The observations of the quasar candidates candidates were accomplished with the Focal Reducer (Lenzen 1989) at the prime focus of the 3.5 meters telescope of the German-Spanish Astronomical Center at Calar Alto (Spain) during six observing runs: October 1989, March 1990, October 1990, February 1991, September 1991 and November 1992.
Our spectra cover a wavelength range from about 4000 to
9000 Å with resolution 
Å per pixel (except for the three last
runs, when the focal reducer optics have been slightly modified giving a
resolution of 
Å per pixel).
When the low dispersion spectrum showed no evident broad emission
lines typical of quasars, the objects, with a few exceptions,
were reobserved at higher dispersion (with a resolution
of 
Å per pixel).
Flux calibration was obtained observing the following standard stars: Feige 98, Feige 15, Eggen 247 and HD 192281. Wavelength calibration spectra were obtained pointing to a screen in the dome illuminated by an He-Ar lamp. We decided to take only one series of He-Ar spectra at the end of each night, instead of one after each object, because of the conspicuous flexures arising from aiming at the screen near the dome floor. These flexures give rise to a wavelength shift which we corrected taking the NaI 5577 Å sky line as a reference zero-point. Furthermore, at low resolution the paucity and the poor definition of some lines of the He-Ar comparison spectrum near 4000 Å, has not allowed to obtain a good wavelength calibration in the blue region. In some cases the redshifts corresponding to the lines lying in the blue have been excluded in the calculation of the mean z.
Some representative spectra are shown in Fig. 4 (click here).
Table 5 (click here) lists the data for 77 of the 93 objects observed. The remaining 16 objects were spectroscopic stars and are listed in Table 6 (click here) together with other objects which changed the original identification, becoming ``Empty Field" or ``Galaxy".
The columns contain the following data: Column 1: name; Column 2: previous identification: B blue object, N red starlike object; Column 3: line identification; Column 4: observed wavelength; Column 5: rest wavelength adopted; Column 6: redshift computed for that line; Column 7: average redshift and eventually new spectroscopic identification, if not confirmed as Quasar.
To ease further studies of these objects, expecially of the few unsolved cases, we provide in Fig. 5 (click here) the finding charts for all the objects listed in the Table 5 (click here) and also for 8 objects listed in Table 6 (click here) identified as stars.
Table 6 (click here) lists objects whose identification changes due to spectroscopic and/or CCD observations. This table is intended to supplement table in Vigotti et al. (1989), where the optical coordinates are quoted.
Figure 4: Some representative spectra for the Quasars in the B3-VLA
sample