Suzaku First Results on Galactic Diffuse Objects

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Suzaku First Results on Galactic Diffuse Objects

• Hironori Matsumoto (Kyoto Univ., Japan)
• and
• The Suzaku team

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Contents

• The Suzaku Satellite
• Galactic center region
• Dark particle accelerators
• SN1006
• Cygnus Loop

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The Suzaku Satellite
Japan 5th X-ray Satellite Launched July 10, 2005
God bird Suzaku from ancient myths
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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 18.13 Mori et al.
XIS (X-ray Imaging Spectrometers)
X-ray CCD x 4 (3FI 1BI) Low stable background
XRTXIS Best for diffuse and dim objects!
Poster 18.24 Tsuru et al.
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The Galactic Center Region
Many emission lines are detected for the first
time! (neutral Ni Ka, He-like Ni Ka, He-like Fe
K? etc.)
5min
G.C. SgrA east
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Galactic Center Image
6.3-6.5 keV (Fe I Ka)
5min
Cool Material (10K)
Galactic center.
6.6-6.8 keV (He-like Fe Ka)
What is the origin? Collisional excitation, or
charge exchange?
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Plasma Diagnostic
Suzaku XIS He-like Fe Ka center
66801eV(stat.)4eV(syst.)
The line center observed with Suzaku favors the
collisional excitation hot plasma (108K)
(See Koyama et al. 2006 PASJ in print
astro-ph/0609215)
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Dark Particle Accelerator?
HESS image in the TeV band
HESSJ1616-508
HESSJ1804-216
XIS FOV
(Thanks to Prof. W. Hoffman and Prof. S. Funk)
Both are bright and diffuse TeV Objects
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XIS Images
HESSJ1616
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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)lt3.1e-13erg/s/cm2
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Real Dark Accelerator!
Target FTeV/FX
HESSJ1616 gt55
HESSJ1804 10
Crab (PWN) 3e-3
RXJ1713 (SNR) 0.06
We see hadronic process?
Matsumoto et al. 2006 PASJ in print
astro-ph/0608475 Bamba et al. 2006 PASJ in print
astro-ph/0608310
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SN1006
O-band image
FI
Mg
BI
Si
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
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Cygnus Loop
XIS BI spectrum
XIS FOV
log
linear
ROSAT HRI
First detection of C N lines!
(Miyata et al. 2006 PASJ in print)
C dominant (C N O 5 2 1) ? He
burning origin (massive star)?
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Summary

1. Suzaku XRTXIS is the best combination for
   studying diffuse emission.
2. The origin of He-like Fe Ka emission at the
   Galactic center is the collisional excitation
   (i.e. hot gas).
3. Real dark particle accelerators are discovered.
4. First detection of S, Ar, Ca, and Fe lines from
   SN1006.
5. We found C and N lines from the Cygnus Loop.

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Get CD-ROM!
You can see many other results from Suzaku !
Distributed at the booth and other places.
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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.)
http//www-cr.scphys.kyoto-u.ac.jp/conference/suza
ku2006/