AGNジェットとSMBH近傍の高密度ガス雲との関係～Physical relationship between AGN jetsand high density gas clouds near SMBHs～

川勝望(呉高専)
星形成と銀河構造における磁場の役割（鹿児島大学郡元キャンパス）2017.12.21

Key words in this WS
star formation,
molecular clouds,
magnetic fields
My interests
Active galactic nuclei; SMBH, AGN torus, jets

Star formation(starburst)
Fueling/Obscuration

Molecular gasTriger

AGN
Feedback(Jet/Radiation)

This talk(1) High density clouds near SMBH (～1 pc)(2) Interaction between AGN jets and clouds

Introduction
What are AGNs ?
NLRv~500km/s
n=102-3cm-3Jets

BLR
v=2000-10,000km/s
n=1010-12cm-3

1-10pc©Ricci Claudio

The circumnuclear matter distribution around AGNs are highly uncertain.

Time variability (X-ray)
Δt = a few months & years
Highly non-uniform ISM such as clumps within 1pc

Miniutti et al. (2013)

AGN-Nuclear starburst (< 100pc) relation

Seyfert galaxies

positive correlation

Esquej+2013(see., Imanishi & Wada 2004; Imanishi+2011)

AGN-Dense molecular gas (< 100pc) relation
CND (<100pc)
Galaxypositive correlation
HCN(1-0)⇒

Izumi+2016

AGN feedback (e.g., Silk & Rees 1998)
Luminosity function of galaxies

AGN feedback(radio mode)⇒Suppress SF

Croton et al. (2006)

Jet-induced star formation in high-z radio galaxies
The direct association of the radio
components with both UVcontinuum and Lyα emission
strongly indicates the jet-induced
star formation.

Bicknell +2000

Simulations of AGN jets interacting with clouds

Early stage

Wagner & Bicknell 2011

1 kpc

Simulations of AGN jets interacting with clouds
RUN C

RUN D

RUN E

Denser and cold clouds→ A bent jet can be formed!

Wang et al. 2010

[Main goals]
・Properties of gas clouds near SMBH
・AGN jet-clouds interaction⇒ How new born jets propagate
NLRjet©Ricci Claudio

1-10pcTarget: 3C 84 (NGC 1275)

Recurrent jets
~ 10 pc
Core of Perseus cluster

Asada et al. 2006

Molecular hydrogen circumnuclear disk
Shock tracers: near infrared H2, [FeII] lines by NIFS Gemini (Scharwachter+13)~50pc rotating discM H2 ( 50 pc) ~ 4  108 M sun
M BH ~ 8  108 M sun
T ~ 1.5  104 K, ne ~ 4  103 cm -3

10 pc-scale free-free-absorbed (FFA) plasma torus
Walker et al. 2000

Imaging @2.3, 5, 8.4, 15.4, 22, 43 GHz
2 pc

NObs.
SNSFFA ff   2Walker found 10 pc uniform
plasma torus (disk).
How about much smaller scale ?

Strong new born radio jet 3C 84 ( ~1pc)

Nagai et al. 2010

Jet –head advancing velocityvh  0.2  0.3c
We did not detect the counter jets so far.
Suzuki et al. 2012

New discovery of ~1 pc FFA plasma torus
KVN and VERA Array (KaVA) 43GHz, KVN 86GHz
KaVA 43.2 GHz2016 Feb 22

N1

KaVA 43.2 GHz (restored)2016 Feb 22
0.18 Jy/b

KVN 86.2 GHz2016 Feb 23

6.28 Jy/b

5.82 Jy/b

6.82 Jy/b

4.71 Jy/b

0.41 Jy/b

C1
C3
0.5 pcWajima, Kino, NK+(cf. Fujita & Nagai 2017)

0.5 pc

0.5 pcF (N1)
 0.025
F (C3)F (N1)
 0.089
F (C3)

Optically thick spectrum of N1 component S   1.2
→ Free-Free Absorption @ ~1pc

Physical properties of absorbing medium at pc scale
1. How about a parsec scale ? Uniform or clumpy ?
F (C3)obs
 ff (43GHz)  ln F (N1) ~ 3.63  ff   0.57 [  ff   2 : homogeneous]obs (86 GHz)  ln F (C3)obs ~ 2.44 ⇒ clumpy absorbing medium
 ff
F (N1)obs

2. Number density of absorbers : FFA formula


2

32

 L   ne   Te    
 ff ( )  0.46  106   1GHz -3  
41pc
K1cm
10  2 ne   Te 
-3  4
 1cm   10 K 32

1

2.1

2.1

 L    
 2.17  106    ff ( )
 1pc   1GHz ne ~ 1.4  105 cm -3 @ 43GHz
5-3n~
2.5

10cm@86GHz
 e(ifT  104 K , L  1pc)

Absorbing medium is clumpy ?
2005～2015
N1 non-detection2016 N1 first detection

N1Large gap

C1
C1
C3Oct. 2014

C3
Intrinsic distance
C1-C3: 1.6pc
C1-N1: 1.4pc

τ(C1-N1) >>τ(N1) → < pc-scale clumpy dense gas clouds ?

