1「すざく」衛星による天の川銀河中心領域の活動性の観測
Ｘ線トモグラフィによるSgr A*の活動（1000年の活動）
GC South/North プラズマ（10万年の活動）
高階電離鉄輝線の起源（100万年？の活動）

鶴 剛 (Kyoto University)
on behalf of the Suzaku GC team.
20131114_GC_Suzaku_UT_IoA_v3.key2

1000年間の活動〜Ｘ線反射星雲の3-D配置〜

Ryu et al. 2009, PASJ, 61, 751
Ryu et al. 2013, PASJ, 65, 33
Ryu FY2012 Doctor Thesis, Kyoto Univ.

Observation of the GC region with Suzaku

1deg

204pointings, 5.96Msec
SWG, AO, LP, KP x2 (|l|<3.5°, |b|<5°)

3

R: 0.5-2.0keV
G: 2.0-5.0keV
B: 5.0-8.0keV

36 refereed papers,
7 Doctor Theses.

4

0.1

He-like S Kα
(2.45-keV line)

Neutral Fe Kα(6.4-keV line)

1deg

Narrow Line

0.01

−1

Counts s keV−1

1

Suzaku Spectrum of the GC region

Mapping1

He-like Fe Kα(6.7-keV line)

2

5
Energy (keV)106.7-keV Line Image (He-like Fe Kα)56.7keV (Continuum subtracted)

CHAPTER 2. REVIEWSgr A*

Photons cm-2 s-1 arcmin

-2

10
10

(a)
-5

•
6.7-keVFe XXV K

-6

10

-8

10

-9

•

GC

10-7

GR

r〜500ly-

F=10×exp(–l/0.6deg) + exp(–l/50deg)

0.01

0.1

1

10

S XV K(b)
ThermalPlasmas10-5
smoothly
distribute in-6
10
the GC region.
-7
10
The origin is still under
debate.
-810
Truly
diffuse plasma-910filling in the GC region.
Or, collectionof faint 1
0.01
0.1
*
unresolved
point
Distancefrom Sgr A along thsources.

Photons cm-2 s-1 arcmin-2

100ly

100

*

Distance from Sgralong
theSgrlongitude
l* A
(deg,
from
A*) |l* | (degree)

Uchiyama+11, +12-

6

6.4-keV Line Image (Neutral Fe Kα)

FeI 6.4 keV Map by Suzaku- 0.0ºSgr B2
M0.74–0.09

Sgr B10.5º

1.0º

Sgr A*

b

Sgr C

0º

-0.5º

Sgr A*

Sgr C

l

-0.9º

CS ( J=1–0) Map by Tsuboi+1999

Sgr B
b
300 pc of the Central Molecular Zonel

• 6.4-keV line generally traces the distribution of the molecular clouds.
• 6.4-keV fluorescence line is emitted from MC.
What is the ionizing particles ? Electrons or X-rays ?

7X-­‐ray	  reﬂec*on	
  vs.	
  Electron	
  bombardment
X-ray reﬂection

Inc
ide

nt

X-

ra

y

EW (keV)〜1-1.5EW(keV)〜0.3-0.6
BremssThomson
ScatterNH 〜1021(cm-2)

NH 〜1024(cm-2)

2

Electron bombardment

6.4 7.1 keV

2

6.4 7.1 keVLarger EW of 6.4 keV line is expected for X-ray reﬂection
σ(Photo Abso)/σ(Thomson) < σ(Innser Shell Ion)/σ(bremss)
Larger absorption NH (cm-2) for X-ray reﬂection
Electrons stop at the surface of MC due to ionization loss.

counts/sec/ke

10 3

8

X-ray Reflection Nebula

HAPTER 2. REVIEW

10 4

2
0
2

0.01

Sgr
(a) B2
Sgr B2
Koyama+07

5(b) M359.47 0.15

• Equivalent Width : 1–2keV• K-edge : N = 2–10 x 10 cm
Time: region after subtra
ig. 2.20.—: X-ray spectra of giant
MCs Variablein the GC•
pectrum of Sgr B2 (Koyama et al., 2007b). (b) spectrum of M 359.43−0
counts/sec/keV

Fig. 5.

