In Fig. \[fig:BASELINEdsc\] we show the normalised differential source counts at 24, 70 and 160 for comparison with the most recent [*Spitzer*]{} MIPS survey results. To generate these plots we used a 4 deg$^{2}$ area of the input radio simulation, coupled with a shallow subset of the full 400 deg$^{2}$ radio simulation area to generate the bright flux ends (above 1.6 at 24, 30 at 70 and 100 at 160). The simulated counts fall decisively short of the observations below 1 and 10 at 24 and 70, respectively. There is a modest excess of simulated sources above $\sim 100$ at 70 and 160, and above $\sim 10$ at 850 (Fig. \[fig:BASELINE850csc\]) where we compare with results from the [*SCUBA*]{} Half Degree Extragalactic Survey (SHADES; Coppin et al. 2006).

Since the source counts are dominated by star-forming galaxies, we show in Fig. \[fig:BASELINEqparams\] the quantity $q_{\rm{IR}} = log (F_{\rm{IR}}/F_{\rm{20 cm}})$ in the 24 and 70 bands for the simulated normal galaxy population. $F_{\rm{IR}}$ and $F_{\rm{20 cm}}$ are the simulated infrared and radio fluxes which would be observed in these bands, i.e. without the application of any K-corrections. The simulated sample is dominated by galaxies substantially fainter than those in current observational 