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Microlensing detections of cool planets are important for the construction ofan unbiased sample to estimate the frequency of planets beyond the snow line,which is where giant planets are thought to form according to the coreaccretion theory of planet formation. In this paper, we report the discovery ofa giant planet detected from the analysis of the light curve of ahigh-magnification microlensing event MOA-2010-BLG-477. The measuredplanet-star mass ratio is $q=(2.181\pm0.004)\times 10^{-3}$ and the projectedseparation is $s=1.1228\pm0.0006$ in units of the Einstein radius. The angularEinstein radius is unusually large $\theta_{\rm E}=1.38\pm 0.11$ mas. Combiningthis measurement with constraints on the "microlens parallax" and the lensflux, we can only limit the host mass to the range $0.13<M/M_\odot<1.0$. Inthis particular case, the strong degeneracy between microlensing parallax andplanet orbital motion prevents us from measuring more accurate host and planetmasses. However, we find that adding Bayesian priors from two effects (Galacticmodel and Keplerian orbit) each independently favors the upper end of this massrange, yielding star and planet masses of $M_*=0.67^{+0.33}_{-0.13}\ M_\odot$and $m_p=1.5^{+0.8}_{-0.3}\ M_{\rm JUP}$ at a distance of $D=2.3\pm0.6$ kpc,and with a semi-major axis of $a=2^{+3}_{-1}$ AU. Finally, we show that thelens mass can be determined from future high-resolution near-IR adaptive opticsobservations independently from two effects, photometric and astrometric.

MOA-2010-BLG-477Lb: constraining the mass of a microlensing planet from microlensing parallax, orbital motion and detection of blended light