disk-outflow connection and the molecular dusty torus
DESCRIPTION
Disk-outflow Connection and the Molecular Dusty Torus. Moshe Elitzur University of Kentucky. Unification 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 PresentationTRANSCRIPT
Disk-outflow Connection and the Molecular Dusty Torus
Moshe Elitzur University of Kentucky
Unification Scheme for AGN
M ~ 106 ndash 1010 M
Rs ~ 1011 ndash 1015
cm
Toroidal
Obscuration
Required by
Unification
SchemesObscuring matter mdash optically thick dusty clouds Krolik amp
Begelman lsquo88
Torus Properties mdash Obscuration
Equatorial V gt~ 30 40
NH gt~ 1023 cm-2
f2 mdash fraction of obscured sources = N2(N1 + N2)
Seyferts f2 = 70 Schmitt+ lsquo01
f2 = 50 Hao+ lsquo05
f2 = sin = 05 mdash 07
asymp 30˚ mdash 45˚
HRo ~ 1
H
Torus Direct Evidence
NGC 1068
D = 144 Mpc
01rdquo = 72 pc
Weigelt+ 04
bispectrum specle interferometry
Jaffe+ 04
VLTI 8-13 m
Torus Size mdash Observations
NGC1068 2m imaging ndash R ~ 1 pc (Weigelt+ 04)
8―13m VLTI ndash R ~ 2 pc (Jaffe+ 04)
Cen A 8―13m VLTI ndash R ~ 03 pc ( Meisenheimer+
07)
Circinus 2m ndash R ~ 1 pc (Prieto+ 04)
8―13m VLTI ndash R ~ 1 pc (Tristram+ 08)
8 amp 18m ndash R lt 2 pc (Packham+ 05)
NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto+ 04)
All observations are consistent with RoutRd no larger than ~2030 and perhaps even
only ~510
Torus orientation amp the host galaxy
AGN axis (jet) randomly oriented with respect to
bull galactic disk in Syefert galaxies (Kinney et al 00)
bull nuclear dust disk in radio galaxies (Schmitt et al 02)
NGC 1068
Galaxy ~ face on
Torus ~ edge on (le5ordm)bull H2O masers
Gallimore+ 01
bull NLR kinematics Crenshaw+ 00
NGC 1068 CO amp H2 observations
Galliano et al rsquo03 HR ~ 015
20 pc
140 pc
bull Molecular disk outside ldquothe torusrdquo
bull Disk amp torus roughly aligned
15ordm
Schinerer+ 00 at R ~ 70 pc H ~ 10 pc HR ~
015
NGC 1068 H2 SINFONI observations
Muller Sanchez+ 08
bull Infall at ~ 10 pc no rotation
bull Torus size lt~ 10 pc
NGC 1068 H2O Masers amp 8 GHz Continuum
Gallimore+
04
04 pc
What is the Torus
Smooth continuation of the BLR
Risaliti Elvis amp Nicastro 02
Smooth distribution of dusty and dust-free (BLR) clouds
X-ray Obscuration
Dusty clouds absorb both UVoptical and X-rays
Dust-free clouds absorb only X-rays
Broad Emission Line
NIR(K-band)
bull Broad-emission line lags for objects that also have infrared lags bull Including Hi amp Lo ionization lines)
(nucleus)
Lag Times ― BLR and near-IRSuganuma et al 06
BLR is dust bound (Netzer amp Laor 93)
No correlation with M
( luminosity)
Rd
r lt Rd mdash dust free clouds Broad Lines Region X-ray Obscuration Region
BLRXOR
r gt Rd mdash dusty clouds Toroidal Obscuration Region
TOR
TOR = Torus
The Dust-Sublimation Transition
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind Paradigm
Grand Unification Theory
masers
Emmering Blandford amp Shlosman 92
BLRXOR
Broad Lines Region
X-ray Obscuration
Region
WA
Warm Absorber
TOR
Toroidal Obscuration
Region
Clumpy Torus Modeling
N0 = 5 ndash 10 clouds
= 30deg ndash 60deg
V = 30 ndash 120
q = 1 ndash 2
Rd = 04Lfrac1245 pc Ro ge 5 Rd
Standard ISM dust works fine
N N0 exp(-22)rq
Nenkova et al lsquo02 lsquo08
s
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Unification Scheme for AGN
M ~ 106 ndash 1010 M
Rs ~ 1011 ndash 1015
cm
Toroidal
Obscuration
Required by
Unification
SchemesObscuring matter mdash optically thick dusty clouds Krolik amp
Begelman lsquo88
Torus Properties mdash Obscuration
Equatorial V gt~ 30 40
NH gt~ 1023 cm-2
f2 mdash fraction of obscured sources = N2(N1 + N2)
Seyferts f2 = 70 Schmitt+ lsquo01
f2 = 50 Hao+ lsquo05
f2 = sin = 05 mdash 07
asymp 30˚ mdash 45˚
HRo ~ 1
H
Torus Direct Evidence
NGC 1068
D = 144 Mpc
01rdquo = 72 pc
Weigelt+ 04
bispectrum specle interferometry
Jaffe+ 04
VLTI 8-13 m
Torus Size mdash Observations
NGC1068 2m imaging ndash R ~ 1 pc (Weigelt+ 04)
8―13m VLTI ndash R ~ 2 pc (Jaffe+ 04)
Cen A 8―13m VLTI ndash R ~ 03 pc ( Meisenheimer+
07)
Circinus 2m ndash R ~ 1 pc (Prieto+ 04)
8―13m VLTI ndash R ~ 1 pc (Tristram+ 08)
