TOI-5108 and TOI 5786 radial velocities Virtual Observatory Resource

Authors
  1. Thomas L.
  2. Hebrard G.
  3. Kellermann H.
  4. Korth J.
  5. Heidari N.
  6. Forveille T.,Sousa S.G.
  7. Schoeller L.
  8. Riffeser A.
  9. Goessl C.
  10. Serrano Bell J.,Kiefer F.
  11. Hara N.
  12. Grupp F.
  13. Ehrhardt J.
  14. Murgas F.
  15. Collins K.A.,Bieryla A.
  16. Parviainen H.
  17. Belinski A.A.
  18. Esparza-Borges E.
  19. Ciardi D.R.,Clark C.A.
  20. Fukui A.
  21. Gilbert E.A.
  22. Hopp U.
  23. Ikuta K.
  24. Jenkins J.M.,Latham D.W.
  25. Narita N.
  26. Nielsen L.D.
  27. Quinn S.N.
  28. Palle E.
  29. Pippert J.-N.,Polanski A.S.
  30. Ries C.
  31. Schmidt M.
  32. Schwarz R.P.
  33. Seager S.
  34. Strakhov I.A.,Striegel S.
  35. van Eyken J.C.
  36. Watanabe N.
  37. Watkins C.N.
  38. Winn J.N.,Ziegler C.
  39. Zoeller R.
  40. Published by
    CDS
Abstract

We report the discovery and characterization of two sub-Saturns from the Transiting Exoplanet Survey Satellite (TESS) using high-resolution spectroscopic observations from the MaHPS spectrograph at the Wendelstein Observatory and the SOPHIE spectrograph at the Haute-Provence Observatory. Combining photometry from TESS, KeplerCam, LCOGT, and MuSCAT2 with the radial velocity measurements from MaHPS and SOPHIE we measure precise radii and masses for both planets. TOI-5108 b is a sub-Saturn with a radius of 6.6+/-0.1R_{Earth}_ and a mass of 32+/-5M_{Earth}_ TOI-5786 b is similar to Saturn with a radius of 8.63+/-0.12R_{Earth}_ and a mass of 72+/-8M_{Earth}_. Both planets are close to their host stars with periods of 6.75 days and 12.78 days respectively. This puts TOI-5108 b just inside the bounds of the Neptune desert while TOI-5786 b is right above the upper edge. We estimate hydrogen-helium envelope mass fractions of 38% for TOI-5108 b and 74% for TOI-5786 b. However, using a model for the interior structure that includes tidal effects the envelope fraction of TOI-5108 b could be much lower (~20$) depending on the obliquity. We estimate mass-loss rates between 1.0x10^9^g/s and 9.8x10^9^g/s for TOI-5108 b and between 3.6x10^8^g/s and 3.5x10^9^g/s for TOI-5786 b. Given their masses, this means that both planets are stable against photoevaporation. Furthermore, at these mass-loss rates, there is likely no detectable signal in the metastable helium triplet with the James Webb Space Telescope. We also detect a transit signal for a second planet candidate around TOI-5786 with a period of 6.998 days and a radius of 3.90+/-0.16R_{Earth}_ Using our RV data and photodynamical modeling, we are able to provide a 3-{sigma} upper limit of 26.5M_{Earth}_ for the mass of the potential inner companion to TOI-5786 b.

Keywords
  1. multiple-stars
  2. exoplanets
  3. radial-velocity
  4. visible-astronomy
Bibliographic source Bibcode
2025A&A...694A.143T
See also HTML
https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/694/A143
IVOA Identifier IVOID
ivo://CDS.VizieR/J/A+A/694/A143

Access

IVOA Table Access TAP
https://tapvizier.cds.unistra.fr/TAPVizieR/tap
Run SQL-like queries with TAP-enabled clients (e.g., TOPCAT).

History

2025-02-07T12:14:53Z
Resource record created
2025-02-07T12:14:53Z
Created
2025-03-03T06:11:11Z
Updated

Contact

Name
CDS support team
Postal Address
CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France
E-Mail
cds-question@unistra.fr