samples, but our $q_{\rm{24}}$ and $q_{\rm{70}}$ values compare reasonably well with those measured locally (Appleton et al. 2004, Beswick et al. 2008 and Garn et al. 2009a,b). For a better comparison with the observations, we applied cuts in flux density to yield the sub-samples also shown in Fig. \[fig:BASELINEqparams\]: at 24, we selected galaxies with $F_{\rm{24}} > 0.3$ and $F_{\rm{20 cm}} > 90$ to mimic the selection of Appleton et al. (2004), but we note that these authors only included sources with spectroscopic redshifts and appear not to discriminate between star-forming galaxies and AGN, biases which we cannot easily accommodate. At 70, we apply cuts of $F_{\rm{70}} > 6$ and $F_{\rm{20 cm}} > 30$ to match the selection of Seymour et al. (2009), who use photometric and spectroscopic redshifts and apply star-forming galaxy/AGN classification. The resulting sample shows only a very modest decline in $q_{\rm{70}}$ out to $z=2$, consistent with the findings of Seymour et al.

![image](24micDSC_RIEKEtemps_AUG1_2010FINAL.ps){width="47.00000%"} ![image](70micDSC_RIEKEtemp_AUG1_2010FINAL.ps){width="47.00000%"} ![image](160micDSC_RIEKEtemp_AUG1_2010FINAL.ps){width="47.00000%"}

![The thin continuous line shows the simulated integral source counts at 850 for the baseline model using a 4 deg$^{2}$ region of the input radio simulation; the contributions of normal and starburst galaxies are shown by the dashed and dot-dashed lines, 