TOI-1807 RV and flux curves

A great contribution to the study of planetary formation processes comes from the study of young, low-mass planets, with short orbital periods (<100 days). In the last three years, the NASA/TESS satellite has identified many planets of this kind, and their characterization is clearly mandatory to understand how they formed and evolved.Within the framework of the Global Architecture of Planetary System (GAPS) project, we performed the validation and characterization (radius and mass) of the ultra-short period planet TOI-1807 b, orbiting its young host star BD+39 2643 (~300Myr) in only 13-hours.

This is the youngest ultra-short period planet discovered so far. Thanks to a joint modeling of the stellar activity and planetary signals in the TESS light curve and in new HARPS-N radial-velocity measurements, which were combined with accurate estimation of stellar parameters, we validated the planetary nature of TOI-1807 b and measured its orbital and physical parameters. By using astrometric, photometric, and spectroscopic observations we found that BD+39 2643 is a young, active K dwarf star, member of a 300+/-80Myr old moving group and that it rotates in P_rot_=8.8+/-0.1-days.