Table 3.
Number of high-redshift sources detected in each AXIS simulation, and logarithm of the 0.5–2 keV luminosity corresponding to the flux at which 20% of the survey area is covered, see Table 2, at different high-z thresholds.
| Gilli et al. (2007) mock |
Vito et al. (2014) mock |
|||||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| AXIS Survey | z > 3 |
z > 4 |
z > 5 |
z > 6 |
z > 7 |
z > 3 | z > 4 | z > 5 | z > 6 | z > 7 | ||||||
| nsrc | Llim | nsrc | Llim | nsrc | Llim | nsrc | Llim | nsrc | Llim | nsrc | nsrc | nsrc | nsrc | nsrc | ||
| Deep | 127 | 41.1 | 27 | 41.3 | 7 | 41.5 | 2 | 41.7 | 1 | 41.9 | 343 | 63 | 15 | 8 | 3 | |
| Intermediate | 1066 | 41.8 | 200 | 42.1 | 61 | 42.3 | 11 | 42.5 | 2 | 42.6 | 1948 | 389 | 103 | 29 | 8 | |
| Wide | 5997 | 42.9 | 966 | 43.2 | 127 | 43.4 | 16 | 43.6 | 11 | 43.7 | 6690 | 1291 | 321 | 63 | 23 | |
Notes. The number of detections are computed rescaling the numbers obtained in the simulations to the survey proposed area (2.5 deg2 for the 300 ks, intermediate-area survey and 50 deg2 for the 15 ks, wide-area survey). On the left, we report the results obtained using the Gilli et al. (2007) mock, while on the right we report the results obtained using the Vito et al. (2014) mock (more details in the text).
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