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\begin{document}
 
\newcommand{\cts}{$\rm {cts\,s}^{-1}$}
\newcommand{\hatom}{$10^{20}$ \mbox{H-atoms\,cm$^{-2}$}}
\newcommand{\R}{ROSAT}
\newcommand{\fxo}{$f_{\rm x}/f_{\rm o}$}

\begin{document}
\setcounter{table}{2}
\begin{table*}[t] 
\caption{Summary of optical identification program of new bright soft
high-galactic-latitude RASS sources with HR1\,$< 0$.  Columns denote
(1) the J\,2000 X-ray position from the RASS BSC, (2) and (3) the
J\,2000 RA and DEC of the optical counterpart, (4) the separation
between optical and X-ray positions in arcsec and (5) in units of the
90\% confidence radii according to Eq. 1, (6) the RASS BSC PSPC count
rate CR in \cts, (7) the hardness ratio HR1, (8) the class and (9)
the type of the optical counterpart, (10) the redshift $z$ if
extragalactic, and (11) the visual magnitude $V$. Errors to CR and HR1
are given in brackets and refer to the last digits. Notes at the end
of the Table refer to the 1RXS\,J numbers in column (1).}
\begin{flushleft} 
\footnotesize 
\begin{tabular}{lrrrrrrrrlrllcll} 
\hline \noalign{\smallskip} 
(1) & \multicolumn{3}{l}{(2)} & \multicolumn{3}{l}{(3)} & (4) & (5) & 
\multicolumn{1}{l}{(6)}
& \multicolumn{1}{l}{(7)} & (8) & (9) & \multicolumn{1}{l}{(10)} & (11) 
& \multicolumn{1}{l}{(12)}\\ 
RASS BSC No. & \multicolumn{6}{c}{RA,DEC(2000)} & 
\multicolumn{2}{c}{Separation}& CR & HR1 & Class & Type & $z$ & $V$ & 
Notes \\ 
1RXS J.....&&&&&&&(\arcsec) & $r_{90}$ &&&&&&\\
\noalign{\smallskip}\hline\noalign{\smallskip} 
 000647.2--332316 &  0 &  6 & 46.7 & --33 & 23 & 11 &   8.0 &  0.35 &  
0.141 (25) &  --0.69 (11) &   AGN   & Sy1  & 0.217  &  16.9 & 1 \\
 002233.8--340722 &  0 & 22 & 33.2 & --34 &  7 & 20 &   7.7 &  0.59 &  
0.418 (37) &  --0.38 (08) &   AGN   & Sy1  & 0.219 &  16.1 & 1,4,6 \\
 005033.3+244901  &  0 & 50 & 33.0 &   24 & 49 &  2 &   4.2 &  0.28 &  
0.444 (58) &  --0.20 (12) &   STAR  & dMe  &       &  12.6 & 1,3 \\
 012237.4--264646 &  1 & 22 & 37.4 & --26 & 46 & 46 &   0.0 &  0.00 &  
0.321 (42) &  --0.65 (08) &   AGN   & Sy1  & 0.417 &  18.8 & 1,6 \\
 012326.1--794139 &  1 & 23 & 16.5 & --79 & 41 & 33 &  26.5 &  1.79 &  
