ALMAワークショップ「AGN銀河の中心1kpc→1pcでの質量降着機構の理解に向けて

核周分子ガス円盤はSMBH成長の担い手となるか？
泉拓磨1,
川勝望2, 河野孝太郎1
1

東京大学
2

呉高専

1

Circumnuclear disk (CND):a direct source of mass supply to a SMBH

• Remaining angular momentum of the accreting gas will form
~10-100 pc scale gaseous CND at the center• An outer envelope of the putative dusty torus?

→ mass? size? structure? kinematics? fueling?
CND

Mgas
Kawakatu & Wada 2008,
ApJ, 681, 73

2HCN in NGC 3227 does originate from the central compact sou
The compact
nature of the HCN
emissiongalaxies
is in stark contrast to
CNDs
in nearby
SeyfertCO(2–1)emission,
as
shown
in
Fig.
5.
Indeed,theCOemissio
NGC 1097 HCN(4-3)
NGC 1068
distributed around the circumnuclear
ring(which
is
also
seen
in
CO(3-2)200 pcH-band stellar continuum, Fig. 5 and Davies et al. 2006), and v
F. Combes et al.: CO in NGC 1566

100 pcIzumi et al. 2013, PASJ, 65, 100b) HCN(J=4-3)

NGC 7469 HCN(4-3)

150 pcGarcia-Burillo et al. 2014, A&A, 567, 125

NGC 6951
HCN(1-0)
Krips et al. 2007, A&A, 468, L63

NGC 1566
HCO+(1-0)

NGC 3227 HCN(1-0)

Fig. 1. Integrated HCN(1–0) emission (black contours) overlaid on CO(2–1) (color scale; Schinnerer et al., in prep., Garc
in natural (left; a) and uniform weighting (right; b); the CO and HCN emission have been both integrated from −200 km
330 pc
50 pc
We used a uv-taper for CO to match the angular resolution of our
HCN data which is by a factor of ∼2 lower, and obtai−100 from003σ(560
run
to 23σ(right:7σ)pc)
in stepsof 1σ=NGC0.06 Jybeam−1derived
km s−1 (right:
1σpc= 0.10 Jythe
beam
km
85
y maps inBlackthe contours
central
8
!
8
pc
!
560
regionof1097,
bycalculating
zeroth
1.0 Jy beam−1 km s−1 (right: 3σ = 1.3 Jy beam−1 km s−1 ). The black line (left) indicates the major axis of the bar (PA = 100◦
icatestheetpeak
positionof (PA
the=860◦ !m continuum. Both maps are shown on the same intensity sc
ofApJ,
the galaxy
130Combes). The blackline(right)represents
velocity
gradients(PA =Izumimajor
al. axis
2015,
811, 39et al.
2014,
A&A,
565, 97the most extreme
Sani et central
al. 2012,
MNRAS,
424, 1963
h
m
s
◦
′
′′
position
αJ2000HCN= 20 37
andemission
δJ2000 = 66 06
20.09
which is slightly
the=
phase
centrethe obse1160
toof1450km
intensity
map isofat the(J 14.123= 4–3)
overa velocity
rangediﬀerent
from Vfrom
LSR.5 Jy beam"1 km s"1 , and the source size is estimated to be 1:00 34 ! 1:00 04 with PA = "9:ı 1. The bea

Spatial scale: ~100 pc or less (they are not fully resolved)"1"1 . (b) Integrat
ntour levels
are 5, (AGN+SB)
10, 20, ### , 70", where
1 "Arpis 0.11beams"1
or 0.60Kkmscomposite
galaxies(e.g.,
220,Jy M82, kmTable
1. HCN(1–0)
lineparameters,
obtained at
1
Fig. 4a)on 6951;
the Missing
dust
emission
atNguyen-Q-Rieu
349
GHz (colorscale
in spatially
Jy beamintegrated) by fitting a Gaussian pr"1
not
Gaocontinuum& Solomon
2004a,b;
et
al.
in
the
scenarioofAGN-fueling!!
ninovera NGCvelocity
range
from
Vlink
=
1215
to
1440
km
s
.
The
value
at the 860 !m peak position i
LSRgion. c) OverlayoftheCO(6–5)intensity
contours(levels
as
in
Fig.
4c)
on
the
dustErrors include uncertainties
weighted)
data.
of t
1992).00 Inactive00galaxies have even lower
ratios of RHCN/CO < 00aı00ıbmated to be 1: 31 ! 1: 06 with PA = "14: 7. The beam size is 1: 49 ! 1: 18 with PA = "71:
3. The cCNDs in nearby Seyfert galaxies
Hicks et al.

