AGN質量降着＠sub-kpc ＠NAOJ

12/21-22/2015

Sub kpc -pcスケールでの質量降着に関して
和田 桂一
鹿児島大学

dL
dt

Phinney'(1994)'in'“Mass1transfer'induced'activity'in'galaxies”

dL=dt(r iF i)

i

{

Fi :

Ljj=Ikdk/dt :dIkj /dt :kgravity(turbulent)/viscosity
magnetic/force

oblique/shock/(e.g./spiral/shock)pressure/gradient
cloud=cloud/collision
merger{{outflow,/star/formation'angular'momentum''transfer'(exchange)Fueling/Problem:/origins/of/torques/viscosity• /kpc/scale/✔/Galaxy/interactions,/major/minor/mergers/(Taniguchi,/KW/
1996,/Saitoh/et/al./2004)/–Dynamical/friction/between/stars/and/gases//✔/Stellar/bar/double/bar/(KW/1992,95)/✔/Spiral/shock/driven/turbulence/(KW,/Koda/2003)/• /100/pc/scale/–/Collision/between/dense/clumps,/dynamical/friction/✔/Gravity=driven/turbulence/(KW,/Meurer,/Norman/2002)/✔/SN=driven/turbulence/in/a/molecular/torus/(KW,/Norman/2002)//✔/Radiation/drag/(Kawakatu,/Saitoh,/KW/2004)/• /pc/and/sub=pc/scales/–MHD/turbulence/–Radiative/avalanche/✔/Radiation=driven/fountain/(KW/2012,/2015)

from kpc to pc: four possible
mechanisms
majer merger■ minor merger■ external accretion (gas streamer)■ secular evolution (bar, spiral)■

from kpc to pc: four possible mechanisms■majer merger

Villforth+2014
z/</0.7/AGNのhostAsymmetry%no/AGN

minor'effect'for'triggering'AGN?
Irregularity

cf.//Karouzos+'2014////////Radio/loud/AGNsとnon=AGNは/環境には違いはないが、close=pairに/Merger

AGNがassociateしているものもmerger'simulation

Volonteri+2015

AGN

Volonteri+2015

SFR'(<'100'pc)とBH'accretion'rate'(<5'pc)は相関
merger/phaseSFR'(<'5'kpc)

SFR'(<'100'pc)

from kpc to pc: four possible mechanisms
major merger■ minor merger■

Neistein,'Netzer'(2015)'''Semi1Analytic'Model※'accretion'rateをSFRと連動させるというモデル

more'major'mergers'in'luminous''AGN

merger'fraction'is'larger'in'AGN'hosts

Formation of a small spiral galaxy
DMgasstars

Saitoh et al. (2004)

3-D structure of the inner gas disk

z=2.1

1kpc
The disk is formed from many ‘rings’, which are remnants of past mergers.

Saitoh et al. (2004)

Evolution of Spin vectorof the gas (R< 5kpc)
Saitoh et al. (2004)

z = 5 --> 2

Z=4.5
Z=3.0,2.5

Z=4
Z=3.5

Z=5yx

Angular momentum does
not change significantly
during evolution.

Z=4Evolution of A.M. vector of the core

Z=2.5

R < 0.5 kpc

Z=3.5

yx

Spin axis of the core changes its
direction often during the formation
process.
The central part has been affectedby mergers w/ different A.M.
Saitoh et al. (2004)

Z=5

Mass accretion to sub kpc is correlated with merger
process of halos
Mbaryon (<300 pc)/MDM ~ 0.04

starsgas

N-body/SPH
Saitoh & Wada (2004)
Saitoh et al. 2008

tidal force due to mergers drives the gas into 100 pc
regionfrom kpc to pc: four possible mechanisms■minor merger

Martini+/2013
dust'in'Early'type'galaxies:''/external'origin?'''How?'(satellite'merger?)“minor1merger”'driven'starburst'and'fuelingsatellite/のBHが落ちてくる

Taniguchi,/KW/(1996)
density
BH/mass/ratio:

Ms/Mp/=/0.1
6'kpc
重力不安定

15

“minor1merger”'driven'starburst'and'fueling

Taniguchi,/KW/(1996)

Ms/Mp/=/0.5
6'kpc

重力不安定16minor'merger'
disk'不安定'or'''''core形成

prograde~300'pc'core

retrogradeTaniguchi,/KW/(1996)

from/kpc/to/pc://four/possible/mechanisms■

secular/evolution

Do'bars'contribute'to'the'nuclear'activity?
1''no'correlation''in'bar1strength'and'X1ray'luminosity:''e.g.//Cisternas+2013

1''molecular'gas'is'concentrated'in'barred'galaxies
e.g./Sakamoto+1999

from kpc to pc: four possible mechanisms■

secular evolution by bar
中心集中度

e.g./Sakamoto+1999

Sakamoto+1999

Bar&spiral1driven'fueling''(Baba'2015)

visualized/by/T./TakedaBars-within-bars: a mechanism for fuelingactive galactic nuclei

