2018年7月24日
第48回 天文・天体物理若手夏の学校

ミリ波サブミリ波観測で挑む
活動銀河中心核サイエンスの最前線

泉 拓磨 (国立天文台/NAOJ Fellow)
1

自己紹介

• Takuma IZUMI (泉拓磨)• 2016 Sept. Ph.D (Univ. of Tokyo)- Prof. Kohno’s group• NAOJ Fellow@NAOJ/Hawaii observatory- 2017 Apr.~• Research interest:- SMBH feeding and feedback- cold ISM properties (w/ ALMA)- SMBH-galaxy co-evolution- early galaxy formation

2目次

1. AGNとは？
2. ミリ波サブミリ波観測の意義
3. ALMAと迎えた大学院時代
4. ポスドクになりまして その1ー迎えた高分解能時代
5. ポスドクになりまして その2ー多波長間連携
6. まとめ：生々流転

31. Active Galactic Nucleus (AGN)• 超巨大ブラックホール (SMBH) への質量降着で輝く- MBH = 106-1010 Msun•

莫大なエネルギー (L > 1012 Lsun: quasar) が、非常にコンパク
ト (< 0.1 pc) な領域から放出されている• しばしば (bi-conicalな) ジェットやアウトフローを伴う→ 母銀河にも影響を与える？（銀河進化と関係）• z = 7.54の宇宙に既に存在 (最遠方記録)

4

(NGC 4258)(memo)
NRO 45m + ultra-wide
NGC SMBHは本当に存在するのか？
4258

Acoustic-optical
Spectrometer (AOS)

5

Nakai et al. 1993, Nature, 361, 45

-1000

↓

1000

↓

•

Nakai
et al.
1992, Nature,45近傍(D=6.4Mpc) 361,
低光度AGNのNGC
4258における、H2Oメーザーの高速度成分の発見• 続く、VLBI干渉計による超高空間分解能観
測によるサイズ測定•

Enclosed mass ~ 4 × 107 Msun
→ 密度 (>4E9 Msun/pc3) が恒星では説明不可
能 → SMBH！？

Miyoshi et al. 1995, Nature, 373, 127

0.3 pcFrom <1 pc to >kpc

6

“銀河への影響”まで考える•from~100 kpcと、AGNサイエンスとして

to less than 1 pc

考慮すべき空間スケールは• 数桁に及ぶ。
	•• ミリ波サブミリ波観測を使って、>10 pcの領域でのアレコレを研究してきた。

• 本講演ではその内容を（泉の個人的な昔話？をしながRobson 1996
“Active Galactic Nuclei”
p. 334ら）概観。
Robson1996“Active Galactic Nuclei”
p. 334

2. ミリ波サブミリ波観測の意義

7

東京大 河野グループHPより

2. ミリ波サブミリ波観測の意義

8• 低温物質（特に分子ガス）は、銀河中心 < 1kpcの”ガス質量”の大半を担う→ SMBHへの降着物質の供給源であり、星形成活動の母体でもある。

• 長波長ゆえ、星間塵（ダスト）による減光を受けない。

→ ダストに埋もれた活動現象（AGN、爆発的星形成）の観測に威力を発揮• ALMAの登場により、高感度・高分解能が達成可能に。
→ <10 pc@nearby, ~kpc@high-z• というか、mm/submmはやっている人が少ない！AGNは本当に少ない！

（世界的にもレア；ある天体の研究者割合は、その天体のcosmic fractionに比例？）→ レア × レア = スーパーレア = 独壇場！ …鶏口牛後！

独創性かつ優位性の高い仕事をするのが大事（スタートアップ）

電波干渉計 …そしてALMAへ
K. Jansky (1931) @20.5 MHz→ flux densityの単位 (Jy)の人

9電波干渉計 …そしてALMAへ
Large Millimeter/submillimeter
Array (ALMA)•K.Atacama
Jansky (1931)@20.5 MHz→ flux densityの単位 (Jy)の人• チリのアタカマ砂漠（標高5000m）に設置。世界最大の電波干渉計。

• EA (incl. Japan), NA, EU, and Chile collaboration• 54 x 12m + 12 x 7m のアンテナ群（移動可能）• 最大基線長：~16 km (→ <0.1”)• 周波数範囲：84 GHz - 950 GHz

910

3. 大学院時代の研究- 星間化学＆質量降着 -ALMA-native?

