2009A&A...507..159D


Query : 2009A&A...507..159D

2009A&A...507..159D - Astronomy and Astrophysics, volume 507, 159-169 (2009/11-3)

Probing variability patterns of the Fe K line complex in bright nearby AGNs.

DE MARCO B., IWASAWA K., CAPPI M., DADINA M., TOMBESI F., PONTI G., CELOTTI A. and MINIUTTI G.

Abstract (from CDS):

The unprecedented sensitivity of current X-ray telescopes allows the issue of the Fe K line complex variability patterns in bright, nearby AGNs to be addressed for the first time. These kinds of studies have the potential to map the accretion flow in the strong gravity regime of supermassive black holes. We examine XMM-Newton observations of the brightest sources of the FERO sample of radio-quiet type 1 AGNs (for a total of 72 observations) with the aim of characterizing the temporal behaviour of Fe K complex features. A systematic mapping of residual flux above and below the continuum in the 4-9keV range was performed in the time vs. energy domain, with the purpose of identifying interesting spectral features in the three energy bands: 5.4-6.1keV, 6.1-6.8keV, and 6.8-7.2keV, respectively corresponding to the redshifted, rest-frame, and either blueshifted or highly ionized Fe Kα line bands. The variability significance of rest frame and energy-shifted Fe K lines was assessed by extracting light curves and comparing them with Monte Carlo simulations. The time-averaged profile of the Fe K complex revealed spectral complexity in several observations. Red- and blue- shifted components (either in emission or absorption) were observed in 30 out of 72 observations, with an average <EW≳90eV for emission and <EW≳-30eV for absorption features. We detected significant line variability (with confidence levels ranging between 90% and 99.7%) within at least one of the above energy bands in 26 out of 72 observations on time scales of Δt∼6-30ks. The reliability of these features has been carefully calculated using this sample and assessed at ∼3σ confidence level. This work increases the currently scanty number of detections of variable, energy-shifted Fe lines and confirms the reliability of the claimed detections. We found that the distribution of detected features is peaked at high variability significances in the red- and blue- shifted energy bands rather than at rest-frame energies, suggesting an origin in a relativistically modified accretion flow.

Abstract Copyright:

Journal keyword(s): line: profiles - relativity - galaxies: active - X-rays: galaxies

Simbad objects: 34

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Number of rows : 34
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 ESO 113-45 Sy1 01 23 45.7631533440 -58 48 20.808928944   14.08 13.83 13.34   ~ 835 0
2 NGC 526 Sy1 01 23 54.3772245792 -35 03 55.710850788   14.76 14.60 13.46   ~ 315 1
3 NGC 863 Sy1 02 14 33.5604714720 -00 46 00.181845336   14.48 13.81 17.9   ~ 650 0
4 ESO 198-24 Sy1 02 38 19.7164562112 -52 11 32.343907596   15.36 14.17 13.75   ~ 155 0
5 2E 1228 Sy1 05 10 45.5396425152 +16 29 58.180436556   15.6 15.774     ~ 108 1
6 Mrk 1095 Sy1 05 16 11.4092471904 -00 08 59.157166920   14.30 13.92     ~ 849 1
7 UGC 3374 Sy1 05 54 53.6080860768 +46 26 21.624853488   15.37 14.62     ~ 500 2
8 IRAS 05563-3820 Sy1 05 58 02.0566707456 -38 20 04.452162288   16.05 14.98 11.6   ~ 217 0
9 Mrk 79 Sy1 07 42 32.8210670808 +49 48 34.783809768   14.74 14.27     ~ 691 1
10 Mrk 704 Sy1 09 18 25.9971991776 +16 18 19.633269600   14.82 14.20     ~ 259 0
11 Mrk 110 Sy1 09 25 12.8479065576 +52 17 10.386311208   16.82 16.41     ~ 566 0
12 ESO 434-40 Sy2 09 47 40.1332188528 -30 56 55.960779696   14.10 13.69 12.44   ~ 524 0
13 NGC 3227 GiP 10 23 30.5765149296 +19 51 54.282206700   12.61 11.79     ~ 1643 1
14 NGC 3516 Sy1 11 06 47.4632200800 +72 34 07.298374656   13.12 12.40     ~ 1496 0
15 NGC 3783 Sy1 11 39 01.7096819040 -37 44 19.009642992   12.46 13.43 11.33 12.1 ~ 1586 0
16 NGC 4051 Sy1 12 03 09.6101337312 +44 31 52.682601288   11.08 12.92 9.94   ~ 2112 1
17 NGC 4253 Sy1 12 18 26.5163572920 +29 48 46.531535472   14.34 13.57     ~ 1009 1
18 NGC 4593 Sy1 12 39 39.4435107024 -05 20 39.034988448   13.95 13.15     ~ 1042 0
19 ESO 383-35 Sy1 13 35 53.7691256160 -34 17 44.160716796   13.89 13.61 8.9   ~ 1451 0
20 ESO 445-50 Sy1 13 49 19.2601801224 -30 18 34.213815504   13.81 13.66 12.18 12.35 ~ 771 0
21 Mrk 279 Sy1 13 53 03.4348964112 +69 18 29.410910460   15.15 14.46     ~ 735 0
22 NGC 5548 Sy1 14 17 59.5400291832 +25 08 12.603122268   14.35 13.73     ~ 2590 0
23 ESO 511-30 Sy1 14 19 22.4047231584 -26 38 41.134476084   13.32 14.9 12.27 12.7 ~ 138 0
24 NAME OKM2018 SWIFT J1705.1-0148 Sy1 17 05 00.3938346624 -01 32 28.533617196   16.84 15.55 12.1   ~ 57 0
25 LEDA 89032 Sy1 18 47 02.6924542152 -78 31 49.609309728   16.14 15.55 13.2   ~ 90 0
26 ESO 141-55 Sy1 19 21 14.1473895816 -58 40 12.982437480   14.36 13.64 13.28   ~ 345 0
27 Mrk 509 Sy1 20 44 09.7504483224 -10 43 24.727155528   13.35 13.12 10.7   ~ 1224 0
28 NGC 7213 Sy1 22 09 16.2100443720 -47 10 00.115999716   10.97 12.08 10.50 10.6 ~ 635 0
29 ClG J2235-2557 ClG 22 35 20.6 -25 57 42           ~ 144 0
30 NGC 7314 Sy1 22 35 46.1985355872 -26 03 01.564993476   11.62 13.11 10.61 11.4 ~ 547 0
31 UGC 12163 Sy1 22 42 39.3363009144 +29 43 31.302092640   14.86 14.16     ~ 674 1
32 NAME MR 2251-178 Sy1 22 54 05.8858611984 -17 34 55.402233708   14.99 14.36 15.12   ~ 413 3
33 NGC 7469 Sy1 23 03 15.674 +08 52 25.28 12.60 13.00 12.34     ~ 2027 3
34 Mrk 926 Sy1 23 04 43.4776098480 -08 41 08.629476864   16.20 15.91 9.4   ~ 433 0

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2023.02.02-18:21:15

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