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, Luca Naponiello, P. Cortés-Zuleta, K. Biazzo, N. C. Santos, A. S. Bonomo, A. Lecavelier des Étangs, Li Zeng, S. Hoyer, A. Sozzetti, L. Affer, J. M. Almenara, S. Benatti, Allyson Bieryla, I. Boisse, X. Bonfils, W. Boschin, A. Carmona, R. Claudi, Karen 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, Jon M. Jenkins, F. Kiefer, G. Lacedelli, David W. Latham, L. Malavolta, L. Mancini, Eder Martioli, G. Micela, Paulo A. Miles-Páez, C. Moutou, D. Nardiello, V. Nascimbeni, M. Pinamonti, G. Piotto, G. Ricker, Richard P. Schwarz, S. Seager, R. G. Stognone, P. A. Wilson, R. Vanderspek, Joshua N. Winn, Justin M. Wittrock
Abstract
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 ( M p = 28.3 ± 4.7 M ⊕ and R p = 5.34 ± 0.11 R ⊕ ) orbiting a G5V dwarf star ( T eff = 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 P rot = 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.