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The AGN Obscuring Torus

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

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  1. The AGN Obscuring Torus Moshe Elitzur University of Kentucky & LAOG, Grenoble

  2. Happy Birthday, young man!

  3. 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

  4. 2-level Atom  = 10-3 : Slab t = 500 Semi-infinite Atmosphere (10-3    107) Elitzur & Asensio Ramos 2006, MNRAS 365, 779

  5. Unified Scheme for AGN Toroidal Obscuration Required by Unification Schemes

  6. 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

  7. 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

  8. Observations – NGC 1068, CO Schinnerer et al ’00 at R ~ 70 pc, H ~ 9 – 10 pc  H/R ~ 0.15

  9. Observations – NGC 1068, CO & H2 20 pc 140 pc Galliano et al ’03: H/R ~ 0.15

  10. 0 IR – Observations • NGC1068: 2m imaging – R ~ 1 pc (Weigelt et al 04) 10m interferometry – R ~ 2 pc (Jaffe et al 04) • Cen A: 2m – R < 0.5 pc (Prieto et al 04) 9 & 10m – R ~ 1.5 pc (Karovska et al 03) • Circinus: 2m – R ~ 1pc (Prieto et al 04) 8 & 18m – R < 2 pc (Packham et al 05) • NGC1097 & NGC5506: 2m – R < 5 pc (Prieto et al 04)

  11. 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

  12. Temperature in Clumpy Medium Tmax Tmin Nenkova et al 2006

  13. Temperature–Distance Relation 0 • Smooth density – T & R uniquely related • Clumpy density – different T at same R different R, same T

  14. 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!

  15. Dynamic Origin of Vertical Structure Cloud accretion from the galaxy? No need in a compact torus!

  16. 0 The Torus as a Disk-Wind Region Bottorff et al 97

  17. 0 Unification Scheme

  18. masers BLR Torus BAL 0 Grand Unification Scheme Emmering, Blandford & Shlosman 92

  19. Cloud Properties in Torus-Wind Size – shear resistance: Density: Mass: Magnetic field: Elitzur & Shlosman 2006

  20. Water Masers – Glimpse of Torus Clouds? NGC 3079 Kondratko, Greenhill & Moran ‘05 High-latitude features – disk rotational imprint: uplifted clouds

  21. Outflow and Accretion Torus disappearance at L  1043 erg s-1 ! Narrow-line Seyfert 1 radio galaxies? Chiaberge et al ’99; Whysong & Antonucci ‘04

  22. Conclusions • No bagel • ToroidalObscurationRequiredbyUnifiedScheme– just a region in the disk-wind

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