Optical and near-infrared stellar activity characterization of the early M dwarf Gl~205 with SOPHIE and SPIRou

P. Cortes-Zuleta; I. Boisse; B. Klein; E. Martioli; P. I. Cristofari; A. Antoniadis-Karnavas; J-F. Donati; X. Delfosse; C. Cadieux; N. Heidari; E. Artigau; S. Bellotti; X. Bonfils; A. Carmona; N. J. Cook; R. F. Diaz; R. Doyon; P. Fouque; C. Moutou; P. Petit; T. Vandal; L. Acuña; L. Arnold; N. Astudillo-Defru; V. Bourrier; F. Bouchy; R. Cloutier; S. Dalal; M. Deleuil; O. D. S. Demangeon; X. Dumusque; T. Forveille; J. Gomes da Silva; N. Hara; G. Hebrard; S. Hoyer; G. Hussain; F. Kiefer; J. Morin; A. Santerne; N. C. Santos; D. Segransan; M. Stalport; S. Udry

doi:10.1051/0004-6361/202245131

Optical and near-infrared stellar activity characterization of the early M dwarf Gl~205 with SOPHIE and SPIRou

P. Cortes-Zuleta, I. Boisse, B. Klein, E. Martioli, P. I. Cristofari, A. Antoniadis-Karnavas, J-F. Donati, X. Delfosse, C. Cadieux, N. Heidari, E. Artigau, S. Bellotti, X. Bonfils, A. Carmona, N. J. Cook, R. F. Diaz, R. Doyon, P. Fouque, C. Moutou, P. PetitT. Vandal, L. Acuña, L. Arnold, N. Astudillo-Defru, V. Bourrier, F. Bouchy, R. Cloutier, S. Dalal, M. Deleuil, O. D. S. Demangeon, X. Dumusque, T. Forveille, J. Gomes da Silva, N. Hara, G. Hebrard, S. Hoyer, G. Hussain, F. Kiefer, J. Morin, A. Santerne, N. C. Santos, D. Segransan, M. Stalport, S. Udry

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

Abstract

Context. The stellar activity of M dwarfs is the main limiting factor in the discovery and characterization of the exoplanets orbiting them, because it induces quasi-periodic radial velocity (RV) variations.

Aims. We aim to characterize the magnetic field and stellar activity of the early, moderately active M dwarf Gl 205 in the optical and near-infrared (NIR) domains.

Methods. We obtained high-precision quasi-simultaneous spectra in the optical and NIR with the SOPHIE spectrograph and SPIRou spectropolarimeter between 2019 and 2022. We computed the RVs from both instruments and the SPIRou Stokes V profiles. We used Zeeman–Doppler imaging (ZDI) to map the large-scale magnetic field over the time span of the observations. We studied the temporal behavior of optical and NIR RVs and activity indicators with the Lomb-Scargle periodogram and a quasi-periodic Gaussian process regression (GPR). In the NIR, we studied the equivalent width of Al I, Ti I, K I, Fe I, and He I. We modeled the activity-induced RV jitter using a multi-dimensional GPR with activity indicators as ancillary time series.

Results. The optical and NIR RVs show similar scatter but NIR shows a more complex temporal evolution. We observe an evolution of the magnetic field topology from a poloidal dipolar field in 2019 to a dominantly toroidal field in 2022. We measured a stellar rotation period of P_rot = 34.4 ± 0.5 days in the longitudinal magnetic field. Using ZDI, we measure the amount of latitudinal differential rotation (DR) shearing the stellar surface, yielding rotation periods of P_eq = 32.0 ± 1.8 days at the stellar equator and P_pol = 45.5 ± 0.3 days at the poles. We observed inconsistencies in the periodicities of the activity indicators that could be explained by these DR values. The multi-dimensional GP modeling yields an RMS of the RV residuals down to the noise level of 3 m s⁻¹ for both instruments while using Hα and the BIS in the optical and the full width at half maximum (FWHM) in the NIR as ancillary time series.

Conclusions. The RV variations observed in Gl 205 are due to stellar activity, with a complex evolution and different expressions in the optical and NIR revealed thanks to an extensive follow-up. Spectropolarimetry remains the best technique to constrain the stellar rotation period over standard activity indicators, particularly for moderately active M dwarfs.

