J/ApJ/700/1173 Analysis of broad-line regions in AGNs (Zhu+, 2009)
Evidence for an intermediate line region in active galactic nuclei's inner torus
region and its evolution from narrow to broad line Seyfert I galaxies.
Zhu L., Zhang S.N., Tang S.
<Astrophys. J., 700, 1173-1189 (2009)>
=2009ApJ...700.1173Z 2009ApJ...700.1173Z
ADC_Keywords: Active gal. nuclei ; Models ; Line Profiles
Keywords: galaxies: active - galaxies: nuclei - galaxies: structure -
Galaxy: evolution - line: profiles - quasars: emission lines
Abstract:
A two-component model for the broad-line region (BLR) of active
galactic nuclei (AGNs) has been suggested for many years but not
widely accepted. This model indicates that the broad line can be
described with the superposition of two Gaussian components (very
broad Gaussian component (VBGC) and intermediate Gaussian component
(IMGC)) which are from two physically distinct regions, i.e., very
broad line region (VBLR) and intermediate line region. We select a
Sloan Digital Sky Survey sample to further confirm this model and give
a detailed analysis of the geometry, density, and evolution of these
two regions.
Description:
The sample contains 90 objects with clear Hα, Hβ, and
Hγ line profiles that can be decomposed. They are selected by
La Mura et al. (2007ApJ...671..104L 2007ApJ...671..104L) from SDSS 3 based on their Balmer
line intensities.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 123 90 Source properties and decomposition parameters
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See also:
J/ApJ/613/682 : AGN central masses and broad-line region sizes (Peterson+,
2004)
J/ApJ/660/1072 : Unified model of active galactic nuclei (Wang+, 2007)
J/MNRAS/383/581 : Broad-line Balmer decrements in blue AGN (Dong+, 2008)
J/ApJ/690/20 : Models of the AGN and black hole populations (Shankar+, 2009)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq Running sequence number
4- 7 A4 --- --- [SDSS]
8- 17 A10 --- Name Object name (JHHMM+DDMM)
19- 23 F5.3 --- z Redshift from La Mura G., private com. (1)
25- 30 F6.2 10+35W L5100 ? Continuum luminosity at the rest frame
wavelength of 5100Å in units of
1042erg/s (2)
32- 38 F7.2 10+5Msun BHMass ? Black hole mass in 105M☉ units (2)
40- 45 F6.2 --- Ha.b ? Hα lines: Hb (height of the VBGC (very
broad Gaussian component))
47- 51 F5.1 --- Ha.i ? Hα lines: Hi (height of the IMGC
(intermediate Gaussian component))
53- 56 I4 km/s W(Ha) ? Hα lines: FWHM
58- 61 I4 km/s Wb(Ha) ? Hα lines: FWHM of broad component
63- 66 I4 km/s Wi(Ha) ? Hα lines: FWHM of intermediate comp.
68- 73 F6.2 --- Hb.b ? Hβ lines: Hb (height of the VBGC)
75- 80 F6.2 --- Hb.i ? Hβ lines: Hi (height of the IMGC)
82- 85 I4 km/s W(Hb) ? Hβ lines: FWHM
87- 90 I4 km/s Wb(Hb) ? Hβ lines: FWHM of broad component
92- 95 I4 km/s Wi(Hb) ? Hβ lines: FWHM of intermediate comp.
97-102 F6.2 --- Hg.b ? Hγ lines: Hb (height of the VBGC)
104-108 F5.2 --- Hg.i ? Hγ lines: Hi (height of the IMGC)
110-113 I4 km/s W(Hg) ? Hγ lines: FWHM
115-118 I4 km/s Wb(Hg) ? Hγ lines: FWHM of broad component
120-123 I4 km/s Wi(Hg) ? Hγ lines: FWHM of intermediate comp.
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Note (1): Reshifts in this column are not associated with the good SDSS
identifications. This mix-up parameter does not affect the other data.
Note (2): From La Mura et al. 2007ApJ...671..104L 2007ApJ...671..104L
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 26-Jul-2011