Unification Issues and the AGN TORUS

Moshe Elitzur

University of Kentucky

Unification prediction 1

type 2 = type 1 + obscuration

namely

every type 1 class has a corresponding

type 2

QSO2 MUST exist

QSO2 DO exist even with hidden type 1

engines at z = 06 (Zakamska et al

05)

MRK1239Rodrigraveguez-Ardila amp Mazzalay lsquo06

Prediction 2 mdash SED 2 = 1 - AGN

IR Puzzle 1

r 17 pc T = 320 K

Jaffe et al lsquo04

VLTI mdash NGC1068

Poncelet et al lsquo06

Lbol = 2middot1045 erg s-1 (Mason et al rsquo06)

T(r = 2pc) = 960 K

r(T = 320 K) = 26 pc

r(T = 226 K) = 57 pc

T gt 800 K

Tmax

Tmin

Temperature in Clumpy Medium

Nenkova et al 2006

IR Puzzle 2

Lutz et al rsquo04 mdash 6microm vs 2-10 keV x-rays Horst et al rsquo06 mdash 12microm vs 2-10 keV x-rays Buchanan et al rsquo06 mdash 5-35microm vs radio

While its obscuration is highly

anisotropic the torus emission is nearly

isotropic

R = IRradio

Clumpy Torus ndash Radial Density Variation

Large q (steep radial decline) mdash

Anisotropic obscuration with nearly isotropic emission

N0 = 5

= 45ordm

V = 60

N N0exp(-22)rq

Clumpy Torus Modeling

N0 = 5 ndash 10 clouds

= 30deg ndash 60deg

V = 40 ndash 120

q = 1 ndash 2

Rs = 09Lfrac1212 pc Ro gt 5

Rs

Standard ISM dust works fine

N N0 exp(-22)rq

Nenkova et al lsquo02 lsquo06

s

Unification Statisticsf2 mdash fraction of obscured sources = N2(N1 + N2)

Seyferts f2 = 70 Schmitt et al 01

f2 = 50 Hao et al 05

f2 decreases with luminosity (Simpson 05 Hao et al)

mdash ldquoreceding torusrdquo (Lawrence 91)

f2 = sin = 05 mdash 07

HR = tan ~ 07 mdash 1

R

Rs

H

Basic Premise AGN type determined uniquely by viewing angle

Clumpy Unification

Nc() = N0 exp(-22)

f2 depends on both and N0

Type 1 sources from ldquotype 2 viewingrdquo and vice versa

Flips between type 1 amp 2 (Aretxaga et al 99)

f2 variations may arise from either or N0 or both

AGN type is a viewing-dependent probability

Unification and X-rays

Evidence for types 1 amp 2 orientation-dependence in

both X-ray absorption and reprocessing

Absorption-corrected type 2 spectra amp luminosities

are similar to type 1 (Smith amp Done 96 Turner et al

97)

BUT

The ldquoX-ray torusrdquo probably

does not coincide with the ldquodusty torusrdquo

Dusty vs X-rays Torus

NH(X-ray) ~ 3 mdash 100 NH(UV) (Maiolino et al 01)

From IR modeling NH(torus) lt~ 1024 cm-2 yet at

least ~50 of Seyfert 2 are Compton thick (Guainazzi

et al 05)

Fast X-ray variations mdash absorbing clouds are dust-

free

Risaliti Elvis amp Nicastro 02

RXRs

Dusty vs X-rays Torus (2)

X-ray observations + IR observations and modeling

NH(X-ray) ~ 10 NH(torus)

If Nclouds ~ 1r2 then RX ~ Rs10 (and Rs ~ 09 L1212 pc)

RX

Rs

f2(X-rays) may be

quite different from

f2(UVoptical) Sarah Gallagher (Tuesday)

Compton thick ldquox-ray onlyrdquo absorption in QSO1 (x-ray and UV not consistent with each other)

Torus Size NGC1068 2m imaging ndash R ~ 1 pc (Weigelt et al 04)

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

04)

Cen A 2m ndash R lt 05 pc (Prieto et al 04)

9 amp 18m ndash R lt 2 pc (Radomski et al 06)

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

8 amp 18m ndash R lt 2 pc (Packham et al 05)

NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto et al 04)All observations are consistent with RoutRs no larger than ~20-30 and perhaps even

only ~5-10

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

Everett amp Konigl 00

Cloud Properties in Torus Outflow

v ~ 20 ndash 150 NH ~ 1022 ndash 1023 cm-2 Resistance to tidal shearing

n gt 107 M7 rpc3 cm-3

Rc lt 1016 NH23 rpc3 M7 cm

Mc lt 710-3 NH23 Rc162 Mo

B ~ 15 1kms n712 mG

Elitzur amp Shlosman 2006

Unification Scheme

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

Unification prediction 1

type 2 = type 1 + obscuration

namely

every type 1 class has a corresponding

type 2

QSO2 MUST exist

QSO2 DO exist even with hidden type 1

engines at z = 06 (Zakamska et al

05)

MRK1239Rodrigraveguez-Ardila amp Mazzalay lsquo06

Prediction 2 mdash SED 2 = 1 - AGN

IR Puzzle 1

r 17 pc T = 320 K

Jaffe et al lsquo04

VLTI mdash NGC1068

Poncelet et al lsquo06

Lbol = 2middot1045 erg s-1 (Mason et al rsquo06)

T(r = 2pc) = 960 K

r(T = 320 K) = 26 pc

r(T = 226 K) = 57 pc

T gt 800 K

Tmax

Tmin

Temperature in Clumpy Medium

Nenkova et al 2006

IR Puzzle 2

Lutz et al rsquo04 mdash 6microm vs 2-10 keV x-rays Horst et al rsquo06 mdash 12microm vs 2-10 keV x-rays Buchanan et al rsquo06 mdash 5-35microm vs radio

