  A revival over the past two decades in planetary nebula (PN) morphological
studies springs from a combination of factors, including the advent of
wide-area, high dynamic range detectors; the growing archives of high
resolution images from the X-ray to the sub-mm; and the advent of sophisticated
models of the co-evolution of PNe and their central stars. Yet the story of PN
formation from their immediate precursors, the AGB stars, is not yet fully
written. PN morphology continues to inspire, provide context for physical
interpretation, and serve as an ultimate standard of comparison for many
investigations in this area of astrophysics. After a brief review of the
remarkable successes of PN morphology, I summarize how this tool has been
employed over the last half-decade to advance our understanding of PNe.