0.282 (45) &    0.05 (15) &   STAR  & K    &       &  10.2 & 1 \\
 013242.8--655434 &  1 & 32 & 42.0 & --65 & 54 & 34 &   4.9 &  0.30 &  
0.276 (38) &  --0.97 (04) &   CV    & AM   &       &  20.0 & 1,8 \\
 013417.2--425821 &  1 & 34 & 16.8 & --42 & 58 & 26 &   6.7 &  0.41 &  
0.168 (23) &  --0.91 (05) &   AGN   & Sy1  & 0.237 &  16.0 & 1,4 \\
 013653.5--351012 &  1 & 36 & 54.3 & --35 &  9 & 53 &  21.4 &  1.63 &  
0.491 (38) &  --0.81 (04) &   AGN   & Sy1  & 0.289 &  18.0 & 1,4 \\
                  &  1 & 54 &  0.9 & --59 & 47 & 49 &  21.9 &  1.11 &  
0.335 (54) &  --0.70 (07) &   CV    & AM   &       &  17.0 & 1,8 \\
 020403.1--510455 &  2 &  4 &  2.7 & --51 &  4 & 57 &   4.3 &  0.33 &  
0.439 (38) &  --0.25 (08) &   AGN   & Sy1  & 0.151 &  16.6 & 1,4 \\
 021257.7--585109 &  2 & 12 & 58.1 & --58 & 51 & 17 &   8.6 &  0.52 &  
0.185 (53) &  --0.10 (27) &   STAR  & dMe  &       &  13.7 & 1 \\
 021754.1--195813 &  2 & 17 & 53.6 & --19 & 58 & 19 &   9.3 &  0.43 &  
0.144 (24) &  --0.37 (15) &   AGN   & Sy1  & 0.468 &  17.1 & 1,6 \\
 022815.6--405712 &  2 & 28 & 15.2 & --40 & 57 & 16 &   6.0 &  0.46 &  
0.437 (55) &  --0.52 (10) &   AGN   & Sy1  & 0.494 &  15.2 & 1,4 \\
 024513.8--434410 &  2 & 45 & 14.1 & --43 & 44 &  1 &   9.6 &  0.58 &  
0.233 (36) &  --0.41 (12) &   STAR  & dMe  &       &  13.8 & 1 \\
 030313.9--474214 &  3 &  3 & 14.2 & --47 & 42 & 13 &   3.2 &  0.24 &  
0.196 (23) &  --0.30 (10) &   AGN   &      &       &  17.3  & 5,8 \\
 031713.9--853231 &  3 & 17 & 20.0 & --85 & 32 & 29 &   7.4 &  0.50 &  
0.204 (22) &  --1.00 (01) &   STAR  & WD   &       &  13.9 & 1,2 \\
 033550.1--471556 &  3 & 35 & 49.7 & --47 & 16 &  0 &   5.7 &  0.39 &  
0.245 (24) &  --0.30 (09) &   AGN   & Sy1  & 0.598 &  17.3 & 1 \\
 033714.6--415541 &  3 & 37 & 15.1 & --41 & 55 & 25 &  16.9 &  0.68 &  
0.145 (34) &  --1.00 (14) &   STAR  & WD   &       & 16.4   & 1 \\
 035514.0--545159 &  3 & 55 & 13.3 & --54 & 51 & 57 &   6.4 &  0.43 &  
0.216 (21) &  --0.68 (07) &   AGN   & Sy1  & 0.269 & 16    & 1 \\
 043513.8--461524 &  4 & 35 & 14.3 & --46 & 15 & 34 &  11.3 &  0.86 &  
0.249 (38) &  --0.48 (11) &   AGN   & Sy1  & 0.070 &  17.1 & 1,4 \\