Shlosman, Frank, Begelman (1989) Nature 338, 45■■

Citation数 545の有名論文■ でも、ちゃんと読んでいる人、たぶん少数回転するgaseous/stellar disk/sphereには、 barmode 不安定■■（global不安定）がある

例） Maclaurin spheroid■
Trot/|W| > 0.2738で不安定例）stellar disk (Ostriker-Peebles criterion)■ T
rot/|W| > 0.14で不安定

Bars=within=Bars/model///Shlosman/et/al./(1989)■

Bar不安定の条件

Trot/|W| > tcrit を、書き換えて、astar/agas > C(tcrit) / g2,■

g, tcrit を与えたとき、どれだけgas diskがshrinkすると、bar不安
定になるか■

e.g. g=0.2, tcrit = 0.14を起こす■■

astar/agas > 10 なら、bar不安定

astar=1 kpc の銀河で、stellar bar-driven fueling
集中■

g=Mgas/Mtotal

agas = 100pc

bar不安定になる

gasが中心質量、角運動量の再分配が起こり、一部のgasが中心に落ち、coreを形成
coreが、 astar/agas > C(tcrit) / g2を満たせば、bar不安定を起こす

結局、角運動量輸送しないとループが完成しないbar'instability'of'rotating'gas'sphere

Smith et al. (1996)

２度目以降のbar不安定は非常に弱い

bar-within-bar ループは完成しない

T/W= 0.24

Bar mode amplitude

3D structure of the nuclear massive disk
5122 x 32 grid points (0.5 pc/grid)

Wada/(2001)

Due'to'radiative'cooling,'
local'instability'dominates'the'bar'instability
Angular'momemtum'
change'by''''''1'''torque'by'spiral'arms'''''1'''turbulent'viscosity

128'pc２つの重要な物理過程：Feeding/Feedback

AGN進化

R/=/pc=数10/pc領域（ダークドメイン）は未解明
UV/optical/infrared,/radio,/X=ray

Spectroscopic
X=ray,/optical,UV

infraredR/=

10=5/pc

1/pc

BH

Accretion/
Disk？
10/pc

Molecular/lines

100/pc

1/kpc

Imaging

10/kpc0.1/Mpc

torus
NLR

BLR

ENLR

Feedback/by/Jet,/outflow,/radiation,…

”Dark'domain"'で何が起こっているか？
Davies+2014
VLT/SINFONI■ velocity field, warm H2 (2µm) in central 100 pc of 10 AGNs
■CMD in all 5 active AGNs

160/pc
H=bandH2'110S(1)NGC/5643/(Seyfert/2)

Davies+2014

IC'5267'(inactive)

H2/1=0S(1)300/pc
H2'110S(1)counter'rotating'gas'disk.''“pre1AGN”'phase?
Davies+2014

VLT/SINFONI

velocity field, warm H2 in central 100 pc of 10 AGNs
■ CMD in all 5 active AGNs
■ lack of gas in inactive galaxies■ no on-going SF in both active and inactive■ molecular outflows (~150 km/s) observed in 4/5 active
galaxies, not in inactive ones
■ two accretion process?
■ long, continuous, internal supply■ circum-nuclear spirals■ short, stochastic, external supply■ counter rotating gas■ HI inter-galactic filaments in group■mismatch'in'time1scale'
AGN'duty1cycle'vs.''accretion'time'scalestarburst-AGN connection
Netzer/2009
high=z/quasars

local/type=2/

Lbol

Castro/et/al./2015
29

Akari

Wada & Norman (2002) ApJ 566, L21

Obscuring “torus” around a supermassive BH with
nuclear starburst
2562 x 128, uniform grid, 0.25pc/gridRadiative cooling (5-108 K), SN feedback, selfgravity
MBH = 108 Msun, Mgas = 107 Msun, SNR = 0.8 yr-1

64 pc

Modeling the ISM in a galactic center: Progress for the last decade• 642/pc/x/32/pc/• self=gravity/• radiajve/cooling/• SNe/• BH

Wada/&/Norman/2002

Gas mass (r < 1 pc)

Esquej+2014
mass accretion rate isenhanced by SNe feedback

Mdot
SFR

Time [Myr]316/26from'kpc'to'sub1pc:''課題・major merger, minor merger, accretion, secular evolutionの相対的重要性(どういう状況で何が効いているのか）・r < 数10 pc- nuclear SF とfuelingの因果関係- AGN feedbackとfuelingの関係（positive or negative?)・r < r̲dust (sub pc)- 外側のaccretion rateとの関係

Ṁ (R)

・AGN構造（accretion disk, BLR, NLR, torus, jet)とaccretionの関係、そのredshift進化