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Published February 2025 | Version Published
Journal Article Open

Characterization of seven transiting systems, including four warm Jupiters from SOPHIE and TESS

Creators

  • 1. ROR icon Institut d'Astrophysique de Paris
  • 2. ROR icon Haute-Provence Observatory
  • 3. ROR icon Laboratório Nacional de Astrofísica
  • 4. ROR icon Harvard-Smithsonian Center for Astrophysics
  • 5. ROR icon Wesleyan University
  • 6. ROR icon Institut de Planétologie et d'Astrophysique de Grenoble
  • 7. ROR icon Adolfo Ibáñez University
  • 8. ROR icon Millennium Institute of Astrophysics
  • 9. ROR icon University of Coimbra
  • 10. ROR icon Institut de Mécanique Céleste et de Calcul des Éphémérides
  • 11. ROR icon University of Porto
  • 12. ROR icon University of New Mexico
  • 13. Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France
  • 14. ROR icon California Institute of Technology
  • 15. ROR icon Shahid Beheshti University
  • 16. ROR icon University of Geneva
  • 17. ROR icon University of Liège
  • 18. ROR icon Massachusetts Institute of Technology
  • 19. ROR icon Instituto de Astrofísica de Canarias
  • 20. ROR icon Austin College
  • 21. ROR icon University of St Andrews
  • 22. ROR icon Netherlands Institute for Space Research
  • 23. ROR icon Max Planck Institute for Astronomy
  • 24. ROR icon Space Telescope Science Institute
  • 25. Flatiron Institute
  • 26. ROR icon Princeton University
  • 27. ROR icon American Museum of Natural History
  • 28. ROR icon University of Tokyo
  • 29. Observatory de Ca l'Ou, Sant Martí Sesgueioles, GEECAT, Barcelona, Spain
  • 30. ROR icon NOIRLab
  • 31. ROR icon Ames Research Center
  • 32. ROR icon Laboratory of Space Studies and Instrumentation in Astrophysics
  • 33. Pl NE, Marysville, WA, 98270, USA
  • 34. ROR icon University of North Carolina at Chapel Hill
  • 35. ROR icon University of La Laguna
  • 36. ROR icon Research Institute in Astrophysics and Planetology
  • 37. ROR icon Vanderbilt University
  • 38. Kotizarovci Observatory, Sarsoni 90, 51216, Viskovo, Croatia
  • 39. ROR icon University of Warwick
  • 40. ROR icon Lomonosov Moscow State University
  • 41. ROR icon University of Arizona
  • 42. ROR icon Lehigh University
  • 43. ROR icon Pontificia Universidad Católica de Chile
  • 44. ROR icon Search for Extraterrestrial Intelligence
  • 45. ROR icon Sofia University
  • 46. ROR icon Heidelberg University
  • 47. ROR icon Stephen F. Austin State University

Abstract

While several thousand exoplanets are now confirmed, the number of known transiting warm Jupiters (10 d < period < 200 d) remains relatively small. These planets are generally believed to have formed outside the snowline and migrated to their current orbits. Because they are sufficiently distant from their host stars, they mitigate proximity effects and so offer valuable insights into planet formation and evolution. Here, we present the study of seven systems, three of which – TOI-2295, TOI-2537, and TOI-5110 – are newly discovered planetary systems. Through the analysis of TESS photometry, SOPHIE radial velocities (RVs), and high-spatial resolution imaging, we found that TOI-2295b, TOI-2537b, and TOI-5110b are transiting warm Jupiters with orbital periods ranging from 30 to 94 d, masses between 0.9 and 2.9 MJ, and radii ranging from 1.0 to 1.5 RJ. Both TOI-2295 and TOI-2537 harbor at least one additional, outer planet. Their outer planets – TOI-2295c and TOI-2537c – are characterized by orbital periods of 966.5-4.2+4.3 and 1920-140+230 d, respectively, and minimum masses of 5.61-0.24+0.23 and 7.23-0.45+0.52 MJ, respectively. We have also investigated and characterized the two recently reported warm Jupiters TOI-1836b and TOI-5076b, which we independently detected in SOPHIE RVs. Our new data allow for further discussion of their nature and refinement of their parameters. Additionally, we study the planetary candidates TOI-4081.01 and TOI-4168.01. For TOI-4081.01, despite our detection in RVs, we cannot rule out perturbation by a blended eclipsing binary, and we thus exercise caution regarding its planetary nature. On the other hand, we identify TOI-4168.01 as a firm false positive; its RV curve exhibits a large amplitude in an antiphase relation with the transit ephemeris observed by TESS, indicating that the detected event is the eclipse of a secondary star rather than a planetary transit. Finally, we highlight interesting characteristics of these new planetary systems. The transits of TOI-2295b are highly grazing, with an impact parameter of 1.056-0.043+0.063. This leaves its radius uncertain but potentially makes it an interesting probe of gravitational dynamics in its two-planet system, as transit shapes for grazing planets are highly sensitive to even small variations in inclination. TOI-2537b, in turn, is a temperate Jupiter with an effective temperature of 307±15 K and can serve as a valuable low-irradiation control for models of hot Jupiter inflation anomalies. We also detected significant transit timing variations (TTVs) for TOI-2537b, which are likely caused by gravitational interactions with the outer planet TOI-2537c. Further transit observations are needed to refine the analysis of these TTVs and enhance our understanding of the system’s dynamics. Finally, TOI-5110b stands out due to its orbital eccentricity of 0.745-0.027+0.030, one of the highest planetary eccentricities discovered thus far. We find no conclusive evidence for an external companion, but an unseen planet with a semi-amplitude smaller than 10 m/s could nonetheless still be exciting its eccentricity.

