Table 5: Previously Known Type 2 AGN, HDF-N.
A03 redshift $\log L_{\rm x}(2{-}8~{\rm keV})$ Notesa
     erg/s  
72 0.936 42.73 m
76 0.637 42.71 m
82 0.681 42.52  
83 0.459 42.41  
90 1.140 43.33  
106 1.017 42.31  
121 0.520 42.27  
122 1.338 42.90 s
127 1.014 43.27 m
142 0.747 42.47  
150 0.762 42.82  
157 1.264 43.89  
158 1.013 43.02  
160 0.847 42.90 m
163 0.485 42.72  
164 0.953 42.92  
170 0.680 42.44  
171 1.995 43.63 m
187 0.847 42.27  
190 2.005 43.76  
191 0.560 42.79 m
201 1.020 42.74 m
217 0.518 42.15  
229 1.487 42.23 s
240 0.961 43.95  
259 1.609 44.48 m
261 0.902 42.15  
267 0.401 42.15  
278 1.023 42.92  
330 3.406 43.43  
352 0.936 42.47  
373 0.475 42.25  
384 1.019 43.45  
390 1.146 44.04 s
398 2.638 44.05 s
405 0.978 42.96  
409 2.240 43.61  
413 0.474 42.60  
439 0.636 42.36  
441 0.634 42.24  
442 0.852 42.33  
448 1.238 43.32  
462 0.511 42.03  
468 0.911 42.39  
a From Barger et al. (2003): s, less secure redshift identification based primarily on a single emission line and the continuum shape; m, complex or multiple structure or possible contamination of the photometry by a nearby brighter object.

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