in the range $160$km/s$ < v_s < 300$km/s. Thus it is clear that the relatively strong \[\] and \[\] lines observed must arise in another region with higher shock velocity.

This is not unexpected, given the appearance of the clouds on the HST images, which often show a bright core in H$\alpha$, surrounded by fainter filamentary structures. We can identify these regions with the bright radiative shocks being driven into the denser cores of these clouds, and a faster, but only partially-radiative shock driven by a similar external ram-pressure sweeping through the less dense outer regions of the same clouds. Indeed in the case of another SNR in the LMC; N49, both the spatial and dynamical distinction between the \[\]${\lambda 5303}$ and the \[\]${\lambda 5159}$ emission are very marked [cf. Fig.3 in @Dopita16].

The detailed diagnostic diagrams for these two Fe species are shown in Figure \[fig12\]. For the standard grid, both fail to reproduce the observed strength of the lines, but the \[\] is particularly bad. Introducing a partially-radiative shock leads to a dramatic improvement. The derivation of the plausible shock parameters [ for these shocks]{} is as follows.

First, we note that the mean cloud shock ram pressure 