Host star metallicities of hot, warm and cold Jupiters: gaia DR3 reveals clues to their formation pathways

It has been evident that planet properties and host star properties are well correlated. One of such interesting correlations is that giant planets are preferentially found around metal rich stars. These giant planets are located at various distances from their host stars, ranging from 0.1 au (hot Jupiters) to 10-100 au (classical Jupiters). Whether the formation mechanisms of these Jupiters are the same at all orbital distance, is an open question, and  a detailed analysis of metallicity and chemical abundances of host stars can provide clues to answer that. Previous studies in this direction suffered from small sample size and inhomogeneous determination of metallicity, but Gaia DR3 provides a homogeneous sample of [Fe/H] and [M/H] of a large number of giant planet hosting stars. After calibrating the field stars with GALAH and LAMOST, we find that hot Jupiters are slightly more metal rich than warm and cold ones. However there is only a marginal trend between host star metallicity and orbital period unlike previous claims (Buchhave et al. 2018). Our result indicates plausible formation channels for these Jupiters are probably the same.