deconvolved for the PSF). Using the velocity dispersion and star formation density of each clump, and fixing the power-law index in the Kennicutt-Schmidt relation to $n$=1.34, we compute their absolute star formation efficiencies, deriving a median $A_{\rm
  clump}$=5.4$\pm$1.5$\times$10$^{-4}$ (Fig. \[fig:KS\]). This corresponds to an offset (at fixed $n$) from the galaxy-average of $A_{\rm clump}$/$A$=1.3$\pm$0.4. Equivalently, if we fix the absolute star formation efficiency to that of the galaxy-average, then the Toomre parameter in these regions is $Q$=0.8$\pm$0.4.

  ------------------ ------------------------ ------------------------ ----------------------- ---------------
  Galaxy                       SFR             $\sigma_{\rm H\alpha}$   \[N[ii]{}\]/H$\alpha$    $r_{\rm h}$
                      (M$_{\odot}$yr$^{-1}$)        (kms$^{-1}$)                                    (kpc)
  SHiZELS-7                0.5$\pm$0.1               40$\pm$10              0.07$\pm$0.03        0.8$\pm$0.2
  SHiZELS-7                1.3$\pm$0.1               61$\pm$12              0.34$\pm$0.03        1.0$\pm$0.2
  SHiZELS-8                2.0$\pm$0.1               79$\pm$10              0.36$\pm$0.03        0.7$\pm$0.2
  SHiZELS-8                1.6$\pm$0.2               95$\pm$14              0.26$\pm$0.04        0.8$\pm$0.2
  SHiZELS-8                1.9$\pm$0.1               140$\pm$20             0.21$\pm$0.04        0.9$\pm$0.2
  SHiZELS-9                2.1$\pm$0.2               97$\pm$15              0.31$\pm$0.04        0.7$\pm$0.2
  SHiZELS-9                2.3$\pm$0.1               80$\pm$10              0.26$\pm$0.03        1.3$\pm$0.2
  SHiZELS-9                0.9$\pm$0.1               86$\pm$14              0.40$\pm$0.03          $< $0.7
  SHiZELS-14               0.5$\pm$0.1               56$\pm$12              0.12$\pm$0.04        0.9$\pm$0.2
  SHiZELS-14               1.1$\pm$0.2               121$\pm$20             0.24$\pm$0.03          $< $0.7
  SHiZELS-14               0.2$\pm$0.1               100$\pm$25           $-$0.03$\pm$0.05       0.9$\pm$0.3
  Median                   1.4$\pm$0.4                88$\pm$9              0.24$\pm$0.06       0.85$\pm$0.10
  \[table:clumps\]                                                                             
  ------------------ ------------------------ ------------------------ ----------------------- ---------------

\
Notes: Half light radius, r$_h$, is deconvolved for PSF and the velocity dispersion, $\sigma$, is corrected for local velocity gradient (see § \[sec:dynSF\]). The star formation rates (SFR) are calculated from the H$\alpha$ line luminosity using SFR$_{\rm
  H\alpha}$=4.6$\times$10$^{-42}$L$_{\rm H\alpha}$.

