and \[\]$\lambda 4881$/H$\beta$ line ratios. This is shown in Figure \[fig9\]. The two lines agree less well with each other, the \[\]$\lambda 4881$/H$\beta$ ratio tending to produce a larger depletion factor. In each line ratio, a much wider range of depletion factors is observed, from -0.25 to $\sim -1.25$. Averaging all measurements, we obtain $\left < \log D_{\rm Fe} \right > = -0.74\pm0.25$. This result is also broadly consistent with what was derived in the case of N49; $\left < \log D_{\rm Fe} \right > = -0.956\pm0.15$ [@Dopita16].

Finally, the analysis for \[\]$\lambda 6087$/H$\alpha$ is shown in Figure \[fig10\]. Note that this line requires shock velocities of $v_s > 180$km/s in order to be produced with appreciable strength in the radiative shock. Here, the inferred depletion factors range from -0.0 to $\sim -0.75$ with $\left < \log D_{\rm Fe} \right > = -0.4$.

Given the intrinsic uncertainties in the atomic data for the forbidden lines of Fe, we can conclude that the \[\] and the \[\] lines imply a mean depletion factor of order $\left < \log D_{\rm Fe} \right > = -0.6\pm0.25$, while the \[\] lines give a depletion factor $\left < \log D_{\rm Fe} \right > = -0.15\pm0.15$. 