& $<$0.23 & $<$0.58 & 1.3$\pm$0.2\
NGC6946 & $<$1.5 & $<$0.39 & $<$12.07\
IC342 & $<$1.7 & $<$15.88 & $<$23.37\
\

[ Col(1): Common Source Names; Col(2) & (3) & (4): Fluxes are in units of 10$^{-21}$ W cm$^{-2}$. 3 $\sigma$ upper limits are reported for nondetections.]{}

All of the staring observations were centered on the nucleus of the galaxy as requested, and generally correspond to the [*2MASS*]{} nuclear coordinates.. We note that the SH and LH staring observations include data from two slit positions overlapping by one third of a slit. Because the slits occupy distinctly different regions of the sky, the flux from the slits cannot be averaged unless the emission originates from a compact source that is contained entirely in each slit. Therefore, the procedure for flux extraction for staring observations was the following: 1) If the fluxes measured from the two slits differed by no more than the calibration error of the instrument, then the fluxes were averaged; otherwise, the slit with the highest measured line flux was chosen. 2) If an emission line was detected in one slit, but not in the other, then the detection was selected. The slit for the SH and LH 