2010A&A...521A..57T


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.21CEST01:09:02

2010A&A...521A..57T - Astronomy and Astrophysics, volume 521, A57-57 (2010/10-1)

Evidence for ultra-fast outflows in radio-quiet AGNs. I. Detection and statistical incidence of FeK-shell absorption lines.

TOMBESI F., CAPPI M., REEVES J.N., PALUMBO G.G.C., YAQOOB T., BRAITO V. and DADINA M.

Abstract (from CDS):

Blue-shifted FeK absorption lines have been detected in recent years between 7 and 10 keV in theX-ray spectra of several radio-quiet AGNs. The derived blue-shifted velocities of the lines can often reach mildly relativistic values, up to 0.2-0.4c. These findings are important because they suggest the presence of a previously unknown massive and highly ionized absorbing material outflowing from their nuclei, possibly connected with accretion disk winds/outflows. The scope of the present work is to statistically quantify the parameters and incidence of the blue-shifted FeK absorption lines through a uniform analysis on a large sample of radio-quiet AGNs. This allows us to assess their global detection significance and to overcome any possible publication bias. We performed a blind search for narrow absorption features at energies greater than 6.4 keV in a sample of 42 radio-quiet AGNs observed with XMM-Newton. A simple uniform model composed by an absorbed power-law plus Gaussian emission and absorption lines provided a good fit for all the data sets. We derived the absorption lines parameters and calculated their detailed detection significance making use of the classical F-test and extensive Monte Carlo simulations. We detect 36 narrow absorption lines on a total of 101 XMM-Newton EPIC pn observations. The number of absorption lines at rest-frame energies higher than 7keV is 22. Their global probability to be generated by random fluctuations is very low, less than 3x10–8, and their detection have been independently confirmed by a spectral analysis of the MOS data, with associated random probability <10–7. We identify the lines as FeXXV and FeXXVI K-shell resonant absorption. They are systematically blue-shifted, with a velocity distribution ranging from zero up to ∼0.3c, with a peak and mean value at ∼0.1c. We detect variability of the lines on both EWs and blue-shifted velocities among different XMM-Newton observations even on time-scales as short as a few days, possibly suggesting somewhat compact absorbers. Moreover, we find no significant correlation between the cosmological red-shifts of the sources and the lines blue-shifted velocities, ruling out any systematic contamination by local absorption. If we define ultra-fast outflows (UFOs) those highly ionized absorbers with outflow velocities higher than 104km/s, then the majority of the lines are consistent with being associated to UFOs and the fraction of objects with detected UFOs in the whole sample is at least ∼35%. This fraction is similar for type 1 and type 2 sources. The global covering fraction of the absorbers is consequently estimated to be in the range C∼0.4-0.6, thereby implying large opening angles. From our systematicX-ray spectral analysis on a large sample of radio-quiet AGNs we have been able to clearly assess the global veracity of the blue-shifted FeK absorption lines at E>7keV and to overcome their publication bias. These lines indicate that UFOs are a rather common phenomenon observable in the central regions of these sources and they are probably the direct signature of AGN accretion disk winds/ejecta. The detailed photo-ionization modeling of these absorbers is presented in a companion paper.

Abstract Copyright:

Journal keyword(s): black hole physics - X-ray: galaxies - galaxies: Seyfert - line: identification

