  Many young stars reside within the central half-parsec from SgrA*, the
supermassive black hole in the Galactic Center. The origin of these stars
remains a puzzle. Recently, Hansen and Milosavljevic (2003, HM) have argued
that an Intermediate-Mass Black Hole (IMBH) could have delivered the young
stars to the immediate vicinity of SgrA*. Here we focus on the final stages of
the HM scenario. Namely, we integrate numerically the orbits of stars which are
initially bound to the IMBH, but are stripped from it by the tidal field of
SgrA*. Our numerical algorithm is a symplectic integrator designed specifically
for the problem at hand; however, we have checked our results with SYMBA, a
version of the widely available SWIFT code. We find that the distribution of
the post-inspiral orbital parameters is sensitive to the eccentricity of the
inspiraling IMBH. If the IMBH is on a circular orbit, then the inclinations of
numerically computed orbits relative to the inspiral plane are almost always
smaller than 10 degrees, and therefore (a) the simulations are in good
agreement with the observed motions of stars in a clockwise-moving stellar
disc, (b) the simulations never reproduce the orbits of stars outside this
disc, which include those in the second thick ring of stars and the randomly
oriented unrelaxed orbits of some of the S-stars. If the IMBH's orbital
eccentricity is e=0.6, then approximately half of the stars end up with orbital
inclinations below 10 degrees, and another half have inclinations anywhere
between 0 and 180 degrees; this is somewhat closer to what's observed. We also
show that if IRS13 cluster is bound by an IMBH, as has been argued by Maillard
et. al. 2004, then the same IMBH could not have delivered all of the young
stars to their present location.
