Disk Winds and Dusty Tori : Theory & Observations
30
Disk Winds and Dusty Tori: Theory & Observations Moshe Elitzur University of Kentucky
description
Disk Winds and Dusty Tori : Theory & Observations. Moshe Elitzur University of Kentucky . Unified Scheme for AGN. T oroidal O bscuration R equired by U nification S chemes. M ~ 10 6 – 10 10 M R s ~ 10 11 – 10 15 cm. - PowerPoint PPT Presentation
Transcript of Disk Winds and Dusty Tori : Theory & Observations
Disk Winds and Dusty Tori Theory amp Observations
Moshe Elitzur University of Kentucky
Unified Scheme for AGN
M ~ 106 ndash 1010 MRs ~ 1011 ndash 1015
cm
Toroidal
Obscuration
Required by
Unification
SchemesObscuring matter mdash optically thick dusty clouds Krolik amp Begelman lsquo88
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind ParadigmBlandford amp Payne lsquo82
Origin of the 100rsquos pc Torus ndash Modeling IR emission
Pier amp Krolik 93
~100 pc
Pier amp Krolik 92
5-10 pc
Granato et al rsquo94 lsquo97bull Uniform densitybull Rout ~ 100 ndash 300 pc
Dearth of IR emission in smooth-density models T r
Torus ndash direct evidence NGC 1068
VLTI 8-13 m
r 17 pc T = 320 K
Jaffe et al lsquo04
T gt 800 K
Close proximity of hot and cooler dust
Very compact torus
D = 144 Mpc 01rdquo = 72 pc
Torus Size
Size scale ndash dust sublimation radius Rd = 04 L45
frac12 pc
All observations are consistent with RoutRd no larger than ~2030 and perhaps even
only ~510
Smooth density ndash T amp R uniquely related
Clumpy density ndash different T at same Rdifferent R same T
Tmax
Tmin
Temperature in a Clumpy Medium
Nenkova+ 08a
Black-Hole Influence Radius RBH
vrot ~ 100 kmsR ~ 100 pc
Sofue et al 99
kmspc1~r
)r(MGr
)r(v 21
3
RBH = 35pc (M721)13
At RBH (RBH) = (RBH) M(RBH) = M
Grand Unification Theory ndash the Disk Wind Scenario
masers
Emmering Blandford amp Shlosman 92
BLR
Broad Line Region WA
Warm Absorber
TOR
Toroidal Obscuration Region
Cloud Properties in TOR OutflowIR modeling v ~ 30 ndash 100 NH ~ 1022 ndash 1023 cm-2
n gt 107 M7 rpc3 cm-3
Rc lt 1016 NH23 rpc3 M7 cm
Mc lt 710-3 NH23 Rc162 M
B ~ 15 1kms n712 mG
Elitzur amp Shlosman 06
Resistance to tidal shearing
Circinus Water Masers
Greenhill+ 03
02 pc
Circinus VLTI Imaging
Tristram+ 07
BLRTOR Mass Outflow Rate
IN)R(vmRM Rdzdout 2 Rd Lfrac12
vz(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
22 cMcML accBHacc lt 1
Rfrac34
frac12
acc
out NLM
MM
BLRTOR outflow must disappear at small L
TOR Disappearance at L lt~ 1042 erg s-1
Obscuration disappears in bull FR I (Chiaberge+ 99)bull Liners (Maoz+ 05) bull low-luminosity Sy2 (Panessa amp Bassani 02)
No torus dust emissionbull in M87 (Whysong amp Antonucci 04 Perlman+
07)bull in FR I and ~ half of FR II (van der Wolk+ 09)
BLR Disappearance in LLAGNsBLR existence L gt C M23 ie L gt C (LEddL)2
log L = 35 + 23 log M
log L = 288 ndash 2 log (LLEdd)
4middot10-4 radiatively inefficient accretion
Elitzur amp Ho 2009
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
Radio-loudness Ho lsquo02
Rrsquo = LradLopt = LLEdd
R = LradLopt = LLEdd
Radio-loudness Sikora+ lsquo07
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Unified Scheme for AGN
M ~ 106 ndash 1010 MRs ~ 1011 ndash 1015
cm
Toroidal
Obscuration
Required by
Unification
SchemesObscuring matter mdash optically thick dusty clouds Krolik amp Begelman lsquo88
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind ParadigmBlandford amp Payne lsquo82
