Coralie radial-velocity search for companions around evolved stars (CASCADES): III. A new Jupiter host-star: in-depth analysis of HD 29399 using TESS data

C. Pezzotti; G. Ottoni; G. Buldgen; A. Lyttle; P. Eggenberger; S. Udry; D. Ségransan; M. Mayor; C. Lovis; M. Marmier; A. Miglio; Y. Elsworth; G. R. Davies; W. H. Ball

doi:10.1051/0004-6361/202040080

Coralie radial-velocity search for companions around evolved stars (CASCADES): III. A new Jupiter host-star: in-depth analysis of HD 29399 using TESS data

C. Pezzotti, G. Ottoni, G. Buldgen, A. Lyttle, P. Eggenberger, S. Udry, D. Ségransan, M. Mayor, C. Lovis, M. Marmier, A. Miglio, Y. Elsworth, G. R. Davies, W. H. Ball

Physics and Astronomy

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Abstract

Context. Increasing the number of detected exoplanets is far from anecdotal, especially for long-period planets that require a long duration of observation. More detections imply a better understanding of the statistical properties of exoplanet populations, and detailed modelling of their host stars also enables thorough discussions of star–planet interactions and orbital evolution of planetary systems.

Aims. In the context of the discovery of a new planetary system, we aim to perform a complete study of HD 29399 and its companion by means of radial-velocity measurements, seismic characterisation of the host-star, and modelling of the orbital evolution of the system.

Methods. High-resolution spectra of HD 29399 were acquired with the CORALIE spectrograph mounted on the 1.2-m Swiss telescope located at La Silla Observatory (Chile) as part of the CASCADES survey. We used the moments of the cross-correlation function profile as well as the photometric variability of the star as diagnostics to distinguish between stellar and planetary-induced signals. To model the host star we combined forward modelling with global and local minimisation approaches and inversion techniques. We also studied the orbital history of the system under the effects of both dynamical and equilibrium tides.

Results. We present the detection of a long-period giant planet. Combining these measurements with photometric observations by TESS, we are able to thoroughly model the host star and study the orbital evolution of the system. We derive stellar and planetary masses of 1.17 ± 0.10 M⊙ and 1.59 ± 0.08 MJup, respectively, and an age for the system of 6.2 Gyr. We show that neither dynamical nor equilibrium tides have been able to affect the orbital evolution of the planet. Moreover, no engulfment is predicted for the future evolution of the system.

Original language	English
Article number	A89
Number of pages	13
Journal	Astronomy and Astrophysics
Volume	657
DOIs	https://doi.org/10.1051/0004-6361/202040080
Publication status	Published - 18 Jan 2022

Bibliographical note

Funding Information:
We thank the referee for the useful comments that helped to improve the quality of the manuscript. This work has been carried out within the framework of the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation. The authors acknowledge the financial support of the SNSF. This publication makes use of the Data & Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planet data visualisation, exchange and analysis. DACE is a platform of the Swiss National Centre of Competence in Research (NCCR) PlanetS, federating the Swiss expertise in Exoplanet research. The DACE platform is available at https://dace.unige.ch. We thank all observers at La Silla Observatory from the past fourteen years for their quality work. We acknowledge financial support from the Swiss National Science Foundation (SNSF). This work has, in part, been carried out within the frame-work of the National Centre for Competence in Research PlanetS supported by SNSF. C.P. acknowledges funding from the Swiss National Science Foundation (project Interacting Stars, number 200020-172505). G.B. acknowledges funding from the SNF AMBIZIONE grant no. 185805 (Seismic inversions and modelling of transport processes in stars). P.E. has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 833925, project STAREX). This article used an adapted version of InversionKit, a software developed within the HELAS and SPACEINN networks, funded by the European Commission’s Sixth and Seventh Framework Programmes. AM acknowledges support from the ERC Consolidator Grant funding scheme (project ASTEROCHRONOMETRY, https://www.asterochronometry.eu, G.A. no. 772293).

Publisher Copyright:
© ESO 2022.

Keywords

Planets and satellites: detection
Stars: fundamental parameters
Stars: individual: HD 29399
Stars: individual: TIC 38828531
Stars: interiors
Techniques: radial velocities

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.1051/0004-6361/202040080Licence: None: All rights reserved

PezzottiC2022CORALIEFinal published version, 4.98 MBLicence: None: All rights reserved

Cite this

Pezzotti, C., Ottoni, G., Buldgen, G., Lyttle, A., Eggenberger, P., Udry, S., Ségransan, D., Mayor, M., Lovis, C., Marmier, M., Miglio, A., Elsworth, Y., Davies, G. R., & Ball, W. H. (2022). Coralie radial-velocity search for companions around evolved stars (CASCADES): III. A new Jupiter host-star: in-depth analysis of HD 29399 using TESS data. Astronomy and Astrophysics, 657, Article A89. https://doi.org/10.1051/0004-6361/202040080

