A super-Earth and a sub-Neptune orbiting the bright, quiet M3 dwarf TOI-1266
Demory, B.-O.; Pozuelos Romero, Francisco José ; Gómez Maqueo Chew, Y. et al. 2020 • In Astronomy and Astrophysics, 642, p. 49 Peer Reviewed verified by ORBi
instrumentation: detectors; planets and satellites: detection; Astrophysics - Earth and Planetary Astrophysics
Abstract :
[en] 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[SUB]-0.12[/SUB][SUP]+0.16[/SUP] R[SUB]⊕[/SUB] and an orbital period of 10.9 days. The outer, smaller planet has a radius of R = 1.56[SUB]-0.13[/SUB][SUP]+0.15[/SUP] R[SUB]⊕[/SUB] 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[SUB]p[/SUB] = 13.5[SUB]-9.0[/SUB][SUP]+11.0[/SUP] M[SUB]⊕[/SUB] (<36.8 M[SUB]⊕[/SUB] at 2-σ) for TOI-1266 b and 2.2[SUB]-1.5[/SUB][SUP]+2.0[/SUP] M[SUB]⊕[/SUB] (<5.7 M[SUB]⊕[/SUB] at 2-σ) for TOI-1266 c. We find small but non-zero orbital eccentricities of 0.09[SUB]-0.05[/SUB][SUP]+0.06[/SUP] (<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.
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Demory, B.-O.; Center for Space and Habitability, University of Bern, Gesellschaftsstrasse 6, 3012, Bern, Switzerland
Pozuelos Romero, Francisco José ; Space Sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liège, Allée du 6 Août 19C, 4000, Liège, Belgium
Gómez Maqueo Chew, Y.; Instituto de Astronomía, Universidad Nacional Autónoma de México, Ciudad Universitaria, Ciudad de México, 04510, México
Sabin, L.; Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 877, 22800, Ensenada, B.C., México
Petrucci, R.; Instituto de Astronomía, Universidad Nacional Autónoma de México, Ciudad Universitaria, Ciudad de México, 04510, México
Schroffenegger, U.; Center for Space and Habitability, University of Bern, Gesellschaftsstrasse 6, 3012, Bern, Switzerland
Grimm, S. L.; Center for Space and Habitability, University of Bern, Gesellschaftsstrasse 6, 3012, Bern, Switzerland
Sestovic, M.; Center for Space and Habitability, University of Bern, Gesellschaftsstrasse 6, 3012, Bern, Switzerland
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Chontos, A.; Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI, 96822, USA
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Huber, D.; Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI, 96822, USA
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Robertson, P.; Department of Physics & Astronomy, University of California Irvine, Irvine, CA, 92697, USA
Roy, A.; Division of Geological and Planetary Sciences, California Institute of Technology, 1200 East California Blvd, Pasadena, CA, 91125, USA
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