学問の流れ
Suzaku から Astro-Hへ

京都大学物理第二教室・宇宙線研究室

鶴20120313_KH_FY2011_GakumonNoNagare_v9.key

剛2006.03 教室発表会
宇宙線研究室X線グループ2005^7ěęĕÍpĖĤm,!

•ĕORģŐŉĿŀŞĺţōšŖŠ
•āĻŏŠľť&ÒÇ次期X線衛星Astro-H (2014~)

京大は
大面積X線
CCDを担当・全長１４m, 重2.4t (最大級)・初の超高分解能分光観測
・初の硬X線撮像分光観測・過去最高の広帯域観測目的：
ブラックホールの周辺や超新星爆発など高エネルギーの現象に満ちた極限宇宙の探査・高温プ
ラズマに満たされた銀河団の観測を行い、宇宙の構造やその進化を探ること。

世界に期待されいる「日本主導」の計画

X線天文：世界との競争
軽量 小型 安い
（予算 人 不足）
6機
5〜6年/1機

実験の本質：現実に持てる装置を最大限活かすこと
トップになるには：誰もが持てない性能の観測装置を持つ宇宙物理として最も重要な性能とは(1) 空間分解能

アメリカ(2) エネルギー分解能

日本＋
高分光性能の検出器

6Great History of
X-ray Spectroscopy

Energy Resolution (eV)

Better 0.1
1

Suzaku ASTRO-H
XMM
Chandra10
100

Uhuru Tenma
OSO-8
HEAO-1

x50

ASCA

1000
10000
1960

1970

1980

1990

2000

Year

2010

2020

2030

ある有名な

ぎんがＸ線天体の(1987年)

1996PASJ...48..249K

スペクトル

あすか

0.1

すざく
(2005年)

0.01

Counts s−1 keV−1

1(1993年)

1

2

5
Energy (keV)

10搭載する観測装置
焦点距離
4.5m

XRT
=X線望遠鏡すざく

XIS=X線CCDカメラ

XRS=マイクロカロリメータ
HXD=硬X線検出器

「あすか」CCD：革命的な性能向上
1年で最高性能が出せなくなった

counts/channel「すざく」Ｘ線CCDカメラ(XIS)

100

60
40

Tomida, TT+97

放射線損傷による電荷トラップ

4100

counts/channel

1997PASJ...49..405T
1997PASJ...49..405T

80

20

劣化の原因を探る 物理教室タンデム
電荷転送の方向劣化前

5
6
X-ray Energy (keV)

7

劣化後

80
60
40
20
4

人工電荷

すざくで電荷注入法を実現【世界初】Uchiyama,TT+09, Ozawa,TT+09, Nakasjima, TT+09 etc

7回復

counts/channel

60

5
6
X-ray Energy (keV)

5年経過した現在も，打ち上げ時と40
同じ世界最高の性能を発揮
20もし無かったら，分解能は４倍に劣化
Yamaguchi
Nobukawa
Uchiyama+09 Ozawa+09 Nakajima+09
4(ΔE = 135eVから500eVに)

SawadaNakashima

5
6
X-ray Energy (keV)

7

HXD PIN、GSO の 4 種類の検出器により、過去最高性能のＸ線CCDカメラ
ギーバンドで観測することができる。
XIS

s

0.2 keV から 600 keV の 3 桁以上のエネル

XMM

Chandra

XIS
0.5
1
2
5
10
赤：「すざく」X-ray Energy (keV)
Comparison of Suzaku 図 3: 「すざく」搭載の X 線 CCD カメラ

黒：チャンドラ(all 4 sensors) with
Chandra/ACIS (S3)
過去最高の分光能力(XIS-FI と BI)過去最高ののバックグラウンドレベル
を、他の X 線天文衛星に搭載されている

低バックグラウンド性能

CCD のそれと比べたもの。「すざく」XIS

2005.7.10 12:30 (JST)ISAS/JAXA

すざく国際会議

(京都)

「The	
  Extreme	
  Universe	
  in	
  the	
  Suzaku	
  Era」	
  2006年12月4日～8日開催	
  at	
  京都テルサ(http://www-cr.scphys.kyoto-u.ac.jp/conference/suzaku2006/)

