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We present the confirmation of a new sub-Neptune close to the transitionbetween super-Earths and sub-Neptunes transiting the M2 dwarf TOI- 269 (TIC220479565, V = 14.4 mag, J = 10.9 mag, Rstar = 0.40 Rsun, Mstar = 0.39 Msun, d= 57 pc). The exoplanet candidate has been identified in multiple TESS sectors,and validated with high-precision spectroscopy from HARPS and ground-basedphotometric follow-up from ExTrA and LCO-CTIO. We determined mass, radius, andbulk density of the exoplanet by jointly modeling both photometry and radialvelocities with juliet. The transiting exoplanet has an orbital period of P =3.6977104 +- 0.37 days, a radius of 2.77 +- 0.12 Rearth, and a mass of 8.8+- 1.4 Mearth. Since TOI-269 b lies among the best targets of its category foratmospheric characterization, it would be interesting to probe the atmosphereof this exoplanet with transmission spectroscopy in order to compare it toother sub-Neptunes. With an eccentricity e = 0.425+0.082-0.086, TOI-269 b hasone of the highest eccentricities of the exoplanets with periods less than 10days. The star being likely a few Gyr old, this system does not appear to bedynamically young. We surmise TOI-269 b may have acquired its high eccentricityas it migrated inward through planet-planet interactions.

TOI-269 b: An eccentric sub-Neptune transiting a M2 dwarf revisited with ExTrA