6.4-keV line

10

−0.07 (a) an

23

H

3

10 4

Energy-2Size ~10 lys, τ ~ 10 yrs

t al., 2009). TheDeep
spectralfeaturessuggest the X-ray origin (see text).
absorption
edge
4

6

(keV)

(a) Sgr B2=−

Fig. 5.
Inui+09, Nobukawa+11
1995

2000

Ionizing particle is X-ray“X-rayReflection Nebula(XRN)”
0
~
~
σ=
±
(b)
Sgr A, G 0.1–0.1(c)2
Need a source.
± .
×
39ergs/s
5
10with LX ~ 10
Energy (keV) = ==No such bright source.
−0.07 (a) andM 359.47−0.15(b).
Sgr A* is only
possiblesource.
. ± . one×2

2005 (year)

•
•
•

−

−

−

−

2

−

−

−

~

−

−

:ı

:ı

Echo of the past activity of Sgr A*
J =

l b =

9

Long Term Light Curve of Sgr A*
d

XRN
is
echo.

Collecting the data of XRNe
allows us to obtain past activityof Sgr A* reaching ~1000yr.

Face on(Top View)

Sgr A*

Very Unique Study

Only Sgr A* allows us to access sucha long-term activity of a SMBH.

• L (Sgr A*) L (XRN) x Mass(XRN) x d^2 The line of sight• Distance “d” between XRN and Sgr A* position of XRN is
X

X→ Look back time.

necessary.

10“X-ray Tomography”• The GC thermal plasma
distributes smoothly.

• If an XRN (MC) is located in thenear side of the thermal plasma,then soft X-rays from the plasma
is absorbed by the XRN due tophoto-absorption.

• In the case that the XRN (MC) is
located in the far side of thethermal plasma, soft X-rays fromthe plasma is un-absorbed.

Absorbed

XRN

GC –

XRN

Near
ObserverThermal PlasmaMC) is located in the GC thermal
plasma.

Thermal Plasma• An XRN (e.g. Molecular Cloud:FarCosmic X-ray Tomography

6.4-keV(XRN) XRN

Far

100 ly2.45-keV(Plasma)
Strongly
Absorbed
100 ly100光年

Absorbed

Sgr A*
XRN

GC –

XRN
Sgr C

Thermal Plasma

6.7-keV(Plasma)

Thermal Plasma

Sgr B2100 ly11

Sgr A*

XRN

Near
A*
超巨大BH
Observer SgrQuantitative studies allow us to obtainthe line of sight potions of the XRNe.

LessAbsorbed

12Spectral Modeling
X-ray spectrum as a function of theline of sight position of XRN.

Cnt/s/keV

FeXXV
6.7 keV– 0.9
XRN

Plasma Emission→

Spectral ModelContinuum of
0.1
Plasma Emission

FeI 6.4 keV

1.0 Far

– 0.8
– 0.7

XRN

– 0.6

R

XRN

0.01

XRN

Decrease

1

3

Energy (keV)

5

Observer– 0.5 Center
– 0.4
– 0.3
– 0.2
– 0.1
0.0 Near
Ryu+09,	
  +13

GC Plasma

Spectral Fitting

1-R
XRN

Abs2

R
ISM

Abs1

Foreground-E

V• Observer
Flux (E) = Abs1 × (GC-Plasma-E × R)
+ Abs1× Abs2 × (GC-Plasma-E × (1–R)+ XRNE )+ Foreground-E + CXB

13

14

3-D distribution of XRNe
Edge-­‐on	
  view

Face-­‐on	
  viewfar

near
Ryu+0.9, +13

XRN with Tomography v.s. MC with Radio Kinematics- X1 elliptical orbit- Arm I & II
are obtained.

(a)Face-on
View

far

30

X2 Orb.

25

I

I
m
r
A
B2

C3

15

C1

Arm I

near

1000
1000

20

B1
M
0.74

-500

X1 Orb.

Sgr A*★

D

0

C2

NH (10222 cm–22)•Assuming the kinematics
model, with the observed
line of sight of speed ofMCs, the structures of500

Y (ly)(ly)Y(Binney+91, Sofue+95)

1000

Line of Sight Position Y (ly)Radio•Central Molecular Zone

E

10
To
X1
majo ~1 Sun
r
5º
axis

500

0

5

-500

Galactic longitude
X (ly) X (ly)-1000

The X-ray result is consistent with the radio one.

Fig. 7.5.—: (a) Face-on distribution of the XRNe aro
Note: X-ray is independent
fromlines)
and dose
not use orbits
the radio
information.
(dashedand possibleof X1and X2 (grey li

16Light curve of Sgr A* in the past
Ryu+0.9, +13

With 90% errors

time variability

LX

Sgr A* is very quiet at present.
← PastTime (year)

Current• Sgr A* had been in active phase 50 - 600 years ago.
• Sgr A* made nearly one order of magnitude variation in ashort time (<10 years) at a couple of times.