参加者398名	
  （国内：215、国外：152、オンサイト：31）

銀河と銀河の間に存在する高温プラズマの起源は？
約3万

約

1万

2千

光

年

8千光
年

約

3千

光

年

・若い銀河が高温プラズマを放出する
・宇宙初期に銀河が激しく活動
TT+90, TT+97, TT+07
銀河間空間に高温プラズマを放出

Ozawa+07

思わぬ発見：若い銀河の中質量ブラックホール
TT+97, Matsumoto, TT99
Matsumoto, TT+01

重力崩壊型超新星
恒星質量BH
大規模な星生成
大量に誕生
星団中心
合体で誕生
中質量BH

Matsumoto+01

銀河中心
合体で誕生
？？？
銀河の超巨大BH

恒星質量BHや星の合体

第１世代の星原始BH

Seed BH = 中質量BH

X線画像
銀河団プラズマ

中質量BH

・超新星爆発＝ 核エネルギー 宇宙での銀河の爆発・ブラックホール ＝ 重力エネルギー 役割
超新星爆発

暖かいプラズマ

銀河と超巨大BH天の川銀河中心領域
500光年

銀河円盤を横から見ている

1deg

銀河面

超巨大BH 射手座A*
最近傍の巨大ブラックホール
最も確実なブラックホール物理学
高いエネルギー密度 × 物質密度
極限天体の探査研究

0.1

中性 鉄
ヘリウム状（電子2個）鉄

1deg

0.01

−1

Counts s keV−1

1

天の川銀河中心領域

水素状（電子1個）鉄
125Energy (keV)

輝線だけでイメージング【成功】10

6.7keV (Continuum subtracted)

Sgr A*
100ly

6.4keV (Continuum subtracted)

Sgr A*
100ly

イオン化したFe輝線 = プラズマ
• 真に広がったプラズマ–トータルエネルギー (50pc x 30pc): 〜10^52 ergs
– 銀河面からの脱出速度 = プラズマの音速 ~1500 km/s
→ 5x10^40 ergs/s■ Sgr A*の10^7倍，超新星爆発レートの100倍• 暗くて分解できない点源– 白色矮星と恒星の連星 (激変星: CV) が候補天体(Savanov et al. 2006)

GlobalDistribution
of Fe ofKαFeLines
in theinGalactic
CenterRegionGlobalDistribution
Kα Lines
the Galactic
CenterRegion(b) (b) vs 恒星の分布
イオン化した鉄の分布
This workThis work
Koyama+07
Koyama+07
Yamauchi+09
Yamauchi+09

x4 〜 x 10 (at b*=0.0)

6.7keV

10-6

10-7

10-5

-8

-7

-8

Nuclear10-5
stellarcluster
10-6(d)Nuclear Galactic Galactic 10-5This workThis work
bulge
disk
stellar Koyama+07
Koyama+07
Yamauchi+09
disk Yamauchi+09

Nuclear bulge(at l =-0.114)
*

10-6

10-7

10-8

0.1
1
0.1
1
*
Distance from
Sgr from
A* along
thelatitudeDistance
Sgr A
along
the|blatitude|b*| (degree)*| (degree)(d)Observed photons cm-s s-1 arcmin-2-6

Observed photons cm-s s-1 arcmin-2

-5

10-7

10-8

10-8
0.01
0.1
1
10
0.01
0.1
1
10
*
Distance from
Sgr from
A* alongthelongitude|l*| (degree)
Distance
Sgr A
along
the longitude|l*| (degree)

)

10-6

10-5
Observed photons cm-s s-1 arcmin-2-7

Observed photons cm-s s-1 arcmin-2

-6

10-5

10-6

10-5
Observed photons cm-s s-1 arcmin-2-5

Observed photons cm-s s-1 arcmin-2

a)

10-6

6.7keV Lines Excess at GC
10-7

10-7

10-7

Truly diffuse plasma
10-8

10-8

10-8

Uchiyama+11

Suzaku/XIS 0.5 - 2.0 keV image

Sgr A*
Galactic Latitude (degree)

