: Cook, N.. University of Montreal; CanadáFil: Artigau, E.. University of Montreal; Canadá. Université de Montpellier; SuizaFil: Fouqué, P.. Université de Toulouse; FranciaFil: Martioli, E.. Laboratório Nacional de Astrofísica; Brasil. Sorbonne University; FranciaFil: Cadieux, C.. University of Montreal; CanadáFil: Forveille, T.. Universite Grenoble Alpes; Francia. Centre National de la Recherche Scientifique; Francia. Sorbonne University; FranciaFil: Boisse, I.. Aix Marseille Université; Francia. Centre National de la Recherche Scientifique; FranciaFil: Hébrard, G.. Sorbonne University; FranciaFil: 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. Consejo Nacional de Investigaciones Científicas y Técnicas. Instituto de Ciencias Físicas. - Universidad Nacional de San Martín. Instituto de Ciencias Físicas; ArgentinaFil: Lafrenière, D.. University of Montreal; CanadáFil: Kiefer, F.. Sorbonne University; Francia. Centre National de la Recherche Scientifique; FranciaFil: Petit, P.. Université de Toulouse; FranciaFil: Doyon, R.. University of Montreal; CanadáFil: Acuña, L.. Centre National de la Recherche Scientifique; FranciaFil: Arnold, L.. Centre National de la Recherche Scientifique; FranciaFil: Santerne, A.. Centre National de la Recherche Scientifique; Francia. Canada France Hawaii Telescope; Estados UnidosFil: Mousis, O.. Université de Montpellier; Francia. Centre National de la Recherche Scientifique; FranciaFil: Ségrasan, D.. Université de Montpellier; FranciaFil: Stalport, M.. l'Université de Genève; SuizaFil: Udry, S.. l'Université de Genève; SuizaEDP Sciences2023-06info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/254133Carmona, A.; Delfosse, X.; Bellotti, S.; Cortés Zuleta, P.; Ould Elhkim, M.; et al.; Near-IR and optical radial velocities of the active M dwarf star Gl 388 (AD Leo) with SPIRou at CFHT and SOPHIE at OHP: A 2.23 day rotation period and no evidence for a corotating planet; EDP Sciences; Astronomy and Astrophysics; 674; 6-2023; 1-250004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202245660info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202245660info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/2303.16712info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:34:14Zoai:ri.conicet.gov.ar:11336/254133instacron: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 09:34:14.36CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Near-IR and optical radial velocities of the active M dwarf star Gl 388 (AD Leo) with SPIRou at CFHT and SOPHIE at OHP: A 2.23 day rotation period and no evidence for a corotating planet
title Near-IR and optical radial velocities of the active M dwarf star Gl 388 (AD Leo) with SPIRou at CFHT and SOPHIE at OHP: A 2.23 day rotation period and no evidence for a corotating planet
spellingShingle Near-IR and optical radial velocities of the active M dwarf star Gl 388 (AD Leo) with SPIRou at CFHT and SOPHIE at OHP: A 2.23 day rotation period and no evidence for a corotating planet
Carmona, A.
planetary systems
stars: low-mass
methods: observational
techniques: spectroscopic
techniques: radial velocities
title_short Near-IR and optical radial velocities of the active M dwarf star Gl 388 (AD Leo) with SPIRou at CFHT and SOPHIE at OHP: A 2.23 day rotation period and no evidence for a corotating planet
title_full Near-IR and optical radial velocities of the active M dwarf star Gl 388 (AD Leo) with SPIRou at CFHT and SOPHIE at OHP: A 2.23 day rotation period and no evidence for a corotating planet
title_fullStr Near-IR and optical radial velocities of the active M dwarf star Gl 388 (AD Leo) with SPIRou at CFHT and SOPHIE at OHP: A 2.23 day rotation period and no evidence for a corotating planet
title_full_unstemmed Near-IR and optical radial velocities of the active M dwarf star Gl 388 (AD Leo) with SPIRou at CFHT and SOPHIE at OHP: A 2.23 day rotation period and no evidence for a corotating planet
title_sort Near-IR and optical radial velocities of the active M dwarf star Gl 388 (AD Leo) with SPIRou at CFHT and SOPHIE at OHP: A 2.23 day rotation period and no evidence for a corotating planet
dc.creator.none.fl_str_mv Carmona, A.
Delfosse, X.
Bellotti, S.
Cortés Zuleta, P.
Ould Elhkim, M.
Heidari, N.
Mignon, L.
Donati, J. F.
Cook, N.
Artigau, E.
Fouqué, P.
Martioli, E.
Cadieux, C.
Forveille, T.
Boisse, I.
Hébrard, G.
Diaz, Rodrigo Fernando
Lafrenière, D.
Kiefer, F.
Petit, P.
