Clouds themselves has greatly increased our understanding of PNe in these systems. Studying PNe in the Magellanic Clouds offers significant advantages compared to studies of the Galactic PN populations [see e.g., @Jacoby03; @Shaw06]. Chief among them is their location in systems at known distance so that large numbers of PNe can be studied in detail, and important physical parameters such as sizes and luminosities can be determined with high accuracy. The average foreground extinction to both the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) is low so that large, complete, flux-limited samples may be obtained without the severe selection biases that apply in the Galaxy. Finally both systems are among the most massive in the Local Group, so that the PN populations total hundreds of objects which enables the study of statistical properties of various sub-samples. Magellanic Cloud PNe have thus been very successfully employed over the past few decades to investigate a number of very important astrophysical questions such as the form and origin of the PN luminosity function, the effects of metallicity and environment on PN properties and the late stages of stellar evolution, and as kinematical probes of the galaxies themselves [e.g., @RP06b]. More recently, 