of the data severely hampers any detailed study of the spatial distribution of the \[NeV\] emission in this galaxy (see Section 5.1 for details). We discuss each galaxy individually in Section 5.1.

 Line Flux Ratios and Luminosities
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Since the ratio of high to low excitation lines depends on the nature of the ionizing source, the \[NeV\]14$\mu$m/\[NeII\]12.8$\mu$m and the \[OIV\]25.9$\mu$m/\[NeII\]12.8$\mu$m line flux ratios have been used to characterize the nature of the dominant ionizing source in galaxies (Genzel et al. 1998; Sturm et al. 2002; Satyapal et al. 2004; Dale et al. 2006). Table 4 lists the \[NeV\]/\[NeII\], \[NeV\]/\[NeIII\], and \[OIV\]/\[NeII\] line flux ratios and the \[NeV\] 14.3$\mu$m line luminosities for the 7 galaxies in which either \[NeV\] line is detected. In NGC 3938 and NGC 4414 the \[NeV\] 14.3$\mu$m line was not detected. In this case, we estimated and use in Table 4 the 14.3$\mu$m line luminosity using the \[NeV\] 24.3$\mu$m line luminosity. The \[NeV\] 14.3$\mu$m and 24.3$\mu$m line luminosities are tightly correlated in a large sample of standard optically-identified AGN recently observed by [*Spitzer*]{} (Dudik et al. 2007) as can be seen in Figure 5. Employing a Spearman rank correlation analysis (Kendall & Stuart 1976) yields a correlation 