AGN structure and Unified models Guido Risaliti INAF – Osservatorio Astrofisico di Arcetri & Harvard-Smithsonian Center for Astrophysics

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

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

TORUS: direct imaging Meisenheimer et al. 2008

TORUS: dust reverberation mapping Pott et al. 2010

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

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

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

Inner TORUS: BLR X-ray absorption DNH~1023 cm-2 DT~2 days NGC 1365 NGC 4151 DNH > 1024 cm-2 DT~10 hours Puccetti et al. 2007 Risaliti et al. 2009 DNH~3*1023 cm-2 DT<15 days DNH~1023 cm-2 DT~20 hours UGC 4203 NGC 7582 Risaliti et al. 2010 Bianchi et al. 2009

Stratified BLR Peterson et al. 2007

Dusty torus + BLR: a possible structure 104 RS

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

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)

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

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

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

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

Cloud structure: comets? Maiolino et al. 2010

Complications: 4. stability 104 RS

STABILITY: Inflow / Outflow ? 104 RS

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

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

Outflows: phenomenological models

Outflows: phenomenological models

Outflows: physical models Proga 2000

Large scale structure NGC 5252: Tadhunter & Tsvetanov 1989

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

Large scale structure Mrk 573 Bianchi et al. 2010

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

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)

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