Presentation on theme: "1 Non-HBLR S2 and Unified Model of AGNs Zhang Enpeng Wang Jianmin 04. 22. 2006."— Presentation transcript:
1 Non-HBLR S2 and Unified Model of AGNs Zhang Enpeng Wang Jianmin 04. 22. 2006
2 Outline Introduction Data and analysis Conclusion
3 I Introduction Carl Seyfert (1943) ( --- Seyfert galaxies) Seyfert galaxies were divided into two classes. (Khachikian & Weedman 1974). (1) FWHM (H ) > 2000 km s 1 S1 (2) FWHM (H ) <2000 km s 1 S2
4 Antonucci & Miller (1985) discovered the polarized broad lines in NGC1068. evidence of the existence of a geometrically and optically thick “torus”.
5 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.
6 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” ) ?
8 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).
9 (3) Related the absence of BLR to low Eddington ratios: (Nicastro 2003)
10 Compared with other sub-class without BLR ---Narrow-line S1s : ( 1) FWHM (H ) < 2000 km s 1 (2) tend to have less M BH, super-Eddington accretion rate. (3) pole-on orientation
11 If non-HBLR S2s are the counterpart of NLS1 viewed at larger angles, (1) Isotropic parameters should have same distributions. ( M BH, accretion rates, AGN strength). (2) Anisotropic parameters should different (orientation indicator)
12 样本选择 （ 1 ）红移 z< 0.05 (2) N H 10 22 cm -2 (absorbed non-HBLR S2) N H < 10 22 cm -2 (unabsorbed non-HBLR S2)
13 II Comparison of properties of NLS1s and non-HBLR S2 (1) Mass of black hole (and accretion rate ):. the similarity means they are in the same (early ) stage of evolution. = FWHM [O III] /2.5/1.34
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