 043554.2--363635 &  4 & 35 & 53.9 & --36 & 36 & 42 &   7.9 &  0.60 &  
0.445 (40) &  --0.28 (08) &   AGN   & Sy1  & 0.141 &  17.1 & 1,4,7 \\
 043830.0--614758 &  4 & 38 & 29.3 & --61 & 47 & 59 &   5.1 &  0.31 &  
0.390 (68) &  --0.00 (17) &   AGN   & Sy1  & 0.069 &  15.7 & 1,4 \\
 043943.2--454039 &  4 & 39 & 44.7 & --45 & 40 & 43 &  16.2 &  0.90 &  
0.319 (39) &  --0.81 (07) &   AGN   & Sy1  & 0.224 &  16.6 & 1,4 \\
 044550.1--385537 &  4 & 45 & 50.7 & --38 & 55 & 38 &   7.1 &  0.39 &  
0.223 (36) &  --0.97 (09) &   STAR  & WD   &       &  17.5 & 1 \\
 045223.8--164926 &  4 & 52 & 24.3 & --16 & 49 & 18 &  10.7 &  0.72 &  
0.431 (35) &  --0.22 (07) &   STAR  & dMe  &       &  12.5 & 1 \\
 045444.5--481300 &  4 & 54 & 42.9 & --48 & 13 & 19 &  24.8 &  0.84 &  
0.145 (26) &  --0.72 (11) &   AGN   & Sy1  & 0.363 &  17.7 & 1,4 \\
 045929.4--222953 &  4 & 59 & 28.9 & --22 & 29 & 55 &   7.2 &  0.36 &  
0.115 (19) &  --0.83 (08) &   GAL   &      & 0.047 &  18   & 1,8 \\
 050146.2--035927 &  5 &  1 & 46.1 & -- 3 & 59 & 32 &   5.2 &  0.29 &  
0.224 (26) &  --0.96 (03) &   CV    & AM   &       &  17.5 & 1,8 \\
 051214.5--324140 &  5 & 12 & 13.1 & --32 & 41 & 38 &  17.8 &  1.35 &  
0.151 (20) &  --0.51 (10) &   CV    & IP   &       &  17.6 & 1,8 \\
 051541.7+010528  &  5 & 15 & 41.3 &    1 &  4 & 40 &  48.4 &  3.68 &  
0.381 (32) &  --0.92 (03) &   CV    & AM   &       &  15.5 & 1,8 \\
 054747.2--195609 &  5 & 47 & 46.9 & --19 & 56 &  9 &   4.2 &  0.28 &  
0.168 (21) &  --0.92 (05) &   AGN   &      & 0.055: & 17.7   & 1,5,8 \\
 060033.1--270918 &  6 &  0 & 33.2 & --27 &  9 & 19 &   1.7 &  0.13 &  
0.404 (42) &  --0.87 (04) &   CV    & AM   &       &  19   & 1,8 \\
 060452.1--343331 &  6 &  4 & 52.0 & --34 & 33 & 43 &  12.1 &  0.92 &  
0.428 (50) &    0.06 (11) &   STAR  & dMe  &       &  13.4 & 1,2 \\
 061544.4--653151 &  6 & 15 & 43.6 & --65 & 31 & 52 &   5.1 &  0.44 &  
0.093 (05) &  --0.03 (05) &   AGN   & Sy1  & 0.227 &  16.6 & 1 \\
                  &  8 &  6 & 21.7 &   15 & 27 & 15 &   7.3 &  0.40 &  
0.158 (27) &  --0.67 (10) &   CV    & IP   &       &  20   & 1,8 \\
                  &  8 & 36 & 50.3 &   15 & 53 & 28 &  35.8 &  2.71 &  
