  Perturber objects interacting with supermassive black hole accretion disks
are often invoked to explain observed quasi-periodic behavior in active
galactic nuclei (AGN). We present global, 3D general relativistic
magnetohydrodynamic (GRMHD) simulations of black holes on inclined orbits
colliding with magnetically arrested thick AGN disks using a binary black hole
spacetime with mass ratio $0.1$. We do this by implementing an approximate
time-dependent binary black hole metric into the GRMHD code Athena++. The
secondary enhances the unbound mass outflow rate 2-4 times above that provided
by the disk in quasi-periodic outbursts, eventually merging into a more
continuous outflow at larger distances. We present a simple analytic model that
qualitatively agrees well with this result and can be used to extrapolate to
unexplored regions of parameter space. We show self-consistently for the first
time that spin-orbit coupling between the primary black hole spin and the
binary orbital angular momentum causes the accretion disk and jet directions to
precess significantly (by 60$^\circ$-80$^\circ$) on long time-scales (e.g.,
$\sim$ 20 times the binary orbital period). Because this effect may be the only
way for thick AGN disks to consistently precess, it could provide strong
evidence of a secondary black hole companion if observed in such a system.
Besides this new phenomenology, the time-average properties of the disk and
accretion rates onto the primary are only marginally altered by the presence of
the secondary, consistent with our estimate for a perturbed thick disk. This
situation might drastically change in cooled thin disks.
