A super-Earth and a sub-Neptune orbiting the bright, quiet M3 dwarf TOI-1266. (arXiv:2009.04317v1 [astro-ph.EP])

A super-Earth and a sub-Neptune orbiting the bright, quiet M3 dwarf TOI-1266. (arXiv:2009.04317v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Demory_B/0/1/0/all/0/1">B.-O. Demory</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pozuelos_F/0/1/0/all/0/1">F.J. Pozuelos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chew_Y/0/1/0/all/0/1">Y. Gomez Maqueo Chew</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sabin_L/0/1/0/all/0/1">L. Sabin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Petrucci_R/0/1/0/all/0/1">R. Petrucci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schroffenegger_U/0/1/0/all/0/1">U. Schroffenegger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grimm_S/0/1/0/all/0/1">S.L. Grimm</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sestovic_M/0/1/0/all/0/1">M. Sestovic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gillon_M/0/1/0/all/0/1">M. Gillon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McCormac_J/0/1/0/all/0/1">J. McCormac</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barkaoui_K/0/1/0/all/0/1">K. 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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
$M_mathrm{p}$ = $13.5_{-9.0}^{+11.0}$ $mathrm{M_{oplus}}$ ($<36.8$
$mathrm{M_{oplus}}$ at 2-$sigma$) for TOI-1266 b and $2.2_{-1.5}^{+2.0}$
$mathrm{M_{oplus}}$ ($<5.7$ $mathrm{M_{oplus}}$ at 2-$sigma$) for TOI-1266
c. We find small but non-zero orbital eccentricities of $0.09_{-0.05}^{+0.06}$
($<0.21$ at 2-$sigma$) for TOI-1266 b and $0.04pm0.03$ ($<0.10$ at
2-$sigma$) for TOI-1266 c. The equilibrium temperatures of both planets are of
$413pm20$ K and $344pm16$ 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.

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