0.0
Jet ?

銀河面

-0.5
-1.0
-1.5

南北にのびる
360光年

巨大プラズマ

-2.0
1.0

0.0

359.0

Galactic Longitude (degree)
Nakashima+12358.0

中性鉄輝線 = 高エネルギー粒子が冷たい分子雲を照射
高エネ粒子とは何？
M 0.66 G 0.570

15pc

時間変動の発見•Decay	  :me	  〜	
  10yrs•Clump	
  Size	  〜	
  10lys•Not	
  integrated	
  point	  sources•Electrons	
  with	
  10-­‐100	
  keV	
  can’t	  travel.	
  •X-­‐ray	  reﬂec:on	
  can	
  explain	
  the	
  :me	
  valiability.

Inui+08

Nobukawa+10

中性鉄輝線 = 高エネルギー粒子が冷たい分子雲を照射

Inui+09 Nobukawa+08Hyodo+08 Takigawa+ Nakajima+09 Nakashima+11

Ryu prep

Uchiyama+11

Sgr	
  B1

E.W : 1–2keV
K-edge : 2–10 x 1023 cm-2

巨大BHからのＸ線照射

I

24
102

思わぬ発見：銀河面に薄く広がる中性鉄輝線
4

3

2
1
0
-1
-2
Galactic longitude l (deg)

-4

deg

6.4 keV line flux

22

Intensity (1e-7 photons /s /cm /arcmin )I (6.4 keV) l profile @ b=-0.046 pm 0.05

-3

10

?
1

10-1

4

3

2
1
0
-1
-2
Galactic Longitude l (deg)-3-4Intensity (K km/s )13CO (NANTEN, Takeuchi+10)
102

10
4

3

2
1
0
-1
-2
Galactic longitude l (deg)

-3

-4

25

銀河面に薄く広がる中性鉄輝線の起源
ASCA : Fe line centerNo. 2, 1998

電離

GALACTIC CENTER CO SUR

12CO (Oka+98)

Maeda89

中性

?
Sgr C
Sgr B

l = 3.5° exhibits
especially strong
6.4 keV line

l = 3.2° “Clump 2”「すざく」キープロジェクト観測（PI=鶴）
1Msecの観測時間 （ほぼ1ヶ月分） を得た．
入射粒子は，光子 or 粒子？

26

If XRNSgr A* Luminosity (ergs/s)

1042
1041

Light Curve of Sgr A*

in 10 years(Gillessen+12)？

？ Clump 2

1040
1039
Sgr B, C
38
10
1037
1036
1035
1034
1033
-1000
Past

Sgr A

Direct observation
with Chandra-100
Time (yr)-10Present

Reveal the Activity of Sgr A* (SMBH) in 2000 years.

Futurewith Astro-H• 2013年度打ち上げの日本主
導の国際共同プロジェクト• 250億円: 日本(80%)、アメリカ(20%)

Suzaku1.7t, 6.5m

Astro-H
2.3t, 14m

ASTRO-H(2013年度)

0.1
0.1

1

(2005年)

ここを拡大（ヘリウム状鉄輝線）

0.01
0.01

−1
1 s−1 keV1
CountsCounts s keV

10
10

すざく

1

1

2

5

2 Energy (keV) 5

10

10

80

マイクロカロリメーター 超精密分光(分解能4eV)40

35倍→世界が変わる
ヘリウム状-鉄-Kα輝線（6.7keV）

CCD(分解能135eV)

0

20Counts s 1 keV 1

60

マイクロカロリメーター

6.55

6.6

6.65
6.7
Energy (keV)

幅・形の変化，シフト

6.75

6.8

仮定無しのダイナミクス

ASTRO-H衛星：X線CCDカメラ（京大）
世界最大の視野ワイドバンドイメージング
新型CCD(ホール読み出し)
検出感度の大幅向上
機械式冷凍機・ASICFPGAイベント処理の採用