Original language	English
Article number	A14
Number of pages	40
Journal	Astronomy & Astrophysics
Volume	673
Early online date	26 Apr 2023
DOIs	https://doi.org/10.1051/0004-6361/202245131
Publication status	Published - May 2023

Keywords

Stars: activity, low mass
Techniques: spectroscopic, radial velocities, polarimetric

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Cortes-Zuleta, P., Boisse, I., Klein, B., Martioli, E., Cristofari, P. I., Antoniadis-Karnavas, A., Donati, J.-F., Delfosse, X., Cadieux, C., Heidari, N., Artigau, E., Bellotti, S., Bonfils, X., Carmona, A., Cook, N. J., Diaz, R. F., Doyon, R., Fouque, P., Moutou, C., ... Udry, S. (2023). Optical and near-infrared stellar activity characterization of the early M dwarf Gl~205 with SOPHIE and SPIRou. Astronomy & Astrophysics, 673, Article A14. https://doi.org/10.1051/0004-6361/202245131

@article{f8383af68d3548ff8b17fc3546d059e3,

title = "Optical and near-infrared stellar activity characterization of the early M dwarf Gl\textasciitilde{}205 with SOPHIE and SPIRou",

abstract = "Context. The stellar activity of M dwarfs is the main limiting factor in the discovery and characterization of the exoplanets orbiting them, because it induces quasi-periodic radial velocity (RV) variations. Aims. We aim to characterize the magnetic field and stellar activity of the early, moderately active M dwarf Gl 205 in the optical and near-infrared (NIR) domains. Methods. We obtained high-precision quasi-simultaneous spectra in the optical and NIR with the SOPHIE spectrograph and SPIRou spectropolarimeter between 2019 and 2022. We computed the RVs from both instruments and the SPIRou Stokes V profiles. We used Zeeman–Doppler imaging (ZDI) to map the large-scale magnetic field over the time span of the observations. We studied the temporal behavior of optical and NIR RVs and activity indicators with the Lomb-Scargle periodogram and a quasi-periodic Gaussian process regression (GPR). In the NIR, we studied the equivalent width of Al I, Ti I, K I, Fe I, and He I. We modeled the activity-induced RV jitter using a multi-dimensional GPR with activity indicators as ancillary time series. Results. The optical and NIR RVs show similar scatter but NIR shows a more complex temporal evolution. We observe an evolution of the magnetic field topology from a poloidal dipolar field in 2019 to a dominantly toroidal field in 2022. We measured a stellar rotation period of Prot = 34.4 ± 0.5 days in the longitudinal magnetic field. Using ZDI, we measure the amount of latitudinal differential rotation (DR) shearing the stellar surface, yielding rotation periods of Peq = 32.0 ± 1.8 days at the stellar equator and Ppol = 45.5 ± 0.3 days at the poles. We observed inconsistencies in the periodicities of the activity indicators that could be explained by these DR values. The multi-dimensional GP modeling yields an RMS of the RV residuals down to the noise level of 3 m s−1 for both instruments while using Hα and the BIS in the optical and the full width at half maximum (FWHM) in the NIR as ancillary time series. Conclusions. The RV variations observed in Gl 205 are due to stellar activity, with a complex evolution and different expressions in the optical and NIR revealed thanks to an extensive follow-up. Spectropolarimetry remains the best technique to constrain the stellar rotation period over standard activity indicators, particularly for moderately active M dwarfs.",

keywords = "Stars: activity, low mass, Techniques: spectroscopic, radial velocities, polarimetric",

author = "P. Cortes-Zuleta and I. Boisse and B. Klein and E. Martioli and Cristofari, \{P. I.\} and A. Antoniadis-Karnavas and J-F. Donati and X. Delfosse and C. Cadieux and N. Heidari and E. Artigau and S. Bellotti and X. Bonfils and A. Carmona and Cook, \{N. J.\} and Diaz, \{R. F.\} and R. Doyon and P. Fouque and C. Moutou and P. Petit and T. Vandal and L. Acu{\~n}a and L. Arnold and N. Astudillo-Defru and V. Bourrier and F. Bouchy and R. Cloutier and S. Dalal and M. Deleuil and Demangeon, \{O. D. S.\} and X. Dumusque and T. Forveille and \{Gomes da Silva\}, J. and N. Hara and G. Hebrard and S. Hoyer and G. Hussain and F. Kiefer and J. Morin and A. Santerne and Santos, \{N. C.\} and D. Segransan and M. Stalport and S. Udry",

