TOI-969: a late-K dwarf with a hot mini-Neptune in the desert and an eccentric cold Jupiter

Lillo-Box, J.; Gandolfi, D.; Armstrong, D. J.; Collins, K. A.; Nielsen, L. D.; Luque, R.; Korth, J.; Sousa, S. G.; Quinn, S. N.; Acuna, L.; Howell, S. B.; Morello, G.; Hellier, C.; Giacalone, S.; Hoyer, S.; Stassun, K.; Palle, E.; Aguichine, A.; Mousis, O.; Adibekyan, V.; Azevedo Silva, T.; Barrado, D.; Deleuil, M.; Eastman, J. D.; Fukui, A.; Hawthorn, F.; Irwin, J. M.; Jenkins, J. M.; Latham, D. W.; Muresan, A.; Narita, N.; Persson, C. M.; Santerne, A.; Santos, N. C.; Savel, A. B.; Osborn, H. P.; Teske, J.; Wheatley, P. J.; Winn, J. N.; Barros, S. C. C.; Butler, R. P.; Caldwell, D. A.; Charbonneau, D.; Cloutier, R.; Crane, J. D.; Demangeon, O. D. S.; Diaz, R. F.; Dumusque, X.; Esposito, M.; Falk, B.; Gill, H.; Hojjatpanah, S.; Kreidberg, L.; Mireles, I.; Osborn, A.; Ricker, G. R.; Rodriguez, J. E.; Schwarz, R. P.; Seager, S.; Serrano Bell, J.; Shectman, S. A.; Shporer, A.; Vezie, M.; Wang, S. X.; Zhou, G.
2023
ASTRONOMY & ASTROPHYSICS
DOI
10.1051/0004-6361/202243879
Context. The current architecture of a given multi-planetary system is a key fingerprint of its past formation and dynamical evolution history. Long-term follow-up observations are key to complete their picture. Aims. In this paper, we focus on the confirmation and characterization of the components of the TOI-969 planetary system, where TESS detected a Neptune-size planet candidate in a very close-in orbit around a late K-dwarf star. Methods. We use a set of precise radial velocity observations from HARPS, PFS, and CORALIE instruments covering more than two years in combination with the TESS photometric light curve and other ground-based follow-up observations to confirm and characterize the components of this planetary system. Results. We find that TOI-969 b is a transiting close-in (P-b similar to 1.82 days) mini-Neptune planet (m(b) = 9.1(-1.0)(+1.1) M-Phi, R-b = 2.765(-0.097)(+0.088) R-Phi), placing it on the lower boundary of the hot-Neptune desert (T-eq,T-b = 941 +/- 31 K). The analysis of its internal structure shows that TOI-969 b is a volatile-rich planet, suggesting it underwent an inward migration. The radial velocity model also favors the presence of a second massive body in the system, TOI-969 c, with a long period of P-c = 1700(-280)(+290) days, a minimum mass of m(c) sin i(c) = 11.3(-0.9)(+1.1) M-Jup, and a highly eccentric orbit of e(c) = 0.628(-0.036)(+0.043). Conclusions. The TOI-969 planetary system is one of the few around K-dwarfs known to have this extended configuration going from a very close-in planet to a wide-separation gaseous giant. TOI-969 b has a transmission spectroscopy metric of 93 and orbits a moderately bright (G = 11.3 mag) star, making it an excellent target for atmospheric studies. The architecture of this planetary system can also provide valuable information about migration and formation of planetary systems.