  The relativistically-broadened reflection spectrum, observed in both AGN and
X-ray binaries, has proven to be a powerful probe of the properties of black
holes and the environments in which they reside. Being emitted from the
inner-most regions of the accretion disk, this X-ray spectral component carries
with it information not only about the plasma that resides in these extreme
conditions, but also the black hole spin, a marker of the formation and
accretion history of these objects. The models currently used to interpret the
reflection spectrum are often simplistic, however, approximating the disk as an
infinitely thin, optically thick plane of material orbiting in circular
Keplerian orbits around the central object. Using a new relativistic ray
tracing suite (Fenrir) that allows for more complex disk approximations, we
examine the effects that disk thickness may have on the reflection spectrum.
Assuming a lamp post corona, we find that finite disk thickness can have a
variety of effects on the reflection spectrum, including a truncation of the
blue wing (from self-shadowing of the accretion disk) and an enhancement of the
red wing (from the irradiation of the central 'eye wall' of the inner disk). We
make a first estimate on the systematic errors on black hole spin and height
that may result from neglecting these effects.