11+ ALMAの科学運用 Phase
2011年

2012年

2017年

2018年

Cycle 0

Cycle 1

Cycle 5

Cycle 6…
+ 泉の研究史2012年

2016年秋

大学院入学

大学院修了

〜ポスドク

ほぼほぼALMAの登場と共に研究を開始。
物心ついたときからALMAがある世代 = ALMA native！
それは空間分解能の向上の歴史でもある → 研究内容に反映

初論文：高密度ガスを使った熱源診断の提唱
ALMA Observations of the Active Nucleus of NGC 1097

NGC 1097 150 pc
HCN(4-3)

12

100-9

• サブミリ波帯の高密度分子ガス放射を~100
pc分解能で観測（低光度AGNでは初めて）- 指導教官にもらったdata & idea

Integrated intensity maps in the central 800 ! 800 (560 pc ! 560 pc) region of NGC 1097, derived by calculating the zeroth moment of the ALMA
bes. The cross indicates the peak position of the 860 !m continuum. Both maps are shown on the same intensity scale so as to allow easyson. (a) Integrated intensity map of the HCN (J = 4–3) emission over a velocity range from VLSR = 1160 to 1450 km s"1 . The value at thepeak position is 7.5 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 beam size is 1:00 50 ! 1:00 20= "72:ı 4. The contour levels are 5, 10, 20, ### , 70 ", where 1 " is 0.11 Jy beam"1 km s"1 or 0.60 K km s"1 . (b) Integrated intensity map of the(J = 4–3) emission over a velocity range from VLSR = 1215 to 1440 km s"1 . The value at the 860 !m peak position is 3.7 Jy beam"1 km s"1 ,source size is estimated to be 1:00 31 ! 1:00 06 with PA = "14:ı 7. The beam size is 1:00 49 ! 1:00 18 with PA = "71:ı 3. The contour levels are 5, 10,
0 ", where 1 " is 0.11 Jy beam"1 km s"1 or 0.60 K km s"1 .

Downloaded from http://pasj.oxfordjournals.org/ at Kokusai Hoken Keikakugaku (UNIV• θ ~100 pcなので詳細な構造は分からず…

初論文：高密度ガスを使った熱源診断の提唱
T. Izumi et al.

[V

Izumi et al. 2013, PASJ, 65, 100

AGN

HCN(4-3)/CS(7-6)

13

星形成銀河

(一部の)AGNで高い輝線強度比→ submm帯の熱源診断法！？

HCN(4-3)/HCO+(4-3)

初論文：高密度ガスを使った熱源診断の提唱
T. Izumi et al.

[V

Izumi et al. 2013, PASJ, 65, 100

AGN

HCN(4-3)/CS(7-6)

13

星形成銀河

AGN周辺環境におけるHCN分子の大量合成(一部の)AGNで高い輝線強度比→ submm帯の熱源診断法！？
→ 極限環境での星間化学

泉 他、2013年プレスリリース（©東京大）HCN(4-3)/HCO+(4-3)

初論文：高密度ガスを使った熱源診断の提唱

14• 星間化学の知見を活かして天体物理に貢献する（熱源診断etc）ということから、案外このネタは受けた（国際的にも）。

• 以降、パラメータスペースを拡げたりサンプルを増やしたりと、その後~2-3年（今も）このネタを追求。
- Izumi et al., 2015, 2016a, 2018d in prep.

• 解析手法（データの整約、モデル技法等）に習熟 + 星間化学の知識を深めた → いざというときに頼れる”地面”を早く作る！

良き指導教官に出会う。学生の特権を活かし、色々教えてもらう！
とにかくそれなりの成果の出る、上手いスタートアップを切る。
（その後の研究人生へのモチベーションが全然違う！...と思う）

Izumi et al. 2016a, ApJ, 818, 42
初論文：高密度ガスを使った熱源診断の提唱

14• 星間化学の知見を活かして天体物理に貢献する（熱源診断etc）ということから、案外このネタは受けた（国際的にも）。

• 以降、パラメータスペースを拡げたりサンプルを増やしたりと、その後~2-3年（今も）このネタを追求。 AGN-dominated- Izumi et al., 2015, 2016a, 2018d in prep.

SB-dominated+ 星間化学の知識を深• 解析手法（データの整約、モデル技法等）に習熟
めた → いざというときに頼れる”地面”を早く作る！

良き指導教官に出会う。学生の特権を活かし、色々教えてもらう！
とにかくそれなりの成果の出る、上手いスタートアップを切る。
Filled: High-res.
Empty: Low-res.

（その後の研究人生へのモチベーションが全然違う！...と思う）

Childhood’s end…

• 自分で研究テーマを設定するのが研究の第一歩（にして、おそらく最も重要な項目）。

• 自分から新しい課題に挑戦した
い！と思うのは非常に健全。

• 幼年期が終わり、独り立ちへの準備をする大事な期間。

• （ただし、一人で勝手に暴走するのは避けましょう！）

15

与えられたテーマは面白い。
だけど他のこともやってみたい！

AGN質量降着の研究（2015~）16

150 pcCircumnuclear
disk = CND

from ~100合体銀河
kpc
to less than 1 pc
Host →• ~100 pc• 100 pc →~1 pc

sub-pc

衝突合体

孤立系
棒状構造

	
?

etc
?

