presented in Table 1. Column (1) gives the UT date of each observation and the Julian Date is given in column (2). The origin of the data (set A or B) appears in column (3). The projected size of the spectrograph entrance aperture was $5\arcsecpoint0\times7\arcsecpoint5$ (i.e., a slit width of $5\arcsecpoint0$ and a cross-dispersion extraction window of $7\arcsecpoint5$) for all set A spectra and $3\arcsecpoint0\times4\arcsecpoint6$ for all set B spectra. In each case, the slit was oriented in the east-west direction (i.e., the slit position angle was always 90). The nominal spectral resolution was 9Å for all set A spectra and 5Å for all set B spectra. The wavelength coverage of each spectrum is given in column (4), and the file name is given in column (5). All of these spectra are publicly available on the International AGN Watch site on the World-Wide Web[^1].

The spectroscopic images were processed in standard fashion for CCD frames, including bias subtraction, dark-count correction when necessary, flat-field correction, wavelength calibration, and flux calibration based on standard-star observations. Since even under photometric conditions, AGN spectrophotometry is rarely more accurate than $\sim$10%, the usual technique of flux calibration by comparison with standard stars is far too 