0000+025A: QSO. The spectrum clearly shows that this is a QSO with z(em)= 1.6843. Absorption lines at {lambda}4343, {lambda}4374, and {lambda}5897 A are probably caused by bad subtraction of strong sky emission lines. A possible broad absortion feature at {lambda}6379 is unidentified. 0000+027A: QSO. ZC1 identified emission lines at 4203 and 5179 A as C IV and C III respectively. They are actually Ly{alpha} and C IV, giving a higher redshift. There is strong absorption line just to the red of the peak of the C IV emission line which is almost certainly associated C IV, absorption, with z(abs)=2.394 and a rest frame equivalent of 3.0 A, because of its strength and position. 0003+011A: star-M4. The spectral features suggest M4 star, while the (B-V) is typical of an M2 star of solar abundance. 0003+011B: star-F. The continuum falls off shortward of 5000 A, and rises slightly into the red, indicating T < 7000 K. Ca II H and K are weak, and there is no break at 4000 A. 0004-005B: QSO. This QSO was identified as Q0004-0032 with z(em)=1.72 and B_J_=18.4 by Foltz et al. (1989). Their spectrum shows four strong emission lines. Two strong absorption lines at {lambda}~=5854 and {lambda}~=5959 are unidentified. They might be Mg II absorption systems. 0004+014: star-G. Ca 11 H,K, and Mg I triplet 5167, 5172.7, and 5183.6 are very strong. H{alpha}, which is very weak, is the only visible Balmer line. The flux drops about 50% across 4000 A. 0005+030: QSO. ZC1 identified an emission line at 4000 A as Ly{alpha}. It is actually C III]1909, which is confirmed by our detection of Mg II at z(em) = 1.0948, and blended Fe II features. 0006+020B: QSO. This QSO was identified as Q0006+0200 with z(em) = 2.35 and B_J_=17.9 by Foltz et al. (1989). ZC1 identified emission lines at 4149 and 5200 A as C IV and C III], respectively. They are actually Ly{alpha} and C IV, at a higher redshift of 2.3483. The two strong absorption lines in this spectrum are 4700 and 5226 A and there is a possible weak line at 5076 A. The absorption feature at 5578 A is considered bogus because it is near to a strong sky line. The strong line at 4700 A and the weak line at 5076 A could be C IV and Al II at z(abs)= 2.035, but the Si II {lambda}1526 line which would be expected at 4634 A is not seen, and the second strong line is not identified. Alternatively, 4700 is Si IV {lambda}1393, 4735 A is Si IV {lambda}1402, and 5226 A is a blended C IV doublet. But then 4700 A must be a blend with another unidentified line because it is twelve times stronger than its doublet partner compared to a maximum allowed ratio of two. The Foltz et al. (1989) spectrum also shows the 4700 line. In a footnote to their Table 2 they suggest possible associated absorption, presumably because they see absorption in the Ly{alpha} emission line, which is consistent with our interpretation of the 5226 line as C IV. 0006+022A: QSO. ZC1 identified emission lines at 3910 and 5056 A as Ly{alpha} and C IV, respectively. They are actually C IV and C III], respectively, at z(em) = 1.5152. We also observe the blue wing of the Mg II emission line which should be centered at about 7039 A. 0006+025: QSO. Foltz et al. (1989) called this QSO Q0006+0230. They saw Ly{alpha} and Si IV + O IV] emission lines in addition to the C IV and C III] which we saw obtained z(em) = 2.09, consistent with our value of 2.0909. Their magnitude of B_J_ = 18.00 is to be preferred to our value of B = 19.19. 0008+008: QSO. The peak of the Ly{alpha} emission line appears at too high a redshift because strong absorption lines destroy the blue side of the line peak. The colors listes in table3 are much redder than those of typical QSO be cause of the Ly{alpha} forest and the Lyman limit system. A Lyman Limit edge is seen at {lambda}~=3750 which corresponds to z_LLS_ = 3.08. This system is at z(abs) = 3.079, and shows strong Ly{alpha} and C IV doublet absorption lines. In addition there is an obvious damped Ly{alpha} absorption line at {lambda}~=4883.5 A (z(abs)~=3.017) with an observed equivalent width of about 96 A, which corresponds to a neutral hydrogen column density of N(HI)~=1021 cm-2. The line absorption system with z(abs) = 3.028 is likely associated with this damped Ly{alpha} line. We found other metal systems, including C IV at z(abs) = 2.625, 2.650, 2.895 and Mg II at z(abs) = 1.194. 