2005MNRAS.364..208D


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.19CEST13:51:33

2005MNRAS.364..208D - Mon. Not. R. Astron. Soc., 364, 208-216 (2005/November-3)

Scaling variability from stellar to supermassive black holes.

DONE C. and GIERLINSKI M.

Abstract (from CDS):

We investigate the correspondence between the variability seen in the stellar and supermassive black holes. Galactic black hole (GBH) power density spectra (PDS) are generally complex, and dependent on spectral state. In the low/hard state the high-frequency rollover in the PDS moves in a way which is not simply related to luminosity. Hence this feature can only be used as an approximate indicator rather than as an accurate tracer of black hole mass in active galactic nuclei (AGNs). The X-ray spectrum in the high/soft state is dominated by the disc in the GBH, which is rather stable. We show that the PDS of the Comptonized tail in GBHs can be much more variable, and that it is this which should be compared to AGNs due to their much lower disc temperature. This bandpass effect removes a problem in interpreting the (often highly variable) narrow-line Seyfert 1 (NLS1) galaxies as the counterparts of the high mass accretion rate GBHs. Additionally, we speculate that some NLS1s (e.g. Akn 564) are counterparts of the very high state. The Comptonized tail in this state is also highly variable, but with PDS which can be roughly described as band-limited noise. This shape is similar to that seen in the low/hard state, so merely seeing such band-limited noise in the power spectrum of an AGN does not necessarily imply low luminosity. We also stress that Cygnus X-1, often used for comparison with AGNs, is not a typical black hole system due to its persistent nature. In particular, the shape of its power spectrum in the high/soft state is markedly different from that of other (transient) GBH systems in this state. The fact that the NLS1s NGC 4051 and MCG -6-30-15 do appear to show a power spectrum similar to that of the high/soft state of Cyg X-1 may lend observational support to theoretical speculation that the hydrogen ionization disc instability does not operate in AGNs.

Abstract Copyright: 2005 The Authors. Journal compilation © 2005 RAS

Journal keyword(s): accretion, accretion discs - X-rays: binaries - X-rays: galaxies

Simbad objects: 15

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Number of rows : 15

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 ESO 113-45 Sy1 01 23 45.7630391439 -58 48 20.811630442   14.08 13.83 13.34   ~ 788 0
2 NGC 3516 Sy1 11 06 47.4596406816 +72 34 07.189563769   13.12 12.40     ~ 1439 0
3 NGC 3783 Sy1 11 39 01.7095761008 -37 44 19.008597647   12.46 13.43 11.33 12.1 ~ 1503 0
4 NGC 4051 Sy1 12 03 09.6098828919 +44 31 52.693714606   11.08 12.92 9.94   ~ 2035 1
5 NGC 4151 Sy1 12 10 32.5771747733 +39 24 21.057727323   12.18 11.48     ~ 3442 2
6 NGC 4253 Sy1 12 18 26.5155239433 +29 48 46.518670434   14.34 13.57     ~ 952 1
7 M 106 Sy2 12 18 57.620 +47 18 13.39   9.14 8.41 8.11   ~ 2180 3
8 NGC 4395 Sy2 12 25 48.8639154223 +33 32 48.694684028 10.84 10.54 10.11 9.98   ~ 1027 1
9 ESO 383-35 Sy1 13 35 53.7686909139 -34 17 44.139127597   13.89 13.61 8.9   ~ 1400 0
10 NGC 5548 Sy1 14 17 59.5401093128 +25 08 12.600227883   14.35 13.73     ~ 2451 0
11 V* V381 Nor HXB 15 50 58.6520652623 -56 28 35.309070422   17.95 16.6     K3III 1062 0
12 [GHJ2008] 3 HXB 16 50 00.980 -49 57 43.60     11.89     K4V 358 0
13 Granat 1915+105 HXB 19 15 11.55576 +10 56 44.9052           ~ 2361 0
14 HD 226868 HXB 19 58 21.6758193269 +35 12 05.782512305 9.38 9.72 8.91 8.42   O9.7Iabpvar 3997 0
15 UGC 12163 Sy1 22 42 39.3364258078 +29 43 31.301194419   14.86 14.16     ~ 632 1

    Equat.    Gal    SGal    Ecl

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