Matsuura,TT+06, TT+05, Takagi,TT+05 etc

TT+06 etc

世界最大の視野ワイドバンドイメージング

新型CCD(ホール読み出し)
検出感度の大幅向上

33

入射粒子
Neutral Iron Line from Sgr B2 by Subrelativistic Protons

XRNとLECRの違い

X-raybombardment
reﬂection
Inc Electron
ide
nt EW(keV)〜0.3-0.6
EW (keV)Xra〜1-1.5yBremssThomson
ScatterNH 〜1021(cm-2)
NH 〜1024(cm-2)

2

LECRe と LECRpの違い
102
Dogiel+11510EW (keV)3]p1

6.4 7.1 keV 0.1
-4

e

0
-3 -2
-1
Spectral Index
Fig. 2. Equivalent width of the K˛ line for the solar abundanceFig. 1. Cross section of electron and proton bremsstrahlung radiation
XRN:
producedby electrons 〜(thick 300
solid line) and600
protons (thinsolid line
at the energy
6.4 keV, d!大きいEWと深い吸収
br =dEX (dashed line), and the cross-sections
LECReeV
for injection energy Einj = 80 MeV, dashed line for injection energy!K of K˛ production for electron (thick solid line) and proton (thin0EinjLECRp= 50 MeV) as a functionof the spectral
index,#.
solid line).
Here, E 0 = E
LECR:
浅い吸収
e for electrons and E = (me =mp )Ep for
〜
500
3000
eV
protons. Also, ! equals 0.3 and " is taken to be twice solar. The data
K

34

LECReとLECRpの区別

最終的にASTRO-Hで決定打
マイクロカロリメーター

p (MeV)σ∼10 eVe- (keV)σ∼0 eV

鉄輝線の幅

宇宙線スペクトルe or plog(個数密度)

EW

O (MeV)σ∼100 eV粒子の最終判定

6.4keV？

GeV/TeV	
  γ線

初めて分かる

p?

keV	
  	
  	
  	
  	
  	
  	
  MeV	
  	
  	
  	
  	
  	
  	
  GeV	
  	
  	
  	
  	
  	
  	
  	
  TeV

宇宙線エネルギー総量
スペクトル，空間分布
元素の組成

35

ASTRO-H : 高温プラズマ• ３つの温度• 電子の温度• イオン化温度• イオンの温度（バリオンの総エネルギー）• 非平衡（eg. 澤田君のSNR）• 成因・時間軸• 衝撃波，BHの光電離• 粒子加速• 輝線の強さ 重元素組成
宇宙の元素合成

輝線幅(イオン)
TeV x B
or IC
電子制動放射
電子温度

ASTRO-H：
輝線だけで全てを決める
SNR, 銀河中心,銀河が噴出するプラズマ

Suzaku/XIS 0.5 - 2.0 keV image

Sgr A*
Galactic Latitude (degree)

0.0
Jet ?

銀河面

-0.5
-1.0
-1.5

南北にのびる
360光年

巨大プラズマ

-2.0
1.0

0.0

359.0

358.0

Galactic Longitude (degree)

再結合プラズマ?

→ GCからの噴出や爆発の証拠

「すざく」新天体の発見・思わぬ発見
7 New SNReS210

M. Sawada et al.

[Vol. 61,

Fig. 1. Wide-band (0.7–5.5 keV) smoothed images by the (a) XIS and (b) MOS shown with the logarithmic intensity scale. Overlaid green contoursin (a) are an 18 cm radio continuum map from the Very Large Array (VLA; Mehringer et al. 1998). The point source extraction aperture size andbackground accumulation region for PS2 and PS3 are shown in (b). See subsubsection 3.2.1 for details. For the XIS image, we merged events with thethree CCDs, subtracted the non-X-ray background (Tawa et al. 2008), corrected for the vignetting, and mosaicked the two fields with different exposure
times normalized. The fields of view are shown with two solid squares with 180 in length. For the MOS image, we merged two CCDs and mosaicked thetwo fields with normalized exposures. The fields are shown with two circles with 300 in diameter.

