strong enough to warrant a full Keplerian orbital analysis. In order to use information that comes with a detection of an orbital motion, we put arbitrary priors on the ratio between projected kinetic and potential energy: $$\frac{E_{\perp,{\rm kin}}}{E_{\perp,{\rm pot}}} = \frac{({{\bm{\gamma}}}s_0 D_l\theta_{\rm E})^2}{{2GM}/{r_{\perp}}},$$ where $D_l$ is lens distance, $\theta_{\rm E}$ is the angular Einstein radius (see next Section), and $r_{\perp}$ is projected star planet separation. The priors[^2] are presented in Fig. \[fig:prior\]. The ratio ${E_{\perp,{\rm kin}}}/{E_{\perp,{\rm pot}}}$ must be smaller than unity so that the solution is bound. Values close to unity are obviously disfavored. We also disfavored small values of ${E_{\perp,{\rm kin}}}/{E_{\perp,{\rm pot}}}$ because they would correspond to the planet lying close to the lens-observer line, which should be small part of the planetary orbit. We note that for a flat distribution in logarithm of semimajor axis (Öpik’s Law) and circular orbits the distribution of projected energy ratio is $2\beta{E_{\perp,{\rm kin}}}/{E_{\perp,{\rm pot}}}$, where $\beta$ is the exponent of semimajor axis distribution. This defines our prior for small values of ${E_{\perp,{\rm kin}}}/{E_{\perp,{\rm pot}}}$. Comparison of the third and fourth columns of Table \[tab:res\] reveals that parameter estimates are consistent and the priors did not significantly affect the precision of most 