While its obscuration is highly

anisotropic the torus emission is nearly

isotropic

R = IRradio

Clumpy Torus ndash Radial Density Variation

Large q (steep radial decline) mdash

Anisotropic obscuration with nearly isotropic emission

N0 = 5

= 45ordm

V = 60

N N0exp(-22)rq

Clumpy Torus Modeling

N0 = 5 ndash 10 clouds

= 30deg ndash 60deg

V = 40 ndash 120

q = 1 ndash 2

Rs = 09Lfrac1212 pc Ro gt 5

Rs

Standard ISM dust works fine

N N0 exp(-22)rq

Nenkova et al lsquo02 lsquo06

s

Unification Statisticsf2 mdash fraction of obscured sources = N2(N1 + N2)

Seyferts f2 = 70 Schmitt et al 01

f2 = 50 Hao et al 05

f2 decreases with luminosity (Simpson 05 Hao et al)

mdash ldquoreceding torusrdquo (Lawrence 91)

f2 = sin = 05 mdash 07

HR = tan ~ 07 mdash 1

R

Rs

H

Basic Premise AGN type determined uniquely by viewing angle

Clumpy Unification

Nc() = N0 exp(-22)

f2 depends on both and N0

Type 1 sources from ldquotype 2 viewingrdquo and vice versa

Flips between type 1 amp 2 (Aretxaga et al 99)

f2 variations may arise from either or N0 or both

AGN type is a viewing-dependent probability

Unification and X-rays

Evidence for types 1 amp 2 orientation-dependence in

both X-ray absorption and reprocessing

Absorption-corrected type 2 spectra amp luminosities

are similar to type 1 (Smith amp Done 96 Turner et al

97)

BUT

The ldquoX-ray torusrdquo probably

does not coincide with the ldquodusty torusrdquo

Dusty vs X-rays Torus

NH(X-ray) ~ 3 mdash 100 NH(UV) (Maiolino et al 01)

From IR modeling NH(torus) lt~ 1024 cm-2 yet at

least ~50 of Seyfert 2 are Compton thick (Guainazzi

et al 05)

Fast X-ray variations mdash absorbing clouds are dust-

free

Risaliti Elvis amp Nicastro 02

RXRs

Dusty vs X-rays Torus (2)

X-ray observations + IR observations and modeling

NH(X-ray) ~ 10 NH(torus)

If Nclouds ~ 1r2 then RX ~ Rs10 (and Rs ~ 09 L1212 pc)

RX

Rs

f2(X-rays) may be

quite different from

f2(UVoptical) Sarah Gallagher (Tuesday)

Compton thick ldquox-ray onlyrdquo absorption in QSO1 (x-ray and UV not consistent with each other)

Torus Size NGC1068 2m imaging ndash R ~ 1 pc (Weigelt et al 04)

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

04)

Cen A 2m ndash R lt 05 pc (Prieto et al 04)

9 amp 18m ndash R lt 2 pc (Radomski et al 06)

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

8 amp 18m ndash R lt 2 pc (Packham et al 05)

NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto et al 04)All observations are consistent with RoutRs no larger than ~20-30 and perhaps even

only ~5-10

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

Everett amp Konigl 00

Cloud Properties in Torus Outflow

v ~ 20 ndash 150 NH ~ 1022 ndash 1023 cm-2 Resistance to tidal shearing

n gt 107 M7 rpc3 cm-3

Rc lt 1016 NH23 rpc3 M7 cm

Mc lt 710-3 NH23 Rc162 Mo

B ~ 15 1kms n712 mG

Elitzur amp Shlosman 2006

Unification Scheme

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

MRK1239Rodrigraveguez-Ardila amp Mazzalay lsquo06

Prediction 2 mdash SED 2 = 1 - AGN

IR Puzzle 1

r 17 pc T = 320 K

Jaffe et al lsquo04

VLTI mdash NGC1068

Poncelet et al lsquo06

Lbol = 2middot1045 erg s-1 (Mason et al rsquo06)

T(r = 2pc) = 960 K

r(T = 320 K) = 26 pc

r(T = 226 K) = 57 pc

T gt 800 K

Tmax

Tmin

Temperature in Clumpy Medium

Nenkova et al 2006

IR Puzzle 2

Lutz et al rsquo04 mdash 6microm vs 2-10 keV x-rays Horst et al rsquo06 mdash 12microm vs 2-10 keV x-rays Buchanan et al rsquo06 mdash 5-35microm vs radio

While its obscuration is highly

anisotropic the torus emission is nearly

isotropic

R = IRradio

Clumpy Torus ndash Radial Density Variation

Large q (steep radial decline) mdash

Anisotropic obscuration with nearly isotropic emission

N0 = 5

= 45ordm

V = 60

N N0exp(-22)rq

Clumpy Torus Modeling

N0 = 5 ndash 10 clouds

= 30deg ndash 60deg

V = 40 ndash 120

q = 1 ndash 2

Rs = 09Lfrac1212 pc Ro gt 5

Rs

Standard ISM dust works fine

N N0 exp(-22)rq

Nenkova et al lsquo02 lsquo06

s

Unification Statisticsf2 mdash fraction of obscured sources = N2(N1 + N2)

Seyferts f2 = 70 Schmitt et al 01

f2 = 50 Hao et al 05

f2 decreases with luminosity (Simpson 05 Hao et al)

mdash ldquoreceding torusrdquo (Lawrence 91)

f2 = sin = 05 mdash 07

HR = tan ~ 07 mdash 1

R

Rs

H

Basic Premise AGN type determined uniquely by viewing angle

Clumpy Unification

Nc() = N0 exp(-22)

f2 depends on both and N0

Type 1 sources from ldquotype 2 viewingrdquo and vice versa

Flips between type 1 amp 2 (Aretxaga et al 99)

f2 variations may arise from either or N0 or both

AGN type is a viewing-dependent probability

Unification and X-rays

Evidence for types 1 amp 2 orientation-dependence in

both X-ray absorption and reprocessing

Absorption-corrected type 2 spectra amp luminosities

are similar to type 1 (Smith amp Done 96 Turner et al

97)

