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Table A.1.

Properties of the Swift type 2 and type 1 sources.

Name z log LX log LBOL log LO log MBH
(1) (2) (3) (4) (5) (6)
Type 2 sources
IRAS F 05189−2524 0.0426 43.40 45.26 7.45
2MASX J07595347+2323241 0.0292 43.25 43.95 7.78
MCG -01-24-12 0.0196 43.24 44.18 7.16
NGC 1275 0.0176 43.98 44.74 7.46
Mrk 348 0.0150 43.44 44.24 7.23
Mrk 1210 0.0135 43.13 44.07 6.78
ESO 234-G -050 0.0088 41.60 42.97 6.00
NGC 2992 0.0077 42.00 42.74 6.72
NGC 7465 0.0065 41.97 43.40 6.54
NGC 5506 0.0062 42.99 44.15 6.86
NGC 1365 0.0055 42.32 43.71 6.65
NGC 1052 0.005 41.62 42.55 6.63
NGC 6221 0.0050 41.20 42.64 6.46
NGC 7314 0.0048 42.33 43.26 6.24
NGC 4395 0.0013 40.50 41.43 5.14
PKS 0326−288 0.108 44.52 45.42
NGC 3079 0.0372 41.30 42.75
Mrk 417 0.0327 43.73 44.65
NGC 612 0.0298 43.94 44.76
NGC 788 0.0136 43.02 43.76
NGC 3281 0.0107 43.12 44.23
NGC 4388 0.0084 43.05 43.98
ESO 005−G004 0.0062 42.78 43.95
NGC 5643 0.004 42.43 43.60
NGC 4941 0.0037 41.25 42.18
NGC 4138 0.003 41.23 42.49

Type 1 sources
Mrk 876 0.129 44.19 45.34 8.54
Mrk 1383 0.087 44.19 45.42 44.89 9.31
Mrk 771 0.063 43.60 45.01 7.94
Mrk 509 0.034 44.08 44.99 44.48 8.08
Mrk 817 0.031 43.49 44.60 44.08 7.90
Mrk 279 0.030 43.41 44.68 44.28 7.59
Mrk 335 0.026 43.24 44.51 44.29 7.21
Mrk 590 0.026 42.70 43.76 7.60
Mrk 79 0.022 43.11 44.18 43.92 8.02
NGC 5548 0.017 43.14 44.21 43.95 7.87
NGC 7469 0.016 43.19 44.42 44.14 7.42
NGC 4748 0.015 42.34 43.72 6.58
NGC 4253 0.013 42.71 43.77 6.21
NGC 3783 0.010 43.43 44.24 43.37 7.38
NGC 3516 0.009 42.72 43.85 7.59
NGC 4593 0.009 42.81 43.72 7.06
NGC 6814 0.005 42.31 43.64 7.30
NGC 3227 0.004 42.10 43.23 7.45
NGC 4151 0.003 42.31 43.66 43.28 7.66
NGC 4051 0.002 41.33 43.03 6.43

Notes. (1) Source name; (2) redshift (Baumgartner et al. 2013); (3) intrinsic logarithmic hard X-ray luminosity (2–10 keV) in erg s−1 units from Ricci et al. (2017a); (4) SED-fitting derived logarithmic bolometric luminosity in erg s−1 units; (5) B-band 4400 Å AGN logarithmic luminosity in erg s−1 units from the photometric data, provided only for type I sources, because the contamination from the galaxy is negligible; (6) logarithmic MBH in M from Onori et al. (2017b) for the type 2 sources and from Ricci et al. (2017c) for the type 1 sources.

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