학술논문
A warm super-Neptune around the G-dwarf star TOI-1710 revealed with TESS, SOPHIE and HARPS-N
Document Type
Working Paper
Author
König, P. -C.; Damasso, M.; Hébrard, G.; Naponiello, L.; Cortés-Zuleta, P.; Biazzo, K.; Santos, N. C.; Bonomo, A. S.; Étangs, A. Lecavelier des; Zeng, L.; Hoyer, S.; Sozzetti, A.; Affer, L.; Almenara, J. M.; Benatti, S.; Bieryla, A.; Boisse, I.; Bonfils, X.; Boschin, W.; Carmona, A.; Claudi, R.; Collins, K. A.; Dalal, S.; Deleuil, M.; Delfosse, X.; Demangeon, O. D. S.; Desidera, S.; Díaz, R. F.; Forveille, T.; Heidari, N.; Hussain, G. A. J.; Jenkins, J.; Kiefer, F.; Lacedelli, G.; Latham, D. W.; Malavolta, L.; Mancini, L.; Martioli, E.; Micela, G.; Miles-Páez, P. A.; Moutou, C.; Nardiello, D.; Nascimbeni, V.; Pinamonti, M.; Piotto, G.; Ricker, G.; Schwarz, R. P.; Seager, S.; Stognone, R. G.; Strøm, P. A.; Vanderspek, R.; Winn, J.; Wittrock, J.
Source
A&A 666, A183 (2022)
Subject
Language
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 (TESS). 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 (MCMC) 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 ($M_{\rm p}=28.3\:\pm\:4.7\:{\rm M}_{\rm Earth}$ and $R_{\rm p}=5.34\:\pm\:0.11\:{\rm R}_{\rm Earth}$) orbiting a G5V dwarf star ($T_{\rm eff}=5665\pm~55\mathrm{K}$) on a nearly circular 24.3-day orbit ($e=0.16\:\pm\:0.08$). The orbital period of this planet is close to the estimated rotation period of its host star $P_{\rm rot}=22.5\pm2.0~\mathrm{days}$ and it has a low Keplerian semi-amplitude $K=6.4\pm1.0~\mathrm{m\:s^{-1}}$; we thus performed additional analyses to show the robustness of the retrieved planetary parameters. With a low bulk density of $1.03\pm0.23~\mathrm{g\:cm^{-3}}$ 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.
Comment: 18 pages, 16 figures, 5 tables, A&A in press
Comment: 18 pages, 16 figures, 5 tables, A&A in press