so the region of the PN being observed was well known for each spectrum. The PNe observed in this survey were chosen to overlap with the near-IR imaging survey (Paper I), along with several other optically-bright PNe and unresolved objects that were not included in the imaging survey.

Observations and Data Reduction
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The observations were performed on several runs during the period 1992 October through 1994 September at the University of Hawaii 2.2m telescope on Mauna Kea, using the near-IR KSPEC spectrograph (Hodapp et al. 1994). KSPEC is a $\lambda = 1 - 2.5$  cross-dispersed spectrograph that has a separate slit-viewing IR array for acquiring the source and guiding. The full spectral range is obtained in a single exposure, resulting in accurate relative line measurements and highly efficient data acquisition. The diffraction orders are well-matched to the atmospheric transmission windows, with the K band in 3rd order (1.9 – 2.5 ), H in 4th order (1.45 – 1.8 ) and J in 5th order (1.15 – 1.32 ), with a resolution R $\sim$ 700. The 1$\times$6 arcsecond slit provides a small aperture that was used to sample different spatial regions of the nebula to search for spectral variations.

Table 