& 12) to very extended/clumpy (e.g. SHiZELS7, 8, 9 & 14). To identify star-forming regions on $\sim $kpc scales and measure their basic properties we isolate the star-forming clumps above the background ($\sigma_{\rm bg}$) by first converting the H$\alpha$ flux map into photon counts (accounting for telescope efficiency) and then search for 3$\sigma_{\rm bg}$ over-densities above the radially averaged background light distribution. In this calculation, we demand that any region is at least as large as the PSF. We identify eleven such regions and highlight these in Fig. \[fig:2dmaps\].

It is still possible that selecting star-forming regions in this way may give misleading results due to random associations and signal-to-noise effects. We therefore use the H$\alpha$ surface brightness distribution from the galaxies and randomly generate $10^5$ mock images to test how many times a “clump” is identified. We find that only 2$\pm$1 spurious clumps (in our sample of eleven galaxies) could be random associations.

Next, we extract the velocity dispersion and luminosity of each clump from the using an isophote defining the star-forming region and report their values in Table 2 (the clump velocity dispersions have been corrected for the local velocity gradient from the galaxy dynamics and sizes are 