Infrared Spectrum and Abundances of the Planetary Nebula Ic 2448

We present the mid-infrared spectrum of the planetary nebula IC 2448. In order to determine the chemical composition of the nebula, we use the infrared line fluxes from the Spitzer spectrum along with optical line fluxes from the literature and ultraviolet line fluxes from archival IUE spectra. We determine an extinction of CHβ = 0.27 from hydrogen recombination lines and the radio to Hβ ratio. Forbidden line ratios give an electron density of 1860 cm−3 and an average electron temperature of 12700 K. The use of infrared lines allows us to determine more accurate abundances than previously possible because abundances derived from infrared lines do not vary greatly with the adopted electron temperature and extinction, and additional ionization stages are observed. Elements left mostly unchanged by stellar evolution (Ar, Ne, S, and O) all have subsolar values in IC 2448, indicating that the progenitor star formed out of moderately metal deficient material. Evidence from the Spitzer spectrum of IC 2448 supports previous claims that IC 2448 is an old nebula formed from a low mass progenitor star. Subject headings: abundances — infrared: general — ISM: lines and bands — planetary nebulae: individual (IC 2448) — stars: AGB and post-AGB