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AGN structure and Unified models

AGN structure and Unified models. Guido Risaliti. INAF – Osservatorio Astrofisico di Arcetri & Harvard-Smithsonian Center for Astrophysics. TODAY: Studying Complexity Luminosity, Spin, BH mass, Edd . ratio; BLR: density, cloud number, size, metallicity

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AGN structure and Unified models

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  1. AGN structure and Unified models Guido Risaliti INAF – OsservatorioAstrofisicodi Arcetri & Harvard-Smithsonian Center for Astrophysics

  2. TODAY: Studying Complexity Luminosity, Spin, BH mass, Edd. ratio; BLR: density, cloud number, size, metallicity Torus: distance, composition (dust/gas), covering factor Unified models: History Polarization 2) Are all the “ingredients” of the structure correct? 3) Any missing piece ? Outflows, multiple tori…. Masers Ionization cones M. Polletta; Urry & Padovani 1995

  3. TORUS: direct imaging Jaffe et al. 2004 Tristram et al. 2007 Greenhill et al. 2003

  4. TORUS: direct imaging Meisenheimer et al. 2008

  5. TORUS: dust reverberation mapping Pott et al. 2010

  6. (dusty) TORUS: clumpy structure Silicates absorption/emission Nenkova et al. 2008a,b

  7. Clumpy torus: Variability of NH in Seyfert Galaxies NH variable in 23/25 sources Timescales from months to years Clumpy absorber Sub-parsec distance Risaliti, Elvis & Nicastro 2002

  8. Inner TORUS: BLR/dust free component Low dust/gas ratio Missing BLR absorption in quasars Maiolino et al. 2001a Maiolino et al. 2001b

  9. Inner TORUS: BLR X-ray absorption NGC1365 NGC 4151 DNH > 1024 cm-2 DT~10 hours Puccetti et al. 2007 DNH~1023 cm-2 DT~2 days Risaliti et al. 2009 DNH~3*1023 cm-2 DT<15 days UGC 4203 NGC 7582 DNH~1023 cm-2 DT~20 hours Risaliti et al. 2010 Bianchi et al. 2009

  10. Stratified BLR Peterson et al. 2007

  11. Dusty torus + BLR: a possible structure 104RS

  12. Complications: 1. At least two tori Most local intermediate Seyferts are found in edge-on galaxies (and with NH~1022-1023 cm-2) Maiolino & Rieke 1995, Risaliti et al. 1999 Dust lanes observed

  13. Complications: 1. At least two tori Compact torus: BLR + hot dust scale (104-106 RG) 2. Dust lanes; 100pc – kpc absorbers Compton-thick, pc-scale torus ? need for a C-thick reflector to explain reflection in some C-thin AGN (NGC 5506, NGC 7582..) (e.g. discussion in Bianchi et al. 2009 on NGC 7582)

  14. Complications: 2. missing BLR Tran 2001 Bian & Gu 2009

  15. Complications: 2. missing BLR “naked” Seyferts: NGC 3147 Bianchi et al. 2009

  16. Complications: 2. missing BLR “naked” quasars: Q2131-427 Panessa et al. 2009

  17. Complications: 3. how many BLR ? From smoothness of observed lines: at least 108 ! Arav et al. 1998

  18. Cloud structure: comets? Maiolino et al. 2010

  19. Complications: 4. stability 104RS

  20. STABILITY: Inflow / Outflow ? 104RS

  21. Outflows: 1. the “common” and “weak” ones UV: NGC 5548 (Crenshaw et al. 2009) X-rays: NGC 1365 (Risaliti et al. 2005)

  22. Outflows: 2. the “strong” ones Optical/UV BAL, z~2 (Dunn et al. 2009) X-rays, PDS 456 (Reeves et al. 2009)

  23. Outflows: phenomenological models

  24. Outflows: phenomenological models

  25. Outflows: physical models Proga 2000

  26. Large scale structure NGC 5252: Tadhunter & Tsvetanov 1989

  27. Large scale structure Mrk 573: X-rays/[O III] Mrk 573: X-rays/Radio Bianchi et al. 2010

  28. Large scale structure Mrk 573 Bianchi et al. 2010

  29. Conclusions • orientation-based unification useful, and • basically correct • (too) many free parameters within the standard • unified picture • Many deviations & extra “ingredients” • New observations reveal this complexity, but also allow us to understand more and more details of the structure of AGN

  30. Disk orientation: aligned with torus ? AGNs with nuclear H2O maser disks are NOT preferentially Compton thick Distribution of EW([OIII]) has no high-EW cut off, as expected with a torus aligned with the disk log NH (cm-2) Zhang+ 06 Risaliti+2010 (poster)

  31. Disk orientation: aligned with torus ? Greenhill et al. 2009

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