with its major axis in the N-S direction, and a bright ring structure closer to the central star (Paper I). The near-IR spectrum from 0.77 to 1.33  was measured by Rudy et al. (1991), and the UV and optical spectrum was recently obtained by Hyung, Aller, & Feibelman (1994), who found evidence of variability.

Figure 5 shows two slit positions on the PN, one on the nebula center, and one on the brightest location in the E lobe of the PN. Both the core and E lobe spectra show a strong contribution from stellar continuum flux. There is strong and line emission, and relatively strong unidentified line emission at 2.199 and 2.286 .

### NGC 6790

This PN has been shown by radio continuum observations to be an elliptically-shaped nebula with a diameter of roughly an arcsecond (Aaquist & Kwok 1990). Aller, Hyung, & Feibelman (1996) obtained UV and optical spectra and suggest that NGC 6790 is a relatively young object, slightly more evolved than Hb 12. Kelly & Latter (1995) obtained a 0.9 – 1.3  spectrum and find similarities to Hb 12 and AFGL 618.

The spectrum of NGC 6790 in Figure 4 shows a stellar contribution because the 