8 amp 18m ndash R lt 2 pc (Packham+ 05)
NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto+ 04)
All observations are consistent with RoutRd no larger than ~2030 and perhaps even
only ~510
Torus orientation amp the host galaxy
AGN axis (jet) randomly oriented with respect to
bull galactic disk in Syefert galaxies (Kinney et al 00)
bull nuclear dust disk in radio galaxies (Schmitt et al 02)
NGC 1068
Galaxy ~ face on
Torus ~ edge on (le5ordm)bull H2O masers
Gallimore+ 01
bull NLR kinematics Crenshaw+ 00
NGC 1068 CO amp H2 observations
Galliano et al rsquo03 HR ~ 015
20 pc
140 pc
bull Molecular disk outside ldquothe torusrdquo
bull Disk amp torus roughly aligned
15ordm
Schinerer+ 00 at R ~ 70 pc H ~ 10 pc HR ~
015
NGC 1068 H2 SINFONI observations
Muller Sanchez+ 08
bull Infall at ~ 10 pc no rotation
bull Torus size lt~ 10 pc
NGC 1068 H2O Masers amp 8 GHz Continuum
Gallimore+
04
04 pc
What is the Torus
Smooth continuation of the BLR
Risaliti Elvis amp Nicastro 02
Smooth distribution of dusty and dust-free (BLR) clouds
X-ray Obscuration
Dusty clouds absorb both UVoptical and X-rays
Dust-free clouds absorb only X-rays
Broad Emission Line
NIR(K-band)
bull Broad-emission line lags for objects that also have infrared lags bull Including Hi amp Lo ionization lines)
(nucleus)
Lag Times ― BLR and near-IRSuganuma et al 06
BLR is dust bound (Netzer amp Laor 93)
No correlation with M
( luminosity)
Rd
r lt Rd mdash dust free clouds Broad Lines Region X-ray Obscuration Region
BLRXOR
r gt Rd mdash dusty clouds Toroidal Obscuration Region
TOR
TOR = Torus
The Dust-Sublimation Transition
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind Paradigm
Grand Unification Theory
masers
Emmering Blandford amp Shlosman 92
BLRXOR
Broad Lines Region
X-ray Obscuration
Region
WA
Warm Absorber
TOR
Toroidal Obscuration
Region
Clumpy Torus Modeling
N0 = 5 ndash 10 clouds
= 30deg ndash 60deg
V = 30 ndash 120
q = 1 ndash 2
Rd = 04Lfrac1245 pc Ro ge 5 Rd
Standard ISM dust works fine
N N0 exp(-22)rq
Nenkova et al lsquo02 lsquo08
s
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Torus Properties mdash Obscuration
Equatorial V gt~ 30 40
NH gt~ 1023 cm-2
f2 mdash fraction of obscured sources = N2(N1 + N2)
Seyferts f2 = 70 Schmitt+ lsquo01
f2 = 50 Hao+ lsquo05
f2 = sin = 05 mdash 07
asymp 30˚ mdash 45˚
HRo ~ 1
H
Torus Direct Evidence
NGC 1068
D = 144 Mpc
01rdquo = 72 pc
Weigelt+ 04
bispectrum specle interferometry
Jaffe+ 04
VLTI 8-13 m
Torus Size mdash Observations
NGC1068 2m imaging ndash R ~ 1 pc (Weigelt+ 04)
8―13m VLTI ndash R ~ 2 pc (Jaffe+ 04)
Cen A 8―13m VLTI ndash R ~ 03 pc ( Meisenheimer+
07)
Circinus 2m ndash R ~ 1 pc (Prieto+ 04)
8―13m VLTI ndash R ~ 1 pc (Tristram+ 08)
8 amp 18m ndash R lt 2 pc (Packham+ 05)
NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto+ 04)
All observations are consistent with RoutRd no larger than ~2030 and perhaps even
only ~510
Torus orientation amp the host galaxy
AGN axis (jet) randomly oriented with respect to
bull galactic disk in Syefert galaxies (Kinney et al 00)
bull nuclear dust disk in radio galaxies (Schmitt et al 02)
NGC 1068
Galaxy ~ face on
Torus ~ edge on (le5ordm)bull H2O masers
Gallimore+ 01
bull NLR kinematics Crenshaw+ 00
NGC 1068 CO amp H2 observations
Galliano et al rsquo03 HR ~ 015
20 pc
140 pc
bull Molecular disk outside ldquothe torusrdquo
bull Disk amp torus roughly aligned
15ordm
Schinerer+ 00 at R ~ 70 pc H ~ 10 pc HR ~
015
NGC 1068 H2 SINFONI observations
Muller Sanchez+ 08
bull Infall at ~ 10 pc no rotation
bull Torus size lt~ 10 pc
NGC 1068 H2O Masers amp 8 GHz Continuum
Gallimore+
04
04 pc
What is the Torus
Smooth continuation of the BLR
Risaliti Elvis amp Nicastro 02
Smooth distribution of dusty and dust-free (BLR) clouds
X-ray Obscuration
Dusty clouds absorb both UVoptical and X-rays
Dust-free clouds absorb only X-rays
Broad Emission Line
NIR(K-band)
bull Broad-emission line lags for objects that also have infrared lags bull Including Hi amp Lo ionization lines)
(nucleus)
Lag Times ― BLR and near-IRSuganuma et al 06