H2 surface brightness [Lsun/pc2]

768:107 (17pp), 2013 May 10

σ [km/s]

2D maps of CO absorption (stars) and H2 emission (molecular gas). Maps are as labeled from left to right: observed flux, velocity,s of CO are in the top row and H2 in the bottom row, as indicated in the lower right of each set along with the galaxy name and pairs up and east is to the left.
available in the online journal.)

ActiveInactive
Radius [pc]AGNs seem to have gaseous disk,
whereas non-AGNs do not.
(Hicks et al. 2013, ApJ, 768, 107)
Radius [pc]

AGN-SB connection@CND?
Diamond-Stanic & Rieke

circumnuclear SFR [Msun/yr]

1E+1

1E0

1398

DAVIES ET AL.

Diamond-Stanic & Rieke 2012,
ApJ, 746, 168

Vol. 671

Davies et al. 2007,
ApJ, 671, 1388

1E-1

Time Delay

1E-2

1E-3

Correlation coeﬃcient = 0.95
Intrinsic scatter = 0.37 dex

1E-4
1E-4

1E-3

1E-2

1E-1

dMBH/dt [Msun/yr]

Fig. 11.—Graphshowing
how theSFR
luminosityof an AGN
be related
the age of the most recent episode of nuclear star formation. On the left is shown the
Figure 5. Relationshipbetween
nuclearas tracedby might
the 11.3µmtoaromatic
luminosity in solar units; on the right, it is with respect to the Eddington luminosity for the black hole. Generally the luminosity of the AGN is not well known and so wefeature and BHAR
as traced by [O iv]. Seyfert galaxies with high accretion rates
have approximated it by 0.5Lbol and adopted an uncertainty of a factor of 2. The starburst age refers to our best estimate of the most recent episode of star formation within
BH
also tend to havenuclear
SFRs.
The
solid
is details
the best-fit
relationshipthe enhanced
central 10Y100
pc, as given
in Table
3. Seethe line
text forof the adopted
uncertainties.

• SFR—dM /dt correlation• Its origin is unknown• Time delay → causal link?

If circumnuclear starburst
regulate
the mass accretion
limit. On the other hand, we have already seen that the low W
replenished by inflow. This picture appears to be borne out by theindicates that there is little ongoing star formation and hence thatobservations presented here.
onto 5.the
SMBH,
how?
the starbursts are short lived. This is important because shortSTARBURST-AGN CONNECTION(Equation (4)), and the dotted lines show the 95% confidence interval on the
regression line.of parsecs they are an order of magnitude below the Eddington
expect that the starburst is then dormant until the gas supply isBr!

lived starbursts fade very quickly. As shown in Figure 6, for a
decay timescale of "SF ¼ 10 Myr, L"bol will have decreased from5
In the previous sections we have presented and discussed evi-

This study• To rebuild the AGN-SB connection individually
by molecular gas observations• To investigate the fueling mechanism of AGN at
the spatial scale of CNDs

6

Data
Total 32 Seyfert galaxies with the following data are used

• HCN(1-0) line luminosity → Mdense- selectively probe orders of magnitude denser gas than that CO(1-0) does
→ e.g., Gao & Solomon 2004, ApJ, 606, 271; Krips et al. 2008, ApJ, 677, 262- 9 interferometric data (ALMA, PdBI, NMA, θmed=200 pc) + 23 single dishdata (NRO45m, IRAM30m, etc, θmed=6.2kpc)→ “from the host galaxy to the CND”

• Absorption corrected 2-10 keV X-ray luminosity → dM /dt
BH- bolometric correction: Marconi et al. 2004, MNRAS, 351, 16- η = 0.1 is assumed, e.g., Alexander & Hickox 2012, New A. Rev. 56, 93• M : Stellar/gas kinematics, maser, reverberation, M-σ
BH*• Bayesian-based regression analysis- linmix_err (IDL routine); Kelly 2007, ApJ, 665, 1489
→ posterior distribution of each regression parameter can be obtained

7

Result: Mdense-dMBH/dt correlation
Interferometer
Single dishInterferometer
Single dish

0.26

0.82

Correlation coeﬃcient

Figure 3. Posterior distributions for the intercept (α), slope (β), intrinsic scatter (σint ), and correlation coefficient1.16(ρ) for the log (Mdense )–log (ṀBH ) r(Figure 2b). Colors indicate the IT- (blue) and SD- (gray) sample, respectively. The width of each bin is fixed to 0.05 in these plots. Note that the′analysis for the log (LHCN)–log (LX ) yields similar parameter distributions like these.

