of the bright ring (Figure 10). In the central position, stellar continuum is visible, rising towards shorter wavelengths. The nebular lines are similar in the central and lobe positions. The halo emission is almost devoid of lines; there is some faint  present as well as . This is possibly reflected from the bright lobes. The main component of the halo emission is a weak continuum that rises toward longer wavelengths.

### IC 2149

This peculiar PN has a bright core and a roughly bipolar nebula extending approximately E-W, but does not show the usual 2 signature of bipolar PN. The two spectra shown in Figure 11 were taken centered on the bright central star, and on the E lobe. The core spectrum shows strong stellar continuum, with the nebular lines superimposed. The E lobe emission is primarily from lines of and , in addition to weak continuum emission which is probably reflected from the central star.

### IC 3568

This round PN consists of spherical shells, an inner bright one and a outer halo. Balick et al. (1987) showed that the structure was consistent with simple hydrodynamic models of PN that are shaped by interior stellar winds. The spectrum taken 