E. Martioli, G. Hébrard, Leandro de Almeida, N. Heidari, D. Lorenzo-Oliveira, F. Kiefer, J. -M. Almenara, A. Bieryla, I. Boisse, X. Bonfils, C. Briceño, K. A. Collins, P. Cortés-Zuleta, S. Dalal, M. Deleuil, X. Delfosse, O. D. S. Demangeon, J. D. Eastman, T. Forveille, E. Furlan, S. B. Howell, S. Hoyer, J. M. Jenkins, D. W. Latham, N. M. Law, A. W. Mann, C. Moutou, N. C. Santos, S. G. Sousa, K. G. Stassun, C. Stockdale, G. Torres, J. D. Twicken, J. N. Winn, C. Ziegler
Abstract
Planetary systems around solar analogs inform us about how planets form and evolve in Solar System-like environments. We report the detection and characterization of two planetary systems around the solar analogs TOI-1736 and TOI-2141 using TESS photometry data and spectroscopic data obtained with the SOPHIE instrument on the 1.93 m telescope at the Observatoire de Haute-Provence (OHP). We performed a detailed spectroscopic analysis of these systems to obtain the precise radial velocities (RV) and physical properties of their host stars. TOI-1736 and TOI-2141 each host a transiting sub-Neptune with radii of 2.44 ± 0.18 R⊕ and 3.05 ± 0.23 R⊕, orbital periods of 7.073088(7) days and 18.26157(6) days, and masses of 12.8 ± 1.8 M⊕ and 24 ± 4 M⊕, respectively. TOI-1736 shows long-term RV variations that are consistent with a two-planet solution plus a linear trend of −0.177 m s−1 day−1. We measured an RV semi-amplitude of 201.1 ± 0.7 m s−1 for the outer companion, TOI-1736 c, implying aprojected mass of mcsin i = 8.09 ± 0.20 MJup. From the Gaia DR3 astrometric excess noise, we constrained the mass of TOI-1736 c at 8.7−0.6+1.5 MJup. This planet is in an orbit of 570.2 ± 0.6 days with an eccentricity of 0.362 ± 0.003 and a semi-major axis of 1.381 ± 0.017 au, where it receives a flux of 0.71 ± 0.08 times the bolometric flux incident on Earth, making it an interesting case of a supergiant planet that has settled into an eccentric orbit in the habitable zone of a solar analog. Our analysis of the mass-radius relation for the transiting sub-Neptunes shows that both TOI-1736 b and TOI-2141 b likely have an Earth-like dense rocky core and a water-rich envelope.
Keywords
planetary systems / stars: individual: TOI-1736 / stars: individual: TOI-2141 / stars: solar-type / techniques: photometric / techniques: radial velocities
Notes
- Full Tables A.1 and A.2 data are available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/680/A84
Astronomy & Astrophysics
Volume 680, Article Number A84, Number of pages 36
2023 December
