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
-