Origin of the 100rsquos pc Torus ndash Modeling IR emission
Pier amp Krolik 93
~100 pc
Pier amp Krolik 92
5-10 pc
Granato et al rsquo94 lsquo97bull Uniform densitybull Rout ~ 100 ndash 300 pc
Dearth of IR emission in smooth-density models T r
Torus ndash direct evidence NGC 1068
VLTI 8-13 m
r 17 pc T = 320 K
Jaffe et al lsquo04
T gt 800 K
Close proximity of hot and cooler dust
Very compact torus
D = 144 Mpc 01rdquo = 72 pc
Torus Size
Size scale ndash dust sublimation radius Rd = 04 L45
frac12 pc
All observations are consistent with RoutRd no larger than ~2030 and perhaps even
only ~510
Smooth density ndash T amp R uniquely related
Clumpy density ndash different T at same Rdifferent R same T
Tmax
Tmin
Temperature in a Clumpy Medium
Nenkova+ 08a
Black-Hole Influence Radius RBH
vrot ~ 100 kmsR ~ 100 pc
Sofue et al 99
kmspc1~r
)r(MGr
)r(v 21
3
RBH = 35pc (M721)13
At RBH (RBH) = (RBH) M(RBH) = M
Grand Unification Theory ndash the Disk Wind Scenario
masers
Emmering Blandford amp Shlosman 92
BLR
Broad Line Region WA
Warm Absorber
TOR
Toroidal Obscuration Region
Cloud Properties in TOR OutflowIR modeling v ~ 30 ndash 100 NH ~ 1022 ndash 1023 cm-2
n gt 107 M7 rpc3 cm-3
Rc lt 1016 NH23 rpc3 M7 cm
Mc lt 710-3 NH23 Rc162 M
B ~ 15 1kms n712 mG
Elitzur amp Shlosman 06
Resistance to tidal shearing
Circinus Water Masers
Greenhill+ 03
02 pc
Circinus VLTI Imaging
Tristram+ 07
BLRTOR Mass Outflow Rate
IN)R(vmRM Rdzdout 2 Rd Lfrac12
vz(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
22 cMcML accBHacc lt 1
Rfrac34
frac12
acc
out NLM
MM
BLRTOR outflow must disappear at small L
TOR Disappearance at L lt~ 1042 erg s-1
Obscuration disappears in bull FR I (Chiaberge+ 99)bull Liners (Maoz+ 05) bull low-luminosity Sy2 (Panessa amp Bassani 02)
No torus dust emissionbull in M87 (Whysong amp Antonucci 04 Perlman+
07)bull in FR I and ~ half of FR II (van der Wolk+ 09)
BLR Disappearance in LLAGNsBLR existence L gt C M23 ie L gt C (LEddL)2
log L = 35 + 23 log M
log L = 288 ndash 2 log (LLEdd)
4middot10-4 radiatively inefficient accretion
Elitzur amp Ho 2009
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
Radio-loudness Ho lsquo02
Rrsquo = LradLopt = LLEdd
R = LradLopt = LLEdd
Radio-loudness Sikora+ lsquo07
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind ParadigmBlandford amp Payne lsquo82
Origin of the 100rsquos pc Torus ndash Modeling IR emission
Pier amp Krolik 93
~100 pc
Pier amp Krolik 92
5-10 pc
Granato et al rsquo94 lsquo97bull Uniform densitybull Rout ~ 100 ndash 300 pc
Dearth of IR emission in smooth-density models T r
Torus ndash direct evidence NGC 1068
VLTI 8-13 m
r 17 pc T = 320 K
Jaffe et al lsquo04
T gt 800 K
Close proximity of hot and cooler dust
Very compact torus
D = 144 Mpc 01rdquo = 72 pc
Torus Size
Size scale ndash dust sublimation radius Rd = 04 L45
frac12 pc
All observations are consistent with RoutRd no larger than ~2030 and perhaps even
only ~510
Smooth density ndash T amp R uniquely related
Clumpy density ndash different T at same Rdifferent R same T
Tmax
Tmin
Temperature in a Clumpy Medium
Nenkova+ 08a
Black-Hole Influence Radius RBH
vrot ~ 100 kmsR ~ 100 pc
Sofue et al 99
kmspc1~r
)r(MGr
)r(v 21
3
RBH = 35pc (M721)13
At RBH (RBH) = (RBH) M(RBH) = M
Grand Unification Theory ndash the Disk Wind Scenario
masers
Emmering Blandford amp Shlosman 92
BLR
Broad Line Region WA
Warm Absorber
TOR
Toroidal Obscuration Region
