et al. 2002), it can be produced purely by photoionization by very hot stars or shock-heated gas (Schaerer & Stasinska 1999) and is therefore not a definitive signature of an AGN. The spectral line fits for the detected \[NeV\] lines as well as the \[OIV\] 26$\mu$m and \[NeIII\] 15.5$\mu$m lines, when detected, for each of the 7 galaxies are shown in Figure 3. We note that the spectral resolution of the SH and LH modules of the IRS is insufficient to resolve the velocity structure for most of the lines.

The optical line ratios of the galaxies with \[NeV\] detections are shown in Figure 1. As can be seen, several of the galaxies with \[NeV\] detections lie significantly to the left of the theoretical limit line from Kewley et al. (2001) indicating that there is no hint of the presence of an AGN from the optical emission lines alone. Three out of the 7 galaxies with \[NeV\] detections are classified by H97 as transition objects as can be seen in Table 1. The \[NeV\] 14.3$\mu$m or 24.3$\mu$m line was not detected in only one out of the 4 transition objects in our sample.

 IR Emission Line Morphologies
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The signal-to-noise 