$\sim5$ times higher than in the surrounding X-ray plasma. The reason for this difference is discussed in Section \[conc\], below. ]{}

The mean pre-shock density inferred for these clouds is surprisingly high; $\left<n_{\mathrm{0}} \right> = 243$cm$^{-3}$ (excluding P08, P09 and P20). However, the pressure in the ISM of the LMC has been estimated using the excited CI emission along a number of sight lines by @Welty16. This analysis gave $\left<\log P/k \right> =4.02$ cm$^{-3}$K. If the N132D clouds were characterised by the same ISM pressure before they were engulfed by the supernova shock wave (which is not at all a certain assumption), then their equilibrium temperature would have been $\sim 40$K, and they can be therefore considered to be part of the cold neutral medium phase of the ISM.

Chemical Abundances & Depletion Factors
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We selected the four brightest clouds; P12, P14, P15 and P18 for detailed study, with the aim of deriving more precise shock parameters, and to derive the chemical abundances of the elements in the ISM of the LMC through high-precision shock modelling.

In order to measure the goodness of fit of any particular model, we measure the degree to which it reproduces the density-sensitive \[SII\] 