@article{3774f3dfc1984545b3c830d5e37eebe7,

title = "Coralie radial-velocity search for companions around evolved stars (CASCADES): III. A new Jupiter host-star: in-depth analysis of HD 29399 using TESS data",

abstract = "Context. Increasing the number of detected exoplanets is far from anecdotal, especially for long-period planets that require a long duration of observation. More detections imply a better understanding of the statistical properties of exoplanet populations, and detailed modelling of their host stars also enables thorough discussions of star–planet interactions and orbital evolution of planetary systems.Aims. In the context of the discovery of a new planetary system, we aim to perform a complete study of HD 29399 and its companion by means of radial-velocity measurements, seismic characterisation of the host-star, and modelling of the orbital evolution of the system.Methods. High-resolution spectra of HD 29399 were acquired with the CORALIE spectrograph mounted on the 1.2-m Swiss telescope located at La Silla Observatory (Chile) as part of the CASCADES survey. We used the moments of the cross-correlation function profile as well as the photometric variability of the star as diagnostics to distinguish between stellar and planetary-induced signals. To model the host star we combined forward modelling with global and local minimisation approaches and inversion techniques. We also studied the orbital history of the system under the effects of both dynamical and equilibrium tides.Results. We present the detection of a long-period giant planet. Combining these measurements with photometric observations by TESS, we are able to thoroughly model the host star and study the orbital evolution of the system. We derive stellar and planetary masses of 1.17 ± 0.10 M⊙ and 1.59 ± 0.08 MJup, respectively, and an age for the system of 6.2 Gyr. We show that neither dynamical nor equilibrium tides have been able to affect the orbital evolution of the planet. Moreover, no engulfment is predicted for the future evolution of the system.",

keywords = "Planets and satellites: detection, Stars: fundamental parameters, Stars: individual: HD 29399, Stars: individual: TIC 38828531, Stars: interiors, Techniques: radial velocities",

author = "C. Pezzotti and G. Ottoni and G. Buldgen and A. Lyttle and P. Eggenberger and S. Udry and D. S{\'e}gransan and M. Mayor and C. Lovis and M. Marmier and A. Miglio and Y. Elsworth and Davies, {G. R.} and Ball, {W. H.}",

note = "Funding Information: We thank the referee for the useful comments that helped to improve the quality of the manuscript. This work has been carried out within the framework of the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation. The authors acknowledge the financial support of the SNSF. This publication makes use of the Data & Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planet data visualisation, exchange and analysis. DACE is a platform of the Swiss National Centre of Competence in Research (NCCR) PlanetS, federating the Swiss expertise in Exoplanet research. The DACE platform is available at https://dace.unige.ch. We thank all observers at La Silla Observatory from the past fourteen years for their quality work. We acknowledge financial support from the Swiss National Science Foundation (SNSF). This work has, in part, been carried out within the frame-work of the National Centre for Competence in Research PlanetS supported by SNSF. C.P. acknowledges funding from the Swiss National Science Foundation (project Interacting Stars, number 200020-172505). G.B. acknowledges funding from the SNF AMBIZIONE grant no. 185805 (Seismic inversions and modelling of transport processes in stars). P.E. has received funding from the European Research Council (ERC) under the European Union{\textquoteright}s Horizon 2020 research and innovation programme (grant agreement no. 833925, project STAREX). This article used an adapted version of InversionKit, a software developed within the HELAS and SPACEINN networks, funded by the European Commission{\textquoteright}s Sixth and Seventh Framework Programmes. AM acknowledges support from the ERC Consolidator Grant funding scheme (project ASTEROCHRONOMETRY, https://www.asterochronometry.eu, G.A. no. 772293). Publisher Copyright: {\textcopyright} ESO 2022.",

year = "2022",

month = jan,

day = "18",

doi = "10.1051/0004-6361/202040080",

language = "English",

volume = "657",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

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Pezzotti, C, Ottoni, G, Buldgen, G, Lyttle, A, Eggenberger, P, Udry, S, Ségransan, D, Mayor, M, Lovis, C, Marmier, M, Miglio, A, Elsworth, Y , Davies, GR & Ball, WH 2022, 'Coralie radial-velocity search for companions around evolved stars (CASCADES): III. A new Jupiter host-star: in-depth analysis of HD 29399 using TESS data', Astronomy and Astrophysics, vol. 657, A89. https://doi.org/10.1051/0004-6361/202040080

TY - JOUR

T1 - Coralie radial-velocity search for companions around evolved stars (CASCADES)

T2 - III. A new Jupiter host-star: in-depth analysis of HD 29399 using TESS data

AU - Pezzotti, C.

AU - Ottoni, G.

AU - Buldgen, G.

AU - Lyttle, A.

AU - Eggenberger, P.

AU - Udry, S.

AU - Ségransan, D.

AU - Mayor, M.

AU - Lovis, C.

AU - Marmier, M.

AU - Miglio, A.

AU - Elsworth, Y.

AU - Davies, G. R.