BLR is dust bound (Netzer amp Laor 93)
No correlation with M
( luminosity)
Rd
r lt Rd mdash dust free clouds Broad Lines Region X-ray Obscuration Region
BLRXOR
r gt Rd mdash dusty clouds Toroidal Obscuration Region
TOR
TOR = Torus
The Dust-Sublimation Transition
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind Paradigm
Grand Unification Theory
masers
Emmering Blandford amp Shlosman 92
BLRXOR
Broad Lines Region
X-ray Obscuration
Region
WA
Warm Absorber
TOR
Toroidal Obscuration
Region
Clumpy Torus Modeling
N0 = 5 ndash 10 clouds
= 30deg ndash 60deg
V = 30 ndash 120
q = 1 ndash 2
Rd = 04Lfrac1245 pc Ro ge 5 Rd
Standard ISM dust works fine
N N0 exp(-22)rq
Nenkova et al lsquo02 lsquo08
s
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Torus Direct Evidence
NGC 1068
D = 144 Mpc
01rdquo = 72 pc
Weigelt+ 04
bispectrum specle interferometry
Jaffe+ 04
VLTI 8-13 m
Torus Size mdash Observations
NGC1068 2m imaging ndash R ~ 1 pc (Weigelt+ 04)
8―13m VLTI ndash R ~ 2 pc (Jaffe+ 04)
Cen A 8―13m VLTI ndash R ~ 03 pc ( Meisenheimer+
07)
Circinus 2m ndash R ~ 1 pc (Prieto+ 04)
8―13m VLTI ndash R ~ 1 pc (Tristram+ 08)
8 amp 18m ndash R lt 2 pc (Packham+ 05)
NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto+ 04)
All observations are consistent with RoutRd no larger than ~2030 and perhaps even
only ~510
Torus orientation amp the host galaxy
AGN axis (jet) randomly oriented with respect to
bull galactic disk in Syefert galaxies (Kinney et al 00)
bull nuclear dust disk in radio galaxies (Schmitt et al 02)
NGC 1068
Galaxy ~ face on
Torus ~ edge on (le5ordm)bull H2O masers
Gallimore+ 01
bull NLR kinematics Crenshaw+ 00
NGC 1068 CO amp H2 observations
Galliano et al rsquo03 HR ~ 015
20 pc
140 pc
bull Molecular disk outside ldquothe torusrdquo
bull Disk amp torus roughly aligned
15ordm
Schinerer+ 00 at R ~ 70 pc H ~ 10 pc HR ~
015
NGC 1068 H2 SINFONI observations
Muller Sanchez+ 08
bull Infall at ~ 10 pc no rotation
bull Torus size lt~ 10 pc
NGC 1068 H2O Masers amp 8 GHz Continuum
Gallimore+
04
04 pc
What is the Torus
Smooth continuation of the BLR
Risaliti Elvis amp Nicastro 02
Smooth distribution of dusty and dust-free (BLR) clouds
X-ray Obscuration
Dusty clouds absorb both UVoptical and X-rays
Dust-free clouds absorb only X-rays
Broad Emission Line
NIR(K-band)
bull Broad-emission line lags for objects that also have infrared lags bull Including Hi amp Lo ionization lines)
(nucleus)
Lag Times ― BLR and near-IRSuganuma et al 06
BLR is dust bound (Netzer amp Laor 93)
No correlation with M
( luminosity)
Rd
r lt Rd mdash dust free clouds Broad Lines Region X-ray Obscuration Region
BLRXOR
r gt Rd mdash dusty clouds Toroidal Obscuration Region
TOR
TOR = Torus
The Dust-Sublimation Transition
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind Paradigm
Grand Unification Theory
masers
Emmering Blandford amp Shlosman 92
BLRXOR
Broad Lines Region
X-ray Obscuration
Region
WA
Warm Absorber
TOR
Toroidal Obscuration
Region
Clumpy Torus Modeling
N0 = 5 ndash 10 clouds
= 30deg ndash 60deg
V = 30 ndash 120
q = 1 ndash 2
Rd = 04Lfrac1245 pc Ro ge 5 Rd
Standard ISM dust works fine
N N0 exp(-22)rq
Nenkova et al lsquo02 lsquo08
s
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
NGC 1068
D = 144 Mpc
01rdquo = 72 pc
Weigelt+ 04
bispectrum specle interferometry
Jaffe+ 04
VLTI 8-13 m
Torus Size mdash Observations
NGC1068 2m imaging ndash R ~ 1 pc (Weigelt+ 04)
8―13m VLTI ndash R ~ 2 pc (Jaffe+ 04)
Cen A 8―13m VLTI ndash R ~ 03 pc ( Meisenheimer+
07)
Circinus 2m ndash R ~ 1 pc (Prieto+ 04)
8―13m VLTI ndash R ~ 1 pc (Tristram+ 08)
8 amp 18m ndash R lt 2 pc (Packham+ 05)
NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto+ 04)
All observations are consistent with RoutRd no larger than ~2030 and perhaps even
only ~510
Torus orientation amp the host galaxy
AGN axis (jet) randomly oriented with respect to
bull galactic disk in Syefert galaxies (Kinney et al 00)
bull nuclear dust disk in radio galaxies (Schmitt et al 02)
NGC 1068
Galaxy ~ face on
Torus ~ edge on (le5ordm)bull H2O masers
Gallimore+ 01
