  Comparable-mass black-hole mergers generically result in moderate to highly
spinning holes, whose spacetime curvature will significantly affect nearby
matter in observable ways. We investigate how the moderate spin of a
post-merger Kerr black hole immersed in a plasma with initially uniform density
and uniform magnetic field affects potentially observable accretion rates and
energy fluxes. Varying the initial specific internal energy of the plasma over
two decades, we find very little change in steady-state mass accretion rate or
Poynting luminosity, except at the lowest internal energies, where fluxes do
not exhibit steady-state behavior during the simulation timescale. Fixing the
internal energy and varying the initial fixed magnetic-field amplitude and
orientation, we find that the steady-state Poynting luminosity depends strongly
on the initial field angle with respect to the black hole spin axis, while the
matter accretion rate is more stable until the field angle exceeds $\sim
45\degree$. The proto-jet formed along the black hole spin-axis conforms to a
thin, elongated cylinder near the hole, while aligning with the asymptotic
magnetic field at large distances.