How about before 600 yrs ago ?

17

No. 2, 1998
GALACTIC CENTER CO SURVE
Access the activityof 1500 yrs
ago

ASCA GIS : Center of Feline complex (6.4-6.9keV)

12CO (Oka+98)

Maeda89l = 3.2° “Clump 2”

?
Sgr C
Sgr B

l = 3.5° exhibits
especially strong
6.4 keV line

• MC called “Clump 2” is located at the
Galactic longitude of 3.2 deg.
• The ASCA data suggest strong 6.4keV
line, which would be due to Clump 2.
• We would be able to access theactivity of 1500 yrs ago (if it would be
an XRN).

FIG. 2.ÈMaps of the 12CO J \ 1È0 and 13CO J \ 1È0 line emission integrated over the veloc
drawn at every 200 K km s~1 for 12CO and at every 100 K km s~1 for 13CO. Mapping areas are ind
beams).

S2

A “cloud” falling into Sgr A*

18

ėDeclination (arcsec)

d

0.2
0.1

2011.3

Sgr A*

S2m2008.3

2004.5

(

0

l

Ă

0.1

[

W

0.2
0.3

0.2

0.1



0

m

Right ascension (arcsec)

Gillessen+2012

A cloud is approaching Sgr A* and will pass at ~3100 times theevent horizon of Sgr A* in the summer of this year (2013).
Sgr A* will be active. Activity lasts in the next 30 years.

N

M

19

GC South Plasma : 10万年前の活動〜再結合プラズマの発見〜
Nakashima et al. 2013, ApJ, 773, 20
To be a part of Nakashima FY2013 Doctor Thesis, Kyoto Univ.

Bipolar X-ray emission
from the GC
1.0 1-3 keVのX線
中性鉄輝線
5-8 keVのX線

銀緯 (度)Sgr A*

0.0

X線反射星雲1E 1740.7-2942(deg.)
Galactic
Galactic latitudelatitude (degree)

GC north

GCDX

200pc

Chandra (1-3 keV)
Suzaku (1-3 keV)

1.0
1.0

0.5

-0.5

20

0.0
0.0

GC North
Galactic plane

Sgr A*GC South

-1.0
-1.0

-1.0

Ｘ線吸収=銀河中心までのKsバンドの吸収
GCのプラズマGC south
-1.5
1.0

•
•

M = 710M@, E = 1.6x1051ergs, n=0.16cm-3
0.5
0.0
-0.5
-1.0
0.5
0.0
エネルギーは10~100個のSNR．星団は無い．
-0.5
銀経 (度)
0.5
0.0
-0.5

Galactic longitude
Galactic
longitude(degree)(deg.)

単一のSNR，Super Bubbleではない．

Recombining plasma
model
Recombining
PlasmaMissing Fe L-shell complex

(a)

−1
χ
Counts s−1 keVCountss−1 keV−1

100

10−2
10−1
(b)

χ

BGD

• 再結合連続線 RRCは，CIE
では極めて弱い．

Fe-L

Fe-L

(c)
(b)

χ2/d.o.f = 1378/350
2617/352

Fe-L

Si XIV Si-RRC

599/348
χ2/d.o.f = 1378/350

Si XIV Si-RRC

(d)

1

2
Energy (keV)• イオン化非平衡
kTZ > kTe
で再現成功

S-RRC

(d)
(c)

0
−5 イオン化非平衡モデル

0−5χ2/d.o.f = 2617/352

GC south0−5 イオン化平衡モデル

5ではフィットできず．

多温度CIEの可能性あり

0
−2
10
−5

5

• 1成分イオン化平衡(1CIE)• H-Si-Kαが強いだけ

Fe-L

χ

Background
Recombining plasma model
Missing Fe L-shell complex
Background

10−1
100

5
χ

– 15 –

(a)

5

21

S-RRC

5 χ2/d.o.f = 599/34810

Fig. 4.— (a) Spectrum extracted from the entire source region. Only the co-added FI spectra