bull NLR kinematics Crenshaw+ 00
NGC 1068 CO amp H2 observations
Galliano et al rsquo03 HR ~ 015
20 pc
140 pc
bull Molecular disk outside ldquothe torusrdquo
bull Disk amp torus roughly aligned
15ordm
Schinerer+ 00 at R ~ 70 pc H ~ 10 pc HR ~
015
NGC 1068 H2 SINFONI observations
Muller Sanchez+ 08
bull Infall at ~ 10 pc no rotation
bull Torus size lt~ 10 pc
NGC 1068 H2O Masers amp 8 GHz Continuum
Gallimore+
04
04 pc
What is the Torus
Smooth continuation of the BLR
Risaliti Elvis amp Nicastro 02
Smooth distribution of dusty and dust-free (BLR) clouds
X-ray Obscuration
Dusty clouds absorb both UVoptical and X-rays
Dust-free clouds absorb only X-rays
Broad Emission Line
NIR(K-band)
bull Broad-emission line lags for objects that also have infrared lags bull Including Hi amp Lo ionization lines)
(nucleus)
Lag Times ― BLR and near-IRSuganuma et al 06
BLR is dust bound (Netzer amp Laor 93)
No correlation with M
( luminosity)
Rd
r lt Rd mdash dust free clouds Broad Lines Region X-ray Obscuration Region
BLRXOR
r gt Rd mdash dusty clouds Toroidal Obscuration Region
TOR
TOR = Torus
The Dust-Sublimation Transition
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind Paradigm
Grand Unification Theory
masers
Emmering Blandford amp Shlosman 92
BLRXOR
Broad Lines Region
X-ray Obscuration
Region
WA
Warm Absorber
TOR
Toroidal Obscuration
Region
Clumpy Torus Modeling
N0 = 5 ndash 10 clouds
= 30deg ndash 60deg
V = 30 ndash 120
q = 1 ndash 2
Rd = 04Lfrac1245 pc Ro ge 5 Rd
Standard ISM dust works fine
N N0 exp(-22)rq
Nenkova et al lsquo02 lsquo08
s
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Torus Size mdash Observations
NGC1068 2m imaging ndash R ~ 1 pc (Weigelt+ 04)
8―13m VLTI ndash R ~ 2 pc (Jaffe+ 04)
Cen A 8―13m VLTI ndash R ~ 03 pc ( Meisenheimer+
07)
Circinus 2m ndash R ~ 1 pc (Prieto+ 04)
8―13m VLTI ndash R ~ 1 pc (Tristram+ 08)
8 amp 18m ndash R lt 2 pc (Packham+ 05)
NGC1097 amp NGC5506 2m ndash R lt 5 pc (Prieto+ 04)
All observations are consistent with RoutRd no larger than ~2030 and perhaps even
only ~510
Torus orientation amp the host galaxy
AGN axis (jet) randomly oriented with respect to
bull galactic disk in Syefert galaxies (Kinney et al 00)
bull nuclear dust disk in radio galaxies (Schmitt et al 02)
NGC 1068
Galaxy ~ face on
Torus ~ edge on (le5ordm)bull H2O masers
Gallimore+ 01
bull NLR kinematics Crenshaw+ 00
NGC 1068 CO amp H2 observations
Galliano et al rsquo03 HR ~ 015
20 pc
140 pc
bull Molecular disk outside ldquothe torusrdquo
bull Disk amp torus roughly aligned
15ordm
Schinerer+ 00 at R ~ 70 pc H ~ 10 pc HR ~
015
NGC 1068 H2 SINFONI observations
Muller Sanchez+ 08
bull Infall at ~ 10 pc no rotation
bull Torus size lt~ 10 pc
NGC 1068 H2O Masers amp 8 GHz Continuum
Gallimore+
04
04 pc
What is the Torus
Smooth continuation of the BLR
Risaliti Elvis amp Nicastro 02
Smooth distribution of dusty and dust-free (BLR) clouds
X-ray Obscuration
Dusty clouds absorb both UVoptical and X-rays
Dust-free clouds absorb only X-rays
Broad Emission Line
NIR(K-band)
bull Broad-emission line lags for objects that also have infrared lags bull Including Hi amp Lo ionization lines)
(nucleus)
Lag Times ― BLR and near-IRSuganuma et al 06
BLR is dust bound (Netzer amp Laor 93)
No correlation with M
( luminosity)
Rd
r lt Rd mdash dust free clouds Broad Lines Region X-ray Obscuration Region
BLRXOR
r gt Rd mdash dusty clouds Toroidal Obscuration Region
TOR
TOR = Torus
The Dust-Sublimation Transition
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind Paradigm
Grand Unification Theory
masers
Emmering Blandford amp Shlosman 92
BLRXOR
Broad Lines Region
X-ray Obscuration
Region
WA
Warm Absorber
TOR
Toroidal Obscuration
Region
Clumpy Torus Modeling
N0 = 5 ndash 10 clouds
= 30deg ndash 60deg
V = 30 ndash 120
q = 1 ndash 2
Rd = 04Lfrac1245 pc Ro ge 5 Rd
Standard ISM dust works fine
N N0 exp(-22)rq
Nenkova et al lsquo02 lsquo08
s
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Torus orientation amp the host galaxy
AGN axis (jet) randomly oriented with respect to
