populates galaxies with accreting SMBHs must be consistent with this observational constraint on the total population. In this paper we compare our model to measurements of the 2–10 keV X-ray luminosity function (XLF) of AGNs at $0.2<z<1.0$.

In Figure \[fig:xlf\] we show binned estimates of the XLF from @Aird10, recalculated in the redshift bins used for this study (black points with error bars). This work applied a sophisticated Bayesian methodology to account for uncertainties in photometric redshifts and X-ray flux estimates, track the X-ray sensitivity, correct for Eddington bias, and correct for incomplete optical identifications. The binned estimates shown in Figure \[fig:xlf\] are calculated using the $N_\mathrm{obs}/N_\mathrm{mdl}$ method [@Miyaji01], which corrects for the effects of the X-ray sensitivity over the width of the bin. Error bars represent $1\sigma$ equivalent Poissonian errors for the number of objects in a bin. We also show a number of best-fit parametric models, including both the luminosity-dependent density evolution (LDDE) model determined by @Aird10 (cyan dashed line) and the conceptually simpler Luminosity And Density Evolution (LADE) model where the XLF evolves in both luminosity and density but retains the same shape at all redshifts (green line). @Aird10 concluded that it was not possible to statistically 