Abstract
ABSTRACT The authors have derived the spatial distribution of the electron temperature and density and the ionic abundances of O+, O++, N+, and S+ from CCD images of the planetary nebulae NGC 40 and NGC 6826 taken in the important emission lines of [O II], [O III], Hβ, [N II], and [S II]. Advantages of the imaging technique include complete spatial coverage and excellent spatial resolution, good light throughput, reduced effects of spatial averaging over filamented and knotted regions, elimination of the effects of atmospheric dispersion, and absolute spectrophotometry for objects having angular sizes of several arcmin. The disadvantages include additional effort to analyze the data, limited spectral coverage, and added difficulties in deblending nearby lines, removing the nebular continuum contribution, and correcting for nonphotometric conditions.
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