12/25-27/2019 理論懇シンポジウム（国立天文台）活動銀河核の新描像
近傍unreso

和田桂一

lve

鹿児島大学d天の川銀河研究センター

Schartmann, M.
Izumi, T.
Imanishi, M.
Norman, C.
Kudoh, Y.
Meijerink, R.
Nagao, T.
Tomisaka, K.
Buchner, Y.
…

近傍２型セイファートで“トーラス”が直接観測
e.g. NGC 1068, Circus galaxy

Combes et al. 201910-20 pc ＝みんなが考えてたより大きい

Imanishi et al. 20182

意外と大きかった “obscuring torus” Combes et al. 20193

Radiation-driven Fountain and Origin of Torus around Active Galactic Nuclei

疑似観測Wada (2012)

radiation-hydro modellingMulti-phase Nature of a Radiation-driven Fountain with Nuclear
Starburst in a Low-mass Active Galactic Nucleus
KW, Schartmann, & Meijerink (2016)

SED fitting for Circinus
Multi-phase Gas in the Circinus galaxy

X-factor, line ratios

I. Non-LTE Calculations of CO Lines

KW, Fukushige, Izumi, & Tomisaka (2016) ApJ 852, 88

II. A Novel View of the Molecular and Atomic
Obscuring Structures Revealed with ALMA

CO(3-2), [CI]Izumi, KW, Fukushige, Hamamura & Kohno, ApJ in press

III. Structures of the Nuclear Ionized Gas

NLRs: [OIII], [NII],…

KW, Yonekura & Nagao, ApJ in pressUnified Structure of AGNs ?

Type 2Type 1

Type 1トーラス
1-100 pc?

NLR
Urry & Padovani (1995)

Super massive BH (106-8 Msun )＋ accretion disk (AU scale）＋ BLR+ NRL + Obscuring molecular torus (1-100 pc) + Jet + ENLR

What is the size? How is the thickness maintained? How
is it formed and How does it evolve?
Origin of polar dust emission?

VLTI/MIDI

5Tristram+2014

赤外放射は、回転軸方向が支配的

Circinus galaxy

6•What we should &did take intoaccount in models.

External gravity, Self-gravity– stars, BH & ISM•

Heating– Supernova feedback– X-ray (AGN):• Compton (for ionized gas)
• Coulomb (for dense atomic, molecular gas)
• Photoionization (atomic/molecular gas)
– UV (AGN & stars）• Photoionization (atomic/molecular gas)
• Photo-electric heating with dust•

Cooling– metals, molecules, bremsstrahlung•

Radiation transfer– non-isotropic direct radiation, scattering– pressure by X-ray, UV, infrared photon for dust &electron– line forces•磁場•Chemistry– XDR, PDR– H2 formation/dissociation–73-D Radiative Hydrodynamics of a gas disk
around a SMBH
Code: RHD.*(Wada12) ,based on HD.* (Wada+09)*Uniform grid 2563
*Ray tracing(2563 rays),* Self-gravity* Radiation pressure* Radiative cooling* X-ray heating* uniform FUV* SNe feedback* non-equilibrium chemistry

LU V ( )cos (1 + 2 cos )potential:fixed, spherically symmetric
SMBH 106-9 Msun

Gas disk~0.1-1.0 MBH
R=16-32 pc8

Chemo-Radia'on Hydrodynamics

i, j, kLXe
2 nrijkijk

ijk =tθr

LU V ( )LXAccretion Disk

ijk

Non-equilibrium
chemistry for 25 speciescos (1 + 2 cos )sphericalÁdámkovics, Glassgold, Meijerink (2011)
Meijerink , Spaans (2005)

H, H2, H+, H2+, H3+, H-, e-, O, O+, O2, O2+, O2H+, OH, OH+,H2O, H2O+, H3O+, C, C+, CO, Na, Na+, He, He+
An example of fountain flow and formation of a “torus-like” structure

density

Wada (2012)

M_BH = 10^7 Msun

M_BH = 10^6 Msun

w/o supernova feedback

with supernova feedback

fast outflowing gas

slow back flowing gas

dense outflowing gas goes around the “torus”
64 pc

32 pc

torus scaleのガスはstatic ではない

Three phases ofhydrogen

Model forCircus galaxy
XDR chemistry is included

分子、中性、電離ガスは

分布もkinematicsも異なる

KW, Schartmann,
Meijerink (2016)12

Radia%on-driven fountain model
観測を説明できるか？
multi-wave length obs.
・SED (type-1, type-2)?