Doyon, R.
Acuña, L.
Arnold, L.
Santerne, A.
Mousis, O.
Ségrasan, D.
Stalport, M.
Udry, S.
author Carmona, A.
author_facet Carmona, A.
Delfosse, X.
Bellotti, S.
Cortés Zuleta, P.
Ould Elhkim, M.
Heidari, N.
Mignon, L.
Donati, J. F.
Cook, N.
Artigau, E.
Fouqué, P.
Martioli, E.
Cadieux, C.
Forveille, T.
Boisse, I.
Hébrard, G.
Diaz, Rodrigo Fernando
Lafrenière, D.
Kiefer, F.
Petit, P.
Doyon, R.
Acuña, L.
Arnold, L.
Santerne, A.
Mousis, O.
Ségrasan, D.
Stalport, M.
Udry, S.
author_role author
author2 Delfosse, X.
Bellotti, S.
Cortés Zuleta, P.
Ould Elhkim, M.
Heidari, N.
Mignon, L.
Donati, J. F.
Cook, N.
Artigau, E.
Fouqué, P.
Martioli, E.
Cadieux, C.
Forveille, T.
Boisse, I.
Hébrard, G.
Diaz, Rodrigo Fernando
Lafrenière, D.
Kiefer, F.
Petit, P.
Doyon, R.
Acuña, L.
Arnold, L.
Santerne, A.
Mousis, O.
Ségrasan, D.
Stalport, M.
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
author
author
author
dc.subject.none.fl_str_mv planetary systems
stars: low-mass
methods: observational
techniques: spectroscopic
techniques: radial velocities
topic planetary systems
stars: low-mass
methods: observational
techniques: spectroscopic
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 search for extrasolar planets around the nearest M dwarfs is a crucial step toward identifying the nearest Earth-like planets. One of the main challenges in this search is that M dwarfs can be magnetically active and stellar activity can produce radial velocity (RV) signals that could mimic those of a planet.Aims: We aim to investigate whether the 2.2-day period observed in optical RVs of the nearby active M dwarf star Gl 388 (AD Leo) is due to stellar activity or to a planet that corotates with the star as suggested in the past.Methods: We obtained quasi-simultaneous RVs of Gl 388 from 2019 to 2021 with SOPHIE, the optical échelle spectrograph (R ~75k) at the Observatoire de Haute-Provence in France, and RV and Stokes V measurements with SPIRou, the near-infrared spectropolarimeter at the Canada France Hawaii Telescope (R ~70k).Results: The SOPHIE RV time series (precision of 3-5 m s-1 per visit) displays a periodic signal with a 2.23 ± 0.01 day period and 23.6 ± 0.5 m s-1 amplitude, which is consistent with previous HARPS observations obtained in 2005-2006. The SPIRou RV time series (precision of 2 ms-1 per visit) is flat at 5 ms-1 rms and displays no periodic signals. RV signals of amplitude higher than 5.3 m s-1 at a period of 2.23 days can be excluded with a confidence level higher than 99%. Using the modulation of the longitudinal magnetic field (Bℓ) measured with SPIRou as a proxy of stellar rotation, we measure a rotation period of 2.2305 ± 0.0016 days.Conclusions: SPIRou RV measurements provide solid evidence that the periodic variability of the optical RVs of Gl 388 is due to stellar activity rather than to a corotating planet. The magnetic activity nature of the optical RV signal is further confirmed by the modulation of Bℓ with the same period. The SPIRou campaign on Gl 388 demonstrates the power of near-infrared RV to confirm or infirm planet candidates discovered in the optical around active stars. Our SPIRou observations additionally reiterate how effective spectropolarimetry is at determining the stellar rotation period from the variations of Bℓ.
