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TOI-1227 b is an 11 Myr old validated transiting planet in the middle of itscontraction phase, with a current radius of 0.85 R$_J$. It orbits a low-masspre-main sequence star (0.170 M$_\odot$, 0.56 R$_\odot$) every 27.4 days. Themagnetic activity of its young host star induces radial velocity jitter andprevents good measurements of the planetary mass. We gathered additionaltransit observations of TOI-1227 b with space- and ground-based telescopes, andwe detected highly significant transit-timing variations (TTVs). Theiramplitude is about 40 minutes and their dominant timescale is longer than 3.7years. Their most probable origin is dynamical interactions with additionalplanets in the system. We modeled the TTVs with inner and outer perturbers nearfirst and second order resonances; several orbital configurations provide anacceptable fit. More data are needed to determine the actual orbitalconfiguration and eventually measure the planetary masses. These TTVs and anupdated transit chromaticity analysis reinforce the evidence that TOI-1227 b isa planet.

Evidence for transit-timing variations of the 11 Myr exoplanet TOI-1227 b