are flagged for removal because W08 included radio-loud AGN with a separate radio luminosity function but this population is also implicitly present in the Ueda et al. luminosity function. The fractions of retained radio-quiet AGN which are unobscured, Compton-thin and Compton-thick obscured are shown as functions of $L_{\rm{X}}$ and redshift in Fig. \[fig:RQAGNfrac\].

![image](RQAGN_hist1_2deg.ps){width="35.00000%"} ![image](RQAGN_hist2_2deg.ps){width="35.00000%"} ![image](RQAGN_hist3_2deg.ps){width="35.00000%"} ![image](RQAGN_hist4_2deg.ps){width="35.00000%"}

### AGN emission

For the retained sources, $L_{\rm{X}}$ is inferred from the radio luminosity using equation (2) of W08. Sources with $L_{\rm{X}}$ above and below a threshold of $3 \times 10^{44}$ are classified as quasars and Seyferts, respectively. Unobscured (type I) quasars are assigned at random one of the three templates for optically-selected QSOs compiled by Polletta et al. (2007) (termed QSO1, BQSO1 and TQSO1, which differ in their relative optical/infrared flux ratios)[^3]. The unobscured Seyferts are assigned SEDs from the online library of models computed by Nenkova et al. (2008) using the [*CLUMPY*]{} code for dust radiative transfer in a clumpy AGN torus. To narrow down the parameter space of available models, we use the results of Thompson et al. (2009) which are based on analysis of Seyfert 1 AGN mid-infrared spectra. They prefer a range of [*CLUMPY*]{} parameter space defined by 