J/ApJ/618/L83 Narrow iron Kα lines in AGN (Zhou+, 2005)
Narrow iron Kα lines in active galactic nuclei: evolving populations.
Zhou X.-L., Wang J.-M.
<Astrophys. J., 618, L83-L86 (2005)>
=2005ApJ...618L..83Z 2005ApJ...618L..83Z (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; X-ray sources ; Spectroscopy
Keywords: galaxies: active - line: profiles
Abstract:
We assemble a sample consisting of 66 active galactic nuclei (AGNs)
from the literature (Page et al., 2004MNRAS.347..316P 2004MNRAS.347..316P) and from the
XMM-Newton archive in order to investigate the origin of the 6.4keV
narrow iron Kα line (NIKAL). The X-ray Baldwin effect of the
NIKAL is confirmed in this sample.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 82 66 The XMM-Newton sample of AGNs
refs.dat 63 24 References
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See also:
B/xmm : XMM-Newton Observation Log (XMM-Newton SOC, 2002)
J/ApJ/613/682 : AGN central masses and broad-line region sizes (Peterson+ 2004)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 15 A15 --- Name Source name
17- 18 A2 --- n_Name [ab ] Note on Name (1)
20- 25 F6.4 --- z Redshift
27- 30 A4 --- Type Source type (2)
32- 36 F5.2 [10-7W] logLbol ? Log of the Bolometric luminosity in erg/s
38 A1 --- f_logLbol Flag on logLbol (3)
40- 44 I5 km/s FWHM ? The Full-Width at Half-Maximum for Hβ
46 A1 --- f_FWHM [c] If full width at half maximum for the
CIV line (1549Å)
48- 51 F4.2 [solMass] logMbh ? Log of the Black Hole mass
53 A1 --- f_logMbh Method for estimate of logMbh (4)
55- 59 F5.2 [-] logce ? Log of the Eddington ratio (5)
61- 65 A5 --- r_logLbol References for optical data
67- 71 F5.2 [10-7W] logLX Log of the rest frame 2-10keV band luminosity
in erg/s
73 A1 --- l_EW Limit flag on EW
74- 76 I3 eV EW Rest frame equivalent width (6)
78- 80 I3 eV e_EW ? Uncertainty in EW
82 I1 --- r_logLX References for X-ray data
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Note (1): Note on Name, defined as follows:
a = Broad line is statistically required in the rest frame band of 2-10keV;
b = Multiple narrow Gaussians in the rest-frame band of 2-10keV.
Note (2): Source type, defined as follows:
NLS1 = narrow-line Seyfert 1 galaxy;
BLS1 = broad-line Seyfert 1 galaxy;
RLQ = radio-loud quasar;
RQQ = radio-quiet quasar.
Note (3): Method for estimates of bolometric luminosity.
R = relation of Lbol=9λLlambda(5100Å) (Kaspi et al.
2000ApJ...533..631K 2000ApJ...533..631K, Netzer 2003ApJ...583L...5N 2003ApJ...583L...5N);
F = spectral energy distribution fitting;
I = flux integration.
Note (4): Method for estimates of black-hole masses
M = reverberation mapping measurement;
R = the empirical reverberation relation;
S = Single-epoch mass determination method:
Mbh/M☉=4.82x106[λLλ,44(5100Å)]0.7*(V3)2
where V3=FWHM(Hbeta)/(10+3km/s) (Vestergaard, 2002ApJ...571..733V 2002ApJ...571..733V);
N = relation for narrow line region size,
RNLR=1.15LHβ,420.49kpc (Netzer et al. 2004ApJ...614..558N 2004ApJ...614..558N);
V = measurements of the central velocity gradient, taken from Schulz et al.
(1994A&A...288..425S 1994A&A...288..425S)
Note (5): Eddington ratio, ce=Lbol/LEdd, where LEdd=1.26x1038Mbh)
Note (6): Of neutral narrow Fe Kα line at 90% error confidence (eV).
The XMM-Newton PN data only are used. As described in Page et al.
2004MNRAS.347..316P 2004MNRAS.347..316P, the spectral fittings are performed via a model
of a simple power law over the rest frame band of 2-10keV modified by
the Fe Kα edge. If there was evidence for the emission of broad
line, a broad Gaussian model is included. Then a narrow Gaussian (the
intrinsic width is fixed at 10eV) is added for the EW measurements.
The neutral reflection component (pexrav in XSPEC, see Magdziarz &
Zdziarski, 1995MNRAS.273..837M 1995MNRAS.273..837M) is also tried for each spectrum.
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ref Reference number
4- 22 A19 --- Bibcode Bibcode
24- 41 A18 --- Aut Author's name
43- 63 A21 --- Com Comment
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 06-Jul-2005