0.246 (50) &  --0.99 (01) &   STAR  & WD   &       &       & 1,8 \\
 085909.5+053703  &  8 & 59 &  9.2 &    5 & 36 & 55 &   9.2 &  0.51 &  
0.233 (28) &  --0.82 (06) &   CV    & AM   &       &   17  & 1,8 \\
 094538.0--005829 &  9 & 45 & 37.9 & -- 0 & 58 & 29 &   1.5 &  0.11 &  
0.381 (31) &  --0.15 (07) &   STAR  & K    &       &  11  & 1 \\
 095308.6+145841  &  9 & 53 &  8.1 &   14 & 58 & 37 &   8.3 &  0.50 &  
0.185 (27) &  --0.74 (08) &   CV    & AM   &       &  17.3 & 1,8 \\
 101402.5+461954  & 10 & 14 &  1.9 &   46 & 19 & 54 &   6.2 &  0.42 &  
0.150 (19) &  --0.66 (09) &   AGN   & Sy1  & 0.324 &  17.1 & 1,3,4,7 \\
 101718.0+291439  & 10 & 17 & 18.3 &   29 & 14 & 34 &   6.4 &  0.56 &  
0.386 (34) &  --0.24 (08) &   AGN   & Sy1  & 0.049 &  15.7 & 1,4,8 \\
 102444.5--302102 & 10 & 24 & 44.2 & --30 & 20 & 59 &   4.9 &  0.30 &  
0.201 (28) &  --1.00 (03) &   STAR  & WD   &       &  15.8 & 1,2 \\
 104614.2+525600  & 10 & 46 & 13.7 &   52 & 55 & 54 &   7.5 &  0.57 &  
0.322 (27) &  --0.82 (04) &   AGN   & Sy1: & 0.51:  &  17.5   & 1,3,8\\
 105055.2+552731  & 10 & 50 & 55.2 &   55 & 27 & 23 &   8.0 &  0.69 &  
0.374 (29) &  --0.69 (05) &   AGN   & Sy1  & 0.333 &  16.7 & 1,3,4 \\
 105355.0+661209  & 10 & 53 & 55.6 &   66 & 12 &  1 &   8.8 &  0.67 &  
0.179 (19) &  --0.76 (06) &   AGN   & Sy1  & 0.117 &  16.8   & 1,3 \\
 105444.4+483145  & 10 & 54 & 44.7 &   48 & 31 & 38 &   7.6 &  0.66 &  
0.454 (32) &  --0.36 (06) &   AGN   & Sy1  & 0.286 &  15.7 & 1,3,7 \\
 110842.1+595010  & 11 &  8 & 41.6 &   59 & 50 &  8 &   4.3 &  0.33 &  
0.160 (19) &  --0.72 (07) &   AGN   & Sy1  & 0.425: &  18   & 1,3,8 \\
 114738.0+050119  & 11 & 47 & 37.6 &    5 &  1 & 10 &  10.8 &  0.82 &  
0.392 (33) &  --0.13 (08) &   STAR  & dMe  &       &  12.1 & 1,3 \\
 120656.2+700754  & 12 &  6 & 55.2 &   70 &  7 & 49 &   7.1 &  0.62 &  
0.436 (26) &  --0.15 (05) &   STAR  & dMe  &       &  11.4 & 1,3 \\
 123220.6+495731  & 12 & 32 & 20.1 &   49 & 57 & 22 &  10.2 &  0.78 &  
0.341 (31) &  --0.60 (07) &   AGN   & Sy1  & 0.262  &  17   & 1,3 \\
\noalign{\smallskip}\hline\noalign{\smallskip} 
\end{tabular}
\end{flushleft}
\end{table*}