bull galactic disk in Syefert galaxies (Kinney et al 00)
bull nuclear dust disk in radio galaxies (Schmitt et al 02)
NGC 1068
Galaxy ~ face on
Torus ~ edge on (le5ordm)bull H2O masers
Gallimore+ 01
bull NLR kinematics Crenshaw+ 00
NGC 1068 CO amp H2 observations
Galliano et al rsquo03 HR ~ 015
20 pc
140 pc
bull Molecular disk outside ldquothe torusrdquo
bull Disk amp torus roughly aligned
15ordm
Schinerer+ 00 at R ~ 70 pc H ~ 10 pc HR ~
015
NGC 1068 H2 SINFONI observations
Muller Sanchez+ 08
bull Infall at ~ 10 pc no rotation
bull Torus size lt~ 10 pc
NGC 1068 H2O Masers amp 8 GHz Continuum
Gallimore+
04
04 pc
What is the Torus
Smooth continuation of the BLR
Risaliti Elvis amp Nicastro 02
Smooth distribution of dusty and dust-free (BLR) clouds
X-ray Obscuration
Dusty clouds absorb both UVoptical and X-rays
Dust-free clouds absorb only X-rays
Broad Emission Line
NIR(K-band)
bull Broad-emission line lags for objects that also have infrared lags bull Including Hi amp Lo ionization lines)
(nucleus)
Lag Times ― BLR and near-IRSuganuma et al 06
BLR is dust bound (Netzer amp Laor 93)
No correlation with M
( luminosity)
Rd
r lt Rd mdash dust free clouds Broad Lines Region X-ray Obscuration Region
BLRXOR
r gt Rd mdash dusty clouds Toroidal Obscuration Region
TOR
TOR = Torus
The Dust-Sublimation Transition
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind Paradigm
Grand Unification Theory
masers
Emmering Blandford amp Shlosman 92
BLRXOR
Broad Lines Region
X-ray Obscuration
Region
WA
Warm Absorber
TOR
Toroidal Obscuration
Region
Clumpy Torus Modeling
N0 = 5 ndash 10 clouds
= 30deg ndash 60deg
V = 30 ndash 120
q = 1 ndash 2
Rd = 04Lfrac1245 pc Ro ge 5 Rd
Standard ISM dust works fine
N N0 exp(-22)rq
Nenkova et al lsquo02 lsquo08
s
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
NGC 1068
Galaxy ~ face on
Torus ~ edge on (le5ordm)bull H2O masers
Gallimore+ 01
bull NLR kinematics Crenshaw+ 00
NGC 1068 CO amp H2 observations
Galliano et al rsquo03 HR ~ 015
20 pc
140 pc
bull Molecular disk outside ldquothe torusrdquo
bull Disk amp torus roughly aligned
15ordm
Schinerer+ 00 at R ~ 70 pc H ~ 10 pc HR ~
015
NGC 1068 H2 SINFONI observations
Muller Sanchez+ 08
bull Infall at ~ 10 pc no rotation
bull Torus size lt~ 10 pc
NGC 1068 H2O Masers amp 8 GHz Continuum
Gallimore+
04
04 pc
What is the Torus
Smooth continuation of the BLR
Risaliti Elvis amp Nicastro 02
Smooth distribution of dusty and dust-free (BLR) clouds
X-ray Obscuration
Dusty clouds absorb both UVoptical and X-rays
Dust-free clouds absorb only X-rays
Broad Emission Line
NIR(K-band)
bull Broad-emission line lags for objects that also have infrared lags bull Including Hi amp Lo ionization lines)
(nucleus)
Lag Times ― BLR and near-IRSuganuma et al 06
BLR is dust bound (Netzer amp Laor 93)
No correlation with M
( luminosity)
Rd
r lt Rd mdash dust free clouds Broad Lines Region X-ray Obscuration Region
BLRXOR
r gt Rd mdash dusty clouds Toroidal Obscuration Region
TOR
TOR = Torus
The Dust-Sublimation Transition
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind Paradigm
Grand Unification Theory
masers
Emmering Blandford amp Shlosman 92
BLRXOR
Broad Lines Region
X-ray Obscuration
Region
WA
Warm Absorber
TOR
Toroidal Obscuration
Region
Clumpy Torus Modeling
N0 = 5 ndash 10 clouds
= 30deg ndash 60deg
V = 30 ndash 120
q = 1 ndash 2
Rd = 04Lfrac1245 pc Ro ge 5 Rd
Standard ISM dust works fine
N N0 exp(-22)rq
Nenkova et al lsquo02 lsquo08
s
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
NGC 1068 CO amp H2 observations
Galliano et al rsquo03 HR ~ 015
20 pc
140 pc
bull Molecular disk outside ldquothe torusrdquo
bull Disk amp torus roughly aligned
15ordm
Schinerer+ 00 at R ~ 70 pc H ~ 10 pc HR ~
015
NGC 1068 H2 SINFONI observations
Muller Sanchez+ 08
bull Infall at ~ 10 pc no rotation
bull Torus size lt~ 10 pc
NGC 1068 H2O Masers amp 8 GHz Continuum
Gallimore+
04
04 pc
What is the Torus
Smooth continuation of the BLR
Risaliti Elvis amp Nicastro 02
Smooth distribution of dusty and dust-free (BLR) clouds
X-ray Obscuration
Dusty clouds absorb both UVoptical and X-rays