Cloud Properties in TOR OutflowIR modeling v ~ 30 ndash 100 NH ~ 1022 ndash 1023 cm-2
n gt 107 M7 rpc3 cm-3
Rc lt 1016 NH23 rpc3 M7 cm
Mc lt 710-3 NH23 Rc162 M
B ~ 15 1kms n712 mG
Elitzur amp Shlosman 06
Resistance to tidal shearing
Circinus Water Masers
Greenhill+ 03
02 pc
Circinus VLTI Imaging
Tristram+ 07
BLRTOR Mass Outflow Rate
IN)R(vmRM Rdzdout 2 Rd Lfrac12
vz(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
22 cMcML accBHacc lt 1
Rfrac34
frac12
acc
out NLM
MM
BLRTOR outflow must disappear at small L
TOR Disappearance at L lt~ 1042 erg s-1
Obscuration disappears in bull FR I (Chiaberge+ 99)bull Liners (Maoz+ 05) bull low-luminosity Sy2 (Panessa amp Bassani 02)
No torus dust emissionbull in M87 (Whysong amp Antonucci 04 Perlman+
07)bull in FR I and ~ half of FR II (van der Wolk+ 09)
BLR Disappearance in LLAGNsBLR existence L gt C M23 ie L gt C (LEddL)2
log L = 35 + 23 log M
log L = 288 ndash 2 log (LLEdd)
4middot10-4 radiatively inefficient accretion
Elitzur amp Ho 2009
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
Radio-loudness Ho lsquo02
Rrsquo = LradLopt = LLEdd
R = LradLopt = LLEdd
Radio-loudness Sikora+ lsquo07
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Origin of the 100rsquos pc Torus ndash Modeling IR emission
Pier amp Krolik 93
~100 pc
Pier amp Krolik 92
5-10 pc
Granato et al rsquo94 lsquo97bull Uniform densitybull Rout ~ 100 ndash 300 pc
Dearth of IR emission in smooth-density models T r
Torus ndash direct evidence NGC 1068
VLTI 8-13 m
r 17 pc T = 320 K
Jaffe et al lsquo04
T gt 800 K
Close proximity of hot and cooler dust
Very compact torus
D = 144 Mpc 01rdquo = 72 pc
Torus Size
Size scale ndash dust sublimation radius Rd = 04 L45
frac12 pc
All observations are consistent with RoutRd no larger than ~2030 and perhaps even
only ~510
Smooth density ndash T amp R uniquely related
Clumpy density ndash different T at same Rdifferent R same T
Tmax
Tmin
Temperature in a Clumpy Medium
Nenkova+ 08a
Black-Hole Influence Radius RBH
vrot ~ 100 kmsR ~ 100 pc
Sofue et al 99
kmspc1~r
)r(MGr
)r(v 21
3
RBH = 35pc (M721)13
At RBH (RBH) = (RBH) M(RBH) = M
Grand Unification Theory ndash the Disk Wind Scenario
masers
Emmering Blandford amp Shlosman 92
BLR
Broad Line Region WA
Warm Absorber
TOR
Toroidal Obscuration Region
Cloud Properties in TOR OutflowIR modeling v ~ 30 ndash 100 NH ~ 1022 ndash 1023 cm-2
n gt 107 M7 rpc3 cm-3
Rc lt 1016 NH23 rpc3 M7 cm
Mc lt 710-3 NH23 Rc162 M
B ~ 15 1kms n712 mG
Elitzur amp Shlosman 06
Resistance to tidal shearing
Circinus Water Masers
Greenhill+ 03
02 pc
Circinus VLTI Imaging
Tristram+ 07
BLRTOR Mass Outflow Rate
IN)R(vmRM Rdzdout 2 Rd Lfrac12
vz(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
22 cMcML accBHacc lt 1
Rfrac34
frac12
acc
out NLM
MM
BLRTOR outflow must disappear at small L
TOR Disappearance at L lt~ 1042 erg s-1
Obscuration disappears in bull FR I (Chiaberge+ 99)bull Liners (Maoz+ 05) bull low-luminosity Sy2 (Panessa amp Bassani 02)
No torus dust emissionbull in M87 (Whysong amp Antonucci 04 Perlman+
07)bull in FR I and ~ half of FR II (van der Wolk+ 09)
BLR Disappearance in LLAGNsBLR existence L gt C M23 ie L gt C (LEddL)2
log L = 35 + 23 log M
log L = 288 ndash 2 log (LLEdd)
4middot10-4 radiatively inefficient accretion
Elitzur amp Ho 2009
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
Radio-loudness Ho lsquo02
Rrsquo = LradLopt = LLEdd
R = LradLopt = LLEdd
Radio-loudness Sikora+ lsquo07
