Table 3
Fraction of sources in the FERO sample with a significant relativistic broad Fe Kα line EW detection for different source type and luminosity class.
| Obj. Class/ | Sample | ||
| Luminosity | FERO | Flux Limited | |
| (%) | (%) | ||
|
|
|||
| Sy+QSO | 9 ± 3 (13/149) | 36 ± 14 (11/31) | |
|
|
|||
| Sy | 13 ± 5 (11/82) | 36 ± 15 (10/28) | |
| QSO | ≤ 6 (2/67) | ≤ 92 (1/3) | |
|
|
|||
| NL | 13 ± 9 (4/30) | ≤ 100 (2/4) | |
| BL | 12 ± 6 (7/60) | 35 ± 18 (7/20) | |
|
|
|||
| L1 (Sy+QSO) | 16 ± 7 (8/50) | 44 ± 22 (8/18) | |
| L2 (Sy+QSO) | 10 ± 6 (5/50) | 27 ± 23 (3/11) | |
| L3 (Sy+QSO) | ≤ 2 (0/49) | ≤ 47 (0/2) | |
|
|
|||
| L Sy | 10 ± 7 (4/40) | 18 ± 14 (3/17) | |
| L QSO | ≤ 10 (2/40) | ≤ 92 (1/3) | |
Notes. Sy: Seyfert galaxy, QSO: quasar; NL: narrow line, BL: broad line; L1: LX < 0.25 × 1044 erg s-1; L2: 0.25 × 1044 < LX < 1.20 × 1044 erg s-1; L3: LX > 1.20 × 1044 erg s-1, where L1, L2 and L3 were chosen to contain the same number of sources (~50); L: 0.15 × 1044 < LX < 2.69 × 1044 erg s-1, L was chosen to contain the same number of Seyfert galaxy and quasars (40) (see text for details).
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