of the parameters. The exceptions are the mass ratio and parameters of the lens orbital motion. Analysis of additional data for this system should allow one to determine whether such priors provide more accurate parameters values.

The trajectory of the source relative to the caustics and lensing system is presented in Figure \[fig:traj\]. Because of the nonzero $\gamma_\perp$, the caustics and the planet are plotted for three selected moments in time.

In Figure \[fig:pred\], we present the predicted brightness variations for the best-fitting models with $u_0>0$ (gray thick line) and $u_0<0$ (dotted line). We also present four randomly chosen models with $\Delta\chi^2 = 9$ to illustrate the uncertainties in our model.

Physical properties
===================

In order to constrain the physical properties of the system one must first estimate the angular Einstein radius $\theta_{\rm E}$. We do this by standard microlensing technique [@yoo04b]. The position of the source star and the blended object on the color-magnitude diagram is presented in Figure \[fig:CMD\]. The position of the source star is consistent with bulge red clump. This figure also presents the brightness and color of the blended light. There is one star of $I$-band brightness between $19.5$ and $20.5~{\rm mag}$ every $3~{\rm arcsec^2}$ 