The Broad Line Region - An Innermost Torus

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1 The Broad Line Region - An Innermost Torus (+ the inevitable radio emission of AGN) Alexei Baskin & Ari Laor

1995 Proga & Kallman 2004 Too compact. 100Rg vs.

2 What is the Origin of the BLR? Line driven wind Shlosman, Vitelo & Shaviv 1985 Murray et al Proga & Kallman 2004 Too compact. 100Rg vs. 10,000R MHD driven wind Emmering, Blandford & Shlosman 1992 Konigl & Kartje 1994 Everett 2005 Assumed solution. Not predictive

3 Czerny & Hryniewicz 2011 A failed dusty disk wind? Illuminated dust sublimation BLR Correct absolute size Correct luminosity dependence Unavoidable Correct CF? Predictions? Need to work out the details AD atmosphere dust sublimation

4 Very different from the regular torus models Vertical support Local accretion disk IR versus UV/X-ray illumination (assuming initially thick) Size The innermost torus, pc versus The regular torus, 1-10 pc Symeonidis+ (2016) Emission NIR - hot dust, 3-5µm versus MIR - warm dust µm

5 What is the predicted size of the BLR? Outer radius set by dust sublimation due to Lbol L bol 4 R 2 out =4 T 4 sub! R out =0.2L 1/2 bol,46 pc Predicted: Netzer & Laor (1993), Observed: Suganuma et al. (2006) Inner radius set by dust sublimation at the disk surface 3 8 GMṀ R 3 in =4 T 4 sub! R in =0.006L 1/2 opt,45 pc Predicted: Czerny & Hryniewicz (2011), Observed:? Reverberation mapping results: R BLR =0.1L 1/2 bol,46 pc

How thick is the inner torus? F apple c F = 3 8 GMṀ R 3 h GM h R 3 3 8 GMṀ R 3 apple c = GMh R 3 R What is kappa?

6 How thick is the inner torus? F apple c F = 3 8 GMṀ R 3 h GM h R GMṀ R 3 apple c = GMh R 3 R What is kappa? The $100K question h = 3 8 Ṁapple c For electron scattering apple es =0.4 > h is constant For dust, depends on grain composition, grain size, wavelength

7 What is Tsub? Guhathakurta & Draine (1989) At BLR density ~10 11 Graphite K Silicate K Only graphites survive at the BLR

8 What is Tgrain? At RBLR Only large grains survive

9 What is the wavelength dependence of κ? A sharp rise with TBB Graphites win again κ can reach ~ 100 But, this is for MRN (Galactic dust) The illuminating radiation

10 What happen to κ when small grains are gone? UV IR κ sharply drops in the UV, but increases in the IR Have the cake, and eat it too! Line suppression is gone (UV absorption) But vertical disk support remains (IR absorption)

11 So, grain size distribution doesn t matter in the IR Volume absorption, rather than surface absorption The winner is the gas metallicity Since dust/gas ~ Z

12 What happens when the dust sees the real light? R BLR Radiation acceleration stop at h, When L bol 4 R 2 cos > 4 T 2 sub the grains sublimate right away (<1h). The implied maximal height but maximal height is reached when v=0 h = 16 R3 4 T 2 sub L bol

13 Dynamic Solution No dust BLR 1 µm 0.1 µm L bol = erg/s M = 10 8 M apple = 200 IR 0.01 µm R BLR BLR =0.15L 1/3 bol,45 2/3 apple 2/

$sublimation radius To explain observed type-ii AGN fraction, it is required that outflow gas is extended to larger$

15 Namekata & Umemura (2016) Contrary to Krolik (2007), the radiation pressure by IR photons is not effective to thicken the disc, but rather compresses it. Thus, it seems difficult for a radiation-supported, geometrically thick, obscuring torus to form near the dust sublimation radius To explain observed type-ii AGN fraction, it is required that outflow gas is extended to larger radii (r>10 pc) or that a denser dusty wind is launched from smaller radii (r 10 4 Rg).

16 Conclusions 1. The BLR forms an inner torus with CF ~ The illuminated side produces the BEL. 3. The back side is a source of the hot dust IR Predictions: BLR (L/L Edd ) 1/3, BLR Z 2/3 What about obscuration?

17 The inevitable radio emission of photoionized gas free-free ~ n 2 T 1/2 may be detectable at GHz Symeonidis (2016) Elvis et al. (1994) free-free Weak (<0.1mJy) but inevitable, and unobscurable

18 The Lradio vs L[O III] relation in RQ AGN Cloudy model results Free-free may be detectable in some objects already at 5 GHz. Xu, Livio & Baum (1999) Spatially resolve the NLR at 50 mas on the VLA at 45 GHz

19 The BLR at micro arc sec resolution

Hot dust, warm dust and star formation in NLS1s

Hot dust, warm dust and star formation in NLS1s Tel Aviv University E-mail: rivay@wise.tau.ac.il Hagai Netzer Tel Aviv University We present the results of a detailed investigation of the near- to far-infrared continuum emission of a large sample of