Bibcode
Hoyer, S.; Gandolfi, D.; Armstrong, D. J.; Deleuil, M.; Acuña, L.; de Medeiros, J. R.; Goffo, E.; Lillo-Box, J.; Delgado Mena, E.; Lopez, T. A.; Santerne, A.; Sousa, S.; Fridlund, M.; Adibekyan, V.; Collins, K. A.; Serrano, L. M.; Cortés-Zuleta, P.; Howell, S. B.; Deeg, H.; Aguichine, A.; Barragán, O.; Bryant, E. M.; Canto Martins, B. L.; Collins, K. I.; Cooke, B. F.; Díaz, R. F.; Esposito, M.; Furlan, E.; Hojjatpanah, S.; Jackman, J.; Jenkins, J. M.; Jensen, E. L. N.; Latham, D. W.; Leão, I. C.; Matson, R. A.; Nielsen, L. D.; Osborn, A.; Otegi, J. F.; Rodler, F.; Sabotta, S.; Scott, N. J.; Seager, S.; Stockdale, C.; Strøm, P. A.; Vanderspek, R.; Van Eylen, V.; Wheatley, P. J.; Winn, J. N.; Almenara, J. M.; Barrado, D.; Barros, S. C. C.; Bayliss, D.; Bouchy, F.; Boyd, P. T.; Cabrera, J.; Cochran, W. D.; Demangeon, O.; Doty, J. P.; Dumusque, X.; Figueira, P.; Fong, W.; Grziwa, S.; Hatzes, A. P.; Kabáth, P.; Knudstrup, E.; Korth, J.; Livingston, J. H.; Luque, R.; Mousis, O.; Mullally, S. E.; Osborn, H. P.; Pallé, E.; Persson, C. M.; Redfield, S.; Santos, N. C.; Smith, J.; Šubjak, J.; Twicken, J. D.; Udry, S.; Yahalomi, D. A.
Bibliographical reference
Monthly Notices of the Royal Astronomical Society
Advertised on:
8
2021
Citations
8
Refereed citations
8
Description
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 $\rm {g\,cm}^{-3}$. 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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