of the observations was insufficient to provide detailed spatial information on the \[NeV\] emission for all 4 of the AGN candidates with mapping observations. However, we show in Figure 4, the detected \[OIV\] 26$\mu$m and \[NeIII\] 15.5$\mu$m images for 3 out of the 4 galaxies with \[NeV\] detections. The signal-to-noise ratio corresponding to both the \[OIV\] and the \[NeIII\] for NGC3968 precluded any analysis of the spatial distribution of the emission in this galaxy. This galaxy is therefore excluded from Figure 4. The ionization potential of OIV and NeIII are 55 eV and 41 eV, respectively. Both species can be produced in gas ionized by hot stars. However in all cases, centrally compact emission is observed, suggestive of an AGN origin.. Although we do not know the spatial morphology of the \[NeV\] emission, it is likely to be similar to the centrally concentrated \[OIV\] and \[NeIII\] emission shown below. We note that there is possibly one anomalous galaxy in our sample of detections. The peak of the \[NeV\] emission in NGC 4536 appears to be offset from the peak of the \[OIV\] and \[NeIII\] emission which both peak at the optical and [*2MASS*]{} nucleus. However, the signal to noise ratio 