simulated galaxies, we assume the non-linear relation given by the solid line: log L(FIR) = 1.1log L(TIR) – 1.42. The dashed line shows the linear relation L(FIR) = 1.91 L(TIR) assumed by Marcillac et al. (2006).[]{data-label="fig:LTIRtoFIR_Rieke"}](RIEKE_FIRvsTIR.ps){width="47.00000%"}

![The star-forming galaxy template SEDs scaled to a common far-infrared luminosity using the L(TIR)–L(FIR) scaling in Fig. \[fig:LTIRtoFIR\_Rieke\]. With increasing L(TIR), the SEDs peak at shorter wavelengths and exhibit weaker spectral features in the $\lambda <20$ region.[]{data-label="fig:RiekesameFIR"}](RIEKEtemplates_NORMsameFIR_tempex.ps){width="47.00000%"}

![Colour of the Rieke templates \[$C = \rm{log} L_{\rm{60}}/L_{\rm{100}}$\] as a function of log L(TIR)(), with the fit given by equation (2) of section 2.1.[]{data-label="fig:RiekeCOLOR"}](RIEKE_COLORvsTIR.ps){width="47.00000%"}

Radio-quiet AGN
---------------

In W08 a population of radio-quiet AGN was incorporated using the Ueda et al. (2003) hard X-ray luminosity function and a relation between 2–10 and 1.4 GHz luminosities. To assign infrared SEDs the first task is to split the population into subgroups of unobscured AGN, and Compton-thin and Compton-thick obscured AGN. This was not done in W08 but is now necessary because the infrared SEDs are sensitive to this classification. We start from the findings of Hasinger (2008), who used a compilation of hard X-ray surveys to parameterise the fraction of obscured Compton-thin AGN (as a proportion of a 