(Latter et al. 1995; hereafter Paper I) presented an infrared imaging survey; here we present the results of a near-infrared spectral survey.

There are several reasons why knowledge of the near-infrared (near-IR) characteristics of PNe is important, as described in Paper I. In order to interpret the imaging results and to learn more about the physical conditions in the nebulae, the spectra of these objects must be examined to understand the processes responsible for the emission. There are many emission lines present in the 1 – 2.5  spectral region, most notably those due to recombination lines of , and lines of vibrationally excited 2. Also present are atomic lines of and \[\], and emission from other molecular species such as CO and C$_2$. These lines can act as diagnostic tools to probe the physical conditions inside the nebula, sampling different regions and ranges of temperature, density, and excitation than is seen by observing the optical line emission. Some PNe also exhibit in the near-IR strong continuum emission from hot dust. This emission becomes significant longward of $\lambda = 2$  in many of the PNe, requiring near-IR spectroscopy to detect it and to differentiate between line and continuum emission sources. Finally, 