A super-Earth and a sub-Neptune orbiting the bright, quiet M3 dwarf TOI-1266

B. O. Demory, F. J. Pozuelos, Y. Gómez Maqueo Chew, L. Sabin, R. Petrucci, U. Schroffenegger, S. L. Grimm, M. Sestovic, M. Gillon, J. McCormac, K. Barkaoui, W. Benz, A. Bieryla, F. Bouchy, A. Burdanov, K. A. Collins, J. De Wit, C. D. Dressing, L. J. Garcia, S. GiacaloneP. Guerra, J. Haldemann, K. Heng, E. Jehin, E. Jofré, S. R. Kane, J. Lillo-Box, V. Maigné, C. Mordasini, B. M. Morris, P. Niraula, D. Queloz, B. V. Rackham, A. B. Savel, A. Soubkiou, G. Srdoc, K. G. Stassun, A. H.M.J. Triaud, R. Zambelli, G. Ricker, D. W. Latham, S. Seager, J. N. Winn, J. M. Jenkins, T. Calvario-Velásquez, J. A. Franco Herrera, E. Colorado, E. O. Cadena Zepeda, L. Figueroa, A. M. Watson, E. E. Lugo-Ibarra, L. Carigi, G. Guisa, J. Herrera, G. Sierra Díaz, J. C. Suárez, D. Barrado, N. M. Batalha, Z. Benkhaldoun, A. Chontos, F. Dai, Z. Essack, M. Ghachoui, C. X. Huang, D. Huber, H. Isaacson, J. J. Lissauer, M. Morales-Calderón, P. Robertson, A. Roy, J. D. Twicken, A. Vanderburg, L. M. Weiss

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Abstract

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 Mp = 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.

Original languageEnglish (US)
Article numberA49
JournalAstronomy and Astrophysics
Volume642
DOIs
StatePublished - Oct 1 2020

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Keywords

  • Instrumentation: detectors
  • Planets and satellites: detection

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