1 / 26

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)

lazar
Download Presentation

Non-HBLR S2 and Unified Model of AGNs

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

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. 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 !

More Related