of a much smaller size than the ionized zone.

The spectrum of NGC 1535 shown in Figure 1 was obtained at a position centered on the brightest part of the ring directly west (W) of the central star. We also fail to detect the 2 emission in the 1 line, at a 1 $\sigma$ level of about $5\times10^{-17}$ ergs cm$^{-2}$ s$^{-1}$ Å$^{-1}$. There is some indication of emission from 2 in the $v
= 1\to 0$ Q(1) and $v=1\to 0$ Q(3) lines at the long wavelength end of the spectrum. However, the spectrum is noisier in this region and there is confusion with the Pfund-series lines, therefore the 2lines are not detected above the 3 $\sigma$ level.

### NGC 2022

NGC 2022 is an early elliptical PN, but is morphologically very similar to NGC 1535 in optical images (e.g., Schwarz et al.1992). The main difference between the two is a different relative outer halo size as compared to the inner ring (the halo is relatively smaller in NGC 2022). Zhang & Kwok (1998) also find similar parameters with their morphological fits of these two PNe. Near-IR images of this PN were presented in Paper I.

NGC 2022 is also spectrally 