0008+010: star-G. This star shows H{alpha}, H{beta}, H{gamma}, and Ca II, all of which are very weak. There is no 4000 A break and Ca II is stronger than Balmer lines. The estimate metallicity of [Fe/H]~=-2.5 is the lowest of our ten stars. 0010-002B: QSO. ZC3 listed a weak emission line at 4203 A, a strong line at 3818 A which they interpreted as Ly{alpha}+NV (rest wavelength 1228 A) at an emission redshift of 2.11. We see weak emission lines at 4872 and 6004 A which we interpret as C IV and C III] at a redshift of 2.1462. A Foltz et al. (1989) spectrum of this object, which they call Q0010-0012, shows Ly{alpha} in addition to the weak C IV and C III] lines which we saw. They obtained z(em)= 2.15, which is consistent with our redshift, and they gave B_J_ = 18.5, which is more reasonable than our B = 20.07. ZC3 also list an absorption line at 3669 A, which is likely to be a strong (probably damped, because it shows up in the prism spectrum) Ly{alpha} line at z(abs) = 2.017. The Foltz et al. (1989) spectrum also shows this line. We see a partially resolved pair of lines at 4690 and 4697.7 A, which we interpret as the C IV doublet in this absorption system, with z(abs) = 2.030 (see also the Foltz et al. spectrum) also see a possible doublet near 6300 A which might be Mg II if it is not simply poor sky subtraction. 0010+008: QSO. There is a possible Lyman limit edge at about 3500-3600 A but the S/N is too low to see possible metal lines in this system. 0010+023: galaxy. This emission line galaxy (z(em) = 0.0879) was observed in both setups A and B. We see stellar absorption immediately surrounding the Balmer emission lines in the setup B spectrum. 0011-002A: galaxy. In addition to the emission lines listed in table5, the 4000 A break is also seen at the expected wavelength of 4463 A. 0011-012A:star-sdB. The Balmer lines are resolved and have large equivalent widths of W(H{alpha}) = 12.1 A, W(H{beta}) = 13.1 A, and W(H{gamma}) = 3.9 A. The spectrum rises to the blue, indicating T>=11000 K, but the slit (B-V) of 0.18 indicates a much lower temperature of T~=8000 K. The absorption feature at the extreme blue end of the spectrum near 4311 A, and the shallower broad feature at 4370 A are both bogus, the latter lying in the region of He 4387. However, He I 4471 A, which is normally stronger, is not seen. H{gamma} at 4345 A may be compromised by these detector problems. The W(H{gamma}) line has a central depth of R_c_=0.33 of the continuum level (measured down from the continuum, so that deeper lines have larger values), a FWHM of 10.5 A, and a width at 20% below the local continuum of D(0.2) = 8.4 A. Both the width measurements have been corrected for the instrumental resolution, but we have not corrected the central depth, which should be greater than the measured value. The corrected width and uncorrected depth place the star amongst sdO, sdB, and hot DA stars of Fig. 2 of Beers et al. (1992). The line profile lacks the extensive wings expected of a white dwarf, but is very similar to a hot sdB (or cool sdO) star with T = 35 000 K and logg = 5 (Fig. 3 of Greenstein 1980). Since the line will be deeper than our measurement, the actual temperature is probably nearer to 25 000 K, and the star would be near to the blue HB. However these high temperatures are inconsistent with the (B-V), and neither the H{gamma} line nor the color can be considered reliable. We can also measure the width of the H line at 0.9 of the continuum level, which increases with both temperatures and gravity (Herbig 1992). The measured value of 36 A implies 18000