1 Non-HBLR S2 and Unified Model of AGNs Zhang Enpeng Wang Jianmin

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” ) ?

7 Tran (2003) Non-HBLS2 HBLS2 S1 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  cm -2 (absorbed non-HBLR S2) N H < 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

14 Host galaxy

15 (2) Potential isotropic properties Indicators of AGN strength thick disk thin disk bulge nucleus halo The [O III] emission is on scale much larger than the torus.

16 The [O III] luminosities are corrected for extinction. (H  /H  ) 0 =2.8

17 Accretion rate L b o l = L [O III]

18 2 Other indicators of AGN strength. Radio emission from the core (within  100pc) can appears as potential isotropic property.

19 There remains controversial issue on the origin of the infrared emission in Seyfert galaxies, Far-infrared Emission

20 3 Potential anisotropic properties Indicators of orientation: The ratio becomes larger with the inclination

21 Suggested Scheme : S1 S2 Non-HBLS2 absorbed HBLS2 NLS1 BLS1 ? ?

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24 unabsorbed Non-HBL S2 (N H < cm -2 ) added Suggested evolution consequence for Seyfert Galaxies: Non-HBLS2 absorbed NLS1 HBLS2 BLS1 Unabsorbed Non-HBLS2

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26 Thanks !