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 .