The browser you are using is not supported by this website. All versions of Internet Explorer are no longer supported, either by us or Microsoft (read more here:

Please use a modern browser to fully experience our website, such as the newest versions of Edge, Chrome, Firefox or Safari etc.


Judith Korth



TOI-220 b : A warm sub-Neptune discovered by TESS


  • S. Hoyer
  • D. Gandolfi
  • D. J. Armstrong
  • M. Deleuil
  • L. Acuña
  • J. R. De Medeiros
  • E. Goffo
  • J. Lillo-Box
  • E. Delgado Mena
  • T. A. Lopez
  • A. Santerne
  • S. Sousa
  • M. Fridlund
  • V. Adibekyan
  • K. A. Collins
  • L. M. Serrano
  • P. Cortés-Zuleta
  • S. B. Howell
  • H. Deeg
  • A. Aguichine
  • O. Barragán
  • E. M. Bryant
  • B. L. Canto Martins
  • K. I. Collins
  • B. F. Cooke
  • R. F. Díaz
  • M. Esposito
  • E. Furlan
  • S. Hojjatpanah
  • J. Jackman
  • J. M. Jenkins
  • E. L.N. Jensen
  • D. W. Latham
  • I. C. Leão
  • R. A. Matson
  • L. D. Nielsen
  • A. Osborn
  • J. F. Otegi
  • F. Rodler
  • S. Sabotta
  • N. J. Scott
  • S. Seager
  • C. Stockdale
  • P. A. Strøm
  • R. Vanderspek
  • V. Van Eylen
  • P. J. Wheatley
  • J. N. Winn
  • J. M. Almenara
  • D. Barrado
  • S. C.C. Barros
  • D. Bayliss
  • F. Bouchy
  • P. T. Boyd
  • J. Cabrera
  • W. D. Cochran
  • O. Demangeon
  • J. P. Doty
  • X. Dumusque
  • P. Figueira
  • W. Fong
  • S. Grziwa
  • A. P. Hatzes
  • P. Kabáth
  • E. Knudstrup
  • J. Korth
  • J. H. Livingston
  • R. Luque
  • O. Mousis
  • S. E. Mullally
  • H. P. Osborn
  • E. Pallé
  • C. M. Persson
  • S. Redfield
  • N. C. Santos
  • J. Smith
  • J. Šubjak
  • J. D. Twicken
  • S. Udry
  • D. A. Yahalomi

Summary, in English

In this paper, we report the discovery of TOI-220 b, a new sub-Neptune detected by the Transiting Exoplanet Survey Satellite (TESS) and confirmed by radial velocity follow-up observations with the HARPS spectrograph. Based on the combined analysis of TESS transit photometry and high precision radial velocity measurements, we estimate a planetary mass of 13.8 ± 1.0 M⊕ and radius of 3.03 ± 0.15 R⊕, implying a bulk density of 2.73 ± 0.47 g cm-3. TOI-220 b orbits a relative bright (V= 10.4) and old (10.1 ± 1.4 Gyr) K dwarf star with a period of ∼10.69 d. Thus, TOI-220 b is a new warm sub-Neptune with very precise mass and radius determinations. A Bayesian analysis of the TOI-220 b internal structure indicates that due to the strong irradiation it receives, the low density of this planet could be explained with a steam atmosphere in radiative-convective equilibrium and a supercritical water layer on top of a differentiated interior made of a silicate mantle and a small iron core.

Publishing year







Monthly Notices of the Royal Astronomical Society





Document type

Journal article


Oxford University Press


  • planets and satellites: fundamental parameters
  • planets and satellites: individual: TYC 8897-01263-1
  • stars: fundamental parameters
  • techniques: photometric
  • techniques: radial velocities




  • ISSN: 0035-8711