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Table 7
Source identification statistics as a function of flux threshold.
| 0.4–2.0 keV | ||||
|
|
||||
| Sample/Flux limit (cgs) | 10-13 | 3 × 10-14 | 10-14 | 5 × 10-15 |
|
|
||||
| All sources | 1 | 15 | 52 | 122 |
| All – extragalactic | 1 | 15 | 52 | 122 |
| Active coronaea | 1 | 12 | 17 | 18 |
| Accreting Candidates | 0 | 2 | 5 | 6 |
| All ids | 1 | 15 | 23 | 25 |
| All ids + stat ids (90%) | 1 | 15 | 39 | 55 |
| All ids + stat ids (50%) | 1 | 15 | 44 | 72 |
| 2.0–10.0 keV | ||||
|
|
||||
| Sample/Flux limit (cgs) | 10-12 | 3 × 10-13 | 10-13 | 5 × 10-14 |
|
|
||||
| All sources | 3 | 10 | 36 | 102 |
| All – extragalacticb | 3 | 7 | 17 | 48 |
| All – extragalacticc | 3 | 9 | 27 | 73 |
| Active coronae | 1 | 1 | 2 | 5 |
| Accreting Candidates | 1 | 4 | 7 | 8 |
| All ids | 2 | 6 | 11 | 15 |
| All ids + stat ids (90%) | 2 | 6 | 12 | 23 |
| All ids + stat ids (50%) | 3 | 7 | 17 | 37 |
Notes.
(a)
The three bright XGPS sources discussed in Sect. 5.5.8 were added to the spectroscopic sample;
(c)
log N(> S) − log S from Mateos et al. (2008)
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