BUT

The ldquoX-ray torusrdquo probably

does not coincide with the ldquodusty torusrdquo

Dusty vs X-rays Torus

NH(X-ray) ~ 3 mdash 100 NH(UV) (Maiolino et al 01)

From IR modeling NH(torus) lt~ 1024 cm-2 yet at

least ~50 of Seyfert 2 are Compton thick (Guainazzi

et al 05)

Fast X-ray variations mdash absorbing clouds are dust-

free

Risaliti Elvis amp Nicastro 02

RXRs

Dusty vs X-rays Torus (2)

X-ray observations + IR observations and modeling

NH(X-ray) ~ 10 NH(torus)

If Nclouds ~ 1r2 then RX ~ Rs10 (and Rs ~ 09 L1212 pc)

RX

Rs

f2(X-rays) may be

quite different from

f2(UVoptical) Sarah Gallagher (Tuesday)

Compton thick ldquox-ray onlyrdquo absorption in QSO1 (x-ray and UV not consistent with each other)

Torus Size NGC1068 2m imaging ndash R ~ 1 pc (Weigelt et al 04)

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

04)

Cen A 2m ndash R lt 05 pc (Prieto et al 04)

9 amp 18m ndash R lt 2 pc (Radomski et al 06)

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

8 amp 18m ndash R lt 2 pc (Packham et al 05)

NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto et al 04)All observations are consistent with RoutRs no larger than ~20-30 and perhaps even

only ~5-10

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

Everett amp Konigl 00

Cloud Properties in Torus Outflow

v ~ 20 ndash 150 NH ~ 1022 ndash 1023 cm-2 Resistance to tidal shearing

n gt 107 M7 rpc3 cm-3

Rc lt 1016 NH23 rpc3 M7 cm

Mc lt 710-3 NH23 Rc162 Mo

B ~ 15 1kms n712 mG

Elitzur amp Shlosman 2006

Unification Scheme

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

IR Puzzle 1

r 17 pc T = 320 K

Jaffe et al lsquo04

VLTI mdash NGC1068

Poncelet et al lsquo06

Lbol = 2middot1045 erg s-1 (Mason et al rsquo06)

T(r = 2pc) = 960 K

r(T = 320 K) = 26 pc

r(T = 226 K) = 57 pc

T gt 800 K

Tmax

Tmin

Temperature in Clumpy Medium

Nenkova et al 2006

IR Puzzle 2

Lutz et al rsquo04 mdash 6microm vs 2-10 keV x-rays Horst et al rsquo06 mdash 12microm vs 2-10 keV x-rays Buchanan et al rsquo06 mdash 5-35microm vs radio

While its obscuration is highly

anisotropic the torus emission is nearly

isotropic

R = IRradio

Clumpy Torus ndash Radial Density Variation

Large q (steep radial decline) mdash

Anisotropic obscuration with nearly isotropic emission

N0 = 5

= 45ordm

V = 60

N N0exp(-22)rq

Clumpy Torus Modeling

N0 = 5 ndash 10 clouds

= 30deg ndash 60deg

V = 40 ndash 120

q = 1 ndash 2

Rs = 09Lfrac1212 pc Ro gt 5

Rs

Standard ISM dust works fine

N N0 exp(-22)rq

Nenkova et al lsquo02 lsquo06

s

Unification Statisticsf2 mdash fraction of obscured sources = N2(N1 + N2)

Seyferts f2 = 70 Schmitt et al 01

f2 = 50 Hao et al 05

f2 decreases with luminosity (Simpson 05 Hao et al)

mdash ldquoreceding torusrdquo (Lawrence 91)

f2 = sin = 05 mdash 07

HR = tan ~ 07 mdash 1

R

Rs

H

Basic Premise AGN type determined uniquely by viewing angle

Clumpy Unification

Nc() = N0 exp(-22)

f2 depends on both and N0

Type 1 sources from ldquotype 2 viewingrdquo and vice versa

Flips between type 1 amp 2 (Aretxaga et al 99)

f2 variations may arise from either or N0 or both

AGN type is a viewing-dependent probability

Unification and X-rays

Evidence for types 1 amp 2 orientation-dependence in

both X-ray absorption and reprocessing

Absorption-corrected type 2 spectra amp luminosities

are similar to type 1 (Smith amp Done 96 Turner et al

97)

BUT

The ldquoX-ray torusrdquo probably

does not coincide with the ldquodusty torusrdquo

Dusty vs X-rays Torus

NH(X-ray) ~ 3 mdash 100 NH(UV) (Maiolino et al 01)

From IR modeling NH(torus) lt~ 1024 cm-2 yet at

least ~50 of Seyfert 2 are Compton thick (Guainazzi

et al 05)

Fast X-ray variations mdash absorbing clouds are dust-

free

Risaliti Elvis amp Nicastro 02

RXRs

Dusty vs X-rays Torus (2)

X-ray observations + IR observations and modeling

NH(X-ray) ~ 10 NH(torus)

If Nclouds ~ 1r2 then RX ~ Rs10 (and Rs ~ 09 L1212 pc)

RX

Rs

f2(X-rays) may be

quite different from

f2(UVoptical) Sarah Gallagher (Tuesday)

Compton thick ldquox-ray onlyrdquo absorption in QSO1 (x-ray and UV not consistent with each other)

Torus Size NGC1068 2m imaging ndash R ~ 1 pc (Weigelt et al 04)

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

04)

Cen A 2m ndash R lt 05 pc (Prieto et al 04)

9 amp 18m ndash R lt 2 pc (Radomski et al 06)

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

8 amp 18m ndash R lt 2 pc (Packham et al 05)

NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto et al 04)All observations are consistent with RoutRs no larger than ~20-30 and perhaps even

only ~5-10

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

Everett amp Konigl 00

Cloud Properties in Torus Outflow

v ~ 20 ndash 150 NH ~ 1022 ndash 1023 cm-2 Resistance to tidal shearing

n gt 107 M7 rpc3 cm-3

Rc lt 1016 NH23 rpc3 M7 cm

Mc lt 710-3 NH23 Rc162 Mo

B ~ 15 1kms n712 mG

Elitzur amp Shlosman 2006

Unification Scheme

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

Tmax

Tmin

Temperature in Clumpy Medium

Nenkova et al 2006

IR Puzzle 2

Lutz et al rsquo04 mdash 6microm vs 2-10 keV x-rays Horst et al rsquo06 mdash 12microm vs 2-10 keV x-rays Buchanan et al rsquo06 mdash 5-35microm vs radio