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Torus ndash direct evidence NGC 1068
VLTI 8-13 m
r 17 pc T = 320 K
Jaffe et al lsquo04
T gt 800 K
Close proximity of hot and cooler dust
Very compact torus
D = 144 Mpc 01rdquo = 72 pc
Torus Size
Size scale ndash dust sublimation radius Rd = 04 L45
frac12 pc
All observations are consistent with RoutRd no larger than ~2030 and perhaps even
only ~510
Smooth density ndash T amp R uniquely related
Clumpy density ndash different T at same Rdifferent R same T
Tmax
Tmin
Temperature in a Clumpy Medium
Nenkova+ 08a
Black-Hole Influence Radius RBH
vrot ~ 100 kmsR ~ 100 pc
Sofue et al 99
kmspc1~r
)r(MGr
)r(v 21
3
RBH = 35pc (M721)13
At RBH (RBH) = (RBH) M(RBH) = M
Grand Unification Theory ndash the Disk Wind Scenario
masers
Emmering Blandford amp Shlosman 92
BLR
Broad Line Region WA
Warm Absorber
TOR
Toroidal Obscuration Region
Cloud Properties in TOR OutflowIR modeling v ~ 30 ndash 100 NH ~ 1022 ndash 1023 cm-2
n gt 107 M7 rpc3 cm-3
Rc lt 1016 NH23 rpc3 M7 cm
Mc lt 710-3 NH23 Rc162 M
B ~ 15 1kms n712 mG
Elitzur amp Shlosman 06
Resistance to tidal shearing
Circinus Water Masers
Greenhill+ 03
02 pc
Circinus VLTI Imaging
Tristram+ 07
BLRTOR Mass Outflow Rate
IN)R(vmRM Rdzdout 2 Rd Lfrac12
vz(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
22 cMcML accBHacc lt 1
Rfrac34
frac12
acc
out NLM
MM
BLRTOR outflow must disappear at small L
TOR Disappearance at L lt~ 1042 erg s-1
Obscuration disappears in bull FR I (Chiaberge+ 99)bull Liners (Maoz+ 05) bull low-luminosity Sy2 (Panessa amp Bassani 02)
No torus dust emissionbull in M87 (Whysong amp Antonucci 04 Perlman+
07)bull in FR I and ~ half of FR II (van der Wolk+ 09)
BLR Disappearance in LLAGNsBLR existence L gt C M23 ie L gt C (LEddL)2
log L = 35 + 23 log M
log L = 288 ndash 2 log (LLEdd)
4middot10-4 radiatively inefficient accretion
Elitzur amp Ho 2009
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
Radio-loudness Ho lsquo02
Rrsquo = LradLopt = LLEdd
R = LradLopt = LLEdd
Radio-loudness Sikora+ lsquo07
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Torus Size
Size scale ndash dust sublimation radius Rd = 04 L45
frac12 pc
All observations are consistent with RoutRd no larger than ~2030 and perhaps even
only ~510
Smooth density ndash T amp R uniquely related
Clumpy density ndash different T at same Rdifferent R same T
Tmax
Tmin
Temperature in a Clumpy Medium
Nenkova+ 08a
Black-Hole Influence Radius RBH
vrot ~ 100 kmsR ~ 100 pc
Sofue et al 99
kmspc1~r
)r(MGr
)r(v 21
3
RBH = 35pc (M721)13
At RBH (RBH) = (RBH) M(RBH) = M
Grand Unification Theory ndash the Disk Wind Scenario
masers
Emmering Blandford amp Shlosman 92
BLR
Broad Line Region WA
Warm Absorber
TOR
Toroidal Obscuration Region
Cloud Properties in TOR OutflowIR modeling v ~ 30 ndash 100 NH ~ 1022 ndash 1023 cm-2
n gt 107 M7 rpc3 cm-3
Rc lt 1016 NH23 rpc3 M7 cm
Mc lt 710-3 NH23 Rc162 M
B ~ 15 1kms n712 mG
Elitzur amp Shlosman 06
Resistance to tidal shearing
Circinus Water Masers
Greenhill+ 03
02 pc
Circinus VLTI Imaging
Tristram+ 07
BLRTOR Mass Outflow Rate
IN)R(vmRM Rdzdout 2 Rd Lfrac12
vz(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
22 cMcML accBHacc lt 1
Rfrac34
frac12
acc
out NLM
MM
BLRTOR outflow must disappear at small L
TOR Disappearance at L lt~ 1042 erg s-1
Obscuration disappears in bull FR I (Chiaberge+ 99)bull Liners (Maoz+ 05) bull low-luminosity Sy2 (Panessa amp Bassani 02)