22

Recombining Plasma
Ionizing plasma v.s. Recombining plasmakT

1.63 keV

kTinitkTz

kTe

0.46 keVNEI

CIE

GC South

5.3 x 1011 s cm-3
Time Scale (nt)~1013 s cm-3

τRP = 1.1x105yr << τcool ~ 1-2x109yr

Recombining Plasma
Ionizing plasma v.s. Recombining plasmakT
kTinitNEI

CIE

Recombining

kTe
Ionizing(standard NEI)
kTinit = 0

Time Scale (nt)~1013 s cm-3

How to make Recombining Plasma
Ionizing plasma v.s. Recombining plasmakT

種1.63 keV

kTinitkTz

kTe

0.46 keVNEI

CIE

GC South

5.3 x 1011 s cm-3
Time Scale (nt)~1013 s cm-3

τRP = 1.1x105yr << τcool ~ 1-2x109yr

24

How to make Recombining Plasma
Ionizing plasma v.s. Recombining plasmakT

1.63 keV

kTinitkTz

kTe種

0.46 keVNEI

CIE

GC South

5.3 x 1011 s cm-3
Time Scale (nt)~1013 s cm-3

τRP = 1.1x105yr << τcool ~ 1-2x109yr

25

26

Plasma Origin• 種プラズマの作り方• Starburst Activityに伴う銀河風• v=510km/s (Cs @ kTe=1.6keV) GCから4x10 yr• 10 -10 yr前にStarburst Activity (Matsunaga+11,Yusef-Zadeh+09)
557• Sgr A*からのエネルギー注入• 600~50yr前の活動 L ~1x10 ergs/s• If これが ~10 yr続いたと仮定 L ~10 ergs ~ E(GC south)
X

5

39

X

51

How to make Recombining Plasma• 電子温度を下げる．
• 初期状態 kTinit = kTz = kTe = 1.63keV• 断熱膨張によりkTeが下がった．
• T V , kTe=1.63→0.46keV(1-γ)

体積が6倍に膨張（サイズ1.8倍）密度は 1cm-3 → 0.16cm-3．

•(97 /1.8)kpc → 97kpc へ音速で膨張に必要な時間 ~ 8x104yr• イオン温度を上げる．
• 初期状態 kTinit = kTz = kTe = 0.46keV• Sgr A*からのＸ線による光電離が起こる．L ~ 7.6x10 ergs/s• GC Plasma には，光電離 (RP)の痕跡がない． ビーミング
X

43

27

28

GC South North〜南があるなら北にも？〜Proposing as a key-project of Suzaku AO9
To be a part of Nakashima FY2013 Doctor Thesis, Kyoto Univ.

How about GC North ?
2.0(a) Suzaku 1-3 keV(b) Chandra 1-4 keV(c) ASCA 1-3 keV

1.5

GC Nouth

Galactic Latitude (degree)

1.0

0.5

Sgr A*

0.0

Sgr A*Sgr A*-0.5-1.0

GC South
GC South

-1.5

-2.0

0.5

0.0

359.5

0.5

0.0

359.5

Galactic Longitude (degree)

0.5

0.0

359.5

Tip of DHN

ASCA 1-3keV
Radio lobe
Molecular
Cloud

Hα
1.0

DHN
0.5

0.0

X-ray
loop?
S-shape
0.5

0.9

0.0

359.5

Galactic Longitude (degree)

359.0

Galactic Latitude (degree)

Galactic Latitude (degree)

1.5

ASCA 3-6keV (Contour)• Sgr A*の活動?
• ジェット or アウトフロー?
• NSCからの磁気タワー?
• 銀河面の高温プラズマの巻き上げ?

Color = Spitzer 22 µm, Contour = ASCA 3-6 keV

0.8

0.7

DHN

Hard
X-ray
Interaction?

0.6

0.2

0.1

0.0

359.9

Galactic Longitude (degree)

Fe-K line (6.4keV ?) from MC interacting Radio Lobe

ASCA 1-3keV
Galactic Latitude (degree)

1.5

Radio lobe
Molecular
Cloud

Hα
1.0

DHN
0.5

0.0

X-ray
loop?
S-shape
0.5

0.0

359.5

359.0

Galactic Longitude (degree)• New XRN ?
• 従来 |b|<0.1度(15pc)• 初めての高銀緯(b=0.1-0.5°)• Cosmic Rays (Electron orProton) from Radio Lobe ?

高階電離鉄輝線の起源：100万年？の活動〜点源寄せ集め or 真に拡がる？〜
Uchiyama et al. (2011) PASJ 63, S903
Uchiyama FY2009 Doctor Thesis, Kyoto Univ.

3. Fe-K Lines (6.7, 6.9 keV) Distributions
Image

Truly Diffuse orPoint Sources ?

