different regime of the AGN population. In our model C, we propose a break in the accretion rate distribution at a point corresponding to the Eddington limit and a steep power-law tail that allows for a rare population of sources with very high (super-Eddington) accretion rates. We also allow for an intrinsic scatter in the scaling between the SMBH mass and the stellar mass of the host galaxy. We find that the bright end of the XLF consists mostly of massive galaxies (${\mathcal{M}_*}\gtrsim10^{11}{\mathcal{M}_{\sun}}$) accreting close to or above their Eddington limits. This population is dominated by AGNs with SMBH masses that are elevated relative to the fiducial [${\mathcal{M}_\mathrm{bh}}$]{}–[${\mathcal{M}_*}$]{} relation, which is a result of scatter in the scaling relation and the steep decline of the SMF at high masses. @Lauer07 discussed how such a bias could affect studies of SMBH mass scaling relations using broad line AGNs outside the local universe. In fact, recent studies have found tentative evidence for strong evolution in the scaling between [${\mathcal{M}_\mathrm{bh}}$]{} and host spheroid mass (e.g. @Treu07 [@Jahnke09; @Merloni10; @Bennert11], [[although see also @Alexander08 [@Cisternas11]]{}]{}). Our model, which assumes a constant scaling and scatter in the [${\mathcal{M}_\mathrm{bh}}$]{}-[${\mathcal{M}_*}$]{} relation, may provide a simple explanation for 