note = "Funding: We acknowledge funding from the French National Research Agency (ANR) under contract number ANR-18-CE31-0019 (SPlaSH). PCZ thanks the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining Grant \#1829740, the Brinson Foundation, and the Moore Foundation; her participation in the program has benefited this work. BK acknowledges funding from the European Research Council (ERC) under the European Union{\textquoteright}s Horizon 2020 research and innovation programme (Grant agreement No. 865624, GPRV). AAK acknowledges that this work was supported by FCT - Funda{\c c}{\~a}o para a Ci{\^e}ncia e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionaliza{\c c}{\~a}o by these grants: UIDB/04434/2020 \& UIDP/04434/2020; PTDC/FIS-AST/32113/2017 \& POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 \& POCI-01- 0145-FEDER-028953; IF/00849/2015/CP1273/CT0003. JFD, CM and PIC acknowledge funding from the European Research Council under the H2020 \& innovation program (grant \#740651 NewWorlds). XD, XB, TF, and AC acknoweldge a funding from the French National Research Agency in the framework of the Investissements d Avenir program (ANR-15-IDEX-02), through the funding of the “Origin of Life{"} project of the Grenoble-Alpes University. SH acknowledges CNES funding through the grant 837319.",

year = "2023",

month = may,

doi = "10.1051/0004-6361/202245131",

language = "English",

volume = "673",

journal = "Astronomy \& Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Cortes-Zuleta, P, Boisse, I, Klein, B, Martioli, E, Cristofari, PI, Antoniadis-Karnavas, A, Donati, J-F, Delfosse, X, Cadieux, C, Heidari, N, Artigau, E, Bellotti, S, Bonfils, X, Carmona, A, Cook, NJ, Diaz, RF, Doyon, R, Fouque, P, Moutou, C, Petit, P, Vandal, T, Acuña, L, Arnold, L, Astudillo-Defru, N, Bourrier, V, Bouchy, F, Cloutier, R, Dalal, S, Deleuil, M, Demangeon, ODS, Dumusque, X, Forveille, T, Gomes da Silva, J, Hara, N, Hebrard, G, Hoyer, S, Hussain, G, Kiefer, F, Morin, J, Santerne, A, Santos, NC, Segransan, D, Stalport, M & Udry, S 2023, 'Optical and near-infrared stellar activity characterization of the early M dwarf Gl~205 with SOPHIE and SPIRou', Astronomy & Astrophysics, vol. 673, A14. https://doi.org/10.1051/0004-6361/202245131

TY - JOUR

T1 - Optical and near-infrared stellar activity characterization of the early M dwarf Gl~205 with SOPHIE and SPIRou

AU - Cortes-Zuleta, P.

AU - Boisse, I.

AU - Klein, B.

AU - Martioli, E.

AU - Cristofari, P. I.

AU - Antoniadis-Karnavas, A.

AU - Donati, J-F.

AU - Delfosse, X.

AU - Cadieux, C.

AU - Heidari, N.

AU - Artigau, E.

AU - Bellotti, S.

AU - Bonfils, X.

AU - Carmona, A.

AU - Cook, N. J.

AU - Diaz, R. F.

AU - Doyon, R.

AU - Fouque, P.

AU - Moutou, C.

AU - Petit, P.

AU - Vandal, T.

AU - Acuña, L.

AU - Arnold, L.

AU - Astudillo-Defru, N.

AU - Bourrier, V.

AU - Bouchy, F.

AU - Cloutier, R.

AU - Dalal, S.

AU - Deleuil, M.

AU - Demangeon, O. D. S.

AU - Dumusque, X.

AU - Forveille, T.

AU - Gomes da Silva, J.

AU - Hara, N.

AU - Hebrard, G.

AU - Hoyer, S.

AU - Hussain, G.

AU - Kiefer, F.

AU - Morin, J.

AU - Santerne, A.

AU - Santos, N. C.

AU - Segransan, D.

AU - Stalport, M.

AU - Udry, S.

N1 - Funding: We acknowledge funding from the French National Research Agency (ANR) under contract number ANR-18-CE31-0019 (SPlaSH). PCZ thanks the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining Grant #1829740, the Brinson Foundation, and the Moore Foundation; her participation in the program has benefited this work. BK acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement No. 865624, GPRV). AAK acknowledges that this work was supported by FCT - Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionalização by these grants: UIDB/04434/2020 & UIDP/04434/2020; PTDC/FIS-AST/32113/2017 & POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 & POCI-01- 0145-FEDER-028953; IF/00849/2015/CP1273/CT0003. JFD, CM and PIC acknowledge funding from the European Research Council under the H2020 & innovation program (grant #740651 NewWorlds). XD, XB, TF, and AC acknoweldge a funding from the French National Research Agency in the framework of the Investissements d Avenir program (ANR-15-IDEX-02), through the funding of the “Origin of Life" project of the Grenoble-Alpes University. SH acknowledges CNES funding through the grant 837319.

