TOI-3288 A b and TOI-4666 b light and RV curves

The resulting RVs are jointly fit with TESS and ground-based photometry to derive the orbital and physical parameters of the systems. We present the GATOS program and its first results. We confirm two gas giants transiting the low-mass stars TOI-3288 A (K9V, Teff=3933+/-48K) and TOI-4666 (M2.5V, Teff=3512+/-36K).

TOI-3288 A hosts a hot Jupiter with a mass of 2.11+/-0.08M_Jup_ and a radius of 1.00+/-0.03R_Jup_, with an orbital period of 1.43 days (Teq=1059+/-20K). TOI-4666 hosts a 0.70+/-0.06M_Jup_ warm Jupiter (Teq=713+/-14K) with a radius of 1.11+/-0.04R_Jup_, with an orbital period of 2.91 days. At a population level, we identify a decrease in planetary mass with spectral type, where late M dwarfs host less massive giant planets than early M dwarfs.

More massive gas giants that deviate from this trend are preferentially hosted by more metal-rich stars. Furthermore, we find an increased binarity fraction among low-mass stars hosting gas giants, which may play a role in enhancing giant planet formation around low-mass stars. These mass characterizations contribute to the growing catalogue of well-defined giant exoplanets around low-mass stars.

The observed population trends agree with theoretical predictions, where higher metallicity can compensate for lower disk masses, and wide binary systems may influence planet formation and migration through Kozai-Lidov cycles or disk instabilities.