models, we present the physical parameters of the lens for both solutions in Table \[tab:phys\]. We assume the source parallax $\pi_s = 0.125~{\rm mas}$ since the source is a bulge red clump star (Figure \[fig:CMD\]). The geocentric proper motion of the lens is $\mu_{\rm geo} = \theta_{\rm E}/t_{\rm E} = 3.3 \pm 0.4~{\rm mas/yr}$. The lens proper motion is consistent with the estimated distance. The proper motion corrected to the heliocentric frame is ${{\bm{\mu}}}_{\rm helio} = \left[3.2\pm1.0,1.6\pm0.4\right]~{\rm mas/yr}$ (North, East). If the next class of adaptive optics systems are build, they should be able to resolve the lens and the source in ten years.

The mass of the lens is [@gould00b]: $$M = \frac{\theta_{\rm E}}{\kappa\pi_{\rm E}};~\kappa=\frac{4G}{c^2{\rm AU}}\approx8.1~\frac{\rm mas}{M_\odot}.$$ The probability distribution of the host mass is shown in Fig. \[fig:mass\] for both $u_0>0$ and $u_0<0$ solutions. The boundary mass of M/K dwarfs of $\approx0.6~M_{\odot}$ is close to the peak of distribution for $u_0>0$ solution. We conclude that the star is either K or M dwarf. The long tail of the mass distribution is caused by the fact that $\pi_{\rm E}$ is detected at only $5\sigma$ and $3\sigma$ for $u_0>0$ and $u_0<0$, respectively. The priors on the projected energy ratio did 