2015 Aug 19 Speak = 5.72 J/b2015 Sep 14 Speak = 5.38 J/b2015 Oct 12 Speak = 4.94 J/b2015 Nov 13 Speak = 4.92 J/b2015 Dec 6 Speak = 5.21 J/b

2016 Jan 5 Speak = 5.18 J/b

2016 Jan 20 Speak = 6.22 J/b

2016 Feb 22 Speak = 6.09 J/b

2016 Mar 20 Speak = 7.84 J/b

2016 Apr 19 Speak = 8.31 J/b

2016 May 23 Speak = 8.94 J/b

2016 Jun 12 Speak = 9.80 J/b–4–2

Relative declination [mas]02
4 –4 –2 02412-Epoch Images of 3C 84 at 43 GHz

0.5 pc20–2

20–2

20 –220 –2
Relative right ascension [mas]

20 –2
20 –2
Wajima,Kino,
NK+In March 2016, N1 disappears again.
→ Absorbing medium would change during ~6 month.
→ clumpy clouds pass though the line of sight ?
tcross rclump
vh rclump   vh ~ 0.6yr 
0.03pc  0.1c 1Schematic picture of 1pc clumpy plasma torus
Parsec-scale clumpy plasma torus

rtorus,in  d tan 40 ~ 0.1pc ~ rsub(d  0.1pc)

N1

Sublimation radius~ inner radius of plasma torus

1.4pc

R ~ 1pc

2dC1

 ff ~ 1
1.6pc

 ~ 40
C3

 ff  1

 ff  1
C1(core) does not obscure.

Have we observed the emission from ionized clumpy
dense gas clouds ? Maybe yes.
NLR ne ~102 -103cm-3

AGN optical spectroscopy
Coronal line region clouds

ne ~105 -106cm-3
r ~1100pc

This workne ~105 cm-3,T 104 K
r ~1pcMurayama & Taniguchi +98

Direct evidence of dense high-ionized gas clouds

Circum-nuclear structure of 3C 84 (< ~10 pc)
Parsec-scale clumpy plasma torusN1

1.4pc

ne ~1056 cm-3,T 104 K
 ~ 40

R ~ 10pc

R ~ 1pc

2dC1

uniform disk (Walker +00)

1.6pc

ne ~104 cm-3,T 104 K
C3Obs.

Flip of C3 peak position~0.35 pc
Start of flux
increase

Flux

C3

Primary jet
direction

C1timeDirect evidence jet-cloud interaction
Ram pressure balance

cloudsRclump ~ 0.14pc

Number density of gas cloudsEnhancement of linear polarization

C3

RM obs   6.3  1.9   10 [rad m ]5

2Nagai +2017

Main component s in C3 is consistent with hot spot (terminal shock).
Clumpy medium interacting with jets is responsible for the observed rotation measure.

ne ~ 104 cm-3 , Rclump ~ 0.03pc

Origin of gas clouds
1. Ionized gas (T >104 K) clouds (NLR clouds)
at ~1pc
The clumpy clouds within ~1pc plasma torus
Clumpy clouds expected by FFA

The radiation feedback drives a“fountain,” that is, a vertical circulationof gas in 1-10pc.
Ionized outflow interact with AGN jets ?

Radiation-driven fountain model (Wada +2012)

2. Self-gravitating cold gas cloudsnc  Rclump M clump,obs  3M sun  4 3  
0.14pc
10cm


 cs

331.5

 cs   r   M BH M clump,crit rclump  0.2 M sun   9
3G
 1km/s   1pc   10 M sun 20.5

Mclump,crit  Mclump,obs
Self-gravitating cloud if Tgas < 100K
The AGN jet-induced SF might be occurred.
It is essential to explore whether cold gas
clouds coexist, together with hot/warm gasby ALMA.

Rclump ~ 0.14pc

Summary・ FFA of new born AGN jets
Discovery of ~ 1pc clumpy plasma torus
Consistent with X-ray/IR obscuration ?

・ Position flip of AGN jets
Direct evidence of AGN jet-clump interaction
NLR clouds or self-gravitating clouds