Table 5.
Expected number of Compton thick AGN (i.e., sources having column density NH > 1024 cm−2) in each of the planned AXIS and ATHENA surveys.
| AXIS |
ATHENA |
||||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Whole sample |
> 100 net counts |
Whole sample |
> 100 net counts |
||||||||||||
| Survey | All |
z > 3 |
All | z > 3 | All |
z > 3 |
All | z > 3 | |||||||
| nsrc | Llim | nsrc | Llim | nsrc | nsrc | nsrc | Llim | nsrc | Llim | nsrc | nsrc | ||||
| Deep | 850 | 37.0 | 62 | 41.6 | 452 | 31 | 4476 | 38.1 | 218 | 43.8 | 2821 | 131 | |||
| Intermediate | 4396 | 37.8 | 268 | 42.3 | 335 | 10 | – | – | – | – | – | – | |||
| Wide | 6113 | 38.9 | 172 | 44.5 | 69 | 0 | 7236 | 38.5 | 236 | 44.2 | 594 | 0 | |||
Notes. We report both the overall results and the number of sources for which more than 100 0.5–7 keV net counts are detected, thus making possible a reliable X-ray spectral analysis. The logarithm of the 0.5–2 keV luminosity is computed using the spectral model described in Sect. 5.3 and a 0.5–2 keV flux corresponding to the one at which 20% of the survey area is covered (see Table 2).
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