No torus dust emissionbull in M87 (Whysong amp Antonucci 04 Perlman+
07)bull in FR I and ~ half of FR II (van der Wolk+ 09)
BLR Disappearance in LLAGNsBLR existence L gt C M23 ie L gt C (LEddL)2
log L = 35 + 23 log M
log L = 288 ndash 2 log (LLEdd)
4middot10-4 radiatively inefficient accretion
Elitzur amp Ho 2009
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
Radio-loudness Ho lsquo02
Rrsquo = LradLopt = LLEdd
R = LradLopt = LLEdd
Radio-loudness Sikora+ lsquo07
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Smooth density ndash T amp R uniquely related
Clumpy density ndash different T at same Rdifferent R same T
Tmax
Tmin
Temperature in a Clumpy Medium
Nenkova+ 08a
Black-Hole Influence Radius RBH
vrot ~ 100 kmsR ~ 100 pc
Sofue et al 99
kmspc1~r
)r(MGr
)r(v 21
3
RBH = 35pc (M721)13
At RBH (RBH) = (RBH) M(RBH) = M
Grand Unification Theory ndash the Disk Wind Scenario
masers
Emmering Blandford amp Shlosman 92
BLR
Broad Line Region WA
Warm Absorber
TOR
Toroidal Obscuration Region
Cloud Properties in TOR OutflowIR modeling v ~ 30 ndash 100 NH ~ 1022 ndash 1023 cm-2
n gt 107 M7 rpc3 cm-3
Rc lt 1016 NH23 rpc3 M7 cm
Mc lt 710-3 NH23 Rc162 M
B ~ 15 1kms n712 mG
Elitzur amp Shlosman 06
Resistance to tidal shearing
Circinus Water Masers
Greenhill+ 03
02 pc
Circinus VLTI Imaging
Tristram+ 07
BLRTOR Mass Outflow Rate
IN)R(vmRM Rdzdout 2 Rd Lfrac12
vz(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
22 cMcML accBHacc lt 1
Rfrac34
frac12
acc
out NLM
MM
BLRTOR outflow must disappear at small L
TOR Disappearance at L lt~ 1042 erg s-1
Obscuration disappears in bull FR I (Chiaberge+ 99)bull Liners (Maoz+ 05) bull low-luminosity Sy2 (Panessa amp Bassani 02)
No torus dust emissionbull in M87 (Whysong amp Antonucci 04 Perlman+
07)bull in FR I and ~ half of FR II (van der Wolk+ 09)
BLR Disappearance in LLAGNsBLR existence L gt C M23 ie L gt C (LEddL)2
log L = 35 + 23 log M
log L = 288 ndash 2 log (LLEdd)
4middot10-4 radiatively inefficient accretion
Elitzur amp Ho 2009
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
Radio-loudness Ho lsquo02
Rrsquo = LradLopt = LLEdd
R = LradLopt = LLEdd
Radio-loudness Sikora+ lsquo07
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Black-Hole Influence Radius RBH
vrot ~ 100 kmsR ~ 100 pc
Sofue et al 99
kmspc1~r
)r(MGr
)r(v 21
3
RBH = 35pc (M721)13
At RBH (RBH) = (RBH) M(RBH) = M
Grand Unification Theory ndash the Disk Wind Scenario
masers
Emmering Blandford amp Shlosman 92
BLR
Broad Line Region WA
Warm Absorber
TOR
Toroidal Obscuration Region
Cloud Properties in TOR OutflowIR modeling v ~ 30 ndash 100 NH ~ 1022 ndash 1023 cm-2
n gt 107 M7 rpc3 cm-3
Rc lt 1016 NH23 rpc3 M7 cm
Mc lt 710-3 NH23 Rc162 M
B ~ 15 1kms n712 mG
Elitzur amp Shlosman 06
Resistance to tidal shearing
Circinus Water Masers
Greenhill+ 03
02 pc
Circinus VLTI Imaging
Tristram+ 07
BLRTOR Mass Outflow Rate
IN)R(vmRM Rdzdout 2 Rd Lfrac12
vz(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
22 cMcML accBHacc lt 1
Rfrac34
frac12
acc
out NLM
MM
BLRTOR outflow must disappear at small L
TOR Disappearance at L lt~ 1042 erg s-1
Obscuration disappears in bull FR I (Chiaberge+ 99)bull Liners (Maoz+ 05) bull low-luminosity Sy2 (Panessa amp Bassani 02)
No torus dust emissionbull in M87 (Whysong amp Antonucci 04 Perlman+
07)bull in FR I and ~ half of FR II (van der Wolk+ 09)
BLR Disappearance in LLAGNsBLR existence L gt C M23 ie L gt C (LEddL)2
