respectively. The asterisks and thick lines show the measured counts and uncertainty region for the SCUBA Half-Degree Extragalactic Survey (Coppin et al. 2006).[]{data-label="fig:BASELINE850csc"}](850micronCUMSC_AUG1_2010FINAL.ps){width="47.00000%"}

![The quantity $q_{\rm{IR}} = log (F_{\rm{IR}}/F_{\rm{20 cm}})$ is used to characterise the far-infrared:radio correlation for star-forming galaxies and is plotted here for the entire population of simulated normal galaxies (black dots) at 24 and 70, using the baseline model of section 2. The red crosses and diamonds are the sources remaining after the application of infrared and radio flux cuts to mimic the selection of Appleton et al. (2004) and Seymour et al. (2009), respectively. []{data-label="fig:BASELINEqparams"}](q24_Rieketemplates_NG_AUG1_plusOBS_tempex.ps "fig:"){width="47.00000%"} ![The quantity $q_{\rm{IR}} = log (F_{\rm{IR}}/F_{\rm{20 cm}})$ is used to characterise the far-infrared:radio correlation for star-forming galaxies and is plotted here for the entire population of simulated normal galaxies (black dots) at 24 and 70, using the baseline model of section 2. The red crosses and diamonds are the sources remaining after the application of infrared and radio flux cuts to mimic the selection of Appleton et al. (2004) and Seymour et al. (2009), respectively. []{data-label="fig:BASELINEqparams"}](q70_Rieketemplates_NG_AUG1_plusOBS.ps "fig:"){width="47.00000%"}

REVISIONS TO THE BASELINE MODEL
===============================

We now adapt the baseline model to provide a better match to the existing infrared source count 