Dust-free clouds absorb only X-rays
Broad Emission Line
NIR(K-band)
bull Broad-emission line lags for objects that also have infrared lags bull Including Hi amp Lo ionization lines)
(nucleus)
Lag Times ― BLR and near-IRSuganuma et al 06
BLR is dust bound (Netzer amp Laor 93)
No correlation with M
( luminosity)
Rd
r lt Rd mdash dust free clouds Broad Lines Region X-ray Obscuration Region
BLRXOR
r gt Rd mdash dusty clouds Toroidal Obscuration Region
TOR
TOR = Torus
The Dust-Sublimation Transition
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind Paradigm
Grand Unification Theory
masers
Emmering Blandford amp Shlosman 92
BLRXOR
Broad Lines Region
X-ray Obscuration
Region
WA
Warm Absorber
TOR
Toroidal Obscuration
Region
Clumpy Torus Modeling
N0 = 5 ndash 10 clouds
= 30deg ndash 60deg
V = 30 ndash 120
q = 1 ndash 2
Rd = 04Lfrac1245 pc Ro ge 5 Rd
Standard ISM dust works fine
N N0 exp(-22)rq
Nenkova et al lsquo02 lsquo08
s
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
NGC 1068 H2 SINFONI observations
Muller Sanchez+ 08
bull Infall at ~ 10 pc no rotation
bull Torus size lt~ 10 pc
NGC 1068 H2O Masers amp 8 GHz Continuum
Gallimore+
04
04 pc
What is the Torus
Smooth continuation of the BLR
Risaliti Elvis amp Nicastro 02
Smooth distribution of dusty and dust-free (BLR) clouds
X-ray Obscuration
Dusty clouds absorb both UVoptical and X-rays
Dust-free clouds absorb only X-rays
Broad Emission Line
NIR(K-band)
bull Broad-emission line lags for objects that also have infrared lags bull Including Hi amp Lo ionization lines)
(nucleus)
Lag Times ― BLR and near-IRSuganuma et al 06
BLR is dust bound (Netzer amp Laor 93)
No correlation with M
( luminosity)
Rd
r lt Rd mdash dust free clouds Broad Lines Region X-ray Obscuration Region
BLRXOR
r gt Rd mdash dusty clouds Toroidal Obscuration Region
TOR
TOR = Torus
The Dust-Sublimation Transition
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind Paradigm
Grand Unification Theory
masers
Emmering Blandford amp Shlosman 92
BLRXOR
Broad Lines Region
X-ray Obscuration
Region
WA
Warm Absorber
TOR
Toroidal Obscuration
Region
Clumpy Torus Modeling
N0 = 5 ndash 10 clouds
= 30deg ndash 60deg
V = 30 ndash 120
q = 1 ndash 2
Rd = 04Lfrac1245 pc Ro ge 5 Rd
Standard ISM dust works fine
N N0 exp(-22)rq
Nenkova et al lsquo02 lsquo08
s
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
NGC 1068 H2O Masers amp 8 GHz Continuum
Gallimore+
04
04 pc
What is the Torus
Smooth continuation of the BLR
Risaliti Elvis amp Nicastro 02
Smooth distribution of dusty and dust-free (BLR) clouds
X-ray Obscuration
Dusty clouds absorb both UVoptical and X-rays
Dust-free clouds absorb only X-rays
Broad Emission Line
NIR(K-band)
bull Broad-emission line lags for objects that also have infrared lags bull Including Hi amp Lo ionization lines)
(nucleus)
Lag Times ― BLR and near-IRSuganuma et al 06
BLR is dust bound (Netzer amp Laor 93)
No correlation with M
( luminosity)
Rd
r lt Rd mdash dust free clouds Broad Lines Region X-ray Obscuration Region
BLRXOR
r gt Rd mdash dusty clouds Toroidal Obscuration Region
TOR
TOR = Torus
The Dust-Sublimation Transition
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind Paradigm
Grand Unification Theory
masers
Emmering Blandford amp Shlosman 92
BLRXOR
Broad Lines Region
X-ray Obscuration
Region
WA
Warm Absorber
TOR
Toroidal Obscuration
Region
Clumpy Torus Modeling
N0 = 5 ndash 10 clouds
= 30deg ndash 60deg
V = 30 ndash 120
q = 1 ndash 2
Rd = 04Lfrac1245 pc Ro ge 5 Rd
Standard ISM dust works fine
N N0 exp(-22)rq
Nenkova et al lsquo02 lsquo08
s
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
What is the Torus
Smooth continuation of the BLR
Risaliti Elvis amp Nicastro 02
Smooth distribution of dusty and dust-free (BLR) clouds
X-ray Obscuration
Dusty clouds absorb both UVoptical and X-rays
Dust-free clouds absorb only X-rays
Broad Emission Line
NIR(K-band)
bull Broad-emission line lags for objects that also have infrared lags bull Including Hi amp Lo ionization lines)
(nucleus)
Lag Times ― BLR and near-IRSuganuma et al 06
