1. The Galactic Diffuse X-Rays and Time Variability of the 6.4-keV ClumpsGC
6.7 keV (He-like Fe)
6.4 keV (Neutral Fe)
2.5 keV (He-like S)
(2) X-ray
irradiation ?
(3) Multiple SNR
(1) ~7 keV Plasma
(4) 銀河中心の統一像へ

2. In preparation: 3—4 Papers. Finally, ~50 Refereed Papers
観測ピリオド 観測回数 総観測時間 (ks) PV
AO (20) (940)
AO (16) (800)
表１（右）
PV, AO1, AO2のGCの観測数と観測時間
表２（下）
GC観測から生まれたRefereed PaperのList
No タイトル（内容） 観測 雑誌 主著者
Line Diagnostics　of GCDX PV Sp Koyama
Spectrum of Sgr A East PV Sp Koyama
Hard X-Ray Emission the Arches Cluster PV Sp Tsujimoto
Diffuse Iron line of the Sgr B2 Region PV Sp Koyama
Peculiar Hot Star in the GC AO Sp Hyodo
A Time Variable X-Ray Echo of Sgr B2 PV Sp Koyama
Diffuse Hard X-ray from the GC AO SP Yuasa
New XRN and SNR in the Sgr B1 Region PV Sp Nobukawa
X-Ray Flare of A-type Star HD AO Sp Miura
SNR Candidate G AO Sp Mori
New X-ray views of the Galactic Center PV CJAA Koyama
X-Ray Observations of the GC PV AN Koyama
Variable Neutral Iron Line in Sgr B2 PV SP Inui
Spatial Distribution of the GCDX PV+AO1 Sp Koyama
New XRN with Large EW in Sgr C PV Sp61 Nakajima
SNR and Outflow in the Sgr C region PV Sp61 Tsuru
Suzaku Observations of Sgr D HII AO Sp Sawada
AXJ AO Sp61 Hyodo
　 SAX　J AO1　　- Sp Nobukawa
20 Iron lines form GR and GC PV Sp61 Yamauchi
An X-ray Super bubble PV+AO1 PASJ Mori
In preparation: 3—4 Papers.
Finally, ~50 Refereed Papers
will be appeared from
the GC Observations.

3. 6.7 keV line Plasma, if diffuse
T ~ 108 K
L2-10 ~ 2x1036ergs/s
Size ~ 50pc x 30pc
nave ~ 0.1cm-3
npeak ~ 0.4cm-3
Egas ~ 3x1052ergs
Escape Time scale: tesc = Size/Cs = 2x104yr
Heating Rate = Egas/tesc~5x1040ergs/s~10-3 SN yr -1
Very High !
(1) High SN rate ! Many SNRs in the GC
(2) Past Activities (Flares) of the Super massive black hole
Sgr A*
(eg. Koyama et al. 1996)

4. l-distribution b-distribution Point source Flux (4.8-8 keV)
The 6.7 keV line flux vs
Integrated point source flux
(Chandra deep exposure)
Near　GC ( |I| < 0.3 deg)
l-distribution b-distribution
Sgr A*
10 x 6.7 keV line (EW=0.5 keV)
Point source Flux (4.8-8 keV)
( ｂ)

5. The 6.7 and 6.96 keV lines in GC and GR 6.7 keV line : Point-sources:
Exponential
FWHM ~ 0.2 deg
Point-sources:
power-law
index = 0.9
(Infrared star numbers,
Chandra point sources)
Temperature
F6.96/F6.7 ~ (GC)
~ (GR)

6. 6.4keV Clump
=XRNの分布
Sgr B2
Sgr B1
New
Sgr C

7. 1994年
X-ray front
2000年
2004年
2005年

8. ＊
Sawada et al. 2004

9. Sgr B Cloud is in fornt of the GC Plasma

10. We found Many SNR Candidates (6 + 1+Sgr A East) Some are Likely Multi-SNe
~1keV
~3 keV

11. GCの統一像をめざして 100F6.7 10F6.4 F6.7 + 0.5F6.4 Power-law + Gaussian lines
Gamma, Fluxes (F) and
Equivalent width (EW)
Gamma :Power-law Index
F : 5-10 keV band
F6.4 , EW6.4 : 6.4 keV line
F6.7 , EW6.7 : 6.7 keV line
F F6.4
100F6.7
10F6.4
EW EW6.4 = Constant

12. 銀河中心の統一描像の樹立へ！ 「すざく」のLegacyを！
6.7keV lines
6.96/6.7 keV
Conclusion
Major fraction of the GCX is diffuse
~7 keV plasma
(2) We found Many SNR Candiates
(~ 1 keV temperature) in the GC.
(3) 6.4 keV line clumps are time variable,
hence is X-ray reflection Nebula
irradiated by the past outburst of Sgr A*
銀河中心の統一描像の樹立へ！　「すざく」のLegacyを！