1. Suzaku First Results on Galactic Diffuse Objects
Hironori Matsumoto (Kyoto Univ., Japan)
and
The Suzaku team

2. Contents The Suzaku Satellite Galactic center region
Dark particle accelerators
SN1006
Cygnus Loop

3. The Suzaku Satellite Japan 5th X-ray Satellite Launched July 10, 2005
God bird “Suzaku”
from ancient myths

4. Best for diffuse and dim objects!
Instruments
XRT (X-Ray Telescope)
HXD (Hard X-ray Detector)
Wide range
(10-600keV)
Low background
Large Effective Area
255cm2x4
Poster 18.29
Kokubun et al.
Poster Mori et al.
XIS (X-ray Imaging Spectrometers)
X-ray CCD x 4
(3FI + 1BI)
Low & stable background
XRT+XIS
Best for diffuse and dim objects!
Poster Tsuru et al.

5. The Galactic Center Region
Many emission lines are detected for the first time!
(neutral Ni Kα, He-like Ni Kα, He-like Fe Kγ etc.)
5min
G.C. & SgrA east

6. Galactic Center Image 5min Galactic center.
keV (Fe I Kα)
5min
Cool Material (～10K)
Galactic center.
keV (He-like Fe Kα)
What is the origin? Collisional excitation, or charge exchange?

7. Plasma Diagnostic Collisional excitation Charge exchange r f i
High res.
Low res. (CCD)
6666±5eV eV
Suzaku XIS: He-like Fe Kα center 6680±1eV(stat.)±4eV(syst.)
The line center observed with Suzaku favors the collisional excitation = hot plasma (108K)
(See Koyama et al PASJ in print; astro-ph/ )

8. Dark Particle Accelerator?
HESS image in the TeV band
HESSJ
HESSJ
XIS FOV
(Thanks to Prof. W. Hoffman and Prof. S. Funk)
Both are bright and diffuse TeV Objects

9. XIS Images No counterpart! HESSJ1616 HESSJ1808 2 1
Center of HESSJ1808
2-10 keV 2 1
3-12 keV
Very dim & compact counterpart?
1: Fx(2-10keV)=2e-13erg/s/cm2
No counterpart!
2: Fx(2-10keV)=4e-13erg/s/cm2
Fx(2-10keV)<3.1e-13erg/s/cm2

10. Real Dark Accelerator! Target FTeV/FX HESSJ1616 >55 HESSJ1804 ~10
Crab (PWN)
3e-3
RXJ1713 (SNR)
~0.06
We see hadronic process?
Matsumoto et al PASJ in print; astro-ph/
Bamba et al PASJ in print; astro-ph/

11. SN1006 O-band image FI Mg Si BI O S Ne Ar Ca Fe
First detection of emission lines from S, Ar, Ca, Fe!
Center energy of Fe: 6.43 keV  low nt (～109cm-3s) plasma

12. Cygnus Loop XIS BI spectrum First detection of C & N lines!
XIS FOV
log
linear
ROSAT HRI
First detection of C & N lines!
(Miyata et al PASJ in print)
C dominant (C : N : O ～ 5 : 2: 1)
 He burning origin (massive star)?

13. Summary
Suzaku XRT+XIS is the best combination for studying diffuse emission.
The origin of He-like Fe Kα emission at the Galactic center is the collisional excitation (i.e. hot gas).
Real dark particle accelerators are discovered.
First detection of S, Ar, Ca, and Fe lines from SN1006.
We found C and N lines from the Cygnus Loop.

14. Get CD-ROM! You can see many other results from Suzaku !
Distributed at the booth and other places.

15. The Extreme Universe in the Suzaku Era Kyoto, Japan, Dec. 4 – 8, 2006
Over 300 participants.
～90 talks will be given.
We still accept your registration.
(Sorry, the call for papers had been closed.)