TOI-1416 radial velocities Virtual Observatory Resource

Authors
  1. Deeg H.J.
  2. Georgieva I.Y.
  3. Nowak G.
  4. Persson C.M.
  5. Cale B.L.
  6. Murgas F.,Palle E.
  7. Godoy-Rivera D.
  8. Dai F.
  9. Ciardi D.R.
  10. Akana Murphy J.M.,Beck P.G.
  11. Burke C.J.
  12. Cabrera J.
  13. Carleo I.
  14. Cochran W.D.
  15. Collins K.A.,Csizmadia Sz.
  16. El Mufti M.
  17. Fridlund M.
  18. Fukui A.
  19. Gandolfi D.
  20. Garcia R.A.,Guenther E.W.
  21. Guerra P.
  22. Grziwa S.
  23. Isaacson H.
  24. Isogai K.
  25. Jenkins J.M.,Kabath P.
  26. Korth J.
  27. Lam K.W.F.
  28. Latham D.W.
  29. Luque R.
  30. Lund M.B.,Livingston J.H.
  31. Mathis S.
  32. Mathur S.
  33. Narita N.
  34. Orell-Miquel J.,Osborne H.L.M.
  35. Parviainen H.
  36. Plavchan P.P.
  37. Redfield S.
  38. Rodriguez D.R.,Schwarz R.P.
  39. Seager S.
  40. Smith A.M.S.
  41. Van Eylen V.
  42. Van Zandt J.,Winn J.N.
  43. Ziegler C.
  44. Published by
    CDS
Abstract

TOI-1416 (BD+42 2504, HIP 70705) is a V=10 late G- or early K-type dwarf star. TESS detected transits in its Sectors 16, 23, and 50 with a depth of about 455ppm and a period of 1.07 days. Radial velocities (RVs) confirm the presence of the transiting planet TOI-1416 b, which has a mass of 3.48+/-0.47M_{Earth}_ and a radius of 1.62+/-0.08R_{Earth}_, implying a slightly sub-Earth density of 4.50^+0.90^_-0.83_g/cm^3^. The RV data also further indicate a tentative planet, c, with a period of 27.4 or 29.5 days, whose nature cannot be verified due to strong suspicions of contamination by a signal related to the Moon's synodic period of 29.53 days. The nearly ultra-short-period planet TOI-1416 b is a typical representative of a short-period and hot (Teq=~1570K) super-Earth-like planet. A planet model of an interior of molten magma containing a significant fraction of dissolved water provides a plausible explanation for its composition, and its atmosphere could be suitable for transmission spectroscopy with JWST. The position of TOI-1416 b within the radius-period distribution corroborates the idea that planets with periods of less than one day do not form any special group. It instead implies that ultra-short-period planets belong to a continuous distribution of super-Earth-like planets with periods ranging from the shortest known ones up to =~30 days; their period-radius distribution is delimited against larger radii by the Neptune Desert and by the period-radius valley that separates super-Earths from sub-Neptune planets. In the abundance of small, short-periodic planets, a notable plateau has emerged between periods of 0.6-1.4 days, which is compatible with the low-eccentricity formation channel. For the Neptune Desert, its lower limits required a revision due to the increasing population of short-period planets; for periods shorter then 2 days, we establish a radius of 1.6R_{Earth}_ and a mass of 0.028M_jup_ (corresponding to 8.9M_{Earth}_) as the desert's lower limits. We also provide corresponding limits to the Neptune Desert against the planets' insolation and effective temperatures.

Keywords
  1. multiple-stars
  2. g-stars
  3. exoplanets
  4. radial-velocity
  5. visible-astronomy
Bibliographic source Bibcode
2023A&A...677A..12D
See also HTML
https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/677/A12
IVOA Identifier IVOID
ivo://CDS.VizieR/J/A+A/677/A12
Document Object Identifer DOI
doi:10.26093/cds/vizier.36770012

Access

Web browser access HTML
http://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/677/A12
https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/677/A12
http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/677/A12
IVOA Table Access TAP
http://tapvizier.cds.unistra.fr/TAPVizieR/tap
Run SQL-like queries with TAP-enabled clients (e.g., TOPCAT).

History

2023-08-28T08:55:25Z
Resource record created
2023-08-28T08:55:25Z
Created
2024-09-02T20:01:18Z
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