H\alpha}$=0.91$\pm$0.21mag. The resulting dust-corrected H$\alpha$ star formation rate for the sample is SFR$_{\rm
  H\alpha}$=16$\pm$5M$_{\odot}$yr$^{-1}$, which is consistent with that inferred from the far-infrared SEDs using stacked [*Herschel*]{} SPIRE observations(SFR$_{\rm
  FIR}$=18$\pm$8M$_{\odot}$yr$^{-1}$; @Swinbank12a)

Next, to investigate the star formation occurring within the ISM of each galaxy, we measure the star formation surface density and velocity dispersion of each pixel in the maps. Since we do not have spatially resolved reddening maps, for each galaxy we simply correct the star formation rate in each pixel using the best-fit E(B$-$V) for that system. We also remove the rotational contribution to the line width at each pixel by calculating the local $\Delta$V/$\Delta$R across the point spread function (PSF) for each pixel [@Davies11]. In Fig. \[fig:SF\_galgal\] we plot the resulting line of sight velocity dispersion ($\sigma$) as a function of star formation surface density ($\Sigma_{\rm SFR}$) for each galaxy in our sample. We see that there appears to be a correlation between $\Sigma_{\rm SFR}$ and $\sigma$, and as @Krumholz10 show, this power-law correlation may be a natural consequence of the gas and star formation surface density scaling laws. For example, first consider the Toomre stability criterion, $Q$, [@Toomre64]. $$Q\,=\,\frac{\sigma\kappa}{\pi G\Sigma_{\rm disk}}
  \label{eqn:toomre}$$ where $\sigma$ denotes the 