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The AGN Obscuring Torus. Moshe Elitzur University of Kentucky & LAOG, Grenoble. Happy Birthday, young man!. optical depth. zone #. t z = t t. z. t z-1. t i. ij = | i – j |. i. i,i-1 T i C i p i n i1 n i2. t i-1. t 2. 2. t 1. 1. C oupled E scape
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The AGN Obscuring Torus Moshe Elitzur University of Kentucky & LAOG, Grenoble
optical depth zone # tz = tt z tz-1 ti ij= |i – j| i i,i-1 Ti Ci pi ni1 ni2 ti-1 t2 2 t1 1 Coupled Escape Probability t0 = 0
2-level Atom = 10-3 : Slab t = 500 Semi-infinite Atmosphere (10-3 107) Elitzur & Asensio Ramos 2006, MNRAS 365, 779
Unified Scheme for AGN Toroidal Obscuration Required by Unification Schemes
Torus Properties 0 • From the statistics of type 1 vs type 2: H/R ~ 1 (Schmitt et al ’01) • R = ? Must rely on IR emission General folklore: R 100 pc
Origin of the 100’s pc Torus – Modeling IR emission Pier & Krolik 93 Pier & Krolik 92 5-10 pc ~100 pc • Granato et al ’94, ‘97: • Uniform density • Rout ~ 100 – 300 pc • = 45° 0 • Dearth of IR emission in smooth-density models T r
Observations – NGC 1068, CO Schinnerer et al ’00 at R ~ 70 pc, H ~ 9 – 10 pc H/R ~ 0.15
Observations – NGC 1068, CO & H2 20 pc 140 pc Galliano et al ’03: H/R ~ 0.15
0 IR – Observations • NGC1068: 2m imaging – R ~ 1 pc (Weigelt et al 04) 10m interferometry – R ~ 2 pc (Jaffe et al 04) • Cen A: 2m – R < 0.5 pc (Prieto et al 04) 9 & 10m – R ~ 1.5 pc (Karovska et al 03) • Circinus: 2m – R ~ 1pc (Prieto et al 04) 8 & 18m – R < 2 pc (Packham et al 05) • NGC1097 & NGC5506: 2m – R < 5 pc (Prieto et al 04)
VLTI – NGC1068: Jaffe et al ‘04 r 1.7 pc: T = 320 K Poncelet et al ‘06 The Torus Size Crisis • Observations – compact (pc-size) torus • Theory – extended (100’s pc) torus Lbol = 2·1045 erg s-1(Mason et al ’06) T(r = 2pc) = 960 K r(T = 320 K) = 26 pc r(T = 226 K) = 57 pc
Temperature in Clumpy Medium Tmax Tmin Nenkova et al 2006
Temperature–Distance Relation 0 • Smooth density – T & R uniquely related • Clumpy density – different T at same R different R, same T
0 AGN Clumpy Torus: Size Effect Ri = 0.9pc L½12Y = Ro/Ri N N0r-q exp(-2/2) N0 = 5 = 45º V = 60 Clumping solves the compact emission problem!
Dynamic Origin of Vertical Structure Cloud accretion from the galaxy? No need in a compact torus!
0 The Torus as a Disk-Wind Region Bottorff et al 97
0 Unification Scheme
masers BLR Torus BAL 0 Grand Unification Scheme Emmering, Blandford & Shlosman 92
Cloud Properties in Torus-Wind Size – shear resistance: Density: Mass: Magnetic field: Elitzur & Shlosman 2006
Water Masers – Glimpse of Torus Clouds? NGC 3079 Kondratko, Greenhill & Moran ‘05 High-latitude features – disk rotational imprint: uplifted clouds
Outflow and Accretion Torus disappearance at L 1043 erg s-1 ! Narrow-line Seyfert 1 radio galaxies? Chiaberge et al ’99; Whysong & Antonucci ‘04
Conclusions • No bagel • ToroidalObscurationRequiredbyUnifiedScheme– just a region in the disk-wind