0.94

Izumi et al. submitted to ApJ.

Table 3Results from the regression analysis

Data

Median aperture

α

(1)

(2)

(3)

β

σint

ρ

(4) Intrinsic(5) scatter(6) [dex]

ogarithmic scale. Blue circles and gray squares indicate that the HCN(1-0)′ emissionlog (LHCN)–log (LX ) correlation
IT-sample) and single dish telescopes (θmed = 6.2 kpc; SD-sample),respectively.
Figure 3. Posterior distributions
for the intercept(α), slope(β), intrinsic scatter (σint ), andIT-sample
195 pc37.45+4.10
0.70+0.55
0.93+0.51
0.74+0.18
BH
−5.05
−0.60
−0.33
−0.42
(Figure2b). ColorsSee
indicate the IT- (blue) and SD- (gray) sample, respectively. The width
shown by the solid and the dashed line for IT- and SD-samples,
respectively.
+0.23′
SD-sample
6.2 kpc
40.05
0.27
1.03
0.23+0.23
analysislog (L+2.70(L+0.34
similarX ) yields
ils about the regression analysis. The best-fit regression
parameters
canfor
bethe
found
in
−2.55
−0.35
−0.18 parameter−0.27distributions like these.
HCN )–log• Positive correlation: importance of external regulator on dM /dt?
→ virtually equivalent to SFR-dMlogBH/dt
correlation(M)–log (Ṁ ) correlation
BH−10.85+7.35
−7.95
+4.35
−5.85−4.05

dense

IT-sample

195 pcSD-sample

6.2 kpc• Large scatter: need for other parameters?

1.06+0.89−0.78
0.34+0.46−0.46

0.94+0.47−0.38
1.16+0.27−0.22

log (Mdense /MBH )–log (ṀBH ) correlation

0.82+0.14−0.39
0.26+0.24−0.29

Table 38

Ṁnuclear
ṀwindAngular momentum loss due
to Supernova-explosions
Strong Turbulence

Ṁacc
ṀBH

∝M

BH

∝Σ

SFR = SFE × Σgas

-1

Supermassive black hole
(MBH )

Circumnuclear disk
(Mdense )rin,eﬀ
Gas accretion rate in a turbulent
nuclear diskroutdࠉ
ln:(r )ṀM ((r)r ) 2SQ 6 (r )d ln rQ

Gas surface density
Mparameter
matic picture for a supernova-driven turbulent accretion model. The vertical height oft the:viscous
circumnuclear
disk (CND) is supported by the turbulent
supernova explosions. rin,eff and rout are the effective innermost radius and the outermost radius of the CND (see also the text for details). This:angular: massacc
BH
g at the rate of Ṁacc as the form of black holeas mass of M
accretionvelocity(ṀBH ) or nuclear wind (Ṁwind ). We sumup
dense
dense fuels the nuclear tevents
into Ṁnuclear .
6 2hU :surface density

Q t DSNvt h, ࠉ: v r

3/2

g

∝

g

BH mass

SFE

3
§
·
r
3
1
in

Macc
rin ) 3SDSNK ESNC*6g (rin ) ¨Ṁ¸ 0.13DSN,1rin,3C*,76g,1M BH,7 [M~yr]
BH ((r)© GM BH ¹
Lª « M Eddº 681, 73
Edd
Kawakatu
&
Wada
2008,
ApJ,
0.22M [M~yr]
c

2

BH,8

»

Ṁnuclear
ṀwindAngular momentum loss due
to Supernova-explosions
Strong Turbulence

Ṁacc
ṀBH

∝M

BH

∝Σ

SFR = SFE × Σgas

-1

Supermassive black hole
(MBH )

Circumnuclear disk
(Mdense )rin,eﬀ
Gas accretion rate in a turbulent
nuclear diskroutdࠉ
ln:(r )ṀM ((r)r ) 2SQ 6 (r )d ln rQ