10μm feature・molecular gas (H2, CO etc.),
・atomic gas (H, [CI] etc.)
・ionized gas(Narrow Line Region, BLR)
・X-ray specram

Wada 2012

Radiation transfer calculation as post-processes

Observing the fountain

Schartmann, KW, Prieto, Tristrum, Burkert (2014)

one snapshot from RHD

3D Monte Carlo (RADMC-3D)

0.1 μm

Ou3lows
face-onedge-on12 μm

Thick warm
disk =‘torus’
500 μmThin colddisk
30 pc
14

SEDs change depending on 'me &viewing angle

Schartmann+2014

non-steady outflows causes the variation in ~Myr
ER=0.130°30°
90°60°

15

Circinus galaxy (Sy2 at 4Mpc)

yellow: i-band
red: HαCase study: Circinus galaxy
12μm

polar emission

hot dust

KW, Schartmann, & Meijerink (2016)

SED and 10 μm absorption arereproduced for viewing angle > 75deg
Nuclear disk should be close toedge-on!
10 μm

cold dust

rotational
axis90deg

17Tristram+ 2014

ALMA Cycle 4 Observations (Band 7 + 8) 18
Izumi, KW+2018

CO(3-2) + [CI](1-0)

ionizing coneedge-on “torus”

30 pccold molecular gas in Circinus KW, Fukushige, Izumi, Tomisaka (2018)

3D non-LTE radiative transfer for CO, CI, …,
based on Wada & Tomisaka (2005): Monte Carlo based code

CO (3-2) integrated intensity map, face-on
CO abundance

density

16 pc

resolution: 0.25 pc
CO abundance 19Quantitative comparison with fountain modelIzumi et al. 2018c

ALMA

分子・原子ガスの速度構造の違いを再現
model[CI]• Indeed, we found diﬀerent line profiles for the simulated CO(3-2) and [CI](1-0)• Triple-Gaussians can well fit the profile → outflow components stand out!
• Good consistency between ALMA obs. and our simulation→ Support the fountain scheme → Physical origin of the “torus” !?

20Origin of NLR in AGN

Circinus

torus? + funnel of ionized gas on 10 pc

extinction map (K/I-band) + [OIII]
brighter regions,higher dust absorption

Mezcua+2016

Origin of NLR?
outflowing ionized gas ?

H+

Fountain model + multi-dimensional RT
using Cloudy (Ferland 2017)

Edge-on view

Hβ[OIII]

AGN

KW, Yonekura, Nagao (2018) 22

Fountain modelの電離ガス[OIII] 88 μm, 52 μmでの構造

３次元構造

松永卒論(予定）

23

A new dynamical, multi-phase picture of AGN,
suggested by solving basic equations
ionized gas = NLR[CI]

neutral gas

fountain flow
= “torus”
nuclear starburst

warm dust
molecular gas + cold dustCOmolecular gas

10 1 110102 pc

Seyfert type AGNの典型的構造？

24•What we should &did take into
account in models.

External gravity, Self-gravity– stars, BH & ISM•

Heating– Supernova feedback– X-ray (AGN):• Compton (for ionized gas)
• Coulomb (for dense atomic, molecular gas)
• Photoionization (atomic/molecular gas)
– UV (AGN & stars）• Photoionization (atomic/molecular gas)
• Photo-electric heating with dust•

Cooling– metals, molecules, bremsstrahlung•

Radiation transfer– non-isotropic direct radiation, scattering– pressure by X-ray, UV, infrared photon for dust &electron– line forces•

磁場•Chemistry– XDR, PDR– H2 formation/dissociation–3D MHD simulation of the torus

25

Kudoh, KW, Norman, in prep.

β < 0.1 の強い磁場、磁気乱流が形成

plasma β＝thermal pressure/ magnetic pressure

26

回転方向

平均磁場の向き逆転：

cooling/heatingを考慮しても起こる（周期は長くなる）
Kudoh, KW, Norman
in prep.

27

BH含むgalaxy mergerの計算

Stellar System
Mass : 10 M⊙
9Black Hole
Mass : 107M⊙

Particles : 106

Radius : 500pc

SBH

Gas Disk
Mass : 108M⊙

PBH

Particles : 2 × 105
Radius : 100pc

28

【Results - Morphology】▷Fiducial Model : SBH Systemを水平にPBH Systemへ向け落とす。

Face-onEdge-on【Results - Accretion Rate】

Kawaguchi, Yutani, KW 2019

MPBH : 1.0 × 107 M ⊙ → 1.7 × 107 M ⊙MSBH : 1.0 × 107 M ⊙ → 2.1 × 107 M ⊙Early Phase▷PBHとSBHが大きく距離を縮めたタイミングに、Super-Eddington質量降着が起こる(PBH : 数Myr, SBH : ~ 10Myr)。

mergerで持ち込まれたガスの行方
Kawaguchi, Yutani, KW 201916%
R > 1000pc

SF

3%

8%
PBH

11%
SBH

Fiducial Model(t = 100Myr時点で)

R < 100pc

100pc < R < 1000pc

25%

37%
▷持ち込まれたガスの10~20%がBHsの成長に使われ、約60%がバイナリ
BH周辺1000pcに滞在する=> obscurationに寄与

Kawaguchi, Yutani, KW 2019

AGN luminosityとcolumn densityの時間変化: luminous phaseはobscureされる

Compton thick今後の課題の一部• high-z, luminous AGNs (quasars)の”torus”構造• Comp'on-thickなdust-free X線散乱体の正体？
• accre'on disk近傍の構造(e.g. BLR,disk wind)との関連• molecular ouXlowの起源
33

X-ray observations suggest a stratified structure of the torus?
X-ray selected ~ 2000 AGNs

Fraction of obscured AGNs depends
on column density?

Buchner+201534おまけ: AGNまわりで「惑星」”blanet” ?

和田、塚本、小久保（2019)