readily identified in four of the PNe, and possibly in a fifth. Perhaps as importantly, it is very clear from the [*HST*]{} images the degree of crowding of stars in the vicinity of each object, which will guide the strategy of follow-up studies. We found [*HST*]{} images of fields surrounding an additional 11 RP objects, but no extended emission was detected at the published coordinates. A close examination shows that the non-detections can always be explained by a combination of inappropriate filters and exposures of insufficient depth to reach the anticipated nebular surface brightness.

All of the RP nebulae identified here are faint and most have very low average surface brightness, which are characteristics common to many of the new PNe in the RP catalog. While these serendipitous, high-resolution images provide a useful validation of the PN morphological classifications, they did not prove to be very useful for detecting or validating the faint, outer shells or halos that @RP06b found for nearly 60% of all PNe in their catalog. Even in the extensive, targeted surveys by @Shaw_etal01 [@Shaw_etal06] and @Stang_etal02 [@Stang_etal03] faint halos were seldom detected. Very much deeper exposures with $\sim$01 resolution will be required to study and understand 