While its obscuration is highly

anisotropic the torus emission is nearly

isotropic

R = IRradio

Clumpy Torus ndash Radial Density Variation

Large q (steep radial decline) mdash

Anisotropic obscuration with nearly isotropic emission

N0 = 5

= 45ordm

V = 60

N N0exp(-22)rq

Clumpy Torus Modeling

N0 = 5 ndash 10 clouds

= 30deg ndash 60deg

V = 40 ndash 120

q = 1 ndash 2

Rs = 09Lfrac1212 pc Ro gt 5

Rs

Standard ISM dust works fine

N N0 exp(-22)rq

Nenkova et al lsquo02 lsquo06

s

Unification Statisticsf2 mdash fraction of obscured sources = N2(N1 + N2)

Seyferts f2 = 70 Schmitt et al 01

f2 = 50 Hao et al 05

f2 decreases with luminosity (Simpson 05 Hao et al)

mdash ldquoreceding torusrdquo (Lawrence 91)

f2 = sin = 05 mdash 07

HR = tan ~ 07 mdash 1

R

Rs

H

Basic Premise AGN type determined uniquely by viewing angle

Clumpy Unification

Nc() = N0 exp(-22)

f2 depends on both and N0

Type 1 sources from ldquotype 2 viewingrdquo and vice versa

Flips between type 1 amp 2 (Aretxaga et al 99)

f2 variations may arise from either or N0 or both

AGN type is a viewing-dependent probability

Unification and X-rays

Evidence for types 1 amp 2 orientation-dependence in

both X-ray absorption and reprocessing

Absorption-corrected type 2 spectra amp luminosities

are similar to type 1 (Smith amp Done 96 Turner et al

97)

BUT

The ldquoX-ray torusrdquo probably

does not coincide with the ldquodusty torusrdquo

Dusty vs X-rays Torus

NH(X-ray) ~ 3 mdash 100 NH(UV) (Maiolino et al 01)

From IR modeling NH(torus) lt~ 1024 cm-2 yet at

least ~50 of Seyfert 2 are Compton thick (Guainazzi

et al 05)

Fast X-ray variations mdash absorbing clouds are dust-

free

Risaliti Elvis amp Nicastro 02

RXRs

Dusty vs X-rays Torus (2)

X-ray observations + IR observations and modeling

NH(X-ray) ~ 10 NH(torus)

If Nclouds ~ 1r2 then RX ~ Rs10 (and Rs ~ 09 L1212 pc)

RX

Rs

f2(X-rays) may be

quite different from

f2(UVoptical) Sarah Gallagher (Tuesday)

Compton thick ldquox-ray onlyrdquo absorption in QSO1 (x-ray and UV not consistent with each other)

Torus Size NGC1068 2m imaging ndash R ~ 1 pc (Weigelt et al 04)

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

04)

Cen A 2m ndash R lt 05 pc (Prieto et al 04)

9 amp 18m ndash R lt 2 pc (Radomski et al 06)

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

8 amp 18m ndash R lt 2 pc (Packham et al 05)

NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto et al 04)All observations are consistent with RoutRs no larger than ~20-30 and perhaps even

only ~5-10

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

Everett amp Konigl 00

Cloud Properties in Torus Outflow

v ~ 20 ndash 150 NH ~ 1022 ndash 1023 cm-2 Resistance to tidal shearing

n gt 107 M7 rpc3 cm-3

Rc lt 1016 NH23 rpc3 M7 cm

Mc lt 710-3 NH23 Rc162 Mo

B ~ 15 1kms n712 mG

Elitzur amp Shlosman 2006

Unification Scheme

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

IR Puzzle 2

Lutz et al rsquo04 mdash 6microm vs 2-10 keV x-rays Horst et al rsquo06 mdash 12microm vs 2-10 keV x-rays Buchanan et al rsquo06 mdash 5-35microm vs radio

While its obscuration is highly

anisotropic the torus emission is nearly

isotropic

R = IRradio

Clumpy Torus ndash Radial Density Variation

Large q (steep radial decline) mdash

Anisotropic obscuration with nearly isotropic emission

N0 = 5

= 45ordm

V = 60

N N0exp(-22)rq

Clumpy Torus Modeling

N0 = 5 ndash 10 clouds

= 30deg ndash 60deg

V = 40 ndash 120

q = 1 ndash 2

Rs = 09Lfrac1212 pc Ro gt 5

Rs

Standard ISM dust works fine

N N0 exp(-22)rq

Nenkova et al lsquo02 lsquo06

s

Unification Statisticsf2 mdash fraction of obscured sources = N2(N1 + N2)

Seyferts f2 = 70 Schmitt et al 01

f2 = 50 Hao et al 05

f2 decreases with luminosity (Simpson 05 Hao et al)

mdash ldquoreceding torusrdquo (Lawrence 91)

f2 = sin = 05 mdash 07

HR = tan ~ 07 mdash 1

R

Rs

H

Basic Premise AGN type determined uniquely by viewing angle

Clumpy Unification

Nc() = N0 exp(-22)

f2 depends on both and N0

Type 1 sources from ldquotype 2 viewingrdquo and vice versa

Flips between type 1 amp 2 (Aretxaga et al 99)

f2 variations may arise from either or N0 or both

AGN type is a viewing-dependent probability

Unification and X-rays

Evidence for types 1 amp 2 orientation-dependence in

both X-ray absorption and reprocessing

Absorption-corrected type 2 spectra amp luminosities

are similar to type 1 (Smith amp Done 96 Turner et al

97)

BUT

The ldquoX-ray torusrdquo probably

does not coincide with the ldquodusty torusrdquo

Dusty vs X-rays Torus

NH(X-ray) ~ 3 mdash 100 NH(UV) (Maiolino et al 01)