log L = 35 + 23 log M
log L = 288 ndash 2 log (LLEdd)
4middot10-4 radiatively inefficient accretion
Elitzur amp Ho 2009
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
Radio-loudness Ho lsquo02
Rrsquo = LradLopt = LLEdd
R = LradLopt = LLEdd
Radio-loudness Sikora+ lsquo07
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Grand Unification Theory ndash the Disk Wind Scenario
masers
Emmering Blandford amp Shlosman 92
BLR
Broad Line Region WA
Warm Absorber
TOR
Toroidal Obscuration Region
Cloud Properties in TOR OutflowIR modeling v ~ 30 ndash 100 NH ~ 1022 ndash 1023 cm-2
n gt 107 M7 rpc3 cm-3
Rc lt 1016 NH23 rpc3 M7 cm
Mc lt 710-3 NH23 Rc162 M
B ~ 15 1kms n712 mG
Elitzur amp Shlosman 06
Resistance to tidal shearing
Circinus Water Masers
Greenhill+ 03
02 pc
Circinus VLTI Imaging
Tristram+ 07
BLRTOR Mass Outflow Rate
IN)R(vmRM Rdzdout 2 Rd Lfrac12
vz(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
22 cMcML accBHacc lt 1
Rfrac34
frac12
acc
out NLM
MM
BLRTOR outflow must disappear at small L
TOR Disappearance at L lt~ 1042 erg s-1
Obscuration disappears in bull FR I (Chiaberge+ 99)bull Liners (Maoz+ 05) bull low-luminosity Sy2 (Panessa amp Bassani 02)
No torus dust emissionbull in M87 (Whysong amp Antonucci 04 Perlman+
07)bull in FR I and ~ half of FR II (van der Wolk+ 09)
BLR Disappearance in LLAGNsBLR existence L gt C M23 ie L gt C (LEddL)2
log L = 35 + 23 log M
log L = 288 ndash 2 log (LLEdd)
4middot10-4 radiatively inefficient accretion
Elitzur amp Ho 2009
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
Radio-loudness Ho lsquo02
Rrsquo = LradLopt = LLEdd
R = LradLopt = LLEdd
Radio-loudness Sikora+ lsquo07
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Cloud Properties in TOR OutflowIR modeling v ~ 30 ndash 100 NH ~ 1022 ndash 1023 cm-2
n gt 107 M7 rpc3 cm-3
Rc lt 1016 NH23 rpc3 M7 cm
Mc lt 710-3 NH23 Rc162 M
B ~ 15 1kms n712 mG
Elitzur amp Shlosman 06
Resistance to tidal shearing
Circinus Water Masers
Greenhill+ 03
02 pc
Circinus VLTI Imaging
Tristram+ 07
BLRTOR Mass Outflow Rate
IN)R(vmRM Rdzdout 2 Rd Lfrac12
vz(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
22 cMcML accBHacc lt 1
Rfrac34
frac12
acc
out NLM
MM
BLRTOR outflow must disappear at small L
TOR Disappearance at L lt~ 1042 erg s-1
Obscuration disappears in bull FR I (Chiaberge+ 99)bull Liners (Maoz+ 05) bull low-luminosity Sy2 (Panessa amp Bassani 02)
No torus dust emissionbull in M87 (Whysong amp Antonucci 04 Perlman+
07)bull in FR I and ~ half of FR II (van der Wolk+ 09)
BLR Disappearance in LLAGNsBLR existence L gt C M23 ie L gt C (LEddL)2
log L = 35 + 23 log M
log L = 288 ndash 2 log (LLEdd)
4middot10-4 radiatively inefficient accretion
Elitzur amp Ho 2009
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
Radio-loudness Ho lsquo02
Rrsquo = LradLopt = LLEdd
R = LradLopt = LLEdd
Radio-loudness Sikora+ lsquo07
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Circinus Water Masers
Greenhill+ 03
02 pc
Circinus VLTI Imaging
Tristram+ 07
BLRTOR Mass Outflow Rate
IN)R(vmRM Rdzdout 2 Rd Lfrac12
vz(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
22 cMcML accBHacc lt 1
Rfrac34
frac12
acc
out NLM
MM
BLRTOR outflow must disappear at small L
TOR Disappearance at L lt~ 1042 erg s-1
Obscuration disappears in bull FR I (Chiaberge+ 99)bull Liners (Maoz+ 05) bull low-luminosity Sy2 (Panessa amp Bassani 02)
No torus dust emissionbull in M87 (Whysong amp Antonucci 04 Perlman+
