well. In the objects where more than one slit position was measured, there is often a large change in the relative line strength of versus 2 emission, indicating that the emission is being produced in different regions of the nebula. In general, the 2 emission is more likely to be in the outer regions of the PNe, whereas the emission lines more closely trace the ionized regions and has similar morphology to the visible appearance. The PNe in this group all have some bipolar symmetry in their shape, most being of the “butterfly” morphology characterized by narrow equatorial regions and large bipolar lobes (e.g., M 2–9, Hb 12). However, some are classified as elliptical based on the shape of the brightest components. Tables 5 and 6 list the line identifications and extracted fluxes for the PNe in this section.

### Molecular hydrogen excitation in PNe

A near-infrared 2 emission line spectrum can occur through slow electric quadrupole vibration-rotation transitions in the ground electronic state. Because the allowed transitions are such that $T_{\rm
ex} \gtrsim 1000$ K is required to produce a detectable near-IR 2 spectrum, special excitation conditions must exist when the near-IR spectrum is present. In Paper I we 