The Inflated, Eccentric Warm Jupiter TOI-4914 B Orbiting a Metal-Poor Star, and the Hot Jupiters TOI-2714 B and TOI-2981 B

Recent observations of giant planets have revealed unexpected bulk densities. Hot Jupiters, in particular, appear larger than expected for their masses compared to planetary evolution models, while warm Jupiters seem denser than expected. These differences are often attributed to the influence of the stellar incident flux, but it has been unclear if they also result from different planet formation processes, and if there is a trend linking the planetary density to the chemical composition of the host star. In this work, we present the confirmation of three giant planets in orbit around solar analogue stars. TOI-2714 b (P similar or equal to 2.5 d, R-p similar or equal to 1.22 RJ, M-p=0.72 M-J) and TOI-2981 b (P similar or equal to 3.6 d, R-P similar or equal to 1.2 R-J, M-P=2M(J)) are hot Jupiters on nearly circular orbits, while TOI-4914 b (P similar or equal to 10.6 d, R-P similar or equal to 1.15 R-J,M-p = 0.72 MJ) is a warm Jupiter with a significant eccentricity (e = 0.41 +/- 0.02) that orbits a star more metal-poor ([Fe/H] = -0.13) than most of the stars known to host giant planets. 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 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-p similar or equal to 1.15 R-J) and low insolation flux (F star < 2 x 10(8 )erg s(-1) 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.