The GAPS programme at TNG. XL. A puffy and warm Neptune-sized planet and an outer Neptune-mass candidate orbiting the solar-type star TOI-1422
Moutou, C.; Pagano, I.; Winn, J. N.; Poretti, E.; Rainer, M.; Sozzetti, A.; Giacobbe, P.; Lanza, A. F.; Maldonado, J.; Piotto, G.; Jenkins, J. M.; Nascimbeni, V.; Ricker, G. R.; Seager, S.; Twicken, J. D.; Borsa, F.; Lillo-Box, J.; Micela, G.; Nardiello, D.; Hébrard, G.; König, P. -C.; Damasso, M.; Naponiello, L.; Biazzo, K.; Bonomo, A. S.; Zeng, L.; Benatti, S.; Bieryla, A.; Claudi, R.; Delfosse, X.; Desidera, S.; Heidari, N.; Latham, D. W.; Mancini, L.; Pinamonti, M.; Stognone, R. G.; Vanderspek, R.; Cosentino, R.; Harutyunyan, A.; Molinari, E.; Pedani, M.; Hellier, C.; Covino, E.; Bignamini, A.; Knapic, C.; Maggio, A.; Morgan, E. H.; Quintana, E. V.; Essack, Z.; Dragomir, D.; Lissauer, J. J.; Molinaro, M.; Magazzù, A.; Eastman, J. D.; Fiorenzano, A. F. M.; Basilicata, M.; de Gurtubai, A.; Pace, E.
Italy, Germany, France, Spain, United States, Iran, United Kingdom
Abstract
Context. Neptunes represent one of the main types of exoplanets and have chemical-physical characteristics halfway between rocky and gas giant planets. Therefore, their characterization is important for understanding and constraining both the formation mechanisms and the evolution patterns of planets.
Aims: We investigate the exoplanet candidate TOI-1422 b, which was discovered by the TESS space telescope around the high proper-motion G2 V star TOI-1422 (V = 10.6 mag), 155 pc away, with the primary goal of confirming its planetary nature and characterising its properties.
Methods: We monitored TOI-1422 with the HARPS-N spectrograph for 1.5 yr to precisely quantify its radial velocity (RV) variation. We analyse these RV measurements jointly with TESS photometry and check for blended companions through high-spatial resolution images using the AstraLux instrument.
Results: We estimate that the parent star has a radius of R⋆ = 1.019−0.013+0.014 R⊙, and a mass of M⋆ = 1.019−0.013+0.014 M⊙. Our analysis confirms the planetary nature of TOI-1422 b and also suggests the presence of a Neptune-mass planet on a more distant orbit, the candidate TOI-1422 c, which is not detected in TESS light curves. The inner planet, TOI-1422 b, orbits on a period of Pb = 12.9972 ± 0.0006 days and has an equilibrium temperature of Teq,b = 867 ± 17 K. With a radius of Rb = 3.96−0.11+0.13 R⊕, a mass of Mb = 9.0−2.0+2.3 M⊕ and, consequently, a density of ρb = 0.795−0.235+0.290g cm−3, it can be considered a warm Neptune-sized planet. Compared to other exoplanets of a similar mass range, TOI-1422 b is among the most inflated, and we expect this planet to have an extensive gaseous envelope that surrounds a core with a mass fraction around 10% - 25% of the total mass of the planet. The outer non-transiting planet candidate, TOI-1422 c, has an orbital period of Pc = 29.29−0.20+0.21 days, a minimum mass, Mcsin i, of 11.1−2.3+2.6 M⊕, an equilibrium temperature of Teq,c = 661 ± 13 K and, therefore, if confirmed, could be considered as another warm Neptune.