the parameters $Y=30$, $q=1$, $\sigma = 45$ deg, $m=2$, $i=30$ deg, $\tau_{\rm{V}}=30-60$ and $N_{\rm{0}} \leq 6$ (see Nenkova et al. 2008 for the meaning of these parameters). 18 CLUMPY models satisfy these constraints and were assigned at random to our type I Seyferts, with the SED consisting of the reprocessed torus emission and direct AGN broken power-law emission (defined as a power-law $F_{\rm{\lambda}} \propto \lambda^{-1.5}$ over 0.1–1 with a Rayleigh-Jeans slope at longer wavelengths).

For the type II Compton-thin AGN, we assigned one of the type 2 QSO templates given by Polletta et al. (2006) and Polletta et al. (2007) (termed QSO2 and Torus, respectively) for the quasars, and one of the aforementioned CLUMPY models (but without the direct AGN emission component) to the Seyferts.

For the Compton-thick AGN, we assigned half the population SEDs using the same prescription as for the type II Compton-thin sources; for the other half of the population, we reflect the growing body of evidence which suggests that a large proportion of Compton-thick AGN are obscured by an extended distribution of cold dust in the host galaxy and not by a nuclear torus (see e.g. Polletta et al., 2006, 2008; Martinez-Sansigre et al. 2006, Lacy 