PY - 2023/5

Y1 - 2023/5

N2 - Context. The stellar activity of M dwarfs is the main limiting factor in the discovery and characterization of the exoplanets orbiting them, because it induces quasi-periodic radial velocity (RV) variations. Aims. We aim to characterize the magnetic field and stellar activity of the early, moderately active M dwarf Gl 205 in the optical and near-infrared (NIR) domains. Methods. We obtained high-precision quasi-simultaneous spectra in the optical and NIR with the SOPHIE spectrograph and SPIRou spectropolarimeter between 2019 and 2022. We computed the RVs from both instruments and the SPIRou Stokes V profiles. We used Zeeman–Doppler imaging (ZDI) to map the large-scale magnetic field over the time span of the observations. We studied the temporal behavior of optical and NIR RVs and activity indicators with the Lomb-Scargle periodogram and a quasi-periodic Gaussian process regression (GPR). In the NIR, we studied the equivalent width of Al I, Ti I, K I, Fe I, and He I. We modeled the activity-induced RV jitter using a multi-dimensional GPR with activity indicators as ancillary time series. Results. The optical and NIR RVs show similar scatter but NIR shows a more complex temporal evolution. We observe an evolution of the magnetic field topology from a poloidal dipolar field in 2019 to a dominantly toroidal field in 2022. We measured a stellar rotation period of Prot = 34.4 ± 0.5 days in the longitudinal magnetic field. Using ZDI, we measure the amount of latitudinal differential rotation (DR) shearing the stellar surface, yielding rotation periods of Peq = 32.0 ± 1.8 days at the stellar equator and Ppol = 45.5 ± 0.3 days at the poles. We observed inconsistencies in the periodicities of the activity indicators that could be explained by these DR values. The multi-dimensional GP modeling yields an RMS of the RV residuals down to the noise level of 3 m s−1 for both instruments while using Hα and the BIS in the optical and the full width at half maximum (FWHM) in the NIR as ancillary time series. Conclusions. The RV variations observed in Gl 205 are due to stellar activity, with a complex evolution and different expressions in the optical and NIR revealed thanks to an extensive follow-up. Spectropolarimetry remains the best technique to constrain the stellar rotation period over standard activity indicators, particularly for moderately active M dwarfs.

AB - Context. The stellar activity of M dwarfs is the main limiting factor in the discovery and characterization of the exoplanets orbiting them, because it induces quasi-periodic radial velocity (RV) variations. Aims. We aim to characterize the magnetic field and stellar activity of the early, moderately active M dwarf Gl 205 in the optical and near-infrared (NIR) domains. Methods. We obtained high-precision quasi-simultaneous spectra in the optical and NIR with the SOPHIE spectrograph and SPIRou spectropolarimeter between 2019 and 2022. We computed the RVs from both instruments and the SPIRou Stokes V profiles. We used Zeeman–Doppler imaging (ZDI) to map the large-scale magnetic field over the time span of the observations. We studied the temporal behavior of optical and NIR RVs and activity indicators with the Lomb-Scargle periodogram and a quasi-periodic Gaussian process regression (GPR). In the NIR, we studied the equivalent width of Al I, Ti I, K I, Fe I, and He I. We modeled the activity-induced RV jitter using a multi-dimensional GPR with activity indicators as ancillary time series. Results. The optical and NIR RVs show similar scatter but NIR shows a more complex temporal evolution. We observe an evolution of the magnetic field topology from a poloidal dipolar field in 2019 to a dominantly toroidal field in 2022. We measured a stellar rotation period of Prot = 34.4 ± 0.5 days in the longitudinal magnetic field. Using ZDI, we measure the amount of latitudinal differential rotation (DR) shearing the stellar surface, yielding rotation periods of Peq = 32.0 ± 1.8 days at the stellar equator and Ppol = 45.5 ± 0.3 days at the poles. We observed inconsistencies in the periodicities of the activity indicators that could be explained by these DR values. The multi-dimensional GP modeling yields an RMS of the RV residuals down to the noise level of 3 m s−1 for both instruments while using Hα and the BIS in the optical and the full width at half maximum (FWHM) in the NIR as ancillary time series. Conclusions. The RV variations observed in Gl 205 are due to stellar activity, with a complex evolution and different expressions in the optical and NIR revealed thanks to an extensive follow-up. Spectropolarimetry remains the best technique to constrain the stellar rotation period over standard activity indicators, particularly for moderately active M dwarfs.

KW - Stars: activity, low mass

KW - Techniques: spectroscopic, radial velocities, polarimetric

UR - https://www.scopus.com/pages/publications/85153348578

U2 - 10.1051/0004-6361/202245131

DO - 10.1051/0004-6361/202245131

M3 - Article

SN - 0004-6361

VL - 673

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - A14

ER -

Optical and near-infrared stellar activity characterization of the early M dwarf Gl~205 with SOPHIE and SPIRou

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Keywords

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