wing), but this filter is not as often used.

The [*HST*]{} images presented here were obtained using the Wide-Field Planetary Camera 2 (WFPC2) or the Advanced Camera for Surveys (ACS). These images were calibrated with the standard reduction pipelines for the instruments used to obtain them. The pipelines perform similar processing: bias correction, dark scaling and subtraction, and flat-fielding. The ACS pipeline also performs a geometric rectification. For many of the objects, multiple exposures were obtained at or near the same location with the same instrument and filter combination. Typically this is done to facilitate the identification and rejection of cosmic rays, to mitigate the effects of detector defects such as charge traps or high dark current, or (in the case of WFPC2) to improve the spatial sampling by dithering the image. These images were combined when possible. For WFPC2 many pre-combined images are available from the Multi-mission Archive at STScI (MAST) as high level science products (HLSP). @Wada_etal06 describe the details of this processing, as well as the quality of the photometry of the resulting images. For the present purpose we are concerned primarily with determining precise coordinates, sizes, and morphologies of the new RP nebulae, so that the 