theguardian.com Martin Elvis Harvard-Smithsonian Center for Astrophysics

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1 theguardian.com Martin Elvis Harvard-Smithsonian Center for Astrophysics

2 Antonucci and Miller 1985 (1) Feedback needs 5% of AGN Hopkins et al power deposited in Host ISM to stop star formation (2) Unified Scheme blocks 80% of AGN power to make Type 2 AGNs

3 Feedback assumes boiling off of ISM Unified Scheme assumes uniformity

4 Hopkins & Elvis, 2010, MNRAS, 401, 7

Kirhakos & Steiner 1990a,b Maiolino & Rieke 1995 Simcoe et al. 1997 Malkan et al.

5 obscuration associated with Host Disk Lawrence & Elvis Malkan 1982 ApJ et al., 256, Keel 1980 Lawrence & Elvis 1982 de Zotti & Gaskell 1985 Thompson & Martin 1988 Kirhakos & Steiner 1990a,b Maiolino & Rieke 1995 Simcoe et al Malkan et al Risaliti et al 2006 log(hβ/l X ) Hβ absorbed See also: Smajic 2011: NGC7172 Edge-on Face-on See also Van der Laan: starburst rings

6 4:1 ratio required by: Lawrence & Elvis 2010, ApJ 714, 561 X-ray background 1. X-ray Background (Gilli et al. 2007) 2. Bi-cone opening Angles +/- ~25 o Type 1 Type 2 Tadhunter & Tsvetanov 1989 Nature 341, 422

$fraction No LINERS ~1:1 Type 2:type 1 ratio$

7 Lawrence & Elvis 2010, ApJ 714, 561 Type 2 fraction No LINERS ~1:1 Type 2:type 1 ratio L(Bol)

$fraction$

8 Lawrence & Elvis 2010, ApJ 714, 561 No LINERS Type 2 fraction L(Bol)

9 1 day NGC 1365 Suzaku Maiolino et al N H Covering Factor

10 Risaliti, Elvis & Nicastro, 2002 N H variable in 23/25 AGNs Timescales of months to years

11 Das et al Optical/X-ray mismatch of types

12 Elvis et al ApJS, 95, 1 Major fraction high covering factor at x r(dust sublimation) Radio IR Opt/UV EUV X-ray Dust emission accre(on disk α ox Peak~10µm T~200K Large Area ~10,000 A Short limit~1µm T~2000K Small area, A 18

13 Covering factor = L(Hot Dust)/L(Disk) Factor ~5 Unification: not so simple Don t over-average. >1 AGN IR template IR Bump 1 µm 40µm UV Bump 1 dex Roseboom et al MNRAS, 429, 1494

14 Martin Elvis. 18 October 2008 Lawrence & Elvis 2010, ApJ 714, 561 Absorbers/re-emitters Emitters Aligned with host Host Narrow Emission Lines (NELR) bicones Realignment? Cool Hot Dust Dust Broad Emission Lines (BELR) Low Aligned with disk Warm Absorber High Black Hole X-ray Continuum Optical/UV continuum

Isotropic accretion events Minor mergers,

2007 Warped Disks - Observed Low warps allow

2010, ApJ 714, 561 NGC4258 Maser also Circinus

15 Isotropic accretion events Minor mergers, molecular clouds Volonteri et al Warped Disks - Observed Low warps allow feedback Event dependent Lawrence & Elvis 2010, ApJ 714, 561 NGC4258 Maser also Circinus Gal Center? NGC1068 CO disk Schinnerer et al Rijkhorst et al. 2005

of type1 covering factor Lawrence & Elvis 2010, ApJ

16 Predicts Observed: 1:1 Type1:Type2 ratio Jet-obscurer axis misalignments Correct distribution of type1 covering factor Lawrence & Elvis 2010, ApJ 714, 561 Roseboom et al. 2013, MNRAS Type 1 Warped disk prediction

17 Feedback needs 5% of AGN power deposited in Host ISM to stop star formation Unified Scheme has 80% of AGN power blocked to make Type 2 AGNs Hopkins & Elvis, 2009, MNRAS, 401, 7 Lawrence & Elvis 2010, ApJ 714, 561 Roseboom, Lawrence, Elvis, Petty, Shen & Hao, 2013, MNRAS, 429, 1494

18 walesonline.co.uk

19 Disk Tearing Nixon et al. 2012ApJ...757L..24N Isotropic accretion events misaligned disk black hole axes Bardeen-Petterson disk warping: vertical viscosty runaway warps r(inner) ~ rg r(outer) ~ few pc counter-rotating: angular momentum cancels feeding

20 Donut Torus? Just say warps Rijkhorst et al. 2005

The Structure of Active Galactic Nuclei on Scales from 100mas to 100µas

The Structure of Active Galactic Nuclei on Scales from 100mas to 100µas Martin Elvis Harvard-Smithsonian Center for Astrophysics Quasars the Quintessential Point Sources 100,000 th Hubble Exposure, 1996.