The AGN Obscuring Torus

Moshe Elitzur

University of Kentucky

& LAOG, Grenoble

Happy Birthday, young man!

zone # optical depth

i-1

i

z-1

z = t

0 = 12

i

z

i,i-1 Ti Ci pi ni1 ni2 ij = |i – j|

Coupled

Escape

Probability

'cr

kT/E

21

21

N

Ne1

AC

121

Semi-infinite Atmosphere(10-3 107)

Time %error

zones ALI CEP ALI CEP

20 0.39 36.3 104

40 1.10 23.9 45.7

100 4.39 0.06 10.9 14.0

200 11.6 0.89 5.5 5.4

600 44.9 1.70 1.6 1.2

Time %error, S

zones ALI CEP ALI CEP

1 0.03 99.5 55.5

20 1.02 88.2 23.0

40 3.29 79.8 15.5

100 12.6 .033 62.5 6.5

200 28.1 .085 46.4 2.2

= 10-3 :

Slab t = 500

2-level Atom

)T(BJ)1(S

Elitzur & Asensio Ramos 2006, MNRAS 365, 779

Unified Scheme for AGN

Toroidal

Obscuration

Required by

Unification

Schemes

Torus Properties

From the statistics of type 1 vs type 2: H/R ~ 1

(Schmitt et al ’01)

R = ? Must rely on IR emission

General folklore: R 100 pc

Origin of the 100’s pc Torus – Modeling IR emission

Pier & Krolik 93

~100 pc

Pier & Krolik 92

5-10 pc

Granato et al ’94, ‘97:

• Uniform density

• Rout ~ 100 – 300 pc

= 45°

Dearth of IR emission in smooth-density models T r

Schinnerer et al ’00

Observations – NGC 1068, CO

at R ~ 70 pc, H ~ 9 – 10 pc H/R ~ 0.15

Observations – NGC 1068, CO & H2

Galliano et al ’03: H/R ~ 0.15

20 pc

140 pc

IR – Observations

NGC1068: 2m imaging – R ~ 1 pc (Weigelt et al 04)

10m interferometry – R ~ 2 pc (Jaffe et al

04)

Cen A: 2m – R < 0.5 pc (Prieto et al 04)

9 & 10m – R ~ 1.5 pc (Karovska et al 03)

Circinus: 2m – R ~ 1pc (Prieto et al 04)

8 & 18m – R < 2 pc (Packham et al 05)

NGC1097 & NGC5506: 2m – R < 5 pc (Prieto et al 04)

The Torus Size Crisis Observations – compact (pc-size) torus

Theory – extended (100’s pc) torus

r 1.7 pc: T = 320 K

Jaffe et al ‘04VLTI – NGC1068:

Poncelet et al ‘06

Lbol = 2·1045 erg s-1 (Mason et al ’06)

T(r = 2pc) = 960 K

r(T = 320 K) = 26 pc

r(T = 226 K) = 57 pc

Tmax

Tmin

Temperature in Clumpy Medium

Nenkova et al 2006

Temperature–Distance Relation

Smooth density – T & R uniquely related

Clumpy density – different T at same R

different R, same T

Ri = 0.9 pc L½12

Y = Ro/Ri

AGN Clumpy Torus: Size Effect

N N0r -q exp(-2/2)

N0 = 5

= 45º

V = 60

Clumping solves the compact emission problem!

Dynamic Origin of Vertical Structure

Cloud accretion from the galaxy?

No need in a compact torus!

The Torus as a Disk-Wind Region

Bottorff et al 97

Unification Scheme

Grand Unification Scheme

BLR

BAL

Torus

masers

Emmering, Blandford & Shlosman 92

Size – shear resistance: 7

3pc23,H16

c M

rNcm10R

Cloud Properties in Torus-Wind

16,c

23,H37

R

Ncm10n Density:

Mass:2

16,c23,H3

c RNM107M

Magnetic field:

2/1

16,c

223,H

R

TNmG2B

Elitzur & Shlosman 2006

Kondratko, Greenhill & Moran ‘05NGC 3079

High-latitude features – disk rotational imprint: uplifted clouds

Water Masers – Glimpse of Torus Clouds?

Outflow and Accretion

145acc yrM/L02.0M

accout2

6T

23,H45 MM)vN(L I

Torus disappearance at L 1043 erg s-1 !

Narrow-line Seyfert 1 radio galaxies?

Chiaberge et al ’99; Whysong & Antonucci ‘04

I 6T

23,H2/145acc

out vNL

1MM

Conclusions

No bagel

Toroidal Obscuration Required by Unified Scheme

– just a region in the disk-wind