1 Non-HBLR S2 and Unified Model of AGNs Zhang Enpeng Wang Jianmin 04. 22. 2006.

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 s1 S1

(2) FWHM (H) <2000 km s1 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 s1

(2) tend to have less MBH ,

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 ):.

25

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

14

• Host galaxy

15

(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.

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

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-HBLS2absorbed

HBLS2

NLS1 BLS1

?

?

22

23

24

unabsorbed Non-HBL S2 (NH< 1022 cm-2 ) added

Suggested evolution consequence for Seyfert Galaxies:

Non-HBLS2absorbed

NLS1

HBLS2

BLS1

UnabsorbedNon-HBLS2

25

26

Thanks !