  Gravitational waves (GWs) from the inspiral of compact remnants (CRs) into
massive black holes (MBHs) will be observable to cosmological distances. While
a CR spirals in, 2-body scattering by field stars may cause it to fall into the
MBH before reaching a short period orbit that would give an observable signal.
As a result, only CRs very near (~0.01 pc) the MBH can spiral in successfully.
In a multi-mass stellar population, the heaviest objects sink to the center,
where they are more likely to slowly spiral into the MBH without being
swallowed prematurely. We study how mass-segregation modifies the stellar
distribution and the rate of GW events. We find that the inspiral rate per
galaxy for white dwarfs is 30 per Gyr, for neutron stars 6 per Gyr, and for
stellar black holes (SBHs) 250 per Gyr. The high rate for SBHs is due to their
extremely steep density profile, n_{BH}(r)\propto r^{-2}. The GW detection rate
will be dominated by SBHs.
