  We present high angular resolution imaging that detects the MOA-2008-BLG-379L
exoplanet host star using Keck adaptive optics and the Hubble Space Telescope.
These observations reveal host star and planet masses of $M_{\rm
host}=0.434\pm0.065 M_\odot$, and $m_p=2.44 \pm 0.49 M_{\rm Jupiter}$. They are
located at a distance of $D_L=3.44\pm0.53\,$kpc, with a projected separation of
$2.70\pm 0.42\,$AU. These results contribute to our determination of exoplanet
host star masses for the Suzuki et al. (2016) statistical sample, which will
determine the dependence of the planet occurrence rate on the mass and distance
of the host stars. We also present a detailed discussion of the image
constrained modeling version of the eesunhong light curve modeling code that
applies high angular resolution image constraints to the light curve modeling
process. This code increases modeling efficiency by a large factor by excluding
models that are inconsistent with the high angular resolution images. The
analysis of this and other events from the Suzuki et al. (2016) statistical
sample reveals the importance of including higher order effects, such as
microlensing parallax and planetary orbital motion even when these features are
not required to fit the light curve data. The inclusion of these effects may be
needed to obtain accurate estimates of the uncertainty of other microlensing
parameters that affect the inferred properties of exoplanet microlens systems.
This will be important for the exoplanet microlensing survey of the Roman Space
Telescope, which will use both light curve photometry and high angular
resolution imaging to characterize planetary microlens systems.