07)bull in FR I and ~ half of FR II (van der Wolk+ 09)
BLR Disappearance in LLAGNsBLR existence L gt C M23 ie L gt C (LEddL)2
log L = 35 + 23 log M
log L = 288 ndash 2 log (LLEdd)
4middot10-4 radiatively inefficient accretion
Elitzur amp Ho 2009
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
Radio-loudness Ho lsquo02
Rrsquo = LradLopt = LLEdd
R = LradLopt = LLEdd
Radio-loudness Sikora+ lsquo07
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Circinus VLTI Imaging
Tristram+ 07
BLRTOR Mass Outflow Rate
IN)R(vmRM Rdzdout 2 Rd Lfrac12
vz(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
22 cMcML accBHacc lt 1
Rfrac34
frac12
acc
out NLM
MM
BLRTOR outflow must disappear at small L
TOR Disappearance at L lt~ 1042 erg s-1
Obscuration disappears in bull FR I (Chiaberge+ 99)bull Liners (Maoz+ 05) bull low-luminosity Sy2 (Panessa amp Bassani 02)
No torus dust emissionbull in M87 (Whysong amp Antonucci 04 Perlman+
07)bull in FR I and ~ half of FR II (van der Wolk+ 09)
BLR Disappearance in LLAGNsBLR existence L gt C M23 ie L gt C (LEddL)2
log L = 35 + 23 log M
log L = 288 ndash 2 log (LLEdd)
4middot10-4 radiatively inefficient accretion
Elitzur amp Ho 2009
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
Radio-loudness Ho lsquo02
Rrsquo = LradLopt = LLEdd
R = LradLopt = LLEdd
Radio-loudness Sikora+ lsquo07
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
BLRTOR Mass Outflow Rate
IN)R(vmRM Rdzdout 2 Rd Lfrac12
vz(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
22 cMcML accBHacc lt 1
Rfrac34
frac12
acc
out NLM
MM
BLRTOR outflow must disappear at small L
TOR Disappearance at L lt~ 1042 erg s-1
Obscuration disappears in bull FR I (Chiaberge+ 99)bull Liners (Maoz+ 05) bull low-luminosity Sy2 (Panessa amp Bassani 02)
No torus dust emissionbull in M87 (Whysong amp Antonucci 04 Perlman+
07)bull in FR I and ~ half of FR II (van der Wolk+ 09)
BLR Disappearance in LLAGNsBLR existence L gt C M23 ie L gt C (LEddL)2
log L = 35 + 23 log M
log L = 288 ndash 2 log (LLEdd)
4middot10-4 radiatively inefficient accretion
Elitzur amp Ho 2009
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
Radio-loudness Ho lsquo02
Rrsquo = LradLopt = LLEdd
R = LradLopt = LLEdd
Radio-loudness Sikora+ lsquo07
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
TOR Disappearance at L lt~ 1042 erg s-1
Obscuration disappears in bull FR I (Chiaberge+ 99)bull Liners (Maoz+ 05) bull low-luminosity Sy2 (Panessa amp Bassani 02)
No torus dust emissionbull in M87 (Whysong amp Antonucci 04 Perlman+
07)bull in FR I and ~ half of FR II (van der Wolk+ 09)
BLR Disappearance in LLAGNsBLR existence L gt C M23 ie L gt C (LEddL)2
log L = 35 + 23 log M
log L = 288 ndash 2 log (LLEdd)
4middot10-4 radiatively inefficient accretion
Elitzur amp Ho 2009
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
Radio-loudness Ho lsquo02
Rrsquo = LradLopt = LLEdd
R = LradLopt = LLEdd
Radio-loudness Sikora+ lsquo07
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
BLR Disappearance in LLAGNsBLR existence L gt C M23 ie L gt C (LEddL)2
log L = 35 + 23 log M
log L = 288 ndash 2 log (LLEdd)
4middot10-4 radiatively inefficient accretion
Elitzur amp Ho 2009
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
Radio-loudness Ho lsquo02
Rrsquo = LradLopt = LLEdd
R = LradLopt = LLEdd
Radio-loudness Sikora+ lsquo07
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
Radio-loudness Ho lsquo02