Gas surface density
Mparameter
matic picture for a supernova-driven turbulent accretion model. The vertical height oft the:viscous
circumnuclear
disk (CND) is supported by the turbulent
supernova explosions. rin,eff and rout are the effective innermost radius and the outermost radius of the CND (see also the text for details). This:angular: massacc
BH
g at the rate of Ṁacc as the form of black holeas mass of M
accretionvelocity(ṀBH ) or nuclear wind (Ṁwind ). We sumup
dense
dense fuels the nuclear tevents
into Ṁnuclear .
6 2hU :surface density

Q t DSNvt h, ࠉ: v r

3/2

g

∝

g

BH mass

SFE

3
§
·
r
3
1
in

Macc
rin ) 3SDSNK ESNC*6g (rin ) ¨Ṁ¸ 0.13DSN,1rin,3C*,76g,1M BH,7 [M~yr]
BH ((r)© GM BH ¹
Lª « M Eddº 681, 73
Edd
Kawakatu
&
Wada
2008,
ApJ,
0.22M [M~yr]
c

2

BH,8

»

Direct
withdisk
the modelGasaccretioncomparison
rate in a turbulent nuclear
Q t :viscous parameter Gas surface densitydࠉ
ln:(r )
ṀMaccr ) 2SQ t 6g (r )BH ((r)d ln rQ t DSNvt h, ࠉ: v r::angular velocity

6g

2hUg :surface density

3/2

BH mass

SFE

3
§
·
r
3
1
in

M
(
r
)
3
SD
K
E
C
6
(
r
)
0.13
D
r
C
6
M
Ṁacc
¸
BH (r)
inSN
SN * g in ¨
SN,1 in,3 *,7 g,1
BH,7 [ M~yr]© GM BH ¹
L

The case of NGC 7469
Criticalmass accretion rateª 
« M Edd¬

6g t 6crit (rin ) 䠖SN-driven accretion
350 pc

 M

| 8.6 u10 D
2

c

º
»
11.3μm PAH feature¼
0.22M BH,8[M~yr]→ SFR~ Parameters= SFE3* M~gas1

HCN(1-0) ALMA Cycle 1

Toomre’s stability criterion
2.12 μm H2 1-0 S(1)N (r)cs
VLT/SINFONI
3
-3/2
1/2
6crit (r)0.66[g/cm ]cs,1rin,3 MBH,7
SG

Edd
2

D SN 1, ࠉK 10 M
rinpc], C* 107 [yr -1 ]3[ࠉg/cm 2 ], M BH 107 ࠉ
6g 1[ࠉ
[ M~]
cs 1[km/ s]

1501/2
pc

3/2
crit
SN,1 in,3 s,1 *, 7
Izumi et al. 2016 in prep.

r c C M BH,7 [ࠉM~yr]
Hicks et al. 2009, ApJ, 696, 448

Esquej et al. 2014, ApJ, 780, 86

reverberation → MBH

䐣 795, 149)
(Peterson et al. 2014, ApJ,
10

CND S IN S EYFERT GALAXIES

Direct comparison with the model= SMBH accretion rates

Izumi et al. submitted to ApJ.

1

%
0
0
%
0
1
1%

= Mass from CNDs 11

CND S IN S EYFERT GALAXIES

Direct comparison with the model= SMBH accretion rates

Izumi et al. submitted to ApJ.

Most mass from the CNDs is
consumed for SMBH growth
1

%
0
0
%
0
1
1%

= Mass from CNDs 11

CND S IN S EYFERT GALAXIES

Direct comparison with the model= SMBH accretion rates

Izumi et al. submitted to ApJ.

Most mass from the CNDs is
consumed for SMBH growth
1

%
0
0
%
0
1
1%

Only < 10% mass from the CNDs
are going to the SMBHs= Mass from CNDs 11

ese two events into Ṁnuclear .

Direct comparison with the model= SMBH accretion + disk wind

Izumi et al. submitted to ApJ.

10

%
0
0
1

%
0
0

Mass from the CND= SMBH accretion+ mass outflow as disk winds= Mass from CNDs

12

ese two events into Ṁnuclear .

Direct comparison with the model= SMBH accretion + disk wind

Izumi et al. submitted to ApJ.

