  We present the results of three body simulations focused on understanding the
fates of intermediate mass black holes (IBH) that drift within the central 0.5
pc of the Galaxy. In particular, we modeled the interactions between pairs of
$4000 {\rm M}_{\odot}$ black holes as they orbit a central blac k hole of mass
$4 \times 10^6 {\rm M}_{\odot}$. The simulations performed assume a
Schwarzschild geometry and account for Chandrasekhar dynamical friction as well
as acceleration resulting from energy lost due to gravitational radiation.
  We found the branching ratio for one of the orbiting IBHs to merge with the
CBH was 0.95 and is independent of the inner IBH's initial eccentricity as well
as the rate of sinking. This, coupled with an infall rate of $\sim 10^7 $ yrs
for an IBH to drift into the Galactic center, results in an IBH-CBH merger
every $\lesssim 11$ Myrs. Lastly we found that the IBH-IBH-CBH triple body
system ``resets'' itself, in the sense that a system with an inner I BH with an
initially circular orbit generally left behind an IBH with a large
eccentricity, whereas a system in which the inner IBH had a high eccentricity
($e_0 \sim 0.9$) usually left a remnant with low eccentricity. Branching ratios
for different outcomes are also similar in the two cases.
