Suzaku perspective on the Galactic Center The 40

What is our Galactic Center ? Who resembles the Milky Way ? M 31

(1) X-ray Reflection Nebula Sgr B 2 M 0. 01 -0. 09 Sgr C

Foreground source (2) Sgr A East =Young SNR Thermal Plasma ( ~ 4 ke.

(3) Non Thermal Structrue Shell of SNR ? like SN 1006 or due to

Non Thermal X-ray Jets and filaments 3 2 1

ASCA Mapping with thw 3 -iron Lines Key Questions on the iron line Which

G 0. 570 -0. 018 Sgr B 2 Chandra 100 ksec other structure XISx

The East of Sgr A* 1 arcmin region spectra Chandra 50 ksec XISx 4

Hard Diffuse Component According to the latitudinal scanning observation of RXTE-PCA, the intensity of

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Suzaku perspective on the Galactic Center The “ 40 -ke. V Plasma” vs “ 10 -ke. V Plasma” What is the Origin of the 6. 7 ke. V-line Plasma ? Are the Galactic Center and Ridge emissions Same Origin ? Big bang of Sgr A* or Multi-SNe or ? (1) X-ray reflection Nebulae: Sgr B 2, Sgr C, M 0. 01 -0. 09 (2) Supernovae and SNRs: Sgr A East, G 359. 8 G 0. 570 (3) Non Thermal Jets, Filaments, and Shell

What is our Galactic Center ? Who resembles the Milky Way ? M 31 M 81 Milky Way 2 5 2 5 10 ke. V 6. 64 ke. V, EW=120 e. V Milky Way NGC 253 NGC 1068 2 10 6. 4 ke. V, EW=1200 e. V 6. 7 1430 e. V 6. 9 494 e. V 5 10 5 NGC 253: Pietsch et al. 2001, M 81: Page et al. 2004, M 31: Takahashi et al. 2004, NGC 1068: Matt et al. 2004 10

(1) X-ray Reflection Nebula Sgr B 2 M 0. 01 -0. 09 Sgr C Under Construction

(1’) Ｏｔｈｅｒ 6. 4 ke. V line Clump

Foreground source (2) Sgr A East =Young SNR Thermal Plasma ( ~ 4 ke. V) Kicked-off Neutron Star ? Park et al. 2005 Sgr A* Sakano et al. 2004 Sgr A East (age ~1000 year) Maeda et al. 2002

(3) Non Thermal Structrue Shell of SNR ? like SN 1006 or due to Nuclear Burst ? Sakano et al. 2003

Non Thermal X-ray Jets and filaments 3 2 1

ASCA Mapping with thw 3 -iron Lines Key Questions on the iron line Which line is cｌumpy ? Only 6. 4 ke. V line (XRN) ? How about 6. 7 and 6. 9 ke. V lines ? Are these intensities and the line ratio uniform ? Any non-thermal structure ? Suzaku Mapping of 6. 4, 6. 7 and 6. 9 ke. V line with a unit scale of ~5 arc-min.

G 0. 570 -0. 018 Sgr B 2 Chandra 100 ksec other structure XISx 4 100 ksec

The East of Sgr A* 1 arcmin region spectra Chandra 50 ksec XISx 4 100 ksec

Hard Diffuse Component According to the latitudinal scanning observation of RXTE-PCA, the intensity of diffuse emission at the Galactic center can be estimated.