降着円盤

銀河中心の~100pc領域の降着過程
Robson 1996
“Active Galactic Nuclei”
p. 334はろくに研究されていない！
Robson1996“Active
Galactic Nuclei”→ ALMAならいけるやろ!
p. 334

M. Krips
al.: HCN(1–0)
emission in NGC6951
has been resolved out at
ouret higher
resolution,and that most of
HCN in NGC 3227 does originate from the central compact17sour
AGN質量降着の研究（2015~）
The compact nature of the HCN emission is in stark contrast toCO(2–1)emission,
as
shown
in
Fig.
5.
Indeed,theCOemissio150
pc
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
L64

F. Combes et al.: CO in NGC 1566

100 pcIzumi et al. 2013, PASJ, 65, 100) 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., García
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 obtain−1
00 from
003σ
contours run
to 23σ(right:7σ)
in stepsof 1σ=NGC0.06 Jybeam−1km s−1 (right:
1σpc= 0.10 Jythe
beam
km
85
maps inBlackthe central
8
!
8
(560
pc
!
560
pc)
regionof
1097,
derivedbycalculating
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◦ )catestheetpeak
positionof (PA
the=860◦!m continuum. Both maps are shown on the same intensity sca
ofApJ,
the galaxy
130Combes). The black(right)represents
velocity
gradients(PA = (
Izumi major
al. axis
2015,
811, 39et al.line
2014,
A&A,
565, 97 the most extreme
Sani et central
al. 2012,
MNRAS,
424, 1963
h
m
s
◦
′
′′
αJ2000HCN= 20 37
andemission
δJ2000 = 66 over
06 20.09
which is slightly
the=
phase
centrethe obser
1160
toof1450km
intensityposition
map isofatthe(J 14.123= 4–3)
a 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 beam

空間スケール: ~100 pc (*依然として分解はされていない)
"1
"1
"1

tour levels
are 5, 10,
20, ### , 70", where
1 " Arpis 0.11beam
s 1. HCN(1–0)
or 0.60Kline
kms . (b)obtained
Integratecomposite(AGN+SB)
galaxies(e.g.,
220,Jy M82, kmTableparameters,
at t
1
n Fig. 4a) on the dust continuum emission at 349 GHz (colorin spatially
Jy beamintegrated) by fitting a Gaussian pro"1 scalenot

AGN質量降着の研究（2015~）

18

※150
Seyfertpc galaxies
CND
Entire galaxy• 降着率とCND-scaleガスの間に正の相関。

• 銀河スケールのガスでは相関は弱い（ほぼ無相関）。

• CND = 降着物質の直接的なX-ray →

供給源

• ということで、CNDスケー
Izumi et al. 2016c
ApJ, 827, 81

HCN(1-0) →ルで降着モデルを色々試すのは本質的に重要と主張できた。

on a logarithmic scale. Blue circles and black squares indicate that the HCN(1 − 0)

降着モデルの検証 (case study!)

19

Kawakatu & Wada 2008,
ApJ, 681, 73

150 pcGas accretion rate in a turbulent nuclear diskdࠉ
ln:(r )Maccr ) 2SQ t 6g (r )Ṁ
BH ((r)d ln rQ t :viscous parameterQ t DSNvt h, ࠉ: v r

SFE::angular velocity

6g

2hUg :surface density

3/2~100 pc
Gas surface density= Mdense/area
BH mass

3
§
·
r
3
1
in

Macc
(
r
)
3
SD
K
E
C
6
(
r
)
0.13
D
r
C
6
M
Ṁ
(r)
¸
BH in
SN
SN * g in ¨
SN,1 in,3 *,7 g,1
BH,7 [ M~yr]© GM BH ¹LªºCND with the gas mass of Mdense fuels the nuclear events at the rate of Ṁacc as the form of black hole mass accretion (ṀBH ) or nuclear wind (Ṁwind ). We sthese two events into Ṁnuclear .

降着モデルの検証 (case study!)

20= SMBH降着 + 円盤風

150 pc

10

%
0
0
1

%
0
0

Izumi et al. 2016c
ApJ, 827, 81= CNDから落ちる質量

CND with the gas mass of Mdense fuels the nuclear events at the rate of Ṁacc as the form of black hole mass accretion (ṀBH ) or nuclear wind (Ṁwind ). We sthese two events into Ṁnuclear .

降着モデルの検証 (case study!)

20= SMBH降着 + 円盤風

150 pc

10

%
0
0
1

%
0
0

Izumi et al. 2016c
ApJ, 827, 81

泉 他、2016年8月プレスリリース画像（©東京大）= CNDから落ちる質量

CND with the gas mass of Mdense fuels the nuclear events at the rate of Ṁacc as the form of black hole mass accretion (ṀBH ) or nuclear wind (Ṁwind ). We sthese two events into Ṁnuclear .

降着モデルの検証 (case study!)