\begin{table*}
\begin{flushleft}
\begin{tabular}{lrrrrrrrrlrllcll} 
\hline \noalign{\smallskip} 
(1) & \multicolumn{3}{l}{(2)} & \multicolumn{3}{l}{(3)} & (4) & (5) & 
\multicolumn{1}{l}{(6)}
& \multicolumn{1}{l}{(7)} & (8) & (9) & \multicolumn{1}{l}{(10)} & (11) 
& \multicolumn{1}{l}{(12)}\\ 
RASS BSC No. & \multicolumn{6}{c}{RA,DEC(2000)} & 
\multicolumn{2}{c}{Separation}& CR & HR1 & Class & Type & $z$ & $V$ & 
Notes \\ 
1RXS J..... &&&&&&&(\arcsec) & $r_{90}$ &&&&&&\\
\noalign{\smallskip}\hline\noalign{\smallskip} 
 131259.1+262825  & 13 & 12 & 59.5 &   26 & 28 & 24 &   5.5 &  0.37 &  
0.418 (39) &  --0.41 (07) &   AGN   & Sy1  & 0.061 &  16 & 1,3,4,7 \\
 150204.3+064521  & 15 &  2 &  4.1 &    6 & 45 & 15 &   6.7 &  0.51 &  
0.472 (50) &  --0.52 (09) &   AGN   & Sy1  & 0.286 &  16.6 & 1,3 \\
 161418.7--083335 & 16 & 14 & 19.0 & -- 8 & 33 & 25 &  10.9 &  0.74 &  
0.240 (26) &  --1.00 (02) &   STAR  & WD   &       &  14   & 1 \\
 164625.8+392922  & 16 & 46 & 26.0 &   39 & 29 & 33 &  11.2 &  0.85 &  
0.396 (28) &  --0.42 (06) &   AGN   & Sy1  & 0.100 &  17.1 & 1,3,4 \\
 165240.0+441632  & 16 & 52 & 40.1 &   44 & 16 & 37 &   5.1 &  0.44 &  
0.489 (29) &  --0.56 (04) &   AGN   & Sy1  & 0.132 &  16.9 & 1,3,7 \\
 171127.2+664532  & 17 & 11 & 27.3 &   66 & 45 & 29 &   3.1 &  0.27 &  
0.235 (10) &  --1.00 (00) &   STAR  & WD   &       &  17   & 1,2 \\
 181810.0+534343  &  &  &  &    &  &  &    &   &  0.479 (18) &  --0.35 
(03) &         &      &       &  15   & 8 \\
 202237.8--395412 & 20 & 22 & 37.3 & --39 & 54 & 13 &   5.8 &  0.35 &  
0.330 (36) &  --0.97 (03) &   CV    & AM   &       &  18.5 & 1,8 \\ 
 203626.2--535222 &    &    &      &      &    &    &       &       &  
0.144 (28) &  --1.00 (05) &   STAR  & WD:  &       &     & 5,8 \\
 214406.1--394900 & 21 & 44 &  5.9 & --39 & 49 &  2 &   3.1 &  0.24 &  
0.412 (37) &  --0.47 (07) &   AGN   & Sy1  & 0.140 &  18.0 & 1,4 \\
 215450.7--441406 & 21 & 54 & 51.0 & --44 & 14 &  6 &   3.2 &  0.24 &  
0.454 (39) &  --0.70 (06) &   AGN   & Sy1  & 0.344 &  15.8 & 1,4 \\
 220416.7--425817 & 22 &  4 & 17.5 & --42 & 58 & 14 &   9.3 &  0.40 &  
0.217 (30) &  --0.72 (09) &   AGN   & Sy1  & 0.639 &  18.7 & 1 \\
 220546.4--405816 & 22 &  5 & 45.4 & --40 & 58 & 18 &  11.5 &  0.64 &  
0.154 (25) &  --0.68 (10) &   AGN   & Sy1  & 0.235 &  18.3 & 1 \\
 221300.5--171015 & 22 & 13 &  0.1 & --17 & 10 & 19 &   7.0 &  0.53 &  
0.425 (42) &  --0.58 (07) &   AGN   & Sy1  & 0.146 &  17.2 & 1,4,6 \\
 221515.2--274225 & 22 & 15 & 14.7 & --27 & 42 & 22 &   7.3 &  0.40 &  