Fil: Carmona, A.. Centre National de la Recherche Scientifique; Francia. Universite Grenoble Alpes; Francia
Fil: Delfosse, X.. Centre National de la Recherche Scientifique; Francia. Universite Grenoble Alpes; Francia
Fil: Bellotti, S.. Université Paul Sabatier; Francia. Université de Toulouse; Francia. Centro Europeo de Investigación y Tecnología Espacial; Países Bajos
Fil: Cortés Zuleta, P.. Aix Marseille Université; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Ould Elhkim, M.. Université Paul Sabatier; Francia. Université de Toulouse; Francia
Fil: Heidari, N.. Consejo Nacional de Investigaciones Cientificas y Tecnicas. Instituto de Ciencias Fisicas. - Universidad Nacional de San Martin. Instituto de Ciencias Fisicas.; Argentina. Aix Marseille Université; Francia
Fil: Mignon, L.. l’Université de Genève; Suiza
Fil: Donati, J. F.. Université de Toulouse; Francia
Fil: Cook, N.. University of Montreal; Canadá
Fil: Artigau, E.. University of Montreal; Canadá. Université de Montpellier; Suiza
Fil: Fouqué, P.. Université de Toulouse; Francia
Fil: Martioli, E.. Laboratório Nacional de Astrofísica; Brasil. Sorbonne University; Francia
Fil: Cadieux, C.. University of Montreal; Canadá
Fil: Forveille, T.. Universite Grenoble Alpes; Francia. Centre National de la Recherche Scientifique; Francia. Sorbonne University; Francia
Fil: Boisse, I.. Aix Marseille Université; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Hébrard, G.. Sorbonne University; Francia
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. Consejo Nacional de Investigaciones Científicas y Técnicas. Instituto de Ciencias Físicas. - Universidad Nacional de San Martín. Instituto de Ciencias Físicas; Argentina
Fil: Lafrenière, D.. University of Montreal; Canadá
Fil: Kiefer, F.. Sorbonne University; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Petit, P.. Université de Toulouse; Francia
Fil: Doyon, R.. University of Montreal; Canadá
Fil: Acuña, L.. Centre National de la Recherche Scientifique; Francia
Fil: Arnold, L.. Centre National de la Recherche Scientifique; Francia
Fil: Santerne, A.. Centre National de la Recherche Scientifique; Francia. Canada France Hawaii Telescope; Estados Unidos
Fil: Mousis, O.. Université de Montpellier; Francia. Centre National de la Recherche Scientifique; Francia
Fil: Ségrasan, D.. Université de Montpellier; Francia
Fil: Stalport, M.. l'Université de Genève; Suiza
Fil: Udry, S.. l'Université de Genève; Suiza
description Context. The search for extrasolar planets around the nearest M dwarfs is a crucial step toward identifying the nearest Earth-like planets. One of the main challenges in this search is that M dwarfs can be magnetically active and stellar activity can produce radial velocity (RV) signals that could mimic those of a planet.Aims: We aim to investigate whether the 2.2-day period observed in optical RVs of the nearby active M dwarf star Gl 388 (AD Leo) is due to stellar activity or to a planet that corotates with the star as suggested in the past.Methods: We obtained quasi-simultaneous RVs of Gl 388 from 2019 to 2021 with SOPHIE, the optical échelle spectrograph (R ~75k) at the Observatoire de Haute-Provence in France, and RV and Stokes V measurements with SPIRou, the near-infrared spectropolarimeter at the Canada France Hawaii Telescope (R ~70k).Results: The SOPHIE RV time series (precision of 3-5 m s-1 per visit) displays a periodic signal with a 2.23 ± 0.01 day period and 23.6 ± 0.5 m s-1 amplitude, which is consistent with previous HARPS observations obtained in 2005-2006. The SPIRou RV time series (precision of 2 ms-1 per visit) is flat at 5 ms-1 rms and displays no periodic signals. RV signals of amplitude higher than 5.3 m s-1 at a period of 2.23 days can be excluded with a confidence level higher than 99%. Using the modulation of the longitudinal magnetic field (Bℓ) measured with SPIRou as a proxy of stellar rotation, we measure a rotation period of 2.2305 ± 0.0016 days.Conclusions: SPIRou RV measurements provide solid evidence that the periodic variability of the optical RVs of Gl 388 is due to stellar activity rather than to a corotating planet. The magnetic activity nature of the optical RV signal is further confirmed by the modulation of Bℓ with the same period. The SPIRou campaign on Gl 388 demonstrates the power of near-infrared RV to confirm or infirm planet candidates discovered in the optical around active stars. Our SPIRou observations additionally reiterate how effective spectropolarimetry is at determining the stellar rotation period from the variations of Bℓ.
publishDate 2023
dc.date.none.fl_str_mv 2023-06
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/11336/254133
Carmona, A.; Delfosse, X.; Bellotti, S.; Cortés Zuleta, P.; Ould Elhkim, M.; et al.; Near-IR and optical radial velocities of the active M dwarf star Gl 388 (AD Leo) with SPIRou at CFHT and SOPHIE at OHP: A 2.23 day rotation period and no evidence for a corotating planet; EDP Sciences; Astronomy and Astrophysics; 674; 6-2023; 1-25
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/254133
identifier_str_mv Carmona, A.; Delfosse, X.; Bellotti, S.; Cortés Zuleta, P.; Ould Elhkim, M.; et al.; Near-IR and optical radial velocities of the active M dwarf star Gl 388 (AD Leo) with SPIRou at CFHT and SOPHIE at OHP: A 2.23 day rotation period and no evidence for a corotating planet; EDP Sciences; Astronomy and Astrophysics; 674; 6-2023; 1-25
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/https://www.aanda.org/10.1051/0004-6361/202245660
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202245660
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/2303.16712
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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