Nebular abundance errors

The errors inherent to the use of the standard ''ionization correction factor'' (''i(CF)'') method of calculating nebular conditions and relative abundances of H, He, N, O, Ne, S, and Ar in emission line nebulae have been investigated under conditions typical for planetary nebulae. The photoionization code CLOUDY was used to construct a series of model nebulae with properties spanning the range typical of PNe. Its radial ''profiles'' of bright, frequently observed optical emission lines were then summed over a variety of ''apertures'' to generate sets of emission Line measurements. These resulting line ratios were processed using the i(CF) method to ''derive'' nebular conditions and abundances. We find that for lines which are summed over the entire nebula the i(CF)-derived abundances differ from the input abundances by less than or equal to 25% for He and O up to less than or equal to 25% or more for Ne, S, and Ar. For resolved observations, however, the discrepancies are often much larger and are systematically variable with radius. This effect is especially pronounced in low-ionization zones where nitrogen and oxygen are neutral or once-ionized such as in FLIERs, ansae and ionization fronts. We argue that the reports of stellar-enriched N in the FLIERs of several PNe are probably specious. (C) 1997 American Astronomical Society.