The SPIRou legacy survey: rotation period of quiet M dwarfs from circular polarization in near-infrared spectral lines - the SPIRou APERO analysis

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dc.creatorPascal Fouqué
dc.creatorEder Martioli
dc.creatorJean-Francois Donati
dc.creatorLisa Theres Lehmann
dc.creatorBonnie Zaire
dc.creatorStefano Bellotti
dc.creatorEric Gaidos
dc.creatorJulien Morin
dc.creatorClaire Moutou
dc.creatorPascal Petit
dc.creatorSilvia Helena Paixão Alencar
dc.creatorLuc Arnold
dc.creatorEtienne Artigau
dc.creatorJean-francois Donati
dc.creatorTianqi Cang
dc.creatorAndres Carmona
dc.creatorNeil James Cook
dc.creatorPía Cortés-Zuleta
dc.creatorPaul Cristofari
dc.creatorXavier Delfosse
dc.creatorRene Doyon
dc.creatorGuillaume Hebrard
dc.creatorLison Malo
dc.creatorCéline Reylé
dc.creatorChristopher Usher
dc.date.accessioned2025-02-04T16:59:34Z
dc.date.accessioned2025-09-08T23:44:29Z
dc.date.available2025-02-04T16:59:34Z
dc.date.issued2023-03-29
dc.format.mimetypepdf
dc.identifier.doihttps://doi.org/10.1051/0004-6361/202345839
dc.identifier.issn0004-6361
dc.identifier.urihttps://hdl.handle.net/1843/79650
dc.languageeng
dc.publisherUniversidade Federal de Minas Gerais
dc.relation.ispartofAstronomy & Astrophysics
dc.rightsAcesso Aberto
dc.subjectEstrelas - Campos magnéticos
dc.subjectDinâmica estelar
dc.subject.otherstars: magnetic field
dc.subject.othertechniques: spectroscopic
dc.subject.othertechniques: polarimetric
dc.subject.otherstars: fundamental parameters
dc.subject.otherstars: low-mass
dc.subject.otherstars: rotation
dc.titleThe SPIRou legacy survey: rotation period of quiet M dwarfs from circular polarization in near-infrared spectral lines - the SPIRou APERO analysis
dc.typeArtigo de periódico
local.citation.epage24
local.citation.spage01
local.citation.volume672
local.description.resumoContext. The rotation period of stars is an important parameter together with mass, radius, and effective temperature. It is an essential parameter for any radial velocity monitoring, as stellar activity can mimic the presence of a planet at the stellar rotation period. Several methods exist to measure it, including long sequences of photometric measurements or temporal series of stellar activity indicators. Aims. Here, we use the circular polarization in near-infrared spectral lines for a sample of 43 quiet M dwarfs and compare the measured rotation periods to those obtained with other methods. Methods. From Stokes V spectropolarimetric sequences observed with SPIRou at the Canada-France-Hawaii Telescope and the data processed with the APERO pipeline, we computed the least-squares deconvolution profiles using different masks of atomic stellar lines with known Landé factor appropriate to the effective temperature of the star. We derived the longitudinal magnetic field to examine its possible variation in 50 to 200 observations of each star. To determine the stellar rotation period, we applied a Gaussian process regression, enabling us to determine the rotation period of stars with evolving longitudinal field. Results. We were able to measure a rotation period for 27 of the 43 stars of our sample. The rotation period was previously unknown for 8 of these stars. Our rotation periods agree well with periods found in the literature based on photometry and activity indicators, and we confirm that near-infrared spectropolarimetry is an important tool for measuring rotation periods, even for magnetically quiet stars. Furthermore, we computed the ages for 20 stars of our sample using gyrochronology.
local.identifier.orcidhttps://orcid.org/0000-0002-1436-7351
local.identifier.orcidhttps://orcid.org/0000-0002-5084-168X
local.identifier.orcidhttps://orcid.org/0000-0001-5541-2887
local.identifier.orcidhttps://orcid.org/0000-0001-7264-0734
local.identifier.orcidhttps://orcid.org/0000-0002-9328-9530
local.identifier.orcidhttps://orcid.org/0000-0002-2558-6920
local.identifier.orcidhttps://orcid.org/0000-0002-5258-6846
local.identifier.orcidhttps://orcid.org/0000-0002-4996-6901
local.identifier.orcidhttps://orcid.org/0000-0002-2842-3924
local.identifier.orcidhttps://orcid.org/0000-0001-7624-9222
local.identifier.orcidhttps://orcid.org/0000-0002-5171-8376
local.identifier.orcidhttps://orcid.org/0000-0002-0111-1234
local.identifier.orcidhttps://orcid.org/0000-0003-3506-5667
local.identifier.orcidhttps://orcid.org/0000-0003-3816-7335
local.identifier.orcidhttps://orcid.org/0000-0003-2471-1299
local.identifier.orcidhttps://orcid.org/0000-0003-4166-4121
local.identifier.orcidhttps://orcid.org/0000-0002-6174-4666
local.identifier.orcidhttps://orcid.org/0000-0003-4019-0630
local.identifier.orcidhttps://orcid.org/0000-0001-5099-7978
local.identifier.orcidhttps://orcid.org/0000-0001-5485-4675
local.identifier.orcidhttps://orcid.org/0000-0001-5450-7067
local.identifier.orcidhttps://orcid.org/0000-0002-8786-8499
local.identifier.orcidhttps://orcid.org/0000-0003-2258-2403
local.identifier.orcidhttps://orcid.org/0000-0002-7383-7106
local.publisher.countryBrasil
local.publisher.departmentICX - DEPARTAMENTO DE FÍSICA
local.publisher.initialsUFMG
local.url.externahttps://www.aanda.org/articles/aa/pdf/2023/04/aa45839-23.pdf

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