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Published December 2023 | Version Published
Journal Article Open

TOI-1736 and TOI-2141: Two systems including sub-Neptunes around solar analogs revealed by TESS and SOPHIE

Creators

  • 1. ROR icon Laboratório Nacional de Astrofísica
  • 2. ROR icon Institut d'Astrophysique de Paris
  • 3. ROR icon Sorbonne University
  • 4. ROR icon Haute-Provence Observatory
  • 5. LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université Paris-Cité, 5 place Jules Janssen, 92195, Meudon, France
  • 6. ROR icon Grenoble Alpes University
  • 7. ROR icon Harvard-Smithsonian Center for Astrophysics
  • 8. ROR icon French National Centre for Scientific Research
  • 9. ROR icon Cerro Tololo Inter-American Observatory
  • 10. ROR icon University of Exeter
  • 11. ROR icon University of Porto
  • 12. ROR icon NASA Exoplanet Science Institute
  • 13. ROR icon Ames Research Center
  • 14. ROR icon University of North Carolina at Chapel Hill
  • 15. ROR icon Research Institute in Astrophysics and Planetology
  • 16. ROR icon Vanderbilt University
  • 17. Hazelwood Observatory, Victoria, Australia
  • 18. ROR icon Search for Extraterrestrial Intelligence
  • 19. ROR icon Princeton University
  • 20. ROR icon Stephen F. Austin State University

Abstract

Planetary systems around solar analogs inform us about how planets form and evolve in Solar System-like environments. We report the detection and characterization of two planetary systems around the solar analogs TOI-1736 and TOI-2141 using TESS photometry data and spectroscopic data obtained with the SOPHIE instrument on the 1.93 m telescope at the Observatoire de Haute-Provence (OHP). We performed a detailed spectroscopic analysis of these systems to obtain the precise radial velocities (RV) and physical properties of their host stars. TOI-1736 and TOI-2141 each host a transiting sub-Neptune with radii of 2.44 ± 0.18 R⊕ and 3.05 ± 0.23 R⊕, orbital periods of 7.073088(7) days and 18.26157(6) days, and masses of 12.8 ± 1.8 M⊕ and 24 ± 4 M⊕, respectively. TOI-1736 shows long-term RV variations that are consistent with a two-planet solution plus a linear trend of −0.177 m s−1 day−1. We measured an RV semi-amplitude of 201.1 ± 0.7 m s−1 for the outer companion, TOI-1736 c, implying aprojected mass of mcsin i = 8.09 ± 0.20 MJup. From the Gaia DR3 astrometric excess noise, we constrained the mass of TOI-1736 c at 8.7−0.6+1.5 MJup. This planet is in an orbit of 570.2 ± 0.6 days with an eccentricity of 0.362 ± 0.003 and a semi-major axis of 1.381 ± 0.017 au, where it receives a flux of 0.71 ± 0.08 times the bolometric flux incident on Earth, making it an interesting case of a supergiant planet that has settled into an eccentric orbit in the habitable zone of a solar analog. Our analysis of the mass-radius relation for the transiting sub-Neptunes shows that both TOI-1736 b and TOI-2141 b likely have an Earth-like dense rocky core and a water-rich envelope.

Copyright and License

© The Authors 2023. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

Acknowledgement

E.M. acknowledges funding from Fundação de Amparo à Pesquisa do Estado de Minas Gerais (FAPEMIG) under project number APQ-02493-22 and research productivity grant (PQ) number 309829/2022-4 awarded by the National Council for Scientific and Technological Development (CNPq), Brazil. We thank the Observatoire de Haute-Provence (CNRS) staff for their support. This work was supported by the “Programme National de Planétologie” (PNP) of CNRS/INSU and CNES. This paper includes data collected with the TESS mission, obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the TESS mission is provided by NASA’s Science Mission Directorate. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. 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 planets data visualization, 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 acknowledge funding from the French ANR under contract number ANR18CE310019 (SPlaSH). X.D. and T.F. acknowledge support by the French National Research Agency in the framework of the Investissement d’Avenir program (ANR-15-IDEX-02), through the funding of the “Origin of Life” project of the Grenoble-Alpes University. 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 Internacionalizacão by these grants: UID/FIS/04434/2019, 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, PTDC/FIS-AST/28987/2017 & POCI-01-0145-FEDER-028987. N.C.S. further acknowledges funding by the European Union (ERC, FIERCE, 101052347). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. KAC acknowledges support from the TESS mission via subaward s3449 from MIT. S.D. is funded by the UK Science and Technology Facilities Council (grant number ST/V004735/1). S.G.S. acknowledges the support from FCT through the contract no.CEECIND/00826/2018 and POPH/FSE (EC).

Additional Information

Based on observations collected with the SOPHIE spectrograph on the 1.93 m telescope at the Observatoire de Haute-Provence (CNRS), France.

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Additional details

Related works

Is new version of
Discussion Paper: arXiv:2311.07011 (arXiv)
Is supplemented by
Dataset: https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/680/A84 (URL)

Funding

Fundação de Amparo à Pesquisa do Estado de Minas Gerais
APQ-02493-22
National Council for Scientific and Technological Development
309829/2022-4
Agence Nationale de la Recherche
ANR18CE310019
Agence Nationale de la Recherche
ANR-15-IDEX-02
Fundação para a Ciência e Tecnologia
UID/FIS/04434/2019
Fundação para a Ciência e Tecnologia
UIDB/04434/2020
Fundação para a Ciência e Tecnologia
UIDP/04434/2020
Fundação para a Ciência e Tecnologia
PTDC/FIS-AST/32113/2017
Fundação para a Ciência e Tecnologia
POCI-01-0145-FEDER-032113
Fundação para a Ciência e Tecnologia
PTDC/FIS-AST/28953/2017
Fundação para a Ciência e Tecnologia
POCI-01-0145-FEDER-028953
Fundação para a Ciência e Tecnologia
PTDC/FIS-AST/28987/2017
Fundação para a Ciência e Tecnologia
POCI-01-0145-FEDER-028987
European Union
101052347
Massachusetts Institute of Technology
s3449
Science and Technology Facilities Council
ST/V004735/1
Fundação para a Ciência e Tecnologia
CEECIND/00826/2018
Fundação para a Ciência e Tecnologia
POPH/FSE

Dates

Accepted
2023-10-06
Available
2023-12-15
Published online

Caltech Custom Metadata

Caltech groups
Infrared Processing and Analysis Center (IPAC), Division of Physics, Mathematics and Astronomy (PMA)
Publication Status
Published