  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 C(H-beta) = 0.27 from hydrogen recombination lines and the
radio to H-beta 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.
