with luminosities of L$_{\rm H\alpha}\sim $10$^{41.4-42.4}$ergs$^{-1}$. Fitting the H$\alpha$ and \[N[ii]{}\]$\lambda\lambda$6548,6583 emission lines pixel-by-pixel using a $\chi^{2}$ minimisation procedure we construct intensity, velocity and velocity dispersion maps of our sample and show these in Fig. \[fig:2dmaps\] (see also @Swinbank12a for details).

Analysis & Discussion
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Galaxy Dynamics and Star Formation {#sec:dynSF}
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As @Swinbank12a demonstrate, the ratio of dynamical-to-dispersion support for this sample is $v$sin($i$)/$\sigma$=0.3–3, with a median of 1.1$\pm$0.3, which is consistent with similar measurements for both AO and non-AO studies of star-forming galaxies at this epoch [e.g.  @ForsterSchreiber09]. The velocity fields and low kinemetry values of the SHiZELS galaxies (total velocity asymmetry, K$_{\rm tot}$=0.2–0.5) also suggest that at least six galaxies (SHiZELS 1, 7, 8, 9, 10, & 11) have dynamics consistent with large, rotating disks, although all display small-scale deviations from the best-fit dynamical model, with $<$data$-$model$>$=30$\pm$10kms$^{-1}$, with a range from $<$data$-$model$>$=15–70kms$^{-1}$ [@Swinbank12a].

We also use the multi-wavelength imaging to calculate the rest-frame SEDs of the galaxies in our sample and so derive the stellar mass, reddenning and estimates of the star-formation history [@Sobral11]. From the broad-band SEDs (Fig. 1 of @Swinbank12a), the average E(B$-$V) for our sample is E(B$-$V)=0.28$\pm$0.10 which corresponds to A$_v$=1.11$\pm$0.27mag and indicates A$_{\rm
  