Rrsquo = LradLopt = LLEdd
R = LradLopt = LLEdd
Radio-loudness Sikora+ lsquo07
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Radio-loudness Ho lsquo02
Rrsquo = LradLopt = LLEdd
R = LradLopt = LLEdd
Radio-loudness Sikora+ lsquo07
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
R = LradLopt = LLEdd
Radio-loudness Sikora+ lsquo07
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
Similar effect in X-ray binaries
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
COSMOS AGN
Trump+11
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Alternative BLRTOR Disappearance
Trump et al lsquo11 variant of Nicastro lsquo00
Prad = Pgas
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Two Independent Boundaries
ldquointermediaterdquo Sy1x H[OIII]5007 lt 1
N00 bound mdash dynamics EH09 bound mdash
ldquokinematicrdquo
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
A Two-Component BLR
Many Sy18 amp 19 show broad double-peaked Balmer lines mdash interpreted as disk emission
A wind+ldquodiskrdquo mix could naturally produce the sequence Sy1 12 15 1819
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
The ldquoAGN-Galaxy Connectionrdquo
MBH 4 mdash why are BH and bulge mass correlated
Causal connection same outflows quench both star formation and BH growth
Lkin ~ 1 LAGN
Ionized outflows detected (Arav+rsquo10) Affect star formation mdash molecular outflows Winds origin
bull Central QSObull Surrounding starburst
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Herschel OH(79m) Observations
Sturm+rsquo11
Mrk231 CO interferometry (Feruglio+rsquo10)
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
SB or AGN Wind
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
AGN Plausible Connection
Powerful Outflows
Clear-Up Timescales
High outflow rates are short lived AGN dominated
SF-dominated
AGN-dominated
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
BLRTOR Energy Outflow Rate
136z
27c
T23H
2145
37w sergvvNL107L I
dAvnvML zc2cc2
1w
Negligible in the AGN energy budget
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Source fAGN ()
LAGN (1011Lo)
Mdot (Moyr
)LAGNc2
(Moyr)Mrk231 71 28 1190 196IRAS08572+3915 72 12 970 084IRAS13120-5453 9 18 130 013IRAS14378-3651 lt45 lt72 740 lt050IRAS17208-0014 11 34 90 024NGC253 0 0 16 000
Outflow Origin
L(outflow) ~ 1LAGN buthellip Mass outflow rate incompatible with BH
accretion
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
Challenges BLRTOR outflow
bull Launch mechanismbull Detailed structurebull Reverberation mapping
LLAGNsbull BLR amp TOR disappearancebull Sy1x mdash 2-component BLRbull Jet dominancebull AGNmdashXRB analogy
AGN-Galaxy connectionbull Outflow mechanism
- Slide 1
- Unified Scheme for AGN
- Slide 3
- Origin of the 100rsquos pc Torus ndash Modeling IR emission
- Slide 5
- Torus Size
- Slide 7
- Black-Hole Influence Radius RBH
- Grand Unification Theory ndash the Disk Wind Scenario
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- BLRTOR Mass Outflow Rate
- TOR Disappearance at L lt~ 1042 erg s-1
- BLR Disappearance in LLAGNs
- Slide 16
- Radio-loudness Ho lsquo02
- Slide 18
- Slide 19
- COSMOS AGN
- Alternative BLRTOR Disappearance
- Two Independent Boundaries
- A Two-Component BLR
- The ldquoAGN-Galaxy Connectionrdquo
- Herschel OH(79m) Observations
- SB or AGN Wind
- AGN Plausible Connection
- BLRTOR Energy Outflow Rate
- Outflow Origin
- Challenges
-
