The high redshift objects discussed in this paper are a subset of the
4C USS sample
described in Chambers et al. 1987 and Paper I. This subset is those
objects that we have
found to have redshifts . All the faint extended objects in the
USS 4C sample were
observed spectroscopically but the objects with the strongest emission
lines are the most
likely to have had their redshifts determined. Objects in the range
are less
likely to have their redshifts determined because no strong emission
lines are redshifted into
the observed bandpass. Many of the spectroscopically unidentified
sources in Paper I have
faint optical identifications and are likely to be additional high
redshift objects. The sample
of eight objects presented here is probably biased towards objects
with strong emission lines.
In Table 1 we list the high redshift 4C USS sources, redshifts, R magnitude,
and integrated radio properties. Offset stars and their coordinates
are also listed. Finder
charts for the 6 previously unidentified high redshift objects are
shown in Figure 1,
finder charts for the other two objects, 4C41.17 and 4C40.36,
are in Chambers
et al. 1988 and Chambers et al. 1990. Table 2 contains the radio
total intensity
and polarization photometry. These are summarized in plots of the
radio spectra of the
individual components of each source in Figure 2. Table 3 lists
details of the optical and infrared photometry.
The registered images of the radio total intensity, radio polarization, infrared, optical broad band, and narrow band emission are shown in Figures 3,4,5,6,7,8,9, and 10. When the radio morphology is simple then we designate the western lobe as lobe A, the eastern lobe as lobe B, and if an unambiguous core is detected it is labeled C. Sub-components are given a numerical subscript. In the same manner as Paper I we show both polarization and total intensity maps and in our discussion of the radio polarization data we use strongly depolarized for objects with a small depolarization measure DP = P20/P6 and weakly depolarized for objects with a large DP. The registration of the optical data with the radio data is crucial to examine the relationship between the radio and optical emission. To emphasize the relationships of all the different kinds of data each panel in the figures has been carefully scaled and registered with the other panels for that object (to within the astrometric accuracy discussed above). The interested reader is encouraged to reproduce each figure on a transparency so that the panels can be overlaid. To aid in the presentation of the data we also include enlarged subsections of certain images. In sections 3.1 through 3.8 below we discuss each individual high redshift object in order of right ascension.