20

150 pc• “mm/submmでAGN”という主軸は維持しつつ、= SMBH降着 + 円盤風

これまでと違う毛色のテーマをやってみた。

or 新しい論文を書く、という%• 新しい研究をする
00
ことくらいでしか、おそらく別テーマの勉強を
10%
0
じっくりすることはない。
10→ 見聞を広める良い機会• “観測と理論の協働”の重要性・威力を痛感→ 今に至る研究スタイルの土壌となった

Izumi et al. 2016c
ApJ, 827, 81

泉 他、2016年8月プレスリリース画像（©東京大）= CNDから落ちる質量

22

4. ポスドクになりまして その1- 迎えた高分解能時代 -ALMAの本気

23• 高分解能観測の幕開けは、
やはりHL Tau（2014冬; 研究会にて激震が走る）• PDになった頃 (2017年) には、ALMAの高分解能観測
は”当たり前”に行われるような時期だった。
→ AGN環境でも、高分解能観測が始まりつつあった。

• AGN＆分子ガス＆高分解能とくれば、狙うはAGNトー©ALMA (ESO/NAOJ/NRAO)

ラスの直接撮像！

SMBH遮蔽現象: AGNトーラス

24

統一モデル
Type-1

Type-2(e.g., Antonucci 1993, ARA&A, 31, 473)

Type-1HαType-2

Polarlized
Urry & Padovani 1995, PASP, 107, 803

λ (Å)

SMBH遮蔽現象: AGNトーラス

24

統一モデル
Type-1

Type-2(e.g., Antonucci 1993, ARA&A, 31, 473)

Type-1HαType-2

Polarlized
Urry & Padovani 1995, PASP, 107, 803

λ (Å)

ALMAで挑むトーラスサイエンス• 直接撮像- 本当に分子・ダストのコンパクトな構造が存在するか？
→ 高空間分解能 = ALMA

• 力学状態の測定- 回転が支配的？速度分散が支配的？
- 幾何構造の指標になる (σ/Vrot ~ H/R; 静水圧平衡)→ 高速度分解能 = ALMA

• トーラスの物理的起源の探査- いったいどうやって分厚い構造を宇宙で作るのか？
- 構造の各種物理パラメータへの依存性の調査

25

COトーラス
in
NGC
1068
(L
Bol ~ 2e45 erg/s)
hysical Journal Letters, 823:L12 (6pp), 2016 May 20
The Astrophysical Journal Letters, 823:L12 (6pp), 2016 May 20

26

García-Burillo et al.

NGC 1068
Luminous Type-2 AGN
CO(6-5)(colour)

Garcia-Burillo et al. 2016,
ApJL, 823, L12

Figure 3. Overlay of the continuum emission contours of Figure 1 on theCO(6–5) emission (color scale) from the AGN torus. Units are in
Jy km s−1beam−1.

• COガスが明確に中心集中している (サイズ ~ 7 pc)

Furthermore, ALMA detects the CO emission from a- Mgas ~ 1e5 Msun; σ/Vrot > 1 (幾何学的に厚い)
トーラス
spatially resolved→
lopsided
disk located at the AGN, as

illustrated in Figure 3. The size (diameter ; 10 ± 1 pc,
minor-to-major axis ratio ;0.5±0.1) and orientation(PAmajor = 112
20 ) of the CO disk, hereafter referred toas the COFigure
torus, are3.close
to thoseofderived
above for theemissi
dust
Overlay
the continuum
torus. The orientation of the CO torus is virtually identical to• (Memo: σ/V ⇄ scale-height to radius = H/R; 静水圧平衡)rot

COトーラス in NGC 1097? (LBol ~ 8e41 erg/s) 27
Izumi et al. 2017,
ApJL, 845, L5

12CO(3-2)• NGC 1068より~1000倍暗い低
光度AGN (Low-luminosity AGN)

• AGNの位置にCO源がない！！
•
10 pc

AGN

Mgas ~ a few × 104 Msun(~1/2 - 1/3 of NGC 1068)• AGN自身の放射にしろ、インフ

ローにしろ、星形成活動にしろ、とにかく”熱源”はNGC 1068より弱い。

• 予測：NGC 1097では、NGC
1068よりも幾何学的に薄いトーラスがあるのだろう。

. Intensity-weighted (a) mean velocity and (b) velocity dispersion maps of the CO(3–2) emission in th
C 1097. The stars mark the AGN location. The systemic velocity is 1254 km s−1 (thick line). Thin cont28
400 km s−1 in steps of 20 km s−1 for (a), and 10 to 40 km s−1 in steps of 10 km s−1 for (b), respectively

有為転変は世の習い？ — AGNトーラスの消失
Izumi et al. 2017, ApJL, 845, L5

(b)
(b)

Rotation Vrot
Dispersion σ

σ/Vσ/Vrot~ H/R
rot ~H/R

Velocity (km/s)(a)

NGC 1068(Luminous)

NGC 1097
CO(3-2)(LLAGN)• σ/V = 0.5 in NGC 1097 (LLAGN) vs. >1 in NGC 1068•
2 ×•10 AGNトーラスは決して定常的ではなく、動的に構造を変えるのだろう。
M , which indicates the importance ofcontribute to squash the thick torus in t
resolution to measure M .
(e.g., Vollmer et al. 2008; Wada et al. 2009;rot(a) Radial profiles of the rotation velocity (Vrot ; squares) and the velocity dispersion (σ; circles) of the cated from our tilted-ring modelings to the CO(3–2) velocity field. (b) Radial profiles of the σ/Vrot ratio
確かにNGC 1097の方が薄い…！
emission line (squares) and NIR H2 emission (circles; divided by three).
8⊙→ 多くの理論予測と整合する。
articularlyinteresting that the σ/Vrot ratio
1097 at the central r < 20 pc (∼ 0.5) is
BH

