emission lines in a spectrum as possible, we decided to use the widest available spectral coverage of $\sim$5100Å (3750–8850Å) and a resolution of $R=1300$. Each spectrum consists of a blue (580V) and a red (385R) channel that were spliced together at 5700Å. Some of the spectra appear to have a “wide broad line” around the splicing wavelength, mimicking the MgII (2800Å) line at a redshift of $z\approx1.04$. We carefully checked all our $z\approx 1$ quasars for possible misidentifications. Our initial goal was to obtain three exposures of $1800$ s per field, resulting in a median signal-to-noise ratio (S/N) of $\sim$25 at $I=19.5$ mag (calculated from obtained spectra). To subtract the sky flux contribution from each spectrum, we initially selected $\sim$50 and finally used $\sim$25 sky fibers, each positioned to avoid stellar emission based on the OGLE-III LMC catalogs (@2008AcA....58...89U). These catalogs were also used to find $\sim$20 single and well separated bright guide stars for each field, of which 4–8 were used for guiding. The AAOmega [FLD]{} files were created with the [Configure]{} software, and the data reduction was performed using the [2dfdr]{} software (@1996ASPC..101..195T).

As in Paper I, we searched each spectrum for the common (redshifted) quasar emission lines 