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Demory, B.-O.; Pozuelos, F. J.; Gómez Maqueo Chew, Y.; Sabin, L.; Petrucci, R.; Schroffenegger, U.; Grimm, S. L.; Sestovic, M.; Gillon, M.; McCormac, J.; Barkaoui, K.; Benz, W.; Bieryla, A.; Bouchy, F.; Burdanov, A.; Collins, K. A.; de Wit, J.; Dressing, C. D.; Garcia, L. J.; Giacalone, S.; Guerra, P.; Haldemann, J.; Heng, K.; Jehin, E.; Jofré, E.; Kane, S. R.; Lillo-Box, J.; Maigné, V.; Mordasini, C.; Morris, B. M.; Niraula, P.; Queloz, D.; Rackham, B. V.; Savel, A. B.; Soubkiou, A.; Srdoc, G.; Stassun, K. G.; Triaud, A. H. M. J.; Zambelli, R.; Ricker, G.; Latham, D. W.; Seager, S.; Winn, J. N.; Jenkins, J. M.; Calvario-Velásquez, T.; Franco Herrera, J. A.; Colorado, E.; Cadena Zepeda, E. O.; Figueroa, L.; Watson, A. M.; Lugo-Ibarra, E. E.; Carigi, L.; Guisa, G.; Herrera, J.; Sierra Díaz, G.; Suárez, J. C.; Barrado, D.; Batalha, N. M.; Benkhaldoun, Z.; Chontos, A.; Dai, F.; Essack, Z.; Ghachoui, M.; Huang, C. X.; Huber, D.; Isaacson, H.; Lissauer, J. J.; Morales-Calderón, M.; Robertson, P.; Roy, A.; Twicken, J. D.; Vanderburg, A.; Weiss, L. M.
Astronomy and astrophysics (Berlin), 10/2020, Letnik: 642Journal Article, Web Resource
We report the discovery and characterisation of a super-Earth and a sub-Neptune transiting the bright ( K = 8.8), quiet, and nearby (37 pc) M3V dwarf TOI-1266. We validate the planetary nature of TOI-1266 b and c using four sectors of TESS photometry and data from the newly-commissioned 1-m SAINT-EX telescope located in San Pedro Mártir (México). We also include additional ground-based follow-up photometry as well as high-resolution spectroscopy and high-angular imaging observations. The inner, larger planet has a radius of R = 2.37 −0.12 +0.16 R ⊕ and an orbital period of 10.9 days. The outer, smaller planet has a radius of R = 1.56 −0.13 +0.15 R ⊕ on an 18.8-day orbit. The data are found to be consistent with circular, co-planar and stable orbits that are weakly influenced by the 2:1 mean motion resonance. Our TTV analysis of the combined dataset enables model-independent constraints on the masses and eccentricities of the planets. We find planetary masses of M p = 13.5 −9.0 +11.0 M ⊕ (<36.8 M ⊕ at 2- σ ) for TOI-1266 b and 2.2 −1.5 +2.0 M ⊕ (<5.7 M ⊕ at 2- σ ) for TOI-1266 c. We find small but non-zero orbital eccentricities of 0.09 −0.05 +0.06 (<0.21 at 2- σ ) for TOI-1266 b and 0.04 ± 0.03 (< 0.10 at 2- σ ) for TOI-1266 c. The equilibrium temperatures of both planets are of 413 ± 20 and 344 ± 16 K, respectively, assuming a null Bond albedo and uniform heat redistribution from the day-side to the night-side hemisphere. The host brightness and negligible activity combined with the planetary system architecture and favourable planet-to-star radii ratios makes TOI-1266 an exquisite system for a detailed characterisation.
