1 lists the nebulae observed and details of the observations. Integration times for each exposure ranged from a few seconds for the extremely bright sources to 5 minutes for faint sources. The off-axis guider was used to keep a consistent on-source slit position. Multiple “Fowler” sampling was used to reduce the read noise. The number of samples for a particular integration ranged from 4 to 16, with more samples used for the longer integration times. The spectra were reduced using IRAF; the extraction and processing of the spectral data were done using the functions in the noao.twodspec and noao.onedspec packages. Alternating source and sky integrations of the same length were taken and differenced to remove sky and telescope background flux. Dome flats were used to correct for pixel-to-pixel gain variations in the array. Stars of known spectral type (either G0 or A0) were observed at the same airmass as the nebulae immediately before and after the PNe observations and were used for correction of the instrumental response and sky transmission. Individual lines were removed from the stellar spectra, and then normalized using a blackbody function of T = 5920 K for the G0 stars and T = 10800 K for 