Copyright and License

© The Authors 2025.

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

We warmly thank the OHP staff for their support on the observations. We received funding from the French Programme National de Physique Stellaire (PNPS) and the Programme National de Planétologie (PNP) of CNRS (INSU). N.H. acknowledges the Centre National d’Études Spatiales (CNES) postdoctoral funding fellowship. This work was supported by CNES, focused on the PLATO mission. This paper made use of data collected by the TESS mission which is publicly available from the Mikulski Archive for Space Telescopes (MAST) operated by 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. A.C.M.C. acknowledges support from the FCT, Portugal, through the CFisUC projects UIDB/04564/2020 and UIDP/04564/2020, with DOI identifiers 10.54499/UIDB/04564/2020 and 10.54499/UIDP/04564/2020, respectively. B.S.S. acknowledges the support of M.V. Lomonosov Moscow State University Program of Development. The results reported herein benefitted from collaborations and/or information exchange within NASA’s Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA’s Science Mission Directorate under Agreement No. 80NSSC21K0593 for the program “Alien Earths”. E.M. acknowledges funding from FAPEMIG under project number APQ-02493-22 and a research productivity grant number 309829/2022-4 awarded by the CNPq, Brazil. X.D. and A.C. acknowledge 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. A.C. acknowledges funding from the French ANR under contract number ANR18CE310019 (SPlaSH). Some of the observations in this paper made use of the High-Resolution Imaging instrument ‘Alopeke and were obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. ‘Alopeke was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. ‘Alopeke was mounted on the Gemini North/South telescopes of the International Gemini Observatory, a program of NSF’s OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This work is partly supported by JSPS KAKENHI Grant Numbers JP24H00017, JP24K00689, and JSPS Bilateral Program Number JPJSBP120249910.nThis paper is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos Sánchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. Based in part on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia e Inovações (MCTI/LNA) do Brasil, the US National Science Foundation’s NOIRLab, the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). DD acknowledges support from the TESS Guest Investigator Program grant 80NSSC22K0185, and from the NASA Exoplanet Research Program grant 18-2XRP18_2-0136. P.C.Z. acknowledges support from STFC consolidated grant number ST/V000861/1, and UKSA grant number ST/X002217/1. The postdoctoral fellowship of K.B. is funded by F.R.S.-FNRS grant T.0109.20 and by the Francqui Foundation.

Data Availability

All appendices for this study are available at https://doi.org/10.5281/zenodo.14514237. Full RV tables are at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/694/A36.

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Additional details

Related works

Is new version of
Discussion Paper: arXiv:2412.08527 (arXiv)
Is supplemented by
Dataset: 10.5281/zenodo.14514237 (DOI)
Dataset: https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/694/A36 (URL)

Funding

Centre National de la Recherche Scientifique
Centre National d'Études Spatiales
Fundação para a Ciência e Tecnologia
UIDB/04564/2020
Fundação para a Ciência e Tecnologia
UIDP/04564/2020
Moscow State University
National Aeronautics and Space Administration
80NSSC21K0593
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
ANR-15-IDEX-02
Université Grenoble Alpes
Agence Nationale de la Recherche
SPlaSH ANR18CE310019
Japan Society for the Promotion of Science
JP24H00017
Japan Society for the Promotion of Science
JP24K00689
Japan Society for the Promotion of Science
JPJSBP120249910
National Aeronautics and Space Administration
TESS Guest Investigator Program 80NSSC22K0185
National Aeronautics and Space Administration
NASA Exoplanet Research Program 18-2XRP18_2-0136
Science and Technology Facilities Council
ST/V000861/1
United Kingdom Space Agency
ST/X002217/1
Fund for Scientific Research
T.0109.20
Fondation Francqui
National Science Foundation
Astronomy and Astrophysics Postdoctoral Fellowship -

Dates

Accepted
2024-11-25
Accepted
Available
2025-02-06
Published online

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