0.315 (39) &  --1.00 (02) &   STAR  & WD   &       &  15.5 & 1 \\
 222149.3--271310 & 22 & 21 & 48.4 & --27 & 13 & 13 &  12.4 &  0.94 &  
0.287 (34) &  --0.57 (08) &   AGN   & Sy1  & 0.177 &  17.7 & 1,4,7 \\
 222650.8--414442 & 22 & 26 & 50.6 & --41 & 44 & 46 &   4.6 &  0.31 &  
0.169 (27) &  --0.69 (10) &   AGN   & Sy1  & 0.307 &  17.0   & 1,7 \\
 223003.8--513702 & 22 & 30 &  4.1 & --51 & 37 &  7 &   5.7 &  0.39 &  
0.217 (27) &  --0.51 (10) &   AGN   & Sy1  & 0.454 &  19.2 & 1 \\
 223244.3--413441 & 22 & 32 & 43.0 & --41 & 34 & 38 &  14.9 &  0.91 &  
0.190 (28) &  --0.56 (12) &   AGN   & Sy1  & 0.075 &  16.9 & 1,4,7 \\
 224155.3--440459 & 22 & 41 & 55.3 & --44 &  4 & 55 &   4.0 &  0.27 &  
0.359 (39) &  --0.68 (07) &   AGN   & Sy1  & 0.545 &  15.8 & 1,4 \\
 224642.0--520638 & 22 & 46 & 42.1 & --52 &  6 & 40 &   2.2 &  0.17 &  
0.706 (67) &    0.14 (09) &   GAL   &      & 0.194 &  18.2 & 1,8 \\
 230358.7--551717 & 23 &  3 & 57.8 & --55 & 17 & 18 &   7.8 &  0.59 &  
0.375 (34) &  --0.34 (08) &   AGN   & Sy1  & 0.084 &  17.5 & 1,4 \\
 230439.3--512804 & 23 &  4 & 38.4 & --51 & 28 &  0 &   9.3 &  0.63 &  
0.356 (39) &  --0.52 (09) &   AGN   & Sy1  & 0.106 &  17.2 & 1,4 \\
 233711.4--593241 & 23 & 37 &  9.0 & --59 & 32 & 25 &  24.3 &  1.23 &  
0.163 (30) &  --0.56 (14) &   AGN   & Sy1  & 0.567  &  17.3 & 1 \\
 234024.3--532913 & 23 & 40 & 23.0 & --53 & 28 & 57 &  19.8 &  0.86 &  
0.230 (46) &  --0.73 (14) &   AGN   & Sy1  & 0.321 &  17.6 & 1,4 \\
 234907.7--331148 & 23 & 49 &  7.3 & --33 & 11 & 44 &   6.4 &  0.49 &  
0.458 (46) &  --0.49 (08) &   AGN   & Sy1  & 0.144 &  16.6 & 1,4,6,7 \\
234939.7--563723 &  &  &  &  &  & &  &  & 0.490 (62) & --0.79 (07) & & 
& & & 
8 \\
\noalign{\smallskip}\hline\noalign{\smallskip} 
\end{tabular}
\end{flushleft}
{\bf Correction to Paper I}
\begin{description}
\item 160518.5+542101: For this source, the identification of Bade et
al. (1997) as an M-star has been cited in Paper I. That star, however,
is 31\arcsec{} from the X-ray position and the more likely candidate is
a 19 mag object at 5\arcsec{} separation which is also a radio source
(White et al. 1997), suggesting a BL Lac identification. For the
M-star, the implied \fxo$\,\simeq\,0.44$ would also be quite
atypical, while the \fxo$\,\simeq\,1.4$ is typical of a BL Lac
object.  The USNO-A1.0 optical position of the BL Lac candidate is
\mbox{RA,~DEC (2000):~16~05~19.0, 54~21~00}, the radio position
\mbox{RA,~DEC (2000):~16~05~19.1, 54~21~00}.
\end{description}
\end{table*}