Note that, very recently, Espada et al. (2017a cold molecular gas deficiency at the hear

トーラスパラダイムへの挑戦
12μm/VLTIU
U2-U 1-U
3 2

N
6

82
A
4
3,
6
5
A
&
ec
Fcor [Jy]

v [m]

E0-G0

0

D0

-B

2
H0-G0

ng
a

4
U3-U

A

4)
1
0
(2

lar

50

8

elo

E

-U3

0
10

Po

U1

U2-U4

tio

100

n!

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A&A 563, A82 (2014)

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and flux levels remain unchanged.llWith
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h edmask. re havet ina shapetions to the values published in 2007. Due
to improvedpsimilar
to
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spectrum.
e
e
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d
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n
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d t calibrationp e a the isk
d tof theli f e n e e
tra is reduced significantly. The wavelength
ne rf i u x b d• 最近のVLTI観測で、Polar方向に伸びたダスト放射が確認された。古典的なトーラスの描像に反する構造。

• 単なるインフローや星形成活動では、この構造を再現するのは難し
いのでは…？？トーラスの物理的起源とはいったい…？

Multi-phase Dynamic Torus model

30

Wada 2012, ApJ, 758, 66

Multi-phase Dynamic Torus model

30

IzumiWadaet al. 2012,2018c,ApJ,
submitted
758, 66

“Fountain”でダスト分布は再現可能
IR emission from central obscuring structures

31

3883

12μm
0.1μm

12μm

30 pc

500μm

Schartmann
et correspondal. 2014,toFigure 3. Wavelength dependence of model ER20 at a time 2.0 Myr after the central radiation has been switched on. The
various columns
inclination angles of 0◦ , 30◦ , 60◦ and 90◦ (from left to right). The rows correspond to wavelengths of 0.1 (upper row), 12 (middlerow) and
5003878µm (lower
MNRAS,
445,row). The dynamic range is chosen to scale from the maximum intensity of dust emission (excluding the central source) down to the 10−6 th fraction of it.
Labels are given in parsec.

i = 0°

30°

60°

90°

• Successfully reproduced the MIR polar elongation!

Our study(1): ガス分布の理論予測

l Journal Letters, 828:L19 (7pp), 2016 September 10

32

Wada, Schartmann, & Meijerink

The Astrophysical Journal, 852:88 (11pp), 2018 January 10

Wada, Fukushige, TI, et al. 2018, ApJ, 852, 88

CO(1-0)• Target: The Circinus galaxy• Hydrodynamic simulation +Chemistry + radiative transfer

Wada et al. 2016,
ApJL, 828, L19• ALMA観測と直接比較できる量を用意

Our study(1): ガス分布の理論予測

l Journal Letters, 828:L19 (7pp), 2016 September 10

32

Wada, Schartmann, & Meijerink

The Astrophysical Journal, 852:88 (11pp), 2018 January 10

Wada, Fukushige,
TI,et
etal.
al.2018c,
2018, ApJ,
852, 88
Izumi
submitted

CO(1-0)• Target: The Circinus galaxy• Hydrodynamic simulation +Chemistry + radiative transfer

Wada et al. 2016,
ApJL, 828, L19• ALMA観測と直接比較できる量を用意33

Out study(2):トーラス領域における多相星間物質の力学探査• 原子ガス vs 分子ガス

→ 原子ガストーラスの方がより分厚い？

• 厚みの起源はAGN-driven fountain？

新しいパラメータスペースを求めて

34

Izumi et al. 2018c, submitted

12CO(3-2)[CI](1-0)

CND
+
Sp

+

ira

la
rm

• “多相ガス間の力学状態の違い”が、fountain modelの重要な予測• いつものCOだけでなく、炭素原子ガス CI も観測→ 新しいパラメータスペースの開拓18

CI vs CO: Multi-phase Torus Dynamics

35

T. Izumi et al.

Izumi et al. 2018c, submitted(a)

Velocity (km/s)

160 Blue = CO(3-2)
Red = [CI](1-0)

12080Dispersion

40
0

(b)

σ/Vrot (~H/R)

Rotation

0

20

0.5

40

60

Radius (pc)

80 100•0.4
0.3• r < 10 pcでは原子円盤の方が厚い!