by external X-ray irradiation (Murakami et al. 2000). H II
regions are also an emerging class of diffuse X-ray sources
with a similar spatial scale. They show a variety of spectral
shapes, including soft thermal (Townsley et al. 2003; Hyodo
et al. 2008), hard thermal (Moffat et al. 2002; Ezoe et al. 2006),
and nonthermal (Wolk et al. 2002; Law & Yusef-Zadeh 2004;
Wang et al. 2006; Tsujimoto et al. 2007; Ezoe et al. 2006) emission. In addition to the X-ray emission, the measurement of the
X-ray absorption gives a constraint on the distance and hence
the physical scale of extended objects.
Several X-ray observations were reported in the Sgr D
region. In a BeppoSAX study (Sidoli et al. 2001), diffuse X-ray
emission was significantly detected from the Sgr D SNR andmarginally detected from the Sgr D H II complex. In an ASCA
study (Sakano et al. 2002), the image was plagued by straylights from a nearby bright source and was unsuitable to searchfor diffuse X-ray sources. In an XMM-Newton study (Sidoli
et al. 2006), dozens of point sources were identified, but nodiffuse emission was detected presumably due to high background. The possible diffuse X-ray detection by BeppoSAX in
the Sgr D H II complex has not been confirmed and no spectral
information exists for this source.
We conducted X-ray observations of the Sgr D H II complex
using the X-ray Imaging Spectrometer (XIS: Koyama et al.
2007a) onboard Suzaku (Mitsuda et al. 2007). The low background of XIS makes it particularly well-suited for finding
diffuse sources of low surface brightness and yielding theirhigh signal-to-noise ratio spectra. Indeed, a series of XIS

studies in the GC region identified several new SNRs andirradiated GMCs (Koyama et al. 2007b; Mori et al. 2008;
Nobukawa et al. 2008) and reported detailed spectroscopy of an
H II region (Tsujimoto et al. 2007). Upon the confirmation of
the previously claimed marginal diffuse detection in the Sgr D
H II complex, we further aim to construct the X-ray spectrum
which gives important insights into the origin of the emission
and the entire complex.
Here, we present a significant detection of diffuse X-ray
emission from the Sgr D H II complex with the Suzaku XIS.
High signal-to-noise ratio spectra were obtained from two
different diffuse sources. We discuss their X-ray characteristics and their association with sources observed in our study
using the 100-m Green Bank Telescope (GBT) and in otherarchived multiwavelength data sets. Based on these data, we
propose a new view of the Sgr D H II complex. In this paper,
we supplement the Suzaku data with those taken by XMMNewton in order to evaluate the contribution of point sources
to the diffuse emission. Throughout this paper, we use east andwest in the Galactic longitude direction, and north and south in
the Galactic latitude direction for simplicity.

13 New XRNe

2. Observations
2.1. Suzaku
We used two XIS fields covering the Sgr D H II complex in
the Suzaku GC mapping project (table 1). We hereafter call thetwo fields as north and south fields (figure 1a). The north field5 New 「すざく」新天体の発見・思わぬ発見
Types of objects
Super Bubble
Super Bubble

H. Mori et al.

7 New SNRe
S210

[Vol. 61,

ChimneyTsuru+09“Chimney”

the Chimney

M. Sawada et al.

RRC-SNR

Tornado[Vol. 61,

0.0b

Sgr A*-0.2

G359.41-0.12

359.4

359.6
0

0.05

0.1

0.15

0.2

0.25

0.3

359.2

l
0.35

0.4

0.45

0.5

0.55

4 Unexpected Phenomena ・ New Perspectives
Fig. 1. Wide-band (0.7–5.5 keV) smoothed images by the (a) XIS and (b) MOS shown with the logarithmic intensity scale. Overlaid green contours

g. 5. GC mosaic images of He-like sulfur
K˛-lineandcontinuumHe-likemap
andH-like
The etimages
binned32 ! aperture
32 pixels
and thein (a)
are an 18(a),cm radio
fromthe Veryiron
LargeK˛-lines
Array (VLA;(b).
Mehringeral. 1998).were
The pointsourceby
extraction
size andregionfor PS2and PS3 are withshown !
in (b).
subsubsection
3.2.1 for details.
XISvignetting
image, we merged
eventsofwith
The exposure
time For
andthetheeffectthetheXRTs
ntinuum fluxes were then subtracted (seebackgroundtext) andaccumulation
the images
weresmoothed= 1See0.66.
three CCDs, subtracted the non-X-ray background (Tawa et al. 2008), corrected for the vignetting, and mosaicked the two fields with different exposure
re corrected. The XIS field of view is indicatedby a red polygon. The GC-ring spectrum was extracted from the elliptical arc-like region encircled
times normalized. The fields of view are shown with two solid squares with 180 in length. For the MOS image, we merged two CCDs and mosaicked thefields with
exposures.
The fields
are shownthe
withsource-extraction
two circles with 300 in diameter.
h solid curves. The background region istwoshown
bynormalized
a dashed
polygonexcludingregion and an ellipse with a red slash.

