Recent stellar population and chemical abundance studies point to an accreted origin of \omega Cen .
In this light , and given the retrograde , small size orbit of \omega Cen , we search for a kinematical signature left by its hypothetical parent galaxy in the Solar neighborhood .
We analyze the largest-to-date sample of metal poor stars ( Beers et al . 2000 ) and we find that , in the metallicity range -2.0 < [ Fe/H ] \leq - 1.5 , a retrograde signature that departs from the characteristics of the inner halo , and that resembles \omega Cen ’ s orbit , can be identified .