From IR modeling NH(torus) lt~ 1024 cm-2 yet at

least ~50 of Seyfert 2 are Compton thick (Guainazzi

et al 05)

Fast X-ray variations mdash absorbing clouds are dust-

free

Risaliti Elvis amp Nicastro 02

RXRs

Dusty vs X-rays Torus (2)

X-ray observations + IR observations and modeling

NH(X-ray) ~ 10 NH(torus)

If Nclouds ~ 1r2 then RX ~ Rs10 (and Rs ~ 09 L1212 pc)

RX

Rs

f2(X-rays) may be

quite different from

f2(UVoptical) Sarah Gallagher (Tuesday)

Compton thick ldquox-ray onlyrdquo absorption in QSO1 (x-ray and UV not consistent with each other)

Torus Size NGC1068 2m imaging ndash R ~ 1 pc (Weigelt et al 04)

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

04)

Cen A 2m ndash R lt 05 pc (Prieto et al 04)

9 amp 18m ndash R lt 2 pc (Radomski et al 06)

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

8 amp 18m ndash R lt 2 pc (Packham et al 05)

NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto et al 04)All observations are consistent with RoutRs no larger than ~20-30 and perhaps even

only ~5-10

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

Everett amp Konigl 00

Cloud Properties in Torus Outflow

v ~ 20 ndash 150 NH ~ 1022 ndash 1023 cm-2 Resistance to tidal shearing

n gt 107 M7 rpc3 cm-3

Rc lt 1016 NH23 rpc3 M7 cm

Mc lt 710-3 NH23 Rc162 Mo

B ~ 15 1kms n712 mG

Elitzur amp Shlosman 2006

Unification Scheme

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

Clumpy Torus ndash Radial Density Variation

Large q (steep radial decline) mdash

Anisotropic obscuration with nearly isotropic emission

N0 = 5

= 45ordm

V = 60

N N0exp(-22)rq

Clumpy Torus Modeling

N0 = 5 ndash 10 clouds

= 30deg ndash 60deg

V = 40 ndash 120

q = 1 ndash 2

Rs = 09Lfrac1212 pc Ro gt 5

Rs

Standard ISM dust works fine

N N0 exp(-22)rq

Nenkova et al lsquo02 lsquo06

s

Unification Statisticsf2 mdash fraction of obscured sources = N2(N1 + N2)

Seyferts f2 = 70 Schmitt et al 01

f2 = 50 Hao et al 05

f2 decreases with luminosity (Simpson 05 Hao et al)

mdash ldquoreceding torusrdquo (Lawrence 91)

f2 = sin = 05 mdash 07

HR = tan ~ 07 mdash 1

R

Rs

H

Basic Premise AGN type determined uniquely by viewing angle

Clumpy Unification

Nc() = N0 exp(-22)

f2 depends on both and N0

Type 1 sources from ldquotype 2 viewingrdquo and vice versa

Flips between type 1 amp 2 (Aretxaga et al 99)

f2 variations may arise from either or N0 or both

AGN type is a viewing-dependent probability

Unification and X-rays

Evidence for types 1 amp 2 orientation-dependence in

both X-ray absorption and reprocessing

Absorption-corrected type 2 spectra amp luminosities

are similar to type 1 (Smith amp Done 96 Turner et al

97)

BUT

The ldquoX-ray torusrdquo probably

does not coincide with the ldquodusty torusrdquo

Dusty vs X-rays Torus

NH(X-ray) ~ 3 mdash 100 NH(UV) (Maiolino et al 01)

From IR modeling NH(torus) lt~ 1024 cm-2 yet at

least ~50 of Seyfert 2 are Compton thick (Guainazzi

et al 05)

Fast X-ray variations mdash absorbing clouds are dust-

free

Risaliti Elvis amp Nicastro 02

RXRs

Dusty vs X-rays Torus (2)

X-ray observations + IR observations and modeling

NH(X-ray) ~ 10 NH(torus)

If Nclouds ~ 1r2 then RX ~ Rs10 (and Rs ~ 09 L1212 pc)

RX

Rs

f2(X-rays) may be

quite different from

f2(UVoptical) Sarah Gallagher (Tuesday)

Compton thick ldquox-ray onlyrdquo absorption in QSO1 (x-ray and UV not consistent with each other)

Torus Size NGC1068 2m imaging ndash R ~ 1 pc (Weigelt et al 04)

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

04)

Cen A 2m ndash R lt 05 pc (Prieto et al 04)

9 amp 18m ndash R lt 2 pc (Radomski et al 06)

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

8 amp 18m ndash R lt 2 pc (Packham et al 05)

NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto et al 04)All observations are consistent with RoutRs no larger than ~20-30 and perhaps even

only ~5-10

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

Everett amp Konigl 00

Cloud Properties in Torus Outflow

v ~ 20 ndash 150 NH ~ 1022 ndash 1023 cm-2 Resistance to tidal shearing

n gt 107 M7 rpc3 cm-3

Rc lt 1016 NH23 rpc3 M7 cm

Mc lt 710-3 NH23 Rc162 Mo

B ~ 15 1kms n712 mG

Elitzur amp Shlosman 2006

Unification Scheme

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

Clumpy Torus Modeling

N0 = 5 ndash 10 clouds

= 30deg ndash 60deg

V = 40 ndash 120

q = 1 ndash 2

Rs = 09Lfrac1212 pc Ro gt 5

Rs

Standard ISM dust works fine

N N0 exp(-22)rq

Nenkova et al lsquo02 lsquo06

s

Unification Statisticsf2 mdash fraction of obscured sources = N2(N1 + N2)

