  In this paper, we present the analysis of the binary gravitational
microlensing event OGLE-2015-BLG-0196. The event lasted for almost a year and
the light curve exhibited significant deviations from the lensing model based
on the rectilinear lens-source relative motion, enabling us to measure the
microlens parallax. The ground-based microlens parallax is confirmed by the
data obtained from space-based microlens observations using the {\it Spitzer}
telescope. By additionally measuring the angular Einstein radius from the
analysis of the resolved caustic crossing, the physical parameters of the lens
are determined up to the two-fold degeneracy: $u_0<0$ and $u_0>0$ solutions
caused by the well-known "ecliptic" degeneracy. It is found that the binary
lens is composed of two M dwarf stars with similar masses $M_1=0.38\pm 0.04\
M_\odot$ ($0.50\pm 0.05\ M_\odot)$ and $M_2=0.38\pm 0.04\ M_\odot$ ($0.55\pm
0.06\ M_\odot$) and the distance to the lens is $D_{\rm L}=2.77\pm 0.23$ kpc
($3.30\pm 0.29$ kpc). Here the physical parameters out and in the parenthesis
are for the $u_0<0$ and $u_0>0$ solutions, respectively.
