1. Our Galactic Center and its Environmemt K. Koyama A. Senda
Our Galactic Center and its Environmemt K. Koyama A. Senda 　　　　　　　 Kyoto University 　　　　　　H. Murakami ISAS / JAXA
Nijyo Castle？ 1

2. Galactic Center Survey with Chandra Wang et al. 2002
Radio Arc & Center
Sgr B2
Sgr C まま
~2 x 1 degrees
1 X-ray Reflection Nebula -> Recent Activity of Sgr A*
2 X-ray Jets from Sgr A* -> Recent Activity of Sgr A*
3 Non-Thermal Filaments -> Recent Activity of the GC 2 2

3. ASCA Spectrum of the Large Scale Diffuse Emission of GC Koyama et al
Neutral Iron 3 3

4. ASCA mosaic Image of the Galactic Center
Koyama et al. 1995
E ~1000SNe
Very Active 　in 105 years
> A few keV plasma
Unbounded ~105 years 4 4

5. SgrB2 with Chandara 6.4 KeV map Simulation Murakami et al 2001.
X-rays
Sgr A* 5

6. Chandra Sgr B2 Spectrum Murakami et al.
<= 6.4 keV
<= 7.1 keV Edge
X-Ray Reflection Nebula (XRN) 6

7. ASCA 6.4　keV Image of Sgr C (XRN)
X-Rays
Sgr A* 7

8. Radio Arc Image of 6. 4 keV (with Chandra) (CS vs 6
Radio Arc Image of 6.4 keV (with Chandra)　 　(CS vs 6.4 keV line)　　　　　　　　　　 　Murakami et　al　　　　
X-Rays From Sgr A* 8

9. X-Ray Spectrum & X-ray Image
The 6.4 keV line is fluorescence by strong X-rays
from the　direction of the Galactic Center Sgr A*.
We need a strong X-ray source at the GC.
But no strong X-ray source is found !
Sgr A* was bright in the past of light traveling time
between Sgr A* and XRN.
 X-ray Echo
Ya hoh 9

10. X-ray light curve of Sgr A* Murakami（PhD)10

11. New Aspects of the GC Regions
(1) 　X-Ray Jetｓ From Sgr A*
（2）　Non Thermal X-Ray Filaments　
(In Strong　Magnetic Field)
　=>　Recent High Energy Activity and Particle Acceleration near the GC 11

12. Non-Thermal X-Ray Filaments
The 3-8 keV band image with Chandra Senda et al. 1 2 3
Γ=2.1 , NH = 8 x1022 Hcm-2
X-ray Reflection Nebula
6.4 keV
7.1 keV
Sgr A*

13. Non-thermal ? Jet Γ=1.5 , NH = 1.2 x1023 Hcm-2 13 Jet1 Jet 1 Jet 2

14. X-Rays Radio Contours For the origin of the nonＶｓ
Radio　
Contours
（６ｃｍ）
For the origin of the non
-thermal X-ray filaments
and X-ray jets, we need more
study. However, we can
safely say that these must
be closely related to the past
high energy activities of the GC. 14

15. Distribution of High Energy Cosmic Rays (> 1019 eV)
From ICRR Home Page
Are the non-thermal X-ray
filaments and Jets the origin
of high energy cosmic rays ?
No Data

16. The END
Thank You