BLR is dust bound (Netzer amp Laor 93)
No correlation with M
( luminosity)
Rd
r lt Rd mdash dust free clouds Broad Lines Region X-ray Obscuration Region
BLRXOR
r gt Rd mdash dusty clouds Toroidal Obscuration Region
TOR
TOR = Torus
The Dust-Sublimation Transition
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind Paradigm
Grand Unification Theory
masers
Emmering Blandford amp Shlosman 92
BLRXOR
Broad Lines Region
X-ray Obscuration
Region
WA
Warm Absorber
TOR
Toroidal Obscuration
Region
Clumpy Torus Modeling
N0 = 5 ndash 10 clouds
= 30deg ndash 60deg
V = 30 ndash 120
q = 1 ndash 2
Rd = 04Lfrac1245 pc Ro ge 5 Rd
Standard ISM dust works fine
N N0 exp(-22)rq
Nenkova et al lsquo02 lsquo08
s
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Risaliti Elvis amp Nicastro 02
Smooth distribution of dusty and dust-free (BLR) clouds
X-ray Obscuration
Dusty clouds absorb both UVoptical and X-rays
Dust-free clouds absorb only X-rays
Broad Emission Line
NIR(K-band)
bull Broad-emission line lags for objects that also have infrared lags bull Including Hi amp Lo ionization lines)
(nucleus)
Lag Times ― BLR and near-IRSuganuma et al 06
BLR is dust bound (Netzer amp Laor 93)
No correlation with M
( luminosity)
Rd
r lt Rd mdash dust free clouds Broad Lines Region X-ray Obscuration Region
BLRXOR
r gt Rd mdash dusty clouds Toroidal Obscuration Region
TOR
TOR = Torus
The Dust-Sublimation Transition
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind Paradigm
Grand Unification Theory
masers
Emmering Blandford amp Shlosman 92
BLRXOR
Broad Lines Region
X-ray Obscuration
Region
WA
Warm Absorber
TOR
Toroidal Obscuration
Region
Clumpy Torus Modeling
N0 = 5 ndash 10 clouds
= 30deg ndash 60deg
V = 30 ndash 120
q = 1 ndash 2
Rd = 04Lfrac1245 pc Ro ge 5 Rd
Standard ISM dust works fine
N N0 exp(-22)rq
Nenkova et al lsquo02 lsquo08
s
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Broad Emission Line
NIR(K-band)
bull Broad-emission line lags for objects that also have infrared lags bull Including Hi amp Lo ionization lines)
(nucleus)
Lag Times ― BLR and near-IRSuganuma et al 06
BLR is dust bound (Netzer amp Laor 93)
No correlation with M
( luminosity)
Rd
r lt Rd mdash dust free clouds Broad Lines Region X-ray Obscuration Region
BLRXOR
r gt Rd mdash dusty clouds Toroidal Obscuration Region
TOR
TOR = Torus
The Dust-Sublimation Transition
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind Paradigm
Grand Unification Theory
masers
Emmering Blandford amp Shlosman 92
BLRXOR
Broad Lines Region
X-ray Obscuration
Region
WA
Warm Absorber
TOR
Toroidal Obscuration
Region
Clumpy Torus Modeling
N0 = 5 ndash 10 clouds
= 30deg ndash 60deg
V = 30 ndash 120
q = 1 ndash 2
Rd = 04Lfrac1245 pc Ro ge 5 Rd
Standard ISM dust works fine
N N0 exp(-22)rq
Nenkova et al lsquo02 lsquo08
s
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Rd
r lt Rd mdash dust free clouds Broad Lines Region X-ray Obscuration Region
BLRXOR
r gt Rd mdash dusty clouds Toroidal Obscuration Region
TOR
TOR = Torus
The Dust-Sublimation Transition
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind Paradigm
Grand Unification Theory
masers
Emmering Blandford amp Shlosman 92
BLRXOR
Broad Lines Region
X-ray Obscuration
Region
WA
Warm Absorber
TOR
Toroidal Obscuration
Region
Clumpy Torus Modeling
N0 = 5 ndash 10 clouds
= 30deg ndash 60deg
V = 30 ndash 120
q = 1 ndash 2
Rd = 04Lfrac1245 pc Ro ge 5 Rd
Standard ISM dust works fine
N N0 exp(-22)rq
Nenkova et al lsquo02 lsquo08
s
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Everett amp Konigl lsquo00
Bottorff+ 97
The Disk Wind Paradigm
Grand Unification Theory
masers
Emmering Blandford amp Shlosman 92
BLRXOR
Broad Lines Region
X-ray Obscuration
Region
WA
Warm Absorber
TOR
Toroidal Obscuration
Region
Clumpy Torus Modeling
N0 = 5 ndash 10 clouds
= 30deg ndash 60deg
V = 30 ndash 120
q = 1 ndash 2
Rd = 04Lfrac1245 pc Ro ge 5 Rd
Standard ISM dust works fine
N N0 exp(-22)rq
Nenkova et al lsquo02 lsquo08
s
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Grand Unification Theory
