  We present a combined analysis of the observations of the gravitational
microlensing event OGLE-2015-BLG-0479 taken both from the ground and by the
{\it Spitzer Space Telescope}. The light curves seen from the ground and from
space exhibit a time offset of $\sim 13$ days between the caustic spikes,
indicating that the relative lens-source positions seen from the two places are
displaced by parallax effects. From modeling the light curves, we measure the
space-based microlens parallax. Combined with the angular Einstein radius
measured by analyzing the caustic crossings, we determine the mass and distance
of the lens. We find that the lens is a binary composed of two G-type stars
with masses $\sim 1.0\ M_\odot$ and $\sim 0.9\ M_\odot$ located at a distance
$\sim 3$ kpc. In addition, we are able to constrain the complete orbital
parameters of the lens thanks to the precise measurement of the microlens
parallax derived from the joint analysis. In contrast to the binary event
OGLE-2014-BLG-1050, which was also observed by {\it Spitzer}, we find that the
interpretation of OGLE-2015-BLG-0479 does not suffer from the degeneracy
between $(\pm,\pm)$ and $(\pm,\mp)$ solutions, confirming that the four-fold
parallax degeneracy in single-lens events collapses into the two-fold
degeneracy for the general case of binary-lens events. The location of the
blend in the color-magnitude diagram is consistent with the lens properties,
suggesting that the blend is the lens itself. The blend is bright enough for
spectroscopy and thus this possibility can be checked from future follow-up
observations.