Seyferts f2 = 70 Schmitt et al 01

f2 = 50 Hao et al 05

f2 decreases with luminosity (Simpson 05 Hao et al)

mdash ldquoreceding torusrdquo (Lawrence 91)

f2 = sin = 05 mdash 07

HR = tan ~ 07 mdash 1

R

Rs

H

Basic Premise AGN type determined uniquely by viewing angle

Clumpy Unification

Nc() = N0 exp(-22)

f2 depends on both and N0

Type 1 sources from ldquotype 2 viewingrdquo and vice versa

Flips between type 1 amp 2 (Aretxaga et al 99)

f2 variations may arise from either or N0 or both

AGN type is a viewing-dependent probability

Unification and X-rays

Evidence for types 1 amp 2 orientation-dependence in

both X-ray absorption and reprocessing

Absorption-corrected type 2 spectra amp luminosities

are similar to type 1 (Smith amp Done 96 Turner et al

97)

BUT

The ldquoX-ray torusrdquo probably

does not coincide with the ldquodusty torusrdquo

Dusty vs X-rays Torus

NH(X-ray) ~ 3 mdash 100 NH(UV) (Maiolino et al 01)

From IR modeling NH(torus) lt~ 1024 cm-2 yet at

least ~50 of Seyfert 2 are Compton thick (Guainazzi

et al 05)

Fast X-ray variations mdash absorbing clouds are dust-

free

Risaliti Elvis amp Nicastro 02

RXRs

Dusty vs X-rays Torus (2)

X-ray observations + IR observations and modeling

NH(X-ray) ~ 10 NH(torus)

If Nclouds ~ 1r2 then RX ~ Rs10 (and Rs ~ 09 L1212 pc)

RX

Rs

f2(X-rays) may be

quite different from

f2(UVoptical) Sarah Gallagher (Tuesday)

Compton thick ldquox-ray onlyrdquo absorption in QSO1 (x-ray and UV not consistent with each other)

Torus Size NGC1068 2m imaging ndash R ~ 1 pc (Weigelt et al 04)

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

04)

Cen A 2m ndash R lt 05 pc (Prieto et al 04)

9 amp 18m ndash R lt 2 pc (Radomski et al 06)

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

8 amp 18m ndash R lt 2 pc (Packham et al 05)

NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto et al 04)All observations are consistent with RoutRs no larger than ~20-30 and perhaps even

only ~5-10

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

Everett amp Konigl 00

Cloud Properties in Torus Outflow

v ~ 20 ndash 150 NH ~ 1022 ndash 1023 cm-2 Resistance to tidal shearing

n gt 107 M7 rpc3 cm-3

Rc lt 1016 NH23 rpc3 M7 cm

Mc lt 710-3 NH23 Rc162 Mo

B ~ 15 1kms n712 mG

Elitzur amp Shlosman 2006

Unification Scheme

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

Unification Statisticsf2 mdash fraction of obscured sources = N2(N1 + N2)

Seyferts f2 = 70 Schmitt et al 01

f2 = 50 Hao et al 05

f2 decreases with luminosity (Simpson 05 Hao et al)

mdash ldquoreceding torusrdquo (Lawrence 91)

f2 = sin = 05 mdash 07

HR = tan ~ 07 mdash 1

R

Rs

H

Basic Premise AGN type determined uniquely by viewing angle

Clumpy Unification

Nc() = N0 exp(-22)

f2 depends on both and N0

Type 1 sources from ldquotype 2 viewingrdquo and vice versa

Flips between type 1 amp 2 (Aretxaga et al 99)

f2 variations may arise from either or N0 or both

AGN type is a viewing-dependent probability

Unification and X-rays

Evidence for types 1 amp 2 orientation-dependence in

both X-ray absorption and reprocessing

Absorption-corrected type 2 spectra amp luminosities

are similar to type 1 (Smith amp Done 96 Turner et al

97)

BUT

The ldquoX-ray torusrdquo probably

does not coincide with the ldquodusty torusrdquo

Dusty vs X-rays Torus

NH(X-ray) ~ 3 mdash 100 NH(UV) (Maiolino et al 01)

From IR modeling NH(torus) lt~ 1024 cm-2 yet at

least ~50 of Seyfert 2 are Compton thick (Guainazzi

et al 05)

Fast X-ray variations mdash absorbing clouds are dust-

free

Risaliti Elvis amp Nicastro 02

RXRs

Dusty vs X-rays Torus (2)

X-ray observations + IR observations and modeling

NH(X-ray) ~ 10 NH(torus)

If Nclouds ~ 1r2 then RX ~ Rs10 (and Rs ~ 09 L1212 pc)

RX

Rs

f2(X-rays) may be

quite different from

f2(UVoptical) Sarah Gallagher (Tuesday)

Compton thick ldquox-ray onlyrdquo absorption in QSO1 (x-ray and UV not consistent with each other)

Torus Size NGC1068 2m imaging ndash R ~ 1 pc (Weigelt et al 04)

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

04)

Cen A 2m ndash R lt 05 pc (Prieto et al 04)

9 amp 18m ndash R lt 2 pc (Radomski et al 06)

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

8 amp 18m ndash R lt 2 pc (Packham et al 05)

NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto et al 04)All observations are consistent with RoutRs no larger than ~20-30 and perhaps even

only ~5-10

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

Everett amp Konigl 00

Cloud Properties in Torus Outflow

v ~ 20 ndash 150 NH ~ 1022 ndash 1023 cm-2 Resistance to tidal shearing

n gt 107 M7 rpc3 cm-3

Rc lt 1016 NH23 rpc3 M7 cm

Mc lt 710-3 NH23 Rc162 Mo

B ~ 15 1kms n712 mG

Elitzur amp Shlosman 2006

Unification Scheme

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

Clumpy Unification

Nc() = N0 exp(-22)

f2 depends on both and N0

Type 1 sources from ldquotype 2 viewingrdquo and vice versa

Flips between type 1 amp 2 (Aretxaga et al 99)

f2 variations may arise from either or N0 or both

AGN type is a viewing-dependent probability

Unification and X-rays

Evidence for types 1 amp 2 orientation-dependence in

both X-ray absorption and reprocessing

Absorption-corrected type 2 spectra amp luminosities

are similar to type 1 (Smith amp Done 96 Turner et al

97)

