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Table 11

Summary.

Name Type log   Lsoft log   Lhard log   MBH Lbol/LEdd Variability T HR
(0.5–2 keV) (2–10 keV) SMF0 SMF1 SMF2 (Years)
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)

NGC 1052 (X) AGN 41.04 41.52 8.07 7.2 × 10-4 ME2PL Nor m 2 N H2 8
1.9 20% 20% 49% 31% 33%
NGC 3226 (X,C) AGN 40.78 41.01 8.22 1.6 × 10-4 2PL N H2 Nor m 2 1
1.9 37% 81% 93% 57%
NGC 4261 (X) AGN 40.98 41.02 8.96 2.9 × 10-5 ME2PL 8
2 0% 0% 0%
(C) ME2PL 6
0% 0% 19%
NGC 4278 (C) AGN 39.80 39.75 8.46 5.0 × 10-6 MEPL Nor m 2 1
1.9 26% 29% 30% 40%*
NGC 4552 (X,C) AGN 39.49 39.45 8.84 1.0 × 10-6 MEPL Nor m 1 Nor m 2 2
2 73% 63% 93% 78%
NGC 5846 (X) Non-AGN 40.29 39.33 8.49 1.8 × 10-6 MEPL 7
2 0% 0% 1%
(C) MEPL 0.6
0% 0% 6%

Notes.Name, and the instrument in parenthesis (Col. 1), type (Col. 2), logarithm of the soft (0.5–2 keV) and hard (2–10 keV) X-ray luminosities, where the mean was calculated or Chandra luminosity was given when both instruments were used, and percentages in flux variations (Cols. 3 and 4), black-hole mass in logarithmical scale, from González-Martín et al. (2009a) (Col. 5), Eddington ratio, calculated from Eracleous (2010) using Lbol = 33  L2−10  keV (Col. 6), best fit for the SMF0 (Col. 7), parameter varying in SMF1, with the percentage of variation (Col. 8), parameter varying in SMF2, with the percentage of variation (Col. 9), the sampling timescale for variations (Col. 10), and variations in the hardness ratios (Col. 11).

(*)

For all Chandra data. With useful spectroscopic data variations are 4%.

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