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We present the analysis of the simultaneous high resolution images from the{\it Hubble Space Telescope} and Keck Adaptive Optics system of the planetaryevent OGLE-2012-BLG-0950 that determine that the system consists of a $0.58 \pm0.04 \rm{M}_\odot$ host star orbited by a $39\pm 8 \rm{M}_\oplus$ planet of atprojected separation of $2.54 \pm 0.23\,$AU. The planetary system is located ata distance of $2.19\pm 0.23$ kpc from Earth. This is the second microlensplanet beyond the snow line with a mass measured to be in the mass range$20$--$80 \rm{M}_\oplus$. The runaway gas accretion process of the coreaccretion model predicts few planets in this mass range, because giant planetsare thought to be growing rapidly at these masses and they rarely completegrowth at this mass. So, this result suggests that the core accretion theorymay need revision. This analysis also demonstrates the techniques that will beused to measure the masses of planets and their host stars by the WFIRSTexoplanet microlensing survey: one-dimensional microlensing parallax combinedwith the separation and brightness measurement of the unresolved source andhost stars to yield multiple redundant constraints on the masses and distanceof the planetary system.

WFIRST Exoplanet Mass Measurement Method Finds a Planetary Mass of $39\pm 8 M_\oplus$ for OGLE-2012-BLG-0950Lb