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I Introduction
• Carl Seyfert (1943) ( --- Seyfert galaxies)
• Seyfert galaxies were divided into two classes. (Khachikian & Weedman 1974) .
(1) FWHM (H) > 2000 km s1 S1
(2) FWHM (H) <2000 km s1 S2
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• Antonucci & Miller (1985) discovered the polarized broad lines in NGC1068 .
• evidence of the existence of a geometrically and optically thick “torus”.
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• Broad- line photons are scattered into the line of sight by free electron . S2 has HBLR
S1, S2 are the same objects The torus is (1) face-on : S1. (2) edge-on : S2.
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• All S2s have HBLR ?
(1) At least 35% of S2s have PBL (Tran 2001; Moran et al. 2000).
(2) Polarimetric surveys of complete samples of S2s suggest up to 50% of these objects have not hidden S1 nucleus.
a class of non-HBLR S2 (“real S2” ) ?
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• Why we can not detect PBLs in some S2s ?
(1) Edge-on line of sight
and hidden of ESR.
(Miller & Goodrich 1990; HLB97)
(2) Some S2s are intrinsically weak and lack of broad line region .
(Tran2001, 2003; Gu & Huang 2002; Laor 2003).
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• Compared with other sub-class without BLR
---Narrow-line S1s :
(1) FWHM (H) < 2000 km s1
(2) tend to have less MBH ,
super-Eddington accretion rate.
(3) pole-on orientation
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• If non-HBLR S2s are the counterpart of NLS1 viewed at larger angles,
(1) Isotropic parameters should have same distributions.
( MBH, accretion rates , AGN strength).
(2) Anisotropic parameters should different
(orientation indicator)
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样本选择 ( 1 )红移 z< 0.05
(2) NH 1022 cm-2 (absorbed non-HBLR S2)
NH< 1022 cm-2 (unabsorbed non-HBLR S2)
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II Comparison of properties of NLS1s and non-HBLR S2
(1) Mass of black hole (and accretion rate ):.
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3 11.464 10
lt-days 10 kmsFWHMBLR
BH
RM M
the similarity means they are in the same (early ) stage of evolution.
= FWHM[O III]/2.5/1.34
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(2) Potential isotropic properties
• Indicators of AGN strength
thick disk
thin diskbulge
nucleus
halo
The [O III] emission is on scale much larger than
the torus.
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2 Other indicators of AGN strength .
• Radio emission from the core (within 100pc) can appears as potential isotropic property.
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There remains controversial issue on the origin of the infrared emission in Seyfert galaxies,
• Far-infrared Emission
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3 Potential anisotropic properties• Indicators of orientation:
The ratio becomes larger with the inclination
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unabsorbed Non-HBL S2 (NH< 1022 cm-2 ) added
Suggested evolution consequence for Seyfert Galaxies:
Non-HBLS2absorbed
NLS1
HBLS2
BLS1
UnabsorbedNon-HBLS2