X-ray Tomography

by external X-ray irradiation (Murakami et al. 2000). H II studies in the GC region identified several new SNRs andregions are also an emerging class of diffuse X-ray sources irradiated GMCs (Koyama et al. 2007b; Mori et al. 2008;
with werea similarsummed
spatial scale.
They show a variety
spectralet al.indicates2008) and reported
spectroscopyof an hasalized by the effective area, andtogether.
shownof in
figureNobukawa
6a, andthat detailed
the X-rayemissionshapes, including soft thermal (Townsley et al. 2003; Hyodo H II region (Tsujimoto et al. 2007). Upon the confirmation ofly, we subtracted the background
spectrum
from
the
ring
a
thin
thermalplasmaorigin.
We
fitted
the
faint
ring
et al. 2008), hard thermal (Moffat et al. 2002; Ezoe et al. 2006), the previously claimed marginal diffuse detection in the Sgr DspecH II complex,
we plasmafurther aimmodel.
to construct
the X-rayspectrumabunrum, which is shown in figure and6a.nonthermal (Wolk et al. 2002; Law & Yusef-Zadeh
trum with2004;
an absorbed
CIE
The
elemental
Wang et al. 2006; Tsujimoto et al. 2007; Ezoe et al. 2006) emis- which gives important insights into the origin of the emission
e spectrum clearly shows the Si,
S, and Ar emission lines, dances of Si, S, and Ar were allowed to vary again. The bestsion. In addition to the X-ray emission, the measurement of the and the entire complex.
dition to a marginal emission line
to He-like
Ca. Wefit parametersconsistent
thosedetection
derivedfromX-raythe ring
X-ray dueabsorption
gives a constraint
on the distanceand hence are
Here,
we present witha significant
of diffuse
the physical scale of extended objects.
emission from the Sgr D H II complex with the Suzaku XIS.
the spectrum by an absorbed CIE
plasma
model
with
the
spectrumincludingtheG
359.77"0.09
andG
359.79"0.26
Several X-ray observations were reported in the Sgr D High signal-to-noise ratio spectra were obtained from two
ble abundances of Si, S, and Ar.
The
best-fit parameters
emission;
the X-rayfromplasmawithcharacteristhe temperregion.
In a BeppoSAX
study (Sidoli et al. 2001),
diffuse X-raydifferentemission
diffuse sources.
Wethe
discuss
their X-ray
emission
was significantly
detected from theSgr D of
SNRkT
and =tics0.96
and theirassociation
with sources
observedinour studykeV
isattenuatedwiththeabsorptionofe absorption column density andtheelectrontemperature
atureemarginally detected from the Sgr D H II complex. In an ASCA using
100-m Green Bank Telescope (GBT) and in other22"2
22 theand kTe study= 0.91keV.
Theelemental! 10archived
cm"2. We summarized
the best-fit
parameters(Sakanoet al.
2002),
the image wasN
plaguedby straymultiwavelength
data sets. Basedon these data,we
H = 5.5 ! 10 cm
H = 5.5
lightsorfroma nearby brightsource The
and was unsuitable
II complex. In
this paper,
proposea newview of the Sgrthe
D H physicaldances of Si, S, and Ar are solar
subsolarvalues.
in tableto search
2. Thisresultstrengthensconnectionoffor diffuse X-ray sources. In an XMM-Newton study (Sidoli we supplement the Suzaku data with those taken by XMMs are summarized in table 2. We
allofofpoint
thesources
best-werethe
faintbutring
to Gto359.77"0.09
and G
et al.note
2006),that
dozensidentified,no emission
Newton in order
evaluate the contributionof 359.79"0.26.
point sources
diffuse emission
was thedetectedpresumably due to high back- to the diffuse emission. Throughout this paper, we use east andrameters of the absorption column
density,electronground. The possible diffuse X-ray detection by BeppoSAX in west in the Galactic longitude direction, and north and south inerature, and the elemental abundancesareintermediate
4. andDiscussion
the Sgr D H II complex has not been confirmed
no spectral the Galactic latitude direction for simplicity.
information
existssubsection
for this source. 3.1)
s between those of G 359.77"0.09
(see
4.1.
359.77"0.09
2. Observations
We conducted X-ray observations of the Sgr
D H IIG
complex
G 359.79"0.26 (see table 3 of Moriet X-rayal. 2008).
using theImaging Spectrometer (XIS: Koyama et al.
2.1. Suzaku
onboard Suzaku(Mitsuda ettheal. 2007). The
The lowX-ray
back- spectrum of G 359.77"0.09 clearly shows therthermore, we made a ring2007a)spectrumexcluding
We used two XIS fields covering the Sgr D H II complex inground of XIS makes it particularly well-suited for finding
9.77"0.09 and G 359.79"0.26
tosurfaceexaminepresence
thermalplasma(kTe #1).0.7
the Suzaku
GC mapping
project(tableWe keV).
hereafterThecall theheavy
diffuseemission
sources of low
brightness andyielding of
theira thin
22 south"2fields (figure 1a). The north field
fieldsasnorthandsignal-to-noise
ratio spectra.
Indeed,absorptiona series of XISof Ntwo
her the region with the fainthighK˛-line
emission
from
=
6.9
!
10
cm
indicatesthattheplasma isH

