Modeling for formation of extrasolar planetary systems Shigeru Ida (Tokyo Institute of Technology) In order to directly compare with observed data of extrasolar planets, we have constructed a numerical scheme to simulate the anticipated mass and semimajor axis distributions of planets based on a comprehensive treatment of the sequential planet formation scenario (Ida & Lin 2004a, b, 2005, 2008a, 2008b, ApJ). In the scheme, we first generate a set of protoplanetary disk models and integrate growth and orbital migration of protoplanetary seeds due to planetesimal accretion. If planetary masses become large enough, gas accretion onto the planets is added. With the model, we have tried to explain statistical features of observed data such as mass and semimajor axis distributions of gas giant planets and large terrestrial planets (gsuper-Earthsh) and their dependences on metallicity and mass of host stars. We also presented theoretical predictions such as "planet desert" in the distributions and anticipated population of terrestrial planets in habitable zones that will be tested by on-going or near future observations. I will summarize our theoretical arguments and discuss about remaining problems and future perspectives in the theoretical modeling and comparison with observations (radial velocity, transit, microlensing, and direct imaging).