0.2

Table 6. Results of the three-component Gaussian fit to[C I](1–0) spectrum→ 多相・多層幾何構造

0.1
0

0

Figure 18.
Line profile of the [C I](1–0) measure
the AGN position (with the single 0′′ .71 × 0′′ .66 beam
the Circinus galaxy. Three-component Gaussian fit waseach component is indicated by the black-da
r > 20formed:
pcでは原子円盤も分子円盤も幾何
lines, and the total model is shown by the red-solid line
spectively. The derived line properties are summarize
学的に薄い
Table 6. (c.f., low-SFR in Circinus)

20

40

60

Radius (pc)

80

CentralPeak(mJy beam−1 )1107.9 ± 1.6

Centroid(km s−1 )453.7 ± 5.6

FWHM(km s−1
97.7 ± 0

T. Izumi et al.
幾何学的厚みの起源は何か？

Flux density (mJy/beam)

1200
1000

36

Nuclear-scale (15 pc) spectrum(b)[CI](1-0)
FWHM ~ 320
km/s[CI](1-0)

FWHM ~ 240 km/s

800
600
400
200

CO(3-2)0
Figure250 300 350 400 450 500 550 600
650 18.

Line profile of the [C I](1–0) measured at
the AGN 中心核近傍の[CI](1-0)スペクトルは、
position (with the single 0′′ .71 × 0′′ .66 beam) of
Velocity (km/s)
the Circinus galaxy. Three-component Gaussian fit was pergure 11. Line profiles of the [C I](1–0) and theCO(3–2)CO(3-2)に比べて線幅が広い。
formed:each
component is indicated by the black-dashed′′′′asured at (a) the inner 10 × 10 box and (b) the AGN
lines, and the total model is shown by the red-solid line, re′′′′ation (with the single 0 .71 × 0 .66 beam) of the Circinus
spectively. The derived line properties are summarized in
Multi-Gaussianフィットで再現可能
axy. The uv-range and the beam size of the CO(3–2) data
Table 6.
matched to those of the [C I](1–0) data. The multiple••
n-line profile in (a) is due to the spiral arms. Results of• アウトフローのようなcoherent motion
gle Gaussian fits to the CO(3–2) and [C ](1–0) spectraI

the AGN position (indicated by the dashed line
and6.
dotTable
Results of the three-component
Gaussian fit to theを強く示唆fountainmodelの出番！？
hed line, respectively) are summarized in Table
5.
[C I](1–0)
spectrumモデルとの”定量”比較37

CO(3-2): TB[CI](1-0): TB(inclination = 75°)
Izumi et al. 2018c, submitted• M , Eddington ratio, CND-scale M : Circinus銀河に合わせた値• Hydrodynamic simulation + XDR chemistry (Wada+16) + rad. transfer• CO(3-2) → 中心面 (i = 75°)
• [CI](1-0) → 中心面 + アウトフローで吹き上げられた成分
BHgas

モデルとの”定量”比較

38

t al.
Izumi et al. 2018c, submitted[CI](1-0)••

igure 18.
Line profile of the [C I](1–0) measured at[CI](1-0)で観測された特異なline profileは、確かにモデルでも再現された。
he AGN position (with the single 0′′ .71 × 0′′ .66 beam) of
he Circinus galaxy. Three-component Gaussian fit was perALMA観測結果と、（それに向けて準備した）simulation結果が整合
rmed:
each component is indicated by the black-dashednes, and the total model is shown by the red-solid line, re→ fountain schemeで、30年来にわたる問題であるAGNトーラスの起源は説
pectively. The derived line properties are summarized inable 明できそう！
6.

モデルとの”定量”比較

38

t al.
Izumi et al. 2018c, submitted• いよいよ高分解能観測時代が本格化[CI](1-0)• …だけでなく、ALMAは多相ガスの観測も可能なことにも注目（装置の性能・各波長帯の輝線の特性等々はよく勉強しておくこと）• 理論と観測を意味のある形で付き合わせることが可能な時代になってきた。

•

igure 18.
Line profileof the [C I](1–0) measured at
理論は理論、観測は観測、はダメ。互いに手を取[CI](1-0)で観測された特異なline profileは、確かにモデルでも再現された。
he AGN position (with the single 0′′ .71 × 0′′ .66 beam) of
り合って課題に挑むべし。
he Circinus galaxy. Three-component
Gaussian fit was perALMA観測結果と、（それに向けて準備した）simulation結果が整合
rmed:
each component is indicated by the black-dashednes, and the total model is shown by the red-solid line, re→ fountain schemeで、30年来にわたる問題であるAGNトーラスの起源は説
pectively. The derived line properties are summarized inable 明できそう！
6.

•
•

39

5. ポスドクになりまして その2- 多波長間連携 -SMBH-galaxy co-evolution

40

• M

BH is tightly correlated with Mbulgeand σ* → Co-evolution• Why do they know each other despite~10 orders of magnitude diﬀerence inspatial scale…?

• Favoured scenario: Merger-induced
Kormendy & Ho 2013, ARA&A, 51, 511

starburst & AGN, and subsequent“AGN feedback” to regulate the starformation (e.g., Hopkins et al. 2008; Fabian 2012,
ARA&A, 50, 455)

• When, how, and where the relation
MBH/Mbulge ~ 1/1000-1/100

has arisen/established?