BUT

The ldquoX-ray torusrdquo probably

does not coincide with the ldquodusty torusrdquo

Dusty vs X-rays Torus

NH(X-ray) ~ 3 mdash 100 NH(UV) (Maiolino et al 01)

From IR modeling NH(torus) lt~ 1024 cm-2 yet at

least ~50 of Seyfert 2 are Compton thick (Guainazzi

et al 05)

Fast X-ray variations mdash absorbing clouds are dust-

free

Risaliti Elvis amp Nicastro 02

RXRs

Dusty vs X-rays Torus (2)

X-ray observations + IR observations and modeling

NH(X-ray) ~ 10 NH(torus)

If Nclouds ~ 1r2 then RX ~ Rs10 (and Rs ~ 09 L1212 pc)

RX

Rs

f2(X-rays) may be

quite different from

f2(UVoptical) Sarah Gallagher (Tuesday)

Compton thick ldquox-ray onlyrdquo absorption in QSO1 (x-ray and UV not consistent with each other)

Torus Size NGC1068 2m imaging ndash R ~ 1 pc (Weigelt et al 04)

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

04)

Cen A 2m ndash R lt 05 pc (Prieto et al 04)

9 amp 18m ndash R lt 2 pc (Radomski et al 06)

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

8 amp 18m ndash R lt 2 pc (Packham et al 05)

NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto et al 04)All observations are consistent with RoutRs no larger than ~20-30 and perhaps even

only ~5-10

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

Everett amp Konigl 00

Cloud Properties in Torus Outflow

v ~ 20 ndash 150 NH ~ 1022 ndash 1023 cm-2 Resistance to tidal shearing

n gt 107 M7 rpc3 cm-3

Rc lt 1016 NH23 rpc3 M7 cm

Mc lt 710-3 NH23 Rc162 Mo

B ~ 15 1kms n712 mG

Elitzur amp Shlosman 2006

Unification Scheme

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

Unification and X-rays

Evidence for types 1 amp 2 orientation-dependence in

both X-ray absorption and reprocessing

Absorption-corrected type 2 spectra amp luminosities

are similar to type 1 (Smith amp Done 96 Turner et al

97)

BUT

The ldquoX-ray torusrdquo probably

does not coincide with the ldquodusty torusrdquo

Dusty vs X-rays Torus

NH(X-ray) ~ 3 mdash 100 NH(UV) (Maiolino et al 01)

From IR modeling NH(torus) lt~ 1024 cm-2 yet at

least ~50 of Seyfert 2 are Compton thick (Guainazzi

et al 05)

Fast X-ray variations mdash absorbing clouds are dust-

free

Risaliti Elvis amp Nicastro 02

RXRs

Dusty vs X-rays Torus (2)

X-ray observations + IR observations and modeling

NH(X-ray) ~ 10 NH(torus)

If Nclouds ~ 1r2 then RX ~ Rs10 (and Rs ~ 09 L1212 pc)

RX

Rs

f2(X-rays) may be

quite different from

f2(UVoptical) Sarah Gallagher (Tuesday)

Compton thick ldquox-ray onlyrdquo absorption in QSO1 (x-ray and UV not consistent with each other)

Torus Size NGC1068 2m imaging ndash R ~ 1 pc (Weigelt et al 04)

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

04)

Cen A 2m ndash R lt 05 pc (Prieto et al 04)

9 amp 18m ndash R lt 2 pc (Radomski et al 06)

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

8 amp 18m ndash R lt 2 pc (Packham et al 05)

NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto et al 04)All observations are consistent with RoutRs no larger than ~20-30 and perhaps even

only ~5-10

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

Everett amp Konigl 00

Cloud Properties in Torus Outflow

v ~ 20 ndash 150 NH ~ 1022 ndash 1023 cm-2 Resistance to tidal shearing

n gt 107 M7 rpc3 cm-3

Rc lt 1016 NH23 rpc3 M7 cm

Mc lt 710-3 NH23 Rc162 Mo

B ~ 15 1kms n712 mG

Elitzur amp Shlosman 2006

Unification Scheme

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

Dusty vs X-rays Torus

NH(X-ray) ~ 3 mdash 100 NH(UV) (Maiolino et al 01)

From IR modeling NH(torus) lt~ 1024 cm-2 yet at

least ~50 of Seyfert 2 are Compton thick (Guainazzi

et al 05)

Fast X-ray variations mdash absorbing clouds are dust-

free

Risaliti Elvis amp Nicastro 02

RXRs

Dusty vs X-rays Torus (2)

X-ray observations + IR observations and modeling

NH(X-ray) ~ 10 NH(torus)

If Nclouds ~ 1r2 then RX ~ Rs10 (and Rs ~ 09 L1212 pc)

RX

Rs

f2(X-rays) may be

quite different from

f2(UVoptical) Sarah Gallagher (Tuesday)

Compton thick ldquox-ray onlyrdquo absorption in QSO1 (x-ray and UV not consistent with each other)

Torus Size NGC1068 2m imaging ndash R ~ 1 pc (Weigelt et al 04)

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

04)

Cen A 2m ndash R lt 05 pc (Prieto et al 04)

9 amp 18m ndash R lt 2 pc (Radomski et al 06)

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

8 amp 18m ndash R lt 2 pc (Packham et al 05)

NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto et al 04)All observations are consistent with RoutRs no larger than ~20-30 and perhaps even

only ~5-10

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

Everett amp Konigl 00

Cloud Properties in Torus Outflow

v ~ 20 ndash 150 NH ~ 1022 ndash 1023 cm-2 Resistance to tidal shearing

n gt 107 M7 rpc3 cm-3

Rc lt 1016 NH23 rpc3 M7 cm

Mc lt 710-3 NH23 Rc162 Mo

B ~ 15 1kms n712 mG

Elitzur amp Shlosman 2006

Unification Scheme

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

Dusty vs X-rays Torus (2)

X-ray observations + IR observations and modeling

NH(X-ray) ~ 10 NH(torus)

If Nclouds ~ 1r2 then RX ~ Rs10 (and Rs ~ 09 L1212 pc)

