Spectrophotometry of extragalactic planetary nebulae in high surface-brightness regions of nearby galaxies is notoriously difficult because of the problem of accurately subtracting the local background of unresolved stars and gaseous emission of the ISM. Conventional slit spectroscopy is not very well suited for providing a good estimate of the two-dimensional surface brightness distribution in the continuum, absorption lines, and superimposed emission lines from all of these background sources. Consequently, the first abundance studies of background-limited extragalactic PNe seem to have significantly suffered from systematic errors related to the background subtraction problem. We present results from a prototype study with PNe in the bulge of M31, using Integral Field (3D) Spectroscopy to overcome these observational problems, arguing that the method is superior to slit spectroscopy and the ideal tool for spectrophotometry of faint sources in crowded field environments. We also present some recent results from observations of PN candidates in the Leo A and Sextans B galaxies using the PMAS 3D instrument at Calar Alto.