Same as Figure 6, but for the Eddington ratio function. Unlike for the BHMF, there is a more significant difference in the BHERFs derived under the two models for the virial mass estimate errors. In all cases the uncertainties on the BHERF are larger for the mode that includes a luminosity-dependent bias. In addition, the BHERF under the model with β ≠ 0 is shifted toward higher values L/ L _Edd. This shift is small in the redshift bins using Hβ, but increases to ≈0.5 dex for the redshift bins using Mg ii and C iv.