procedure by calculating point source magnifications for all the images that are outside the map. This allows us to make the map smaller and for calculations to be more accurate. The map is placed around the planet because it caused the anomaly and has the radius of $\theta_{\rm E}q^{1/2}$. Mapmaking implicitly assumes $\gamma_\parallel = (ds/dt)/s_0 = 0$; thus, we constructed the map at ${\rm HJD'} = 6113.5846$. We have checked that ignoring $ds/dt$ during the $0.12~{\rm d}$ time interval affects the calculated magnifications at a level that is much smaller than the photometric errors.

The parameters of the best-fitting models are presented in Table \[tab:res\]. The quantity $\rho$ is the source source size relative to Einstein ring radius and $f_b/f_s$ denotes blend to source flux ratio. The model with both the binary motion and the microlensing parallax gives the smallest $\chi^2$. It has $u_0>0$ and the solution with $u_0<0$ is worse by $\Delta\chi^2=13.6$. We report parameters of both models. The positive/negative $u_0$ ambiguity is not fully removed; thus, we present analysis of both cases. For the best-fitting model without lens orbital motion as well as the one without parallax, we present the $u_0>0$ solution only, consistently with the lowest $\chi^2$ 