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Non-HBLR S2 and Unified Model of AGNs

Non-HBLR S2 and Unified Model of AGNs. Zhang Enpeng Wang Jianmin 04. 22. 2006. Outline. Introduction Data and analysis Conclusion. I Introduction Carl Seyfert (1943) ( --- Seyfert galaxies)

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Non-HBLR S2 and Unified Model of AGNs

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  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. S1, S2 are the same objects The torus is (1) face-on : S1. (2) edge-on : S2. • Broad- line photons are scattered into the line of sight by free electron . S2 has HBLR

  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. S2 HBLS2 Non-HBLS2 S1 • Tran (2003)

  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 lessMBH , 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. ( MBH, accretion rates , AGN strength). (2) Anisotropic parameters should different (orientation indicator)

  12. 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)

  13. II Comparison of properties of NLS1s and non-HBLR S2 (1) Mass of black hole (and accretion rate ):.  = FWHM[O III]/2.5/1.34 the similarity means they are in the same (early ) stage of evolution.

  14. Host galaxy

  15. halo bulge thin disk thick disk nucleus (2) Potential isotropic properties • Indicators of AGN strength 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 = 350 0 L[O III]

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

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

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

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

  22. Non-HBLS2 absorbed HBLS2 NLS1 BLS1 unabsorbed Non-HBL S2 (NH< 1022 cm-2 ) added Suggested evolution consequence for Seyfert Galaxies: Unabsorbed Non-HBLS2

  23. Thanks !

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