Non hblr s2 and unified model of agns
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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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Non hblr s2 and unified model of agns

Non-HBLR S2 and Unified Model of AGNs

Zhang Enpeng

Wang Jianmin

04. 22. 2006


Outline

Outline

  • Introduction

  • Data and analysis

  • Conclusion


Non hblr s2 and unified model of agns

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


Non hblr s2 and unified model of agns

  • Antonucci & Miller (1985) discovered the polarized broad lines in NGC1068 .

  • evidence of the existence of a geometrically and optically thick “torus”.


Non hblr s2 and unified model of agns

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


Non hblr s2 and unified model of agns

  • 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” ) ?


Non hblr s2 and unified model of agns

S2

HBLS2

Non-HBLS2

S1

  • Tran (2003)


Non hblr s2 and unified model of agns

  • 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).


Non hblr s2 and unified model of agns

(3) Related the absence of BLR to low Eddington ratios: (Nicastro 2003)


Non hblr s2 and unified model of agns

  • 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


Non hblr s2 and unified model of agns

  • 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)


Non hblr s2 and unified model of agns

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)


Ii comparison of properties of nls1s and non hblr s2

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.


Non hblr s2 and unified model of agns

  • Host galaxy


2 potential isotropic properties

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.


Non hblr s2 and unified model of agns

  • The [O III] luminosities are corrected for extinction.

(H/H)0=2.8


Non hblr s2 and unified model of agns

  • Accretion rate

    L b o l = 350 0 L[O III]


2 other indicators of agn strength

2 Other indicators of AGN strength .

  • Radio emission from the core (within 100pc) can appears as potential isotropic property.


Non hblr s2 and unified model of agns

  • Far-infrared Emission

There remains controversial issue on the origin of the infrared emission in Seyfert galaxies,


3 potential anisotropic properties

3 Potential anisotropic properties

The ratio becomes larger with the inclination

  • Indicators of orientation:


Non hblr s2 and unified model of agns

S2

Non-HBLS2

absorbed

HBLS2

?

NLS1

BLS1

?

S1

Suggested Scheme :


Non hblr s2 and unified model of agns

Non-HBLS2

absorbed

HBLS2

NLS1

BLS1

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

Suggested evolution consequence for Seyfert Galaxies:

Unabsorbed

Non-HBLS2


Non hblr s2 and unified model of agns

Thanks !


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