2011A&A...527A.127M


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.21CET05:47:32

2011A&A...527A.127M - Astronomy and Astrophysics, volume 527A, 127-127 (2011/3-1)

Broad iron emission lines in Seyfert galaxies - re-condensation of gas onto an inner disk below the ADAF?

MEYER-HOFMEISTER E. and MEYER F.

Abstract (from CDS):

The number of strong iron Kα line detections in Seyfert AGN is clearly growing in the Chandra, XMM-Newton and Suzaku era. The iron emission lines are broad, some are relativistically blurred. These relativistic disk lines have also been observed for galactic black hole X-ray binaries. Thermal components found in hard spectra were interpreted as an indication for a weak inner cool accretion disk underneath a hot corona. Accretion in low-mass X-ray binaries (LMXB) occurs during phases of high and low mass accretion rate, outburst and quiescence, soft and hard spectral state, respectively. After the soft/hard transition for some sources a thermal component is found, which can be interpreted as sustained by re-condensation of gas from an advection-dominated flow (ADAF) onto the disk. In view of the similarity of accretion flows around stellar mass and supermassive black holes we discuss whether the broad iron emission lines in Seyfert 1 AGN (active galactic nuclei) can be understood as arising from a similar accretion flow geometry as in X-ray binaries. We derive accretion rates for those Seyfert galaxies for which broad iron emission lines were observed, the ``best candidates'' in the investigations of Miller (2007ARA&A..45..441M) and Nandra et al. (2007MNRAS.382..194N). For the evaluation of the Eddington-scaled rates we use the observed X-ray luminosity, bolometric corrections and black hole masses from the literature. The accretion rates derived for the Seyfert galaxies in our sample are less than 0.1 of the Eddington rate for more than half of the sources. For 107 to 108M black holes in Seyfert 1 AGN this limit corresponds to 0.01 to 0.2M/yr. This documents that the sources probably are in a hard spectral state and iron emission lines can arise from an inner weak accretion disk surrounded by an ADAF as predicted by the re-condensation model. Some of the remaining sources with higher accretion rates may be in a spectral state that is comparable to the ``very high'' state of LMXBs. Our investigation shows that in quite a number of Seyfert AGN the broad iron emission lines may indeed originate in a weak inner disk below the ADAF, close to the black hole, indicating the same accretion flow geometry as recently found for LMXBs. For the accretion history one then concludes that the accretion rates were higher in the outer radii at some earlier time.

Abstract Copyright:

Journal keyword(s): accretion, accretion disks - X-rays: galaxies - black hole physics - galaxies: Seyfert - galaxies: individual: MCG-6-30-15 - galaxies: individual: 1H 0707-495

Simbad objects: 26

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Number of rows : 26

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 863 Sy1 02 14 33.5610949475 -00 46 00.180128181   14.48 13.81 17.9   ~ 548 0
2 Mrk 1506 Sy1 04 33 11.0958197353 +05 21 15.617543663   15.72 15.05 10.08   ~ 1808 2
3 Mrk 1095 Sy1 05 16 11.4093760763 -00 08 59.158774578   14.30 13.92     ~ 752 0
4 4U 0708-49 Sy1 07 08 41.4887418009 -49 33 06.308287663   16.02 15.7 12.7   ~ 410 0
5 Mrk 110 Sy1 09 25 12.8479868736 +52 17 10.386808297   16.82 16.41     ~ 493 0
6 NGC 3227 GiP 10 23 30.57 +19 51 54.3   12.61 11.79     ~ 1495 2
7 NGC 3516 Sy1 11 06 47.4596406816 +72 34 07.189563769   13.12 12.40     ~ 1390 0
8 NGC 3783 Sy1 11 39 01.7095761008 -37 44 19.008597647   12.46 13.43 11.33 12.1 ~ 1446 0
9 NGC 4051 Sy1 12 03 09.6098828919 +44 31 52.693714606   11.08 12.92 9.94   ~ 1954 1
10 NGC 4151 Sy1 12 10 32.5771747733 +39 24 21.057727323   12.18 11.48     ~ 3308 2
11 NGC 4253 Sy1 12 18 26.5155239433 +29 48 46.518670434   14.34 13.57     ~ 912 1
12 NGC 4395 Sy2 12 25 48.8639154223 +33 32 48.694684028 10.84 10.54 10.11 9.98   ~ 957 1
13 NGC 4593 Sy1 12 39 39.4435521178 -05 20 39.035028119   13.95 13.15     ~ 917 0
14 ESO 383-35 Sy1 13 35 53.7686909139 -34 17 44.139127597   13.89 13.61 8.9   ~ 1361 0
15 NGC 5506 AGN 14 13 14.901 -03 12 27.22   15.25 14.38     ~ 971 0
16 NGC 5548 Sy1 14 17 59.5401093128 +25 08 12.600227883   14.35 13.73     ~ 2336 0
17 [GHJ2008] 3 HXB 16 50 00.980 -49 57 43.60           K4V 340 0
18 XTE J1652-453 XB* 16 52 20.330 -45 20 39.99           ~ 41 1
19 V* V821 Ara HXB 17 02 49.3810714542 -48 47 23.163091737 16.20 16.30 15.5     ~ 1705 0
20 NAME Sgr A* X 17 45 40.03599 -29 00 28.1699           ~ 3286 3
21 2MAXI J1753-013 LXB 17 53 28.2897263704 -01 27 06.256526637 15.30 16.73 16.46 16.15 15.64 ~ 266 0
22 [KRL2007b] 312 LXB 18 17 43.537 -33 01 07.80           ~ 136 0
23 HD 226868 HXB 19 58 21.6758193269 +35 12 05.782512305 9.38 9.72 8.91 8.42   O9.7Iabpvar 3849 0
24 Mrk 509 Sy1 20 44 09.7504131334 -10 43 24.724854084   13.35 13.12 10.7   ~ 1094 0
25 UGC 12163 Sy1 22 42 39.3364258078 +29 43 31.301194419   14.86 14.16     ~ 601 1
26 NGC 7469 Sy1 23 03 15.674 +08 52 25.28 12.60 13.00 12.34     ~ 1845 3

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2019.11.21-05:47:32

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