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There are two planetary formation scenarios: core accretion and gravitationaldisk instability. Based on the fact that gaseous objects are preferentiallyobserved around metal-rich host stars, most extra-solar gaseous objectsdiscovered to date are thought to have been formed by core accretion. Here, wepresent 569 samples of gaseous planets and brown dwarfs found in 485 planetarysystems that span three mass regimes with boundary values at 4 and 25Jupiter-mass masses through performing cluster analyses of these samplesregarding the host-star metallicity, after minimizing the impact of theselection effect of radial-velocity measurement on the cluster analysis. Thelarger mass is thought to be the upper mass limit of the objects that wereformed during the planetary formation processes. In contrast, the lower masslimit appears to reflect the difference between planetary formation processesaround early-type and G-type stars; disk instability plays a greater role inthe planetary formation process around early-type stars than that around G-typestars. Population with masses between 4 and 25 Jupiter masses that orbitearly-type stars comprise planets formed not only via the core-accretionprocess but also via gravitational disk instability because the populationpreferentially orbits metal-poor stars or is independent of the host-starmetallicity. Therefore, it is essential to have a hybrid scenario for theplanetary formation of the diverse systems.

Multiple Populations of Extrasolar Gas Giants