obscuring torus Combes et al. 2019 3 Radiation-driven Fountain and - - PDF document

活動銀河核の新描像


• 12/25-27/2019 理論懇シンポジウム （国立天文台）

和田桂一 鹿児島大学 天の川銀河研究センター

u n r e s

• l

v e d

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

近傍

2

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

10-20 pc ＝みんなが考えてたより大きい

Imanishi et al. 2018

Combes et al. 2019

3

Combes et al. 2019

意外と大きかった “obscuring torus”

Multi-phase Gas in the Circinus galaxy

• I. Non-LTE Calculations of CO Lines
• II. A Novel View of the Molecular and Atomic

Obscuring Structures Revealed with ALMA

KW, Fukushige, Izumi, & Tomisaka (2016) ApJ 852, 88 Izumi, KW, Fukushige, Hamamura & Kohno, ApJ in press

• III. Structures of the Nuclear Ionized Gas

KW, Yonekura & Nagao, ApJ in press Radiation-driven Fountain and Origin of Torus around Active Galactic Nuclei Wada (2012)

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

radiation-hydro modelling SED fitting for Circinus CO(3-2), [CI] NLRs: [OIII], [NII],… X-factor, line ratios 疑似観測

Type 1 Type 2 Type 1

Unified Structure of AGNs ?

1-100 pc? 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?

Urry & Padovani (1995) 5

トーラス NLR Origin of polar dust emission?

6

VLTI/MIDI Tristram+2014

赤外放射は、回転軸方向が支配的

Circinus galaxy

• 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 – 7

What we should & did take into account in models.

3-D Radiative Hydrodynamics of a gas disk around a SMBH

potential: fixed, spherically symmetric Gas disk ~0.1-1.0 MBH R=16-32 pc SMBH 106-9 Msun

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

8

LUV (θ) ∝ cos θ(1 + 2 cos θ)

Chemo-Radia'on Hydrodynamics

Ádámkovics, Glassgold, Meijerink (2011)

Accretion Disk

i, j, k

r

θ

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+

Non-equilibrium chemistry for 25 species

ξijk = LX r2

ijknijk

e−τijk

∆t

LUV (θ) ∝ cos θ(1 + 2 cos θ)

LX

spherical

An example of fountain flow and formation of a “torus-like” structure

Wada (2012) density

M_BH = 10^7 Msun M_BH = 10^6 Msun

w/o supernova feedback with supernova feedback

64 pc 32 pc

dense outflowing gas goes around the “torus”

fast outflowing gas slow back flowing gas

torus scaleのガスはstatic ではない

12

Three phases of hydrogen Model for Circus galaxy

KW, Schartmann, Meijerink (2016)

XDR chemistry is included

分子、中性、電離ガスは 分布もkinematicsも異なる

Radia%on-driven fountain model

観測を説明できるか？

・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

?

Radiation transfer calculation as post-processes

Wada 2012

multi-wave length obs.

14

0.1 μm 12 μm 500 μm face-on edge-on

Ou3lows

30 pc

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

Observing the fountain

Thick warm disk =‘torus’ Thin cold disk

3D Monte Carlo (RADMC-3D)

• ne snapshot from RHD

SEDs change depending on 'me &viewing angle

15

ER=0.13

0° 60° 90° 30° non-steady outflows causes the variation in ~Myr

Schartmann+2014

yellow: i-band red: Hα

Circinus galaxy (Sy2 at 4Mpc)

17

Case study: Circinus galaxy

SED and 10 μm absorption are reproduced for viewing angle > 75deg Nuclear disk should be close to edge-on! 10 μm 90deg

polar emission

12μm

KW, Schartmann, & Meijerink (2016)

Tristram+ 2014

rotational axis cold dust hot dust

18

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

ionizing cone

Izumi, KW+2018

edge-on “torus”

30 pc

ALMA Cycle 4 Observations (Band 7 + 8)

19

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

KW, Fukushige, Izumi, Tomisaka (2018) 16 pc

cold molecular gas in Circinus

resolution: 0.25 pc

CO abundance CO abundance density

20

• 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” !?

Quantitative comparison with fountain model

Izumi et al. 2018c

ALMA model [CI]

分子・原子ガスの速度構造の違いを再現

extinction map (K/I-band) + [OIII]

Circinus

brighter regions, higher dust absorption

torus? + funnel of ionized gas on 10 pc Origin of NLR in AGN

Mezcua+2016

22

Fountain model + multi-dimensional RT using Cloudy (Ferland 2017) KW, Yonekura, Nagao (2018)

AGN

H+

Edge-on view

Hβ

[OIII]

Origin of NLR?

• utflowing ionized gas ?

23

松永卒論(予定）

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

３次元構造

24

A new dynamical, multi-phase picture of AGN, suggested by solving basic equations

molecular gas warm dust nuclear starburst neutral gas

ionized gas = NLR

molecular gas + cold dust

10−1

1

10 102 pc

fountain flow = “torus”

[CI] CO Seyfert type AGNの典型的構造？

• 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 – 25

What we should & did take into account in models.

26

3D MHD simulation of the torus

Kudoh, KW, Norman, in prep.

plasma β ＝ thermal pressure/ magnetic pressure

β < 0.1 の強い磁場、磁気乱流が形成

27

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.

28

BH含むgalaxy mergerの計算

PBH SBH

Black Hole

Mass : 107M⊙

Stellar System

Mass : 109M⊙ Particles : 106 Radius : 500pc

Gas Disk

Mass : Particles : Radius : 100pc

108M⊙

2 × 105

【Results - Morphology】

Edge-on Face-on

▷Fiducial Model : SBH Systemを水平にPBH Systemへ向け落とす。

【Results - Accretion Rate】

MPBH : 1.0 × 107M⊙ → 1.7 × 107M⊙ MSBH : 1.0 × 107M⊙ → 2.1 × 107M⊙

▷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)。

Early Phase

Kawaguchi, Yutani, KW 2019

mergerで持ち込まれたガスの行方

16% 3% 37% 25% 11% 8%

PBH SBH R < 100pc 100pc < R < 1000pc R > 1000pc SF

Fiducial Model (t = 100Myr時点で) ▷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

Kawaguchi, Yutani, KW 2019

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 34

Buchner+2015

X-ray selected ~ 2000 AGNs

X-ray observations suggest a stratified structure of the torus?

?

Fraction of obscured AGNs depends

• n column density

和田、塚本、小久保（2019)

おまけ: AGNまわりで「惑星」”blanet” ?