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We report the discovery of a massive planet OGLE-2008-BLG-355Lb. The lightcurve analysis indicates a planet:host mass ratio of q = 0.0118 +/- 0.0006 at aseparation of 0.877 +/- 0.010 Einstein radii. We do not measure a significantmicrolensing parallax signal and do not have high angular resolution imagesthat could detect the planetary host star. Therefore, we do not have a directmeasurement of the host star mass. A Bayesian analysis, assuming that all hoststars have equal probability to host a planet with the measured mass ratioimplies a host star mass of M_h = 0.37_{-0.17}^{+0.30} M_Sun and a companion ofmass M_P = 4.6^{+3.7}_{-2.2} M_Jup, at a projected separation of r_proj =1.70^{+0.29}_{-0.30} AU. The implied distance to the planetary system is D_L =6.8 +/- 1.1 kpc. A planetary system with the properties preferred by theBayesian analysis would be a challenge to the core-accretion model of planetformation, as the core-accretion model predicts that massive planets are farmore likely to form around more massive host stars. This core accretion modelprediction is not consistent with our Bayesian prior of an equal probability ofhost stars of all masses to host a planet with the measured mass ratio. So, ifthe core accretion model prediction is right, we should expect that follow-uphigh angular resolution observations will detect a host star with a mass in theupper part of the range allowed by the Bayesian analysis. That is, the hostwould probably be a K or G dwarf.

OGLE-2008-BLG-355Lb: A Massive Planet around A Late type Star