static binary-lens model and run it on a wide grid of $q$, $s_0$ and $\alpha_0$ parameters (planet-host mass ratio and separation, and the source trajectory angle, respectively).[^1] The limb-darkening coefficient $u_I = 0.450$ ($\Gamma_I = 0.353$) was assumed. We try to fit models in which the source passes the lensing star on the same side as planetary caustic as well as the opposite side. Only the former ones resulted in acceptable fits. After the first well fitting models were found the microlensing parallax ($\pi_{{\rm E},N}$, $\pi_{{\rm E},E}$) and lens orbital motion ($\gamma_\parallel$, $\gamma_\perp$) were taken into account. We check models with both positive and negative values of the impact parameter $u_0$ to examine a well-known degeneracy [@smith03]. See @skowron11 for detailed description of standard microlensing parameters. The source was passing the caustic for much shorter time than the orbital period of the system, thus the lens orbital motion is approximated by two components of instantaneous velocity. The magnification is calculated using the hexadecapole approximation [@gould08; @pejcha09] except the points with the highest magnification. These are four points with ${\rm HJD'}$ in the range $6113.56501 - 6113.68359$. For them we use the “mapmaking” method [@dong06; @dong09b]. We further enhanced the mapmaking 