high resolution imaging and spectroscopy have been employed to study the coevolotion of individual nebulae [@Shaw_etal01; @Stang_etal02; @Stang_etal03; @Shaw_etal06] and their central stars [@Villa03; @Villa04; @Villa07].

Observing PNe in the Magellanic Clouds is not without its challenges, however. The fields are extremely crowded, the individual nebulae cannot be resolved in useful detail except with [*HST*]{} or advanced optical systems on large, ground-based telescopes, and the LMC in particular is permeated with very bright, spatially complex nebular emission from a variety of sources including regions, supernova remnants, and wind-blown nebulae around O-stars. In addition, the Magellanic Clouds extend over a wide area of sky. These issues complicate the task of conducting uniform, deep surveys for PNe over the full spatial extent of these galaxies. The heterogeneity of prior surveys in the spatial coverage, depth, discovery technique, and the lack of complete follow-up spectroscopy for verifying the classification have been the principal barriers to realizing the full potential of Magellanic Cloud PN studies until recently.

Recent surveys with wider areal coverage, uniform depth, and greatly increased sensitivity have been published by @JD02 for the SMC and by @RP06a [@RP06b] for the LMC; another in the LMC is underway [@Smith99]. See [@Jacoby03] and 