<< back
A warm super-Neptune around the G-dwarf star TOI-1710 revealed with TESS, SOPHIE, and HARPS-N

P. C. König, M. Damasso, G. Hébrard, L. Naponiello, P. Cortés-Zuleta, K. Biazzo, N. C. Santos, A. S. Bonomo, A. Lecavelier Des Etangs, L. Zeng, S. Hoyer, A. Sozzetti, L. Affer, J. -M. Almenara, S. Benatti, A. Bieryla, I. Boisse, X. Bonfils, W. Boschin, A. Carmona, R. Claudi, K. A. Collins, S. Dalal, M. Deleuil, X. Delfosse, O. D. S. Demangeon, S. Desidera, R. F. Díaz, T. Forveille, N. Heidari, G. A. J. Hussain, J. S. Jenkins, G. Lacedelli, D. W. Latham, L. Malavolta, L. Mancini, E. Martioli, G. Micela, P. Miles-Páez, C. Moutou, D. Nardiello, V. Nascimbeni, M. Pinamonti, G. Piotto, G. R. Ricker, R. P. Schwarz, S. Seager, S. Seager, P. A. Strøm, R. K. Vanderspek, J. N. Winn, J. Wittrock

We report the discovery and characterization of the transiting extrasolar planet TOI-1710 b. It was first identified as a promising candidate by the Transiting Exoplanet Survey Satellite. Its planetary nature was then established with SOPHIE and HARPS-N spectroscopic observations via the radial-velocity method. The stellar parameters for the host star are derived from the spectra and a joint Markov chain Monte-Carlo adjustment of the spectral energy distribution and evolutionary tracks of TOI-1710. A joint MCMC analysis of the TESS light curve and the radial-velocity evolution allows us to determine the planetary system properties. From our analysis, TOI-1710 b is found to be a massive warm super-Neptune (Mp = 28.3 ± 4.7 M and Rp = 5.34 ± 0.11 R) orbiting a G5V dwarf star (Teff = 5665 ± 55 K) on a nearly circular 24.3-day orbit (e = 0.16 ± 0.08). The orbital period of this planet is close to the estimated rotation period of its host star Prot = 22.5 ± 2.0 days and it has a low Keplerian semi-amplitude K = 6.4 ± 1.0 m s−1; we thus performed additional analyses to show the robustness of the retrieved planetary parameters. With a low bulk density of 1.03 ± 0.23 g cm−3 and orbiting a bright host star (J = 8.3, V = 9.6), TOI-1710 b is one of the best targets in this mass-radius range (near the Neptunian desert) for atmospheric characterization via transmission spectroscopy, a key measurement in constraining planet formation and evolutionary models of sub-Jovian planets.

planetary systems / techniques: photometric / techniques: spectroscopic / techniques: radial velocities / star: activity

Astronomy & Astrophysics
Volume 666, Article Number A183, Number of pages 17
2022 October

>> ADS>> DOI

Faculdade de Ciências da Universidade de Lisboa Universidade do Porto Faculdade de Ciências e Tecnologia da Universidade de Coimbra
Fundação para a Ciência e a Tecnologia COMPETE 2020 PORTUGAL 2020 União Europeia