Divided into small
areas and made
spectra, fit theindividual spectrumwith a power-law+ Gaussians.
Fluxes (F)F6.7 : 6.7 keV line
F6.9 : 6.95 keV lineSurface brightness(10-6 ph/s/cm2/arcmin2)

B：EastR：West• The border between

GC and GR is locatedat l = 1〜2deg.

Ridge: Yamauchi
GC: Nobukawa+• The temperature of GC
would be higher thanGR.

Nobukawa, Hyodo+,
Yamauchi+09

GlobalDistribution
of Fe ofKαFeLines
in theinGalactic
CenterRegionGlobalDistribution
Kα Lines
the Galactic
CenterRegion(b)
6.7keV Line Profile vs (b)Stellar
Mass Distribution
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

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)

-6

-7

-8

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

Nuclear10-5
stellarcluster
10-6

(d)

10-7

Nuclear bulge

10-8

10-6

10-7

10-8

(d)

A new population of
10
point sources with astrong 6.7keV line.
10orTruly diffuse
10plasma

10-6

6.7keV Lines Origin of 6.7keV
10
10
Excess atline in GC is
GC
different from GR-7(at l =-0.114)*

10-8

Nuclear Galactic Galactic 10-5This workThis work
bulge
disk
stellar Koyama+07
Koyama+07
Yamauchi+09
disk Yamauchi+09
Observed photons cm-s s-1 arcmin-2

)

10-6

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

Observed photons cm-s s-1 arcmin-2

-6

10-5

-7

10-8

0.1
1
0.1
1
*
Distance from
Sgr from
A* along
thelatitudeDistance
Sgr A
along
the|blatitude|b*| (degree)*| (degree)-5

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

Observed photons cm-s s-1 arcmin-2

a)

-6

-7

Uchiyama+11
10-8

The 6.7 keV line flux vsIntegrated point source flux
(Chandra deep exposure)
Near GC ( < 0.3 deg)
Nobukawa, Hyodo+l-distribution
Sgr A*

b-distribution
Sgr A*

10 x 6.7 keV line (EW=0.5 keV)Distribution of Point source flux (4.8-8 keV)The 6.7keV has more extended
distribution than point sources.

( ｂ)Plasma Parameters (assuming ZFe=1.2)• Size ~ 50pc x 30pc
~0.70°• L ~ 2×10 ergs/s ~0.36°• n ~ 0.1cm• n ~ 0.4cm• E ~ 3×10 ergs R: 6.7keV, G:2.45keV, B: 6.4keV• Escape Time scale (latutude) τ = Size/Cs = 2×10 yr• Heating Rate = E /τ ~ 5×10 ergs/s ~ 10 SN yr

Tsuru+ (Suzaku2007)

2-10
ave

36

-3

-3

peak
gas

52

4

esc

gas

esc

40

-3

-1

*
Much higher than the current activity of Sgr A and~10-5 SN yr-1 expected from the stellar mass in thisregion.
Plasma is in the ionization equilibrium or not ?

EI or NEI

6.7keV Center Energy

6.65

Tsuru+ (Suzaku2007)8

6.7-keV Line
Center

10

6.55
6.5

11
1012
1010
Normalizatino
Ratio 10
6.9/6.7keV
kT=6.5keV
nt [sec/cm3]

0.33±0.02

13
10
VNEI

Line ratio
6.9/6.7-keV

0.05

0.1

0.2

kTe=6.5keV

kTe=6.5keV

0.02
0.01

Koyama, Hyodo
et al. (2007)

Normalizatino Ratio 6.9/6.7keVnτion > 2×1012 sec cm-3>> nτesc ~ 1×1011 sec cm-3
small escape (age > 6e+5yr)

66680 +3,-6eV

6.6• Suzaku spectrum••

kT=6.5keV

1010

10
10

1011

11
10

1012
nt [sec/cm3]

12
10

1013

13
10
nt (sec cm-3)

1014

14
10

Confinement by Magnetic Field ?

•Tsuru+ (Suzaku2007)(eg.Yamauchi+90, Koyama+96, Muno+04)
Pressure
B = 0.1mG~1mG
PB/k =106-108 K/cm3 ~ Pgas/k =2×107 K/cm3••• The strength of the magnetic field can confine 6.7keV plasma.
• Slow diffusion → Makes the required heating rate lower.
• But, the orientation of the mag. is vertical against the disk.
→ Easy to escape.

