Ultraviolet Observations of the Planetary Nebula NGC 2242

We present IUE observations of the high-ionization planetary nebula NGC 2242. The ultraviolet spectrum exhibits stong emission lines of C IV, He II, C III], and [Ne IV], plus weaker emission from O IV and N IV. We have also obtained narrow-band imaging of NGC 2242 in the He II 4686 A emission line; comparison of the λ 4686 flux from this image with the λ 1640 flux from the UV spectrum gives a reddening coefficient c (Hβ) = 0.37, consistent with that derived from our optical spectrum. From the UV data and previously published optical spectra, we estimate abundances for He, C, O, Ne, and Ar. The oxygen abundance is approximately one-sixth the solar value for T_e_= 25,000 K; Ne/H and Ar/H are down by a factor of two to three from typical disk PN values. C/O is probably not greater than unit. Helium is not enhanced, arguing against classification as a Type 1 PN. The observed abundance pattern in NGC 2242 resembles that seen in the halo planetary DDDM-1, except for the strikingly low C/O ratio in the latter object. We suggest that a proper-motion study be done to determine whether NGC 2242 is a member of the disk or of the halo population.