Trace (i) SMBH feeding/feedbackand (ii) galaxy growth over thecosmic time

SMBH-galaxy co-evolution

40

• M

BH is tightly correlated with Mbulgeand σ* → Co-evolution• Why do they know each other despite~10 orders of magnitude diﬀerence inspatial scale…?

• Favoured scenario: Merger-induced
Kormendy & Ho 2013, ARA&A, 51, 511

starburst & AGN, and subsequent“AGN feedback” to regulate the starformation (e.g., Hopkins et al. 2008; Fabian 2012,
ARA&A, 50, 455)

• When, how, and where the relation
MBH/Mbulge ~ 1/1000-1/100

has arisen/established?

Trace (i) SMBH feeding/feedbackand (ii) galaxy growth over thecosmic time
Hopkins et al. 2008, ApJS, 175, 356

SMBH-galaxy co-evolution

40

• M

BH is tightly correlated with Mbulgeand σ* → Co-evolution• Why do they know each other despite~10 orders of magnitude diﬀerence inspatial scale…?

• Favoured scenario: Merger-induced
Kormendy & Ho 2013, ARA&A, 51, 511

starburst & AGN, and subsequent“AGN feedback” to regulate the starformation (e.g., Hopkins et al. 2008; Fabian 2012,
ARA&A, 50, 455)

• When, how, and where the relation
MBH/Mbulge ~ 1/1000-1/100

has arisen/established?

Trace (i) SMBH feeding/feedbackand (ii) galaxy growth over thecosmic timeEnhanced merger-frequency at high-z?
The Astrophysical Journal, 836:8 (21pp), 2017 February 10[CII] obs. w/ ALMA

Trakhtenbrot et al.

42

Trakhtenbrot et al. 2017, ApJ, 836, 8• Associated SMGs in 3/6 luminous quasars at z ~ 5 (50%!!)• Strongly support “merger-induced” SMBH growth

Figure 1. Large-scale continuum emission maps derived from the new ALMA datafor the six quasar systems in our sample: the three FIR-bright sources (toprow)and the three FIR-faint sources (bottom row). In each panel, the quasar and any accompanying sub-millimeter galaxies are marked as “QSO” and “SMG,”
respectively. The gray-scale map shows the continuum emission, determined from the line-free ALMA spectral windows. Cyan and blue contours trace emission
levels at different positive and negative signiﬁcance levels, respectively, with the ﬁrst contour tracing the region where the continuum emission exceeds 2.5σ, andconsecutive contours plotted in steps of 2.5s . The ALMA beams are shown as red ellipses near the bottom-right of each panel. Red crosses mark the locations of thequasars’ optical emission (taken from the SDSS). Interacting companions, i.e., sources that have clear detections of [C II] with redshifts consistent with those of thequasars, are marked as “SMG.” The continuum source accompanying J1511 that lacks signiﬁcant [C II] emission is marked as “B.”

Early co-evolution: biased view?
alog M• /M

10b

Kormendy & Ho 2013, ARA&A, 51, 511•

z = 0.1–1.0 AGNsz = 1.0–2.0 QSOs
z = 2.0–4.0 QSOs
z = 4.0–7.0 QSOs
z ≈ 2 RGsz ≈ 2 SMGs

•

9

8

7

43

z = 0 ellipticals
MBHz =of0 classical(some)
optically-luminous
bulgespseudobulges
z >zBulge-dominated
6= 0quasars
are over-massive→ SMBH
Spiral bulgeearlier, galaxies later?
Spiral total
ObscuredBut
we ↓should care about a
Obscured

selection bias to prefer luminous(~ massive) objects

Häring & Rix 2004

9

10

11

12

log M*,bulge /M※ Mdyn~Mstar is usually assumed in quasars

c

2

9

10

11

log M*,bulge/M

12

Early co-evolution: likely a biased one

44

Probing-down low luminosity objects→ Depict a less-biased mass distribution!

Subaru/Hyper Suprime-Cam

ALMA3.3 Survey fields

Hyper Suprime-Cam Survey of quasars

45

HSC-D

R.A.

HSC-W

PI: Miyazaki (NAOJ)
Co-PI: Iwata (NAOJ)
168 participants from 36
institutes on the initial
proposal

Subaru strategic program (SSP) with HSC
HSC-D/UDDEC•

Galactic Extinction E(B-V)

First 1000deg2 class survey with
an 8m class telescope- 300 nights: Feb. 2014 - Jan. 2019
- g,r,i,z,y bands
3.3.- Survey~2 magfields
deeper than previous
surveys
Table 3.3 and Figure 3.3 summarize the target fields for the HSC-Wide, Deep, and Ultradeep(e.g., rAB <27.1 mag in the Deeplayers. We employ
the following requirements for the survey field selection:
27 deg2)

Figure 3.3.: The location of the HSC-Wide, Deep, and Ultradeep fields on the sky in equatorial coordinates.
From HSC-SSP proposal
Footprints of various spectroscopic surveys and surveys in other wavelengths are also indicated. Color contours show
the Galactic extinction map (Schlegel et al. 1998). The gray-shaded regions show regions that are accessible fromthe ACT/ACTPol with reasonably good observational conditions.

