1. X-rays from the Galactic Center
2-10 keV
Iron K-shell Line Flux

2. The Galactic Center X-Rays: Connection withTeV Emissions
Si13+Kα
S14+Kα
Ar16+Kα
Fe Kα
Fe24+Kα
Ca18+Kα
Si12+Kα
S15+Kα
Fe25+Kα
Ni26+Kα
S14+Kβ
Ar16+Kβ
Si12+Kβ
Ni27+Kα
Ar17+Kα
Ca19+Kα
Fe　Kβ
Fe24+Kβ
Fe25+Kβ
Ni Kα
Energy 6 7
K-shell ｌines
from neutral
atoms
K-shell ｌine
from highly
ionized atoms 8
6.7 keV (He-like Fe)
6.4 keV (Neutral Fe)
2.5 keV (He-like S)
(1) ~7 keV Plasma
(2) Outburst of Sgr A*
(3) Multiple SNR
(4) Non-Thermal Filaments and/or PWNe

3. 6.7 keV line Plasma if diffuse
kT ~ 7 keV (F6.95/F6.7)
L2-10 ~ 2x1036erg/s
Size ~ 50pc x 30pc
nave ~ 0.1cm-3
npeak ~ 0.4cm-3
Egas ~ 3x1052ergs
if diffuse
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)
(1) ~7 keV Diffuse Plasma
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 the GC and GP 6.7 keV line :
Exponential
FWHM ~ 0.2 deg
6.7keV lines
Point-sources:
power-law
index = 0.9
(Infrared star numbers,
Chandra point sources)
6.96/6.7 keV
Temperature
F6.96/F6.7 ~ (GC)
~ (GR)

6. 6.4keV Clump =XRN (2) Outburst of Sgr A* Sgr B2 Sgr B1 New Sgr C Radio
continuum
Sgr B2
Sgr B1
New
Sgr C

7. The Sgr B2 Cloud This flux change can not be explained by electrons.
Variability time
scale of the 6.4
keV flux ~ ys
(Inui et al. 2008)
M 0.66
G 0.570
~10pc
This flux change
can not be
explained by
electrons.
We need X-ray
irradiation.
Where is the
X-ray source ?

8. 1994年
X-ray front
10 ly
2000年
2004年
2005年

9. 2ay=x2 - a2: a = 300 light-yr: by Sgr B2 obs.＊
Sawada et al. 2004
2ay=x2 - a2: a = 300 light-yr: by Sgr B2 obs.

10. Sgr B Cloud is in font of the GC Plasma
sensitive for NH~1023

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

12. 4) Non-thermal shells and/or PWNe Near the GC
Contour:
Non-thermal
X-rays
Colar Image:
Radio
continuum
Large Filaments
G (Lu et al. 2003) G G
(Sakano et al. 2002)

13. Non-Thermal Emission of Cas A
Extapolation of the power-law to 9—11 keV
helser & Vink 2008

14. Jet 1
Jet 2
Jet 3 13

15. Conclusion Major fraction of the GCX is diffuse of ~7 keV plasma
(2) 6.4 keV line clumps are time variable,
hence the most probable origin is
the reflection/fluorescence of the Sgr A*
X-ray in an outburst of ~ AD 1700.
(3) Many SNR Candidates are found in the
GC. The plasma temperatures are 1—3 keV.
(4) Most of the Non-thermal clumps are due to
Sgr A East & Sgr A*. Some are associated to
the radio filamnets.

16. Future observations to search for Possible
Connection with the HESS TeV Emission:
(1) Spectral study of the non-thermal emissions
(2) Observations on the HESS soureces