PNe. Such a high number of serendipitous observations is due in large part to the popularity of the Magellanic Clouds for various [*HST*]{} research programs, particularly for stellar populations. Many additional exposures were obtained through pure parallel programs. Although the majority of the objects were observed with more than one filter, more often than not these were broad-band filters which were not well suited for detecting emission line nebulae, in that they do not include the strongest nebular emission lines within the bandpass. However, when available these filters were useful for identifying extremely blue stars in the vicinity, which aided the identification of the likely source of the nebular ionization. Fortunately, some of the archival images that match RP catalog positions were taken through more suitable filters. The WFPC2/F300W bandpass includes nebular \[\] $\lambda3727$ and \[\] $\lambda3889$ emission when present, but the system efficiency is quite low. The F555W filter includes H$\beta$ and the strong \[\] $\lambda\lambda4959+5007$ emission lines, plus H$\alpha$ + \[\] $\lambda\lambda6548+6583$ at lower efficiency. F606W, which has the highest overall system efficiency, includes the \[\], H$\alpha$, and \[\] emissions mentioned above. The clearest detections were made with the F656N filter (which includes some \[\] emission in the 