Table 2
Sources within the FERO sample where a relativistic Fe Kα line is detected with a significance ≥ 5σ.
| Source | Type(1) |
|
Cts2−10 keV | EW | θ | a | β | χ2/d.o.f. | References(2) |
| (1042 erg s-1) | (105 cts) | (eV) | (°) | ||||||
|
|
|||||||||
| IC 4329A | BLSY | 56.4 | 9.123 ± 0.009 | 39 |
28 |
≥ 0.0 | < 1.3 | 238.1/161 | (1), (2), (3), (4) |
| MCG-5-23-16 | NCSY | 14.2 | 8.853 ± 0.009 | 36 |
21 |
≥ 0.0 | < 1.6 | 271.4/162 | (5), (6) |
| ESO511-G030 | NCSY | 22.4 | 1.740 ± 0.004 | 57 |
18 |
≥ 0.0 | < 1.1 | 198.2/161 | |
| MCG-6-30-15 | BLSY | 5.4 | 13.927 ± 0.012 | 260 |
40 |
0.86 |
4.1 |
227.6/161 | (7), (8), (9), (10) |
| NGC 4051 | NLSY | 0.3 | 2.040 ± 0.004 | 260 |
22 |
> 0.46 | 2.9 |
198.8/162 | (11), (12), (13) |
| NGC 3516 | BLSY | 3.6 | 2.810 ± 0.005 | 227 |
27 |
> 0.48 | 2.8 |
223.1/161 | (14), (15), (16) |
| NGC 3783 | BLSY | 11.4 | 9.440 ± 0.010 | 88 |
< 8 | > 0.16 | 2.7 |
304.5/161 | (17), (18) |
| NGC 3227 | BLSY | 1.2 | 3.541 ± 0.006 | 66 |
23 |
≥ 0.0 | 1.9 |
230.9/162 | (19), (20) |
| MRK 509 (*) | BLQ | 103.5 | 7.471 ± 0.009 | 170 |
53 |
0.78 |
> 3.8 | 277.3/158 | (21), (22) |
| MRK 766 (*) | NLSY | 6.1 | 7.816 ± 0.008 | 234 |
20 |
> 0.47 | 2.7 |
300.3/160 | (23), (24) |
| ARK 120 (*) | BLSY | 90.5 | 3.473 ± 0.006 | 140 |
> 59 | ≥ 0.0 | 2.2 |
212.3/158 | (25) |
| 1H0707-495 | NLSY | 46.8 | 0.110 ± 0.001 | 1775 |
54 |
≥ 0.93 | 4.13 |
107.6/116 | (26), (27), (28) |
| PG 1211+143 | NLQ | 49.4 | 0.171 ± 0.001 | 635 |
52 |
≥ 0.92 | > 4.37 | 160.7/139 | (29), (30) |
Notes. (*) 6.7 keV Kα line is preferred; * Sources for which there is a significant detection of a relativistic ionised 6.7 keV Kα line (see text for details). The first 11 sources listed in the table belong to the flux-limited sample. θ, a, and β are the disc inclination angle with respect to the observer, the black hole spin and disc emissivity, respectively, of the best-fit parameters of the Kyrline model. Except for the hard X-ray counts where 1σ errors are given, errors in any given parameter are given at the 90% confidence level. Also, upper and lower limits in any relevant paremeter are given at the 90% confidence level.
References where evidence for a relativistic Fe Kα line for a particular object is reported (references marked in bold) as well as those where alternative scenarios are provided. The list of references is not meant to be complete.
References. (1) Done et al. (2000); (2) McKernan & Yaqoob (2004); (3) Steenbrugge et al. (2005); (4) Gondoin et al. (2001); (5) Reeves et al. (2007); (6) Braito et al. (2007); (7) Wilms et al. (2001); (8) Fabian et al. (2002); (9) Vaughan & Fabian (2004); (10) Miller et al. (2008); (11) Ponti et al. (2006); (12) Uttley et al. (2004); (13) Pounds et al. (2004); (14) Iwasawa et al. (2004); (15) Nandra et al. (1999); (16) Turner et al. (2008); (17) Tombesi et al. (2007); (18) Reeves et al. (2004); (19) Markowitz et al. (2009); (20) Gondoin et al. (2003); (21) Ponti et al. (2009); (22) Page et al. (2003); (23) Pounds et al. (2003b); (24) Miller et al. (2007); (25) Vaughan et al. (2004); (26) Fabian et al. (2009); (27) Fabian et al. (2004); (28) Gallo et al. (2004); (29) Pounds et al. (2003a); (30) Pounds et al. (2009).
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