Simbad objects: 42

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Number of rows : 42

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 Mrk 335 Sy1 00 06 19.5371542746 +20 12 10.617456059   14.19 13.85     ~ 1060 0
2 Ton S 180 Sy1 00 57 20.2038086128 -22 22 56.577563819   14.60 14.34 15.23   ~ 266 0
3 ESO 113-45 Sy1 01 23 45.7630391439 -58 48 20.811630442   14.08 13.83 13.34   ~ 745 0
4 NGC 526 Sy1 01 23 54.3778199024 -35 03 55.695504754   14.76 14.60 13.46   ~ 291 1
5 NGC 863 Sy1 02 14 33.5610949475 -00 46 00.180128181   14.48 13.81 17.9   ~ 546 0
6 ESO 198-24 Sy1 02 38 19.7165906722 -52 11 32.346023872   15.36 14.17 13.75   ~ 135 0
7 LB 1727 Sy1 04 26 00.7188445954 -57 12 01.772037544 13.68 14.58 14.37 14.8   ~ 230 0
8 2E 1228 Sy1 05 10 45.5390847005 +16 29 58.176227369   15.6 15.774     ~ 89 1
9 Mrk 1095 Sy1 05 16 11.4093760763 -00 08 59.158774578   14.30 13.92     ~ 751 0
10 NGC 2110 Sy2 05 52 11.3760694860 -07 27 22.489931610   14.77 13.51 11.86   ~ 559 1
11 UGC 3374 Sy1 05 54 53.6085733702 +46 26 21.625853190   15.37 14.62     ~ 446 2
12 2MASX J05580206-3820043 Sy1 05 58 02.0566732230 -38 20 04.453517461   16.05 14.98 11.6   ~ 196 1
13 Mrk 79 Sy1 07 42 32.8212778143 +49 48 34.787882233   14.74 14.27     ~ 611 1
14 Mrk 704 Sy1 09 18 25.9973268093 +16 18 19.630187097   14.82 14.20     ~ 234 0
15 Mrk 110 Sy1 09 25 12.8479868736 +52 17 10.386808297   16.82 16.41     ~ 492 0
16 ESO 434-40 Sy2 09 47 40.1345889569 -30 56 55.959492708   14.10 13.69 12.44   ~ 475 0
17 NGC 3227 GiP 10 23 30.57 +19 51 54.3   12.61 11.79     ~ 1494 2
18 NGC 3516 Sy1 11 06 47.4596406816 +72 34 07.189563769   13.12 12.40     ~ 1389 0
19 NGC 3783 Sy1 11 39 01.7095761008 -37 44 19.008597647   12.46 13.43 11.33 12.1 ~ 1445 0
20 NGC 4051 Sy1 12 03 09.6098828919 +44 31 52.693714606   11.08 12.92 9.94   ~ 1951 1
21 NGC 4151 Sy1 12 10 32.5771747733 +39 24 21.057727323   12.18 11.48     ~ 3306 2
22 PB 3894 Sy1 12 14 17.6737003918 +14 03 13.182526431   14.46 14.19     ~ 723 0
23 NGC 4253 Sy1 12 18 26.5155239433 +29 48 46.518670434   14.34 13.57     ~ 912 1
24 Mrk 205 Sy1 12 21 44.0723278508 +75 18 38.242986688   15.64 15.24 14.7   ~ 444 0
25 NGC 4507 Sy2 12 35 36.6328010225 -39 54 33.661858548   12.95 13.54 11.70 12.4 ~ 429 0
26 NGC 4593 Sy1 12 39 39.4435521178 -05 20 39.035028119   13.95 13.15     ~ 916 0
27 ESO 323-77 Sy2 13 06 26.1213873662 -40 24 52.594127368   13.58 13.42 12.01   ~ 183 0
28 ESO 383-35 Sy1 13 35 53.7686909139 -34 17 44.139127597   13.89 13.61 8.9   ~ 1361 0
29 ESO 445-50 Sy1 13 49 19.2607281800 -30 18 34.224136831   13.81 13.66 12.18   ~ 717 0
30 Mrk 279 Sy1 13 53 03.4356451470 +69 18 29.410672989   15.15 14.46     ~ 675 0
31 NGC 5506 AGN 14 13 14.901 -03 12 27.22   15.25 14.38     ~ 971 0
32 NGC 5548 Sy1 14 17 59.5401093128 +25 08 12.600227883   14.35 13.73     ~ 2334 0
33 ESO 511-30 Sy1 14 19 22.4042606652 -26 38 41.130443100   13.32 14.9 12.27 12.7 ~ 111 0
34 Mrk 841 Sy1 15 04 01.1935077982 +10 26 15.778741853   14.50 14.27     ~ 574 0
35 Mrk 290 Sy1 15 35 52.4036488201 +57 54 09.516647866   15.55 15.27     ~ 434 0
36 Mrk 509 Sy1 20 44 09.7504131334 -10 43 24.724854084   13.35 13.12 10.7   ~ 1093 0
37 NGC 7172 Sy2 22 02 01.897 -31 52 11.60   12.72 13.61 11.15   ~ 455 1
38 NGC 7213 Sy1 22 09 16.2106632887 -47 10 00.082166299   10.97 12.08 10.50 10.6 ~ 572 0
39 NGC 7314 Sy1 22 35 46.1969940596 -26 03 01.574026329   11.62 13.11 10.61 11.4 ~ 490 0
40 UGC 12163 Sy1 22 42 39.3364258078 +29 43 31.301194419   14.86 14.16     ~ 601 1
41 NGC 7469 Sy1 23 03 15.674 +08 52 25.28 12.60 13.00 12.34     ~ 1843 3
42 NGC 7582 GiP 23 18 23.621 -42 22 14.06 11.62 10.92 10.62     ~ 777 2

    Equat.    Gal    SGal    Ecl

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2019.10.21-01:09:02

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