\clearpage
\vspace{5mm}
\footnotesize 
\noindent 
{\bf Notes to Table 3}
\vspace*{-2mm}

\begin{description}
\item \hspace{-2mm}{\bf 1:} Spectroscopic identification, this work

\item \hspace{-2mm}{\bf 2:} WFC identification (Pye et al. 1995, Mason
et al. 1995)

\item \hspace{-2mm}{\bf 3:} Hamburg/RASS identification (Bade et al. 
1997)

\item \hspace{-2mm}{\bf 4:} see also Grupe et al. 1998

\item \hspace{-2mm}{\bf 5:} Inferred identification from the Digitized
Sky Survey

\item \hspace{-2mm}{\bf 6:} Radio source

\item \hspace{-2mm}{\bf 7:} Listed also by Veron-Cetty \&\ Veron (1996)

\item \hspace{-2mm}{\bf 8:} Remarks to individual sources
\end{description}

\vspace*{-5mm}
\begin{description}
\item 013242.8--655434: AM Herculis binary (Burwitz et
al. 1996)
\item 015400.9--594749: AM Herculis binary (Beuermann \&\ Thomas
1993). The variable X-ray source is not contained in the RASS BSC. The
J\,2000 X-ray position derived from the PET is 
1~54~00.8~~\mbox{--59~48~10}.
\item 030313.9--474214: CCD image shows galaxy with bright nucleus
within 3\arcsec{} from X-ray position, B = 18.2 (ROE finding chart). 
The
14\,mag star 20\arcsec{} NE of spectral type $\sim$K1 is probably
unrelated to the X-ray source 
\item 045929.4-222953: Our R filter image shows a galaxy with a bright
core. Our two spectra show red-shifted absorption lines of the galaxy
but no emission lines.
\item 050146.1--035932: AM Herculis binary (Burwitz et al.  1998, in
preparation)
\item 051213.1--324138: Soft Intermediate Polar (Burwitz et al. 1997) 
\item 051541.3--010440: AM Herculis binary (Shafter et al. 1995)
\item 054747.2-195609: The CCD image shows galaxy with bright nucleus
5\arcsec{} W of X-ray position. Our spectrum misses the nucleus and
shows a weak absorption spectrum with z = 0.055:. A probably unrelated
late F star is 31\arcsec{} E
\item 060033.2--270919: AM Herculis binary (Beuermann \& Burwitz 1995)
\item 080621.7--152715: Intermediate Polar. The highly variable X-ray
source is not contained in the RASS BSC. The J\,2000 X-ray position 
derived
from the PET is 8~06~22.2~~15~27~14
\item 083650.3--155328: White dwarf. Only a non-calibrated spectrum is
available. The X-ray source is not contained in the RASS BSC. The 
J\,2000 
X-ray position derived from the PET is. 8~36~52.2~~15~53~51
\item 085909.5--053703: AM Herculis binary (Beuermann \& Burwitz
1995), V = 16.5--18.7
\item 095308.1--145837: AM Herculis binary (Beuermann \& Burwitz 1995)
\item 101718.0+291439: This active galaxy is known as CASG\,59
(Salzer et al. 1995)
\item 104614.2+525600: The Hamburg survey lists this source as an
AGN. Our segments of blue and red spectra miss MgII and
H$\beta$. H$\gamma$ is very weak. Weaker spectral features yield
$z\,=\,0.510\pm0.003$.
\item 110842.1+595010: Our spectrum contains only one Balmer line
adjacent to a broad Fe-line complex. Interpreting the line as H$\beta$.
yields the quoted redshift.
\item 181810.0--534343: The 90\% confidence error circle contains
three objects. The $V\sim15$ object 15\arcsec{} SW is a G-star, no
spectrum is available of the $V=14.5$ candidate 5\arcsec{} NE and the
$V \sim 19$ candidate 12\arcsec{} SSE. 
\item 202237.3--395413: AM Herculis binary (Burwitz et al. 1996) 
\item 203626.2--535222: HR1 $\simeq -1$ suggests a WD. Candidate 1 is
$\sim 20$\arcsec{} NW, has \mbox{B\,=\,12}, and is of spectral type
$\sim$K0; candidate 2 is 10\arcsec{} E, has \mbox{B\,=\,17} and B--V =
0.6; candidate 3 is 23\arcsec{} E, has \mbox{B\,=\,16} and B--V =
0.9. If the WD is associated with the K-star it should be fainter than
$B\,\simeq\,15.5$
\item 224642.0--520638: Galaxy, no emission lines. Final $CR-HR1$
values place the source outside our sample.
\item 234939.7--563723: A close pair of a \mbox{B\,=\,13} star of
spectral type $\sim$K0 and an $\sim$15 mag object is 19\arcsec{} NW,
two faint red objects 18\arcsec{} S. The X-ray source is variable and
could be an AGN or a CV.
\end{description}
\end{document}
