Our Galactic Center and its Environmemt K Koyama

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

Galactic Center Survey with Chandra 　　　　　　 Wang et al. 2002 Radio Arc & Center Sgr B 2 Sgr C ~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

ASCA Spectrum of the Large Scale Diffuse Emission of GC Koyama et al. 1996 Neutral Iron 3 3

ASCA mosaic Image of the Galactic Center Koyama et al. 1995 E ~1000 SNe > A few ke. V plasma 5 years Very Unbounded Active 　in 10 ~10 4 4

　　　　　 Sgr. B 2 with Chandara 　　　　6. 4 Ke. V map 　　　　　　Simulation 　　　　　Murakami et al 2001 . 5 Sgr A* X-rays

Chandra Sgr B 2 Spectrum Murakami et al. <= 6. 4 ke. V <= 7. 1 ke. V Edge X-Ray Reflection Nebula (XRN)

ASCA 6. 4　ke. V Image of Sgr C (XRN) X-Rays Sgr A*

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

X-Ray Spectrum & X-ray Image The 6. 4 ke. V 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

X-ray light curve of Sgr A* 　　　　Murakami（Ph. D)

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 　

Non-Thermal X-Ray　Filaments The 3 -8 ke. V band image with Chandra Senda et al. 3 2 1 Γ=2. 1 , NH = 8 x 1022 Hcm-2 X-ray Reflection Nebula 6. 4 ke. V 7. 1 ke. V Sgr A*

13 Jet 1 Jet 2 Non-thermal ? Jet 3 Jet 1 Γ=1. 5 , NH = 1. 2 x 1023 Hcm-2

14 X-Rays Ｖｓ Radio　 Contours For the origin of the non （６ｃｍ） -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.

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

The END