Recoiling supermassive black holes in analytical and numerical galaxy
  potential
  We follow trajectories of recoiling supermassive black holes (SMBHs) in
analytical and numerical models of galaxy merger remnants with masses of
$10^{11} \rm{M_{sun}}$ and $10^{12} \rm{M_{sun}}$. We construct various merger
remnant galaxies in order to investigate how the central SMBH mass and the mass
ratio of progenitor galaxies influence escape velocities of recoiling SMBHs.
Our results show that static analytical models of major merger remnant galaxies
overestimate the SMBHs escape velocities. During major mergers violent
relaxation leads to the decrease of galaxy mass and lower potential at large
remnant radii. This process is not depicted in static analytical potential but
clearly seen in our numerical models. Thus, the evolving numerical model is a
more realistic description of dynamical processes in galaxies with merging
SMBHs. We find that SMBH escape velocities in numerical major merger remnant
galaxies can be up to 25 per cent lower compared to those in analytical models.
Consequently, SMBHs in numerical models generally reach greater galactocentric
distances and spend more time on bound orbits outside of the galactic nuclei.
Thus, numerical models predict a greater number of spatially-offset active
galactic nuclei (AGNs).