masers
Emmering Blandford amp Shlosman 92
BLRXOR
Broad Lines Region
X-ray Obscuration
Region
WA
Warm Absorber
TOR
Toroidal Obscuration
Region
Clumpy Torus Modeling
N0 = 5 ndash 10 clouds
= 30deg ndash 60deg
V = 30 ndash 120
q = 1 ndash 2
Rd = 04Lfrac1245 pc Ro ge 5 Rd
Standard ISM dust works fine
N N0 exp(-22)rq
Nenkova et al lsquo02 lsquo08
s
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Clumpy Torus Modeling
N0 = 5 ndash 10 clouds
= 30deg ndash 60deg
V = 30 ndash 120
q = 1 ndash 2
Rd = 04Lfrac1245 pc Ro ge 5 Rd
Standard ISM dust works fine
N N0 exp(-22)rq
Nenkova et al lsquo02 lsquo08
s
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Cloud Properties in TOR Outflow
IR modeling
v ~ 30 ndash 120 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
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Circinus Water Masers
Greenhill+ 03
02 pc
Circinus VLTI Imaging
Tristram+ 07
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Circinus VLTI Imaging
Tristram+ 07
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Geometry
Clouds rise and expand
Column density decreases
Toroidal structure for both BLR XOR and
TOR
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
TOR Mass Outflow Rate
Torus should disappear at small LLEdd
THdd
TORout N)R(vRM
2TORacc
2BHacc cMcML
v(Rd) vK(Rd) (MbullRd)frac12 (LEddLfrac12)frac12
TH
21Edd
41TORacc
TORout N
LL
LM
M
Rd Lfrac12
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Torus Disappearance at Low Luminosities
Nucleus visible in FR I radio galaxies (Chiaberge+
99)
hellip and LINERs too (Maoz+ 05)
LINER 1 amp 2 UV colors similar (AV lt~ 1)
No torus dust emission in M87 (Whysong amp
Antonucci 04 Perlman+ 07)
No torus dust emission in FR I and ~ half of FR II
(van der Wolk+ 08)
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
If only TOR is removed all low-luminosity AGN become
type 1HOWEVER
Both type 1 and type 2 LINERs do exist
(Maoz et al 05)
ldquotruerdquo type 2 AGN exist at L lt 1042 erg
s-1 (Panessa amp Bassani 02 Laor 03)
THEREFORE
BLR must disappear at some lower L
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Ho 08 BLR disappears at LLAGN
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Wind diminishes mdash mass outflow directed to jets ()
Ho lsquo02 Sikora et al lsquo07 Radio loudness (LradLopt) varies inversely with Macc
BLR TOR
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
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
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Accre
tion R
ate
(LL
Edd)
Radio
Lo
ud
ness
Full Unification Scheme
both type 1 amp 2
molecular outflow extinguished
Torus disappears type 1 only
atomic outflow extinguished
BLR disappears ldquotruerdquo type 2
High
High
Low
Low
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
TOR Energy Outflow Rate
Negligible in the energy budget
13
36
T23H
2145
35w sergvNL107L I
dAvnvML cc2cc2
1w
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
-
Final Speculation
With ~ 01 the required accretion rate is
Macc ~ 01 L45 M yr-1
The AGN phase lasts ~ 107 108 yrs
Overall accreted mass ~ 106 107 L45 M
Is the whole Seyfert phenomenon the accretion of
just a single GMC
Are QSO triggered differently (mergers)
- Disk-outflow Connection and the Molecular Dusty Torus
- Unification Scheme for AGN
- Torus Properties mdash Obscuration
- Slide 4
- Slide 5
- Torus Size mdash Observations
- Torus orientation amp the host galaxy
- NGC 1068
- NGC 1068 CO amp H2 observations
- NGC 1068 H2 SINFONI observations
- NGC 1068 H2O Masers amp 8 GHz Continuum
- What is the Torus
- X-ray Obscuration
- Lag Times ― BLR and near-IR
- The Dust-Sublimation Transition
- Slide 16
- Grand Unification Theory
- Clumpy Torus Modeling
- Cloud Properties in TOR Outflow
- Circinus Water Masers
- Circinus VLTI Imaging
- Geometry
- TOR Mass Outflow Rate
- Torus Disappearance at Low Luminosities
- Slide 25
- Slide 26
- Slide 27
- Slide 28
- Slide 29
- Slide 30
- TOR Energy Outflow Rate
- Final Speculation
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