FWHM, and the amount of flux falling outside of the slit was then calculated. This was typically 20 – 30% of the total light for a single integration. The calibration for each star was corrected by this factor, along with corrections for airmass. Comparing results from different standard stars taken throughout the night indicated that this method is accurate to approximately 20%. For the observations of the PNe, no correction was applied for the slit width or length. The length along the slit of the extracted regions for the three bands were 20 (J), 35 (H), and 40 (K).

Results 
========

The spectra are presented in Figures 1 – 32. One to three PNe spectra are plotted in each figure. Tables 2 through 7 list the line identifications and extracted fluxes with uncertainties for the spectra shown in the Figures. The PN in this section are listed in Tables 2, 3, and 4. There are a number of features not identified (indicated by question marks in the tables). These features tend to appear above the $\sim3\sigma$ level and must be considered real, though confirming spectra would be valuable. Our search for possible identifications for these lines has been careful, but 