%
00

Are we 1dissolving
the balance of
0
%
0
0
1
mass flow at the nuclearof
Mass from regions
the CND= SMBH accretion
Seyfert galaxies??
+ mass outflow as disk winds= Mass from CNDs

12

Speculation on this scenario• CNDは星形成活動を示すので、SNeも自然と期待できる。
e.g., Esquej et al. 2014, ApJ, 780, 86→ ~ 103-4 yrに一回爆発• 爆発の影響で、ガスはclumpyな構造に。
→ clumpy torus? nuclear obscuration?
66• 粘性降着のタイムスケールは、

WADA, PAPADO

SN rate = 5.4×10-5 yr-1

- CND: a few Myr- 降着円盤: < ~a few×10 Myr• 星形成の持続時間は~100Myr程度→ AGN-SBのcausal connectionは可能

Wada et al. 2009, ApJ, 702, 63
13

Speculation on this scenarioe.g., Esquej et al. 2014, ApJ, 780, 86→ ~ 103-4 yrに一回爆発

log NH• CNDは星形成活動を示すので、SNeも自然と期待できる。

• 爆発の影響で、ガスはclumpyな構造に。

水素柱密度のViewing Angle依存性→ clumpy torus? nuclear obscuration?
66
WADA, PAPADO• 粘性降着のタイムスケールは、

Viewingangle
SN rate= [deg]5.4×10-5 yr-1

- CND: a few Myr- 降着円盤: < ~a few×10 Myr• 星形成の持続時間は~100Myr程度→ AGN-SBのcausal connectionは可能

Wada et al. 2009, ApJ, 702, 63
13

Speculation on this scenario• Can we form high mass end (MBH ~ 1e9 Msun) SMBHs within 1e9 year?
- Partial fraction of the CND's gas will consumed for SF- Enormous amount of gas (>~1e10-11Msun) is required even when we
assume the SMG-class SFE

2
Yan et al.
merger is critical for making high-mass-end
objects?
• SMBHlog (Lλ/erg/s/cm2/A)

al.

4000 Å-10000 Å. If this sharp drop off is due to extinction, it
requires a large dust reddening of Av ∼ 7 mag at λ ∼ 2500 −
4000 Å and a small dust reddening ∼ 0.5 mag at < 2500 Å
Mrk 231(Veilleux et al. 2013). Thus, an unusual complex geometricstructure for the extinction material surrounding the disk must
be designed (Veilleux et al. 2013; Leighly et al. 2014).
Second, Mrk 231 is an extremely powerful Fe II emitter assuggested by the spectrum on the blue side of Hα and on bothsides of Hβ . Such a high level of optical Fe line emission
suggests a significant amount of Fe line emission at the UV
band; however, it is not visible in the observed UV spectrum(Veilleux et al. 2013; Leighly et al. 2014).
Third, a number of broad low-ionization absorption line
systems, suchas Na I D, Ca II,4000
Mg II, Mg I, and Fe
II, have been
2000
6000
8000
identified in the optical-to-UV spectrum, which suggests thatMrk 231 should be an Fe low-ionization broad absorption line
quasar (FeLoBAL) (Veilleux et al. 2013). However, the exYan
2015, ApJ, 809, 117
pected corresponding absorption features at theUV etandal.
FUV
bands are not evident.

λ (A)

14

First 10 pc (!) scale view of thenuclear region of a type-1 AGN
NGC 1097 (type-1 LLAGN)• Colour = HCN(4-3)• Contour = continuum@350GHz→ significant time variability!

• Surprisingly, no emission of~10 pcKohno et al. in prep.
Izumi et al. in prep.

HCN(4-3), as well as the dust
continuum, were detected at thenucleus of this LLAGN→ disappearance of dusty torus
in the low-luminosity regime?
15

Summary• Positive correlation between M

dense and dMBH/dt- virtual equivalence to the SFR-dMBH/dt correlation- large scatter (need other parameters?)- better correlation for nuclear scale gas than the galactic one• Invoke SN-driven turbulence model to discuss mass accretion• Direct comparison of dM /dt and mass accreted from the CND
BH- part of the gas from the CND is consumed for the black hole growth- with accounting for the disk wind, we found a fairy good agreementin NGC 4051 and NGC 7469
→ start to dissolve the balance of mass flow!?

→ see more details in Izumi et al. (submitted to ApJ)
16