RX

Rs

f2(X-rays) may be

quite different from

f2(UVoptical) Sarah Gallagher (Tuesday)

Compton thick ldquox-ray onlyrdquo absorption in QSO1 (x-ray and UV not consistent with each other)

Torus Size NGC1068 2m imaging ndash R ~ 1 pc (Weigelt et al 04)

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

04)

Cen A 2m ndash R lt 05 pc (Prieto et al 04)

9 amp 18m ndash R lt 2 pc (Radomski et al 06)

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

8 amp 18m ndash R lt 2 pc (Packham et al 05)

NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto et al 04)All observations are consistent with RoutRs no larger than ~20-30 and perhaps even

only ~5-10

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

Everett amp Konigl 00

Cloud Properties in Torus Outflow

v ~ 20 ndash 150 NH ~ 1022 ndash 1023 cm-2 Resistance to tidal shearing

n gt 107 M7 rpc3 cm-3

Rc lt 1016 NH23 rpc3 M7 cm

Mc lt 710-3 NH23 Rc162 Mo

B ~ 15 1kms n712 mG

Elitzur amp Shlosman 2006

Unification Scheme

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

Torus Size NGC1068 2m imaging ndash R ~ 1 pc (Weigelt et al 04)

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

04)

Cen A 2m ndash R lt 05 pc (Prieto et al 04)

9 amp 18m ndash R lt 2 pc (Radomski et al 06)

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

8 amp 18m ndash R lt 2 pc (Packham et al 05)

NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto et al 04)All observations are consistent with RoutRs no larger than ~20-30 and perhaps even

only ~5-10

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

Everett amp Konigl 00

Cloud Properties in Torus Outflow

v ~ 20 ndash 150 NH ~ 1022 ndash 1023 cm-2 Resistance to tidal shearing

n gt 107 M7 rpc3 cm-3

Rc lt 1016 NH23 rpc3 M7 cm

Mc lt 710-3 NH23 Rc162 Mo

B ~ 15 1kms n712 mG

Elitzur amp Shlosman 2006

Unification Scheme

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

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

Everett amp Konigl 00

Cloud Properties in Torus Outflow

v ~ 20 ndash 150 NH ~ 1022 ndash 1023 cm-2 Resistance to tidal shearing

n gt 107 M7 rpc3 cm-3

Rc lt 1016 NH23 rpc3 M7 cm

Mc lt 710-3 NH23 Rc162 Mo

B ~ 15 1kms n712 mG

Elitzur amp Shlosman 2006

Unification Scheme

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

The Torus as a Disk-Wind Region

Bottorff et al 97

Everett amp Konigl 00

Cloud Properties in Torus Outflow

v ~ 20 ndash 150 NH ~ 1022 ndash 1023 cm-2 Resistance to tidal shearing

n gt 107 M7 rpc3 cm-3

Rc lt 1016 NH23 rpc3 M7 cm

Mc lt 710-3 NH23 Rc162 Mo

B ~ 15 1kms n712 mG

Elitzur amp Shlosman 2006

Unification Scheme

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

Cloud Properties in Torus Outflow

v ~ 20 ndash 150 NH ~ 1022 ndash 1023 cm-2 Resistance to tidal shearing

n gt 107 M7 rpc3 cm-3

Rc lt 1016 NH23 rpc3 M7 cm

Mc lt 710-3 NH23 Rc162 Mo

B ~ 15 1kms n712 mG

Elitzur amp Shlosman 2006

Unification Scheme

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

Unification Scheme

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

Grand Unification Scheme

masersEmmering Blandford amp Shlosman 92

BLR

Broad Lines

Region BALBroad Absorption

Lines

TORUS

Toroidal Obscuration Required by Unified

Schemes

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

Outflow and Accretion

145acc yrML020M

Torus disappears at L lt~ 1042 erg s-1

1I 6T

23H2145acc

out vNL

1MM

116

T23H

2145out yrMvNL020M I

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

Torus Disappearance at Low Luminosities

Nucleus visible at L lt~ 1042 erg s-1 radio galaxies

(Chiaberge et al 99) and LINERs (Maoz et al 05)

No torus dust emission in M87 (Whysong amp

Antonucci 04 Perlman et al 06) and NGC 1097

(Masson et al 06)

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

If only TORUS is removed all low-luminosity AGN become

type 1HOWEVER

Both type 1 and type 2 LINERs do exist

(Maoz et al 05)

ldquotruerdquo type 2 AGN exist at L lt 1042 erg

s-1 (Laor 03)

THEREFORE

BLR must disappear at some lower L

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

TorusBLR

Wind diminishes mdash mass outflow directed to jets ()

Ho (2002) Radio loudness varies inversely with Macc

Similar effect in x-ray binaries

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

Accre

tion R

ate

Radio

Lo

ud

ness

Full Unification Scheme

both type 1 amp 2

molecular outflow extinguished

Torus disappears type 1 only

atomic outflow extinguished

BLR disappears ldquotruerdquo type 2

High

High

Low

Low

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study

Issues for Study

Itrsquos all probabilities

X-ray vs UVoptical TORUS properties

f2 decrease at high L mdash NH or

TORUS disappearance at low L mdash NH or

v

Low-luminosity end of AGN

bull IR emission

bull Switch from outflow to jets

• Unification Issues and the AGN TORUS
• Unification prediction 1
• Slide 3
• IR Puzzle 1
• Temperature in Clumpy Medium
• IR Puzzle 2
• Clumpy Torus ndash Radial Density Variation
• Clumpy Torus Modeling
• Slide 9
• Slide 10
• Unification and X-rays
• Dusty vs X-rays Torus
• Dusty vs X-rays Torus (2)
• Torus Size
• Dynamic Origin of Vertical Structure
• The Torus as a Disk-Wind Region
• Cloud Properties in Torus Outflow
• Unification Scheme
• Grand Unification Scheme
• Outflow and Accretion
• Torus Disappearance at Low Luminosities
• Slide 22
• Slide 23
• Slide 24
• Issues for Study