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Publication Detail
TOI-220 b: a warm sub-Neptune discovered by TESS
  • Publication Type:
    Journal article
  • Publication Sub Type:
    Article
  • Authors:
    Hoyer S, Gandolfi D, Armstrong DJ, Deleuil M, Acuña L, de Medeiros JR, Goffo E, Lillo-Box J, Mena ED, Lopez TA, Santerne A, Sousa S, Fridlund M, Adibekyan V, Collins KA, Serrano LM, Cortés-Zuleta P, Howell SB, Deeg H, Aguichine A, Barragán O, Bryant EM, Martins BLC, Collins KI, Cooke BF, Díaz RF, Esposito M, Furlan E, Hojjatpanah S, Jackman J, Jenkins JM, Jensen ELN, Latham DW, Le ao IC, Matson RA, Nielsen LD, Osborn A, Otegi JF, Rodler F, Sabotta S, Scott NJ, Seager S, Stockdale C, Strøm PA, Vanderspek R, Van Eylen V, Wheatley PJ, Winn JN, Almenara JM, Barrado D, Barros SCC, Bayliss D, Bouchy F, Boyd PT, Cabrera J, Cochran WD, Demangeon O, Doty JP, Dumusque X, Figueira P, Fong W, Grziwa S, Hatzes AP, Kabáth P, Knudstrup E, Korth J, Livingston JH, Luque R, Mousis O, Mullally SE, Osborn HP, Pallé E, Persson CM, Redfield S, Santos NC, Smith J, Šubjak J, Twicken JD, Udry S, Yahalomi DA
  • Publisher:
    Oxford University Press (OUP)
  • Publication date:
    01/08/2021
  • Journal:
    Monthly Notices of the Royal Astronomical Society
  • Status:
    Published
  • Print ISSN:
    0035-8711
  • Language:
    en
Abstract
Abstract 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.
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