•• The HSC footprints should overlap the SDSS/BOSS footprint, because we use the SDSS for
Will
discovermany less-luminous
photometricand astrometriccalibration of the HSC data (Chapter 4). The BOSS data will
provide a huge spectroscopic sample of galaxies up to z ∼ 0.7, which will be used to calibrate
quasars
at z > 6 → less-biased picture
photometric redshifts and the cluster-finding algorithm, and can be used for cosmologicalof analyses.
early SMBH evolution
45• The fields should be well distributed over a widerange
RA, suchproposalthat fields are reachable
from
theof
HSC-SSPSHELLQs

Subaru High-z Exploration of Low-Luminosity Quasars

Members
Y. Matsuoka1 (PI)
M. Akiyama2, N. Asami3, S. Foucaud, T. Goto4, Y. Harikane5, H. Ikeda1, M. Imanishi1, K. Iwasawa6, T.
Izumi5, N. Kashikawa1 T. Kawaguchi7, S. Kikuta1, K. Kohno5, C.-H. Lee1, R. H. Lupton9, T. Minezaki5, T.
Morokuma5, T. Nagao8, M. Niida8, M. Oguri5, Y. Ono5, M. Onoue1, M. Ouchi5, P. Price9, H. Sameshima10,
A. Schulze5, T. Shibuya5, H. Shirakata11, J. D. Silverman5, M. A. Strauss9, M. Tanaka1, J. Tang12, Y. Toba8
1NAOJ, 2Tohoku, 3JPSE, 4Tsinghua, 5Tokyo, 6Barcelona, 7Sapporo Medical, 8Ehime, 9Princeton, 10Kyoto Sangyo, 11Hokkaido,
12ASIAAHSC-project (#123):
Submm follow-up observations toward
HSC-detected high-z quasars with ALMA
Izumi et al. 2018a, PASJ, 70, 36
Based on: ALMA Cycle 4 (2016.1.01423.S)

What happens to the early, but representative quasar host galaxies?
→ SFR, M
What is the bias-corrected co-evolutionary relationship at z ~ 6?

Results: Spatial distribution

Color = [CII]48
Contour = FIR continuum
Izumi et al. 2018a, PASJ, 70, 36

J0859

θ = 0.64” x 0.47”

J1152

θ = 0.52” x 0.47”

J2216

θ = 0.54” x 0.43”

J1202

θ = 0.79” x 0.71”

Band 6 spectrum: J2216-0016
Izumi et al. 2018a, PASJ, 70, 36

49

g

r

z

y

i

HSC image~0.18 mJy @dV = 50 km/s
(on-source time ~ 1.7h)[CII]

Early co-evolution in z ~6 quasars
50

Izumi et al. 2018a, PASJ, 70, 36

Luminous

Low-luminosity

Early co-evolution in z ~6 quasars
51

Izumi et al. 2018a, PASJ, 70, 36

Group-2
Group-1

Early co-evolution in z ~6 quasars
52

Group-1

NGC 1277• Roughly follow the local relation→ Standard merger-induced
SMBH-galaxy evolution model may
explain (although many of themmust live in quite massive halos)• Quite hard to reproduce with theν2GC scheme; another paths??

• Will appear as over-massive MBH
at z ~ 0? (like NGC 1277)• Or get closer to the local relation
via dry mergers?

~60% Mbulge
SMBH mass (Msun)

Group-2~10 kpc

van den Bosch et al. 2012,
Nature, 491, 729

Bulge Luminosity (LK,sun)

Early co-evolution in z ~6 quasars
52

Group-1

NGC 1277• Roughly follow the local relation~10 kpc→ Standard merger-induced
SMBH-galaxy evolution model may
explain (although many of them
多波長連携が威力を発揮し、銀河形成
must live in quite massive halos)

Panchromaticな研究を！

• Quite hard to reproduce with theν2GC scheme; another paths??

• Will appear as over-massive MBH
at z ~ 0? (like NGC 1277)• Or get closer to the local relation
via dry mergers?

SMBH mass (Msun)

Group-2に物申す時代！ぜひ同士を集めて~60% Mbulge

van den Bosch et al. 2012,
Nature, 491, 729

Bulge Luminosity (LK,sun)まとめ：生々流転• 大学院時代から、”ミリ波サブミリ波でAGN”という内容で、色々な研究をしてきた。

- この人と言えばこれ！という武器を持つと強い！

- その武器を手に、様々なテーマに挑戦すると良い。

• 院生時代に、何かこれは！という軸足を持っておく（で、さっさと論文にする）。

- 良いスタートアップを切るのは（精神衛生・実務両面で）大事。

• 幼年期の終わりは研究者として成長してきた証拠！
- どんどん研究の幅を広げよう。

• 時代は理論と観測の協働、多波長連携！
• アーカイブデータを含め、最新の研究をすぐに始められる環境が整ってきている。

- いろんな方と積極的に話して、どんどん新しいことに挑戦しよう！

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