distinguish between these models and thus advocated the simpler LADE model. In addition, we show the best fit LDDE parameterizations from @Ueda03, @Ebrero09, and @Silverman08.

All of the model parameterizations demonstrate the same basic evolutionary trend, namely a reduction in the number density of more luminous AGNs, which can be characterized by an overall shift of the AGN population to lower luminosities as cosmic time progresses. This luminosity evolution dominates the evolution described by the LADE parameterization of @Aird10 at these redshifts ($z<1$) and has also been quantified by pure luminosity evolution models in earlier works [e.g. @Barger05]. However, the LDDE parameterizations indicate that the shape of the XLF may be changing with redshift. Given these differences in the parameterizations of the XLF, we choose to adopt the observed, binned data points and their uncertainties when comparing with our model predictions. Outside the range of the @Aird10 data (${L_\mathrm{X}}\gtrsim10^{45}$[$\mathrm{erg\;s^{-1}}$]{}at these redshifts) we conservatively take the minimum and maximum of the 5 model parameterizations shown in Figure \[fig:xlf\] to represent current uncertainties in the XLF. This XLF estimate is shown by the light-green hatched region in subsequent plots.

An observationally motivated model to connect the AGN and galaxy populations {#sec:model}
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