\[\] and \[\] - emitting shocks cover a greater area than the cloud shocks which are bright in H$\alpha$. This is shown in Figure \[fig13\], in which we have constructed an image in H$\alpha$ (red), \[\] (green) and \[\] (blue). In this image the clouds show up as red or mauve blobs, while the \[\] emission forms diffuse halos about these clouds, and is much more extensive. In general, the \[\] emission is much more closely spatially correlated with the *Chandra X-Ray Observatory* images [@Borkowski07], an effect which is also seen in both N49 in the LMC [@Dopita16] and in the SMC SNR; 1E 0102.2-7219 [@Vogt17].

Detailed Cloud Shock Modelling {#cloudshocks}
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Cloud Shock Parameters {#cloudparms}
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From the generalised shock diagnostic diagrams, we now turn to the derivation of the shock parameters of the individual shocked ISM clouds in N132D. First, using the shock velocities estimated from both the \[\] and He II/He I diagnostic diagrams, the measured \[\] electron densities given by the \[\] $\lambda\lambda 6731/6717$ ratios, and the mean \[\] electron densities given from the model grid at the same shock velocity, we can estimate the pre-shock particle density, $n_{\mathrm{0}}$, and the ram pressure driving the shock; 