  Quasar absorption spectra measurements suggest that reionization proceeded
rapidly, ended late at $z \sim 5.5$, and was followed by a flat evolution of
the ionizing background. Simulations that can reproduce this behavior often
rely on a fine-tuned galaxy ionizing emissivity, which peaks at $z \sim 6 - 7$
and drops by a factor of $1.5-2.5$ by $z \sim 5$. This is puzzling since the
abundance of galaxies has been observed to grow monotonically during this
period. Explanations for this include effects such as dust obscuration of
ionizing photon escape and feedback due to photo-heating of the IGM. We explore
the possibility that this drop in emissivity is instead an artifact of one or
more modeling deficiencies in reionization simulations. These include possibly
incorrect assumptions about the ionizing spectrum and/or inaccurate modeling of
the clumpiness of the IGM. Our results suggest that the need for a drop could
be alleviated if simulations are underestimating the IGM opacity from massive,
star-forming halos. Other potential modeling issues either have a small effect
or require a steeper drop when remedied. We construct an illustrative model in
which the emissivity is nearly flat at the end of reionization, evolving only
$\sim 0.05$ dex at $5 < z < 7$. More realistic scenarios, however, require a
$\sim 0.1-0.3$ dex drop. We also study the evolution of the Ly$\alpha$
effective optical depth distribution in these scenarios and compare them to
recent measurements. We find models that feature a hard ionizing spectrum
and/or are driven by faint, low-bias sources can most easily reproduce the mean
transmission and optical depth distribution of the forest simultaneously.
Lastly, we show that the reduced speed of light approximation and low spatial
resolution in the forest can lead to erroneous conclusions about the end of
reionization.
