Exoplanets and their host stars in the era of GAIA DR3

Statistical analysis of exoplanets poses several challenges, such as low number statistics (for a given parameter) and non-homogeneous estimation of stellar and planetary parameters coming from several sources. However, with the recent GAIA DR3 data release, it is possible to have a larger sample of stars whose parameters are determined homogeneously. In this work, we present the preliminary chemical and kinematic analysis results using the latest GAIA DR3 data for a sample of 3600+ exoplanet host stars. We revisit the planet-mass vs stellar-metallicity correlation for the planet-hosting stars. Our preliminary findings suggest that the metallicities estimates from the GAIA DR3 are systematically underestimated for our stars compared to prior high-resolution spectroscopic studies. Since parallaxes, proper motions, and radial velocities are also available homogeneously (and with better accuracy) for the exoplanet hosting stars (from GAIA DR3), we also performed a kinematic analysis and computed the galactic orbital parameters for our stars. We find that the population of stars hosting small planets differ significantly from giant planet-hosting stars statistically regarding galactic orbital parameters. Most of our findings using the GAIA DR3 data release seem consistent with prior studies done with a much lower number of samples.