2007.12頃こんなことを考えていた...
→西山さん，長田さんに相談%$

**"*.

Ks polarization map 32 (P/P  2)UPU[S-

0.5%

VP
WUS-
Nishiyama+13, ApJL, 769, 28

Fig. 5.— Polarimetry results covering 3.◦ 0 × 2.◦ 0in the Galactic coordinate, together with an intensity map of 6.7 keV line emission (Nobukawa et al.
2012). The cyan vectors show the inferred magnetic field direction, and the lengths are proportional to polarization percentage. The vectors areaveraged in a circle of 2." 4 radius with a 3." 0 grid,and plotted with thick bars (detected with morethan 3σ) and thin bars (detected with◦ 2 − 3σ).
Fig. 5.— Polarimetry results covering 3. 0 × 2.◦ 0n the Galactic coordinate, together with an intenThe obtained polarization map (Fig. 5) sugsity map of 6.7 keV line emission (Nobukawa et al.
gests a large-scale toroidal MF configuration in the2012). The cyan vectors show the inferred magNB. The histogram (Fig. 6) of the MF directions
netic field direction,and the lengths are proporat | b |< 0.◦ 4 has a clear peak at 90◦ which is the

Number ofwith the scale height of the 6.7 keV emission, 0. 27(Uchiyama60et al. 2013).
120

100

Number of Fields

ment does not work well, although observations
the Galactic plane has been claimed in the GC
of the MF in the NB have been limited to the(Nishiyama et al. 2010).
region in dense molecular clouds (Novak et al.
2000, 2003; Chuss et al. 2003) and very thin,
non-thermal radio filaments (Tsuboi et al. 1986;
Yusef-Zadeh et al. 1997; Lang et al. 1999). Recent
observations have revealed that NIR and widefield polarimetry offers a promising tool to tracea large-scale MF, and a troidal configuration near
the Galactic plane has been claimed in the GC(Nishiyama et al. 2010).

80

40

20

all
o
|b|< 0.4o| b | > 0.4

0
0

20

40

60

80

100

120

140

160

180

Position Angle [degree]
60

Fig. 6.— Histograms of the magnetic field direction40at | b |≤ 0.◦ 4 (red), | b |> 0.◦ 4 (blue), and both(black). The red histogram has a clear peak at20
the direction
almost parallel to the Galactic plane(90◦ ), while the blue one has a peak at ∼ 150◦ ,0 perpendicular to the plane.
almost020
40
60
80 100 120 140 160 180
Position Angle [degree]

The determination of the MF strength is stillquite difficult in this region, but it seems to
Fig.converge
6.— Histogramsof theofmagnetic
field
directo◦ the value
50
"
B
[µ
G]
" 200
◦
tion(e.g.,
at | b Ferrière|≤ 0. 4 (red),|> 0. 4 (blue),both At
2011;| b Crocker
et al. and2011).
(black).
The strength,
red histogram
has a clear
peakdensity
atthis field
the magnetic
energythe (∼
direction
almostparallelto theGalactic
plane
−3
0.1
−
1
keV
cm
)
reachesnearlyequipartition◦(90◦with), while
the
blue
one
has
a
peak
at
∼
150
those of diffuse hot plasma (∼ 0.5 keV cm,−3 )almostthe plane.
and perpendicular
gas turbulenceto(seeFig. 4 in Crocker et al.
2010). This suggests that MFs provide significant
The determination of the MF strength is stillpressure support against the diffusion of the hotquite difficult in this region, but it seems toplasma.
converge to the value of 50 " B [µ G] " 200
the plasma
not etsupported,
it At
would
(e.g., If
Ferrière2011; were
Crockeral.
2011).
Nishiyama+13,
ApJL,
769,
28

磁場は銀河面に平行→閉じ込められる可能性あり

Summary42• Ｘ線トモグラフィによるXRNの３次元配置の解明．
• XRNを用いてSgr A* の過去50-600年の光度曲線．
• ほぼLX ~1039ergs/sで一定で， 少なくとも2回ほど，1桁近い時間変動があった．

• GCの南200pc (GC South)および北 (GC North)の領域に SNRの10~100
個分のエネルギーを持つプラズマを発見した．

•• GC Northは様々な構造を持つ．

GC Southは~105yr前に過電離状態になった再結合プラズマ．

• 高階電離鉄輝線の起源は，暗く鉄輝線の強い未知のX線天体種族．本質的に拡がったプラズマ．

• 本質的に拡がったプラズマの場合，磁場閉じ込め可能性あり．

Thank you.