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Disk-outflow Connection and the Molecular Dusty Torus

Disk-outflow Connection and the Molecular Dusty Torus. Moshe Elitzur University of Kentucky. Unification Scheme for AGN. T oroidal O bscuration R equired by U nification S chemes. M ~ 10 6 – 10 10 M  R s ~ 10 11 – 10 15 cm.

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Disk-outflow Connection and the Molecular Dusty Torus

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  1. Disk-outflow Connection and the Molecular Dusty Torus Moshe Elitzur University of Kentucky

  2. Unification Scheme for AGN Toroidal Obscuration Required by Unification Schemes M~ 106 – 1010 MRs ~ 1011 – 1015 cm Obscuring matter — optically thick dusty clouds Krolik & Begelman ‘88

  3. H Torus Properties — Obscuration • Equatorial V>~ 30  40 • NH>~ 1023 cm-2 f2 — fraction of obscured sources = N2/(N1 + N2) Seyferts: f2 = 70% Schmitt+ ‘01 f2 = 50% Hao+ ‘05 f2 = sin  = 0.5 — 0.7  ≈ 30˚ — 45˚ H/Ro ~ 1

  4. Torus: Direct Evidence

  5. Weigelt+ 04 bispectrum specle interferometry NGC 1068 Jaffe+ 04 VLTI 8-13 m D = 14.4 Mpc 0.1” = 7.2 pc

  6. Torus Size — Observations 0 • NGC1068: 2m imaging – R ~ 1 pc (Weigelt+ 04) 8―13m VLTI – R ~ 2 pc (Jaffe+ 04) • Cen A: 8―13m VLTI – R ~ 0.3 pc (? Meisenheimer+ 07) • Circinus: 2m – R ~ 1 pc (Prieto+ 04)8―13m VLTI – R ~ 1 pc (Tristram+ 08)8 & 18m – R < 2 pc (Packham+ 05) • NGC1097 & NGC5506: 2m – R < 5 pc (Prieto+ 04) All observations are consistent with Rout/Rd no larger than ~2030, and perhaps even only ~510

  7. Torus orientation & the host galaxy 0 • AGN axis (jet) randomly oriented with respect to • galactic disk in Syefert galaxies (Kinney et al 00) • nuclear dust disk in radio galaxies (Schmitt et al 02)

  8. NGC 1068 • Galaxy ~ face on • Torus ~ edge on (≤5º): • H2O masers Gallimore+ 01 • NLR kinematics Crenshaw+ 00

  9. NGC 1068, CO & H2 observations 15º 20 pc 140 pc Galliano et al ’03: H/R ~ 0.15 Schinerer+ 00: at R ~ 70 pc, H ~ 10 pc  H/R ~ 0.15 • Molecular disk outside “the torus” • Disk & torus roughly aligned

  10. NGC 1068, H2 SINFONI observations • Muller Sanchez+ 08: • Infall at ~ 10 pc, no rotation! • Torus size <~ 10 pc

  11. NGC 1068, H2OMasers & 8 GHz Continuum 0.4 pc Gallimore+ 04

  12. What is the Torus? Smooth continuation of the BLR

  13. X-ray Obscuration • Dusty clouds absorb both UV/optical andX-rays • Dust-free clouds absorb only X-rays Risaliti, Elvis & Nicastro 02: Smooth distribution of dusty and dust-free (BLR) clouds

  14. Lag Times ― BLR and near-IR Suganuma et al 06 No correlation with M!!! NIR(K-band) Broad Emission Line • Broad-emission line lags for objects that also have infrared lags • Including Hi & Lo ionization lines) (luminosity) (nucleus) BLR is dust bound (Netzer & Laor 93)

  15. BLR/XOR TOR The Dust-Sublimation Transition Rd r < Rd — dust free clouds:Broad Lines Region/ X-ray Obscuration Region r > Rd — dusty clouds:Toroidal Obscuration Region TOR = Torus

  16. 0 The Disk Wind Paradigm Everett & Konigl ‘00 Bottorff+ 97

  17. masers BLR/XOR TOR WA Toroidal Obscuration Region Broad Lines Region/ X-ray Obscuration Region Warm Absorber Grand Unification Theory 0 Emmering, Blandford & Shlosman 92

  18. Clumpy Torus Modeling • N0 = 5 – 10 clouds •  = 30° – 60° • V= 30 – 120 • q = 1 – 2 • Rd = 0.4L½45 pc; Ro ≥ 5 Rd s N  N0 exp(-2/2)/rq Standard ISM dust works fine Nenkova et al ‘02, ‘08

  19. Cloud Properties in TOR Outflow IR modeling: v ~ 30 – 120  NH ~ 1022 – 1023 cm-2 Resistance to tidal shearing: n > 107M●7 /rpc3 cm-3 Rc < 1016 NH,23 rpc3 /M●7 cm Mc < 7·10-3 NH,23 Rc,162 M B ~ 1.5 1km/s n71/2 mG Elitzur & Shlosman 06

  20. Circinus Water Masers 0.2 pc Greenhill+ 03

  21. Circinus VLTI Imaging Tristram+ 07

  22. Geometry • Clouds rise and expand  • Column density decreases  • Toroidal structure for both BLR, XOR and TOR

  23. TOR Mass Outflow Rate Rd L½ v(Rd) vK(Rd)  (M•/Rd)½  (LEdd/L½)½ Torus should disappear at small L/LEdd!

  24. Torus Disappearance at Low Luminosities • Nucleus visible in FR I radio galaxies (Chiaberge+ 99) • … and LINERs too (Maoz+ 05) • LINER 1 & 2 UV colors similar (AV <~ 1) • No torus dust emission in M87 (Whysong & Antonucci 04; Perlman+ 07) • No torus dust emission in FR I and ~ half of FR II (van der Wolk+ 08)

  25. If only TOR is removed, all low-luminosity AGN become type 1 HOWEVER • Both type 1 and type 2 LINERs do exist (Maoz et al 05) • “true” type 2 AGN exist at L < 1042 erg s-1 (Panessa & Bassani 02; Laor 03) THEREFORE BLR must disappear at some lower L

  26. Ho 08: BLR disappears at LLAGN

  27. TOR BLR • Wind diminishes — mass outflow directed to jets (?) • Ho ‘02, Sikora et al ‘07: Radio loudness (Lrad/Lopt) varies inversely with Macc! .

  28. Radio-loudness; Sikora+ ‘07 R = Lrad/Lopt = L/LEdd

  29. Wind diminishes — mass outflow directed to jets (?) • Ho ‘02, Sikora et al ‘07: Radio loudness (Lrad/Lopt) varies inversely with Macc! . • Similar effect in X-ray binaries

  30. High Low Full Unification Scheme; both type 1 & 2 Accretion Rate (L/LEdd) Radio Loudness molecular outflow extinguished Torus disappears; type 1 only atomic outflow extinguished BLR disappears; “true” type 2 High Low

  31. TOR Energy Outflow Rate Negligible in the energy budget

  32. Final Speculation . • With  ~ 0.1, the required accretion rate is Macc ~ 0.1 L45 M yr-1 • The AGN phase lasts ~ 107 108 yrs • Overall accreted mass ~ 106  107 L45 M Is the whole Seyfert phenomenon the accretion of just a single GMC? Are QSO triggered differently (mergers)?

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