AU - Ball, W. H.

N1 - Funding Information: We thank the referee for the useful comments that helped to improve the quality of the manuscript. This work has been carried out within the framework of the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation. The authors acknowledge the financial support of the SNSF. This publication makes use of the Data & Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planet data visualisation, exchange and analysis. DACE is a platform of the Swiss National Centre of Competence in Research (NCCR) PlanetS, federating the Swiss expertise in Exoplanet research. The DACE platform is available at https://dace.unige.ch. We thank all observers at La Silla Observatory from the past fourteen years for their quality work. We acknowledge financial support from the Swiss National Science Foundation (SNSF). This work has, in part, been carried out within the frame-work of the National Centre for Competence in Research PlanetS supported by SNSF. C.P. acknowledges funding from the Swiss National Science Foundation (project Interacting Stars, number 200020-172505). G.B. acknowledges funding from the SNF AMBIZIONE grant no. 185805 (Seismic inversions and modelling of transport processes in stars). P.E. has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 833925, project STAREX). This article used an adapted version of InversionKit, a software developed within the HELAS and SPACEINN networks, funded by the European Commission’s Sixth and Seventh Framework Programmes. AM acknowledges support from the ERC Consolidator Grant funding scheme (project ASTEROCHRONOMETRY, https://www.asterochronometry.eu, G.A. no. 772293). Publisher Copyright: © ESO 2022.

PY - 2022/1/18

Y1 - 2022/1/18

N2 - Context. Increasing the number of detected exoplanets is far from anecdotal, especially for long-period planets that require a long duration of observation. More detections imply a better understanding of the statistical properties of exoplanet populations, and detailed modelling of their host stars also enables thorough discussions of star–planet interactions and orbital evolution of planetary systems.Aims. In the context of the discovery of a new planetary system, we aim to perform a complete study of HD 29399 and its companion by means of radial-velocity measurements, seismic characterisation of the host-star, and modelling of the orbital evolution of the system.Methods. High-resolution spectra of HD 29399 were acquired with the CORALIE spectrograph mounted on the 1.2-m Swiss telescope located at La Silla Observatory (Chile) as part of the CASCADES survey. We used the moments of the cross-correlation function profile as well as the photometric variability of the star as diagnostics to distinguish between stellar and planetary-induced signals. To model the host star we combined forward modelling with global and local minimisation approaches and inversion techniques. We also studied the orbital history of the system under the effects of both dynamical and equilibrium tides.Results. We present the detection of a long-period giant planet. Combining these measurements with photometric observations by TESS, we are able to thoroughly model the host star and study the orbital evolution of the system. We derive stellar and planetary masses of 1.17 ± 0.10 M⊙ and 1.59 ± 0.08 MJup, respectively, and an age for the system of 6.2 Gyr. We show that neither dynamical nor equilibrium tides have been able to affect the orbital evolution of the planet. Moreover, no engulfment is predicted for the future evolution of the system.

AB - Context. Increasing the number of detected exoplanets is far from anecdotal, especially for long-period planets that require a long duration of observation. More detections imply a better understanding of the statistical properties of exoplanet populations, and detailed modelling of their host stars also enables thorough discussions of star–planet interactions and orbital evolution of planetary systems.Aims. In the context of the discovery of a new planetary system, we aim to perform a complete study of HD 29399 and its companion by means of radial-velocity measurements, seismic characterisation of the host-star, and modelling of the orbital evolution of the system.Methods. High-resolution spectra of HD 29399 were acquired with the CORALIE spectrograph mounted on the 1.2-m Swiss telescope located at La Silla Observatory (Chile) as part of the CASCADES survey. We used the moments of the cross-correlation function profile as well as the photometric variability of the star as diagnostics to distinguish between stellar and planetary-induced signals. To model the host star we combined forward modelling with global and local minimisation approaches and inversion techniques. We also studied the orbital history of the system under the effects of both dynamical and equilibrium tides.Results. We present the detection of a long-period giant planet. Combining these measurements with photometric observations by TESS, we are able to thoroughly model the host star and study the orbital evolution of the system. We derive stellar and planetary masses of 1.17 ± 0.10 M⊙ and 1.59 ± 0.08 MJup, respectively, and an age for the system of 6.2 Gyr. We show that neither dynamical nor equilibrium tides have been able to affect the orbital evolution of the planet. Moreover, no engulfment is predicted for the future evolution of the system.

KW - Planets and satellites: detection

KW - Stars: fundamental parameters

KW - Stars: individual: HD 29399

KW - Stars: individual: TIC 38828531

KW - Stars: interiors

KW - Techniques: radial velocities

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DO - 10.1051/0004-6361/202040080

M3 - Article

SN - 0004-6361

VL - 657

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A89

ER -

Coralie radial-velocity search for companions around evolved stars (CASCADES): III. A new Jupiter host-star: in-depth analysis of HD 29399 using TESS data

Abstract

Bibliographical note

Keywords

ASJC Scopus subject areas

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