高温プラズマ

1000年
0.9

1994$(ASCA)$

time variable 6.4 keV line

2000$(Chanrda)$ 2003$(XMM)$$$$$$$$$2005$(Suzaku)

M359.47–0.15

M359.43–0.07

13 New XRNe
0.8

1.0°

射手座B2

0.5°

0.7
M0.13–0.13
0.6
-0.5°

射手座A*
射手座B1 0.4

-1.0°

射手座C

300年

Neutral lines from light elements

0.3

M0.74–0.09
ke sulfur (referred as to faintring hereafter) is related located in the GC. Using the best-fit plasma parameters derived
ese two bright clumps. The excluded regions for from the G 359.77"0.09 spectral analysis, we can estimate
M0.74–sub 0.2as that
100光年
9.77"0.09 and G 359.79"0.26 are the same
some physical properties. Assuming that the distance to theibed in subsection 3.1 (see also the solid ellipse in plasma is 8.5 kpc, the emission measure is estimated to be 6.940
0.1 et al. ! 1058 cm"3 . If the plasma is an ellipsoid with dimensionse 1a) and that described in section 3 of Mori
Gas8), respectively. As is shownin figure 5b, the periphery of 4 0.9 ! 2 0.4 ! 2 0.4, corresponding to 12 pc ! 6.0 pc ! 6.0 pc
25NH
359.77"0.09 shows relatively bright K˛-line emission in the GC, the volume of the X-ray emitting plasma is 3.910highly ionized 22iron becauseof its location. Thus, in ! 1058 cm3 . The electron density of the plasma is then derived
-2)
(10
cm
to extract the corresponding background spectrum, we to be 1.3f "1=2 cm"3 , where f is a filling factor.
ved the areaRyu,TT+09
overlapped with the dashed rectangle shown
The elemental abundances of the plasma are consistent withure 1a from the background region. We again subtracted the solar values, which implies that the X-ray emitting plasma
ackground spectrum after applying the vignetting correc- has an interstellar medium (ISM) origin. The total mass of the

観測者
V
•

1=2

Thin Extended
6.4keV line
emission「あすか」の思わぬ発見が「すざく」で花開いている• 中質量BH• GCの6.4keV輝線• SNRの過電離プラズマ「あすか」がきっかけ「すざく」の思わぬ発見がASTRO-Hで花開くでしょう