TOI-4914, TOI-2714 and TOI-2981 RV curves

Similarly, TOI-2981 b orbits a metal-poor star ([Fe/H]~=-0.11), while TOI-2714 b orbits a metal-rich star ([Fe/H]~=0.30). Our radial velocity (RV) follow-up with the HARPS spectrograph allows us to detect their Keplerian signals at high significance (7, 30, and 23{sigma}, respectively) and to place a strong constraint on the eccentricity of TOI-4914 b (18{sigma}). TOI-4914 b, with its large radius (R_mp_~=1.15R_mJ_) and low insolation flux (F_star_<2x10^8^merg/s/cm^2^), appears to be more inflated than what is supported by current theoretical models for giant planets.

Moreover, it does not conform to the previously noted trend that warm giant planets orbiting metal-poor stars have low eccentricities. This study thus provides insights into the diverse orbital characteristics and formation processes of giant exoplanets, in particular the role of stellar metallicity in the evolution of planetary systems.