The GAPS programme at TNG. LVII. TOI-5076b: A warm sub-Neptune planet orbiting a thin-to-thick-disk transition star in a wide binary system
Scandariato, G.; Pagano, I.; Winn, J. N.; Sozzetti, A.; Lanza, A. F.; Montalto, M.; Nascimbeni, V.; Seager, S.; Nardiello, D.; Damasso, M.; Naponiello, L.; Biazzo, K.; Bonomo, A. S.; Bieryla, A.; Desidera, S.; Latham, D. W.; Mancini, L.; Fong, W.; Andreuzzi, G.; Cosentino, R.; Pedani, M.; Bignamini, A.; Cabona, L.; Maggio, A.; Mantovan, G.; Singh, V.; Briceño, C.; Mann, A. W.; Strakhov, I. A.; Safonov, B. S.; Zingales, T.; Ziegler, C.; Law, N.; Molinaro, M.; Greco, N.; Fiorenzano, A.; Goeke, B.; Hesse, K. M.; Kostov, V. B.
Italy, Spain, United States, Australia, Chile, Germany, Russia
Abstract
Aims: We report the confirmation of a new transiting exoplanet orbiting the star TOI-5076.
Methods: We present our vetting procedure and follow-up observations which led to the confirmation of the exoplanet TOI-5076b. In particular, we employed high-precision TESS photometry, high-angular-resolution imaging from several telescopes, and high-precision radial velocities from HARPS-N.
Results: From the HARPS-N spectroscopy, we determined the spectroscopic parameters of the host star: Teff = (5070±143) K, log 𝑔 = (4.6±0.3), [Fe/H] = (+0.20±0.08), and [α/Fe] = 0.05±0.06. The transiting planet is a warm sub-Neptune with a mass mp = (16±2) M⊙, a radius rp =(3.2±0.l) R⊙ yielding a density ρp = (2.8±0.5) g cm−3. It revolves around its star approximately every 23.445 days.
Conclusions: The host star is a metal-rich, K2V dwarf, located at about 82 pc from the Sun with a radius of R⋆ = (0.78±0.01) R⊙ and a mass of M⋆ = (0.80±0.07) M⊙. It forms a common proper motion pair with an M-dwarf companion star located at a projected separation of 2178 au. The chemical analysis of the host-star and the Galactic-space velocities indicate that TOI-5076 belongs to the old population of thin-to-thick-disk transition stars. The density of TOI-5076b suggests the presence of a large fraction by volume of volatiles overlying a massive core. We found that a circular orbit solution is marginally favored with respect to an eccentric orbit solution for TOI-5076b.