  The final inspiral and coalescence of a black hole binary can produce highly
beamed gravitational wave radiation. To conserve linear momentum, the black
hole remnant can recoil with "kick" velocity as high as 4000 km/s. We present
two sets of full N-body simulations of recoiling massive black holes (MBH) in
high-resolution, non-axisymmetric potentials. The host to the first set of
simulations is the main halo of the Via Lactea I simulation (Diemand et al.
2007). The nature of the resulting orbits is investigated through a numerical
model where orbits are integrated assuming an evolving, triaxial NFW potential,
and dynamical friction is calculated directly from the velocity dispersion
along the major axes of the main halo of Via Lactea I. By comparing the
triaxial case to a spherical model, we find that the wandering time spent by
the MBH is significantly increased due to the asphericity of the halo. For
kicks larger than 200 km/s, the remnant MBH does not return to the inner 200 pc
within 1 Gyr, a timescale an order of magnitude larger than the upper limit of
the estimated QSO lifetime. The second set of simulations is run using the
outcome of a high-resolution gas-rich merger (Mayer et al. 2007) as host
potential. In this case, a recoil velocity of 500 km/s cannot remove the MBH
from the nuclear region.
