other surveys [@Tacconi10; @Daddi10; @Swinbank11].

Finally, with estimates of the disk surface density, we can use Eq. \[eqn:toomre\] to construct maps of the spatially resolved Toomre parameter, $Q(x,y)$. Since we set $Q$=1 to derive the coefficients $n$ and $A$, by construction the average $Q$ across the population is unity, but the relative range of $Q(x,y)$ within the ISM of each galaxy is unaffected by this assumption. In Fig. \[fig:2dmaps\] we show the maps of $Q(x,y)$ for each galaxy in our sample (with contours marking $Q(x,y)$=0.5, 1.0 and 2.0). This shows that there is a range of Toomre $Q$ across the ISM, and to highlight the variation with radius, in Fig. \[fig:Q\_r\] we show the Toomre parameter within each pixel of each galaxy as a function of radius (normalised to the half light radius, $r_{\rm h}$). This shows that in the central regions, on average the Toomre $Q$ increases by a factor $\sim $4$\times$ compared to $Q$ at the half light radius, whilst a radii greater than $r_{\rm h}$, $Q$ decreases by approximately the same factor.

### Identification of Star-Forming Regions {#sec:SFregions}

As Fig. \[fig:2dmaps\] shows, the galaxies in our sample exhibit a range of H$\alpha$ morphologies, from compact (e.g. SHiZELS11 