@Veilleux87 diagnostic diagrams. The depletion factors of the heavy elements caused by the condensation of these elements onto dust are defined as the ratio of the gas phase abundance to the total element abundance. The depletion factors are derived from the formulae of @Jenkins09, extended to the other elements on the basis of their condensation temperatures and/or their position on the periodic table. In these shock models, following @Dopita16 we have investigated the effect of changing the logarithmic Fe depletion, $\log D_{\rm Fe}$ in the range $0.0 > \log \left [ D_{\rm Fe} \right ] > -1.0$.

The abundance set adopted for the theoretical grid at the various values of $\log D_{\rm Fe}$ is given in Table \[table2\]. The abundances of C, Mg, and Si are not constrained by our observations and for these we fix the abundances at half of the LGC values. We produce a more refined estimate of the LMC chemical abundances when we build detailed models for the brightest clouds, below.

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The line intensities and line ratios given in this paper comprise the sum of the radiative shock and its photoionised precursor. In the case of the fastest shock, the extent of the photoionised precursor 