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

B. -O. Demory, F. J. Pozuelos, Y. Gomez 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. Jofre, S. R. Kane, J. Lillo-Box, V. Maigne, 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-Velasquez, 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 Diaz, J. C. Suarez, 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-Calderon, 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 M\'artir (Mexico). 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$_{\oplus}$ and an orbital period of 10.9 days. The outer, smaller planet has a radius of $R=1.56_{-0.13}^{+0.15}$ R$_{\oplus}$ 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 $M_\mathrm{p}$ = $13.5_{-9.0}^{+11.0}$ $\mathrm{M_{\oplus}}$ ($
Original languageEnglish
JournalA&A
Volume642
DOIs
Publication statusPublished - 9 Sep 2020

Bibliographical note

In press. Accepted for publication in Astronomy and Astrophysics on 20 July 2020

Keywords

  • astro-ph.EP

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