coefficient of r$_{\rm S}$ = 0.97 between the \[NeV\] 14.3$\mu$m and 24.3$\mu$m line luminosities, with a probability of chance correlation of 6.7 $\times$ 10$^{-12}$, indicating a significant correlation. This relation implies similar densities to the \[NeV\]-emitting gas in the galaxies in the sample. The best-fit linear relation yields: $$\log(L_{\rm [NeV]14}) =  (0.995)\log(L_{\rm [NeV]24}) + 0.0566$$

with an rms scatter of 0.219 dex. We note that equation (1) is consistent with the relationship between the \[NeV\] 14.3$\mu$m and 24.3$\mu$m line luminosities in standard AGN observed by [*ISO*]{} (Sturm et al. 2002), as well as NGC 3367, the one galaxy in our current sample in which both lines were detected. The \[NeV\]/\[NeII\] line flux ratio for the 13 AGN with both \[NeV\] and \[NeII\] detections by the [*Infrared Space Observatory (ISO)*]{} ranges from 0.06 to 2.11, with a median value of 0.47 (Sturm et al. 2002). \[NeV\]/\[NeII\] ratios for our 7 galaxies range from approximately 0.01 to 0.27, with most falling below the lowest value observed in standard AGN by ISO. The \[OIV\]/\[NeII\] line flux ratio for the 17 [*ISO*]{} AGN with both lines detected ranges from 0.15 to 8.33, with a median value of 1.73 (Sturm et al. 2002). The \[OIV\]/\[NeII\] 