not significantly affect the lens mass estimate. The values of kinetic to potential projected energy ratio [@batista11] are consistent with a bound system.

The values of all the quantities presented in this section together with $M_p$, $D_L$ and $r_{\perp}$ are given in Table \[tab:phys\]. Since the positive/negative $u_0$ degeneracy is not fully removed, we present results for both solutions.

Discussion and summary
======================

We presented the microlensing detection of a super-Jupiter orbiting low-mass star. The lens mass can be used to estimate how far from the star the snow line lies. It is approximately $2.7~{\rm AU}(M/M_{\odot}) = 1.6~{\rm AU}$, which is significantly smaller than the derived projected separation of $3.8 \pm 0.6~{\rm AU}$. We note that OGLE-2012-BLG-0406Lb is the fourth super-Jupiter orbiting a low-mass star beyond the snow line discovered by the microlensing method. The existence of such objects is a challenge for the core accretion theory of planetary formation and to our knowledge has not been addressed. For a recent review on the core accretion theory see @zhou12.

Single telescope data were used to discover OGLE-2012-BLG-0406Lb, what makes this planet unique among microlensing discoveries with well characterized host lensing and planetary anomaly. We note that if the unfortunate Moon 