Spectroscopy

The redshifts of the objects were determined from low resolution spectra obtained using the KPNO Cryogenic Camera and the Lick Cassegrain CCD Spectrograph. With the Cryocam we used the 810 lines mm grating, GG420 order sorting filter, and 2.5" slit, corresponding to a wavelength resolution of about 30A and a pixel separation of 0.84" and 10 Åin the spatial and wavelength directions respectively. The Lick spectrograph was used in the UV mode with a 2.0" slit, corresponding to a wavelength resolution of 8 Åper pixel and a pixel separation of 0.66" in the spatial and wavelength directions respectively. With both instruments the observing procedure was to center a nearby star in the slit of the spectrograph and then offset the telescope to the position of the optical identification. The data were reduced with IRAF. The CCD data were bias subtracted, and flat fielded with a spectral flats made by dividing a polynomial fit to the tungsten lamp source. The wavelength scale was fit with a 5th order polynomial for the Cryocam and a 3rd order for the Lick UV Spectrograph. Redshifts were determined for sources with two or more emission lines. Follow up intermediate resolution long slit spectroscopy is presented in Chambers et al. 1996b (Paper III).