1 / 33

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

misu
Download Presentation

AGN structure and Unified models

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related