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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.

(1)

SY: Seyfert, Q: quasar, NL: narrow line, BL: broad line, NC: not classified.

(2)

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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