Bright extragalactic planetary nebulae have served as a probe of the chemical evolution of several nearby dynamically hot systems (DHSs: ellipticals, bulges, and dwarf spheroidals). There is a pronounced symbiotic relationship between our understanding of the evolution of planetary nebulae and their use to understand the chemical evolution of their host galaxies. We have learned that bright extragalactic planetary nebulae are similar to their Milky Way counterparts and that they are useful probes of chemical evolution, though the interpretation of their chemical abundances is not necessarily simple. From the chemical abundances of the planetary nebulae in DHSs, we have learned that DHSs follow a metallicity-luminosity relation and probably did not evolve as closed systems even while forming their stars. The currently-available data, however, have yet to be fully exploited, primarily because a quantitative understanding of the evolution of planetary nebulae is lacking. Addressing this deficiency is perhaps most easily done via observations of extragalactic planetary nebulae themselves and will result not only in a better understanding of planetary nebulae, but also of the evolution of their host galaxies and of the role of planetary nebulae in shaping that evolution.