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
Contents
•The Suzaku Satellite•Galactic center region•Dark particle accelerators•SN1006•Cygnus Loop
The Suzaku SatelliteJapan 5th X-ray SatelliteLaunched July 10, 2005
God bird “Suzaku”from ancient
myths
InstrumentsXRT (X-Ray Telescope)
XIS (X-ray Imaging Spectrometers)
HXD (Hard X-ray Detector)
X-ray CCD x 4 (3FI + 1BI)
Low & stable background
Large Effective Area 255cm2x4
Wide range (10-600keV)Low background
Poster 18.24 Tsuru et al.
Poster 18.29 Kokubun et al.Poster 18.13 Mori et al.
XRT+XISBest for diffuse
and dim objects!
The Galactic Center RegionMany emission lines are detected for the first time!(neutral Ni Kα, He-like Ni Kα, He-like Fe Kγ etc.)
G.C. & SgrA east 5min
Galactic Center Image6.3-6.5 keV (Fe I Kα)
6.6-6.8 keV (He-like Fe Kα)
Cool Material ( ~ 10K)
What is the origin? Collisional excitation, or charge exchange?
Galactic center.
5min
Plasma DiagnosticCollisional excitation Charge exchange
r
f
i
fr
iHigh res. High res.Low res. (CCD) Low res. (CCD)
6666±5eV6680-6685eV
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. 2006 PASJ in print; astro-ph/0609215)
Dark Particle Accelerator?
HESSJ1616-508 HESSJ1804-216
HESS image in the TeV band
XIS FOV
Both are bright and diffuse TeV Objects
(Thanks to Prof. W. Hoffman and Prof. S. Funk)
XIS ImagesHESSJ1616
No counterpart!
Very dim & compact counterpart?3-12 keV
HESSJ1808 Center of HESSJ1808
2-10 keV
Fx(2-10keV)<3.1e-13erg/s/cm2
1: Fx(2-10keV)=2e-13erg/s/cm2
2: Fx(2-10keV)=4e-13erg/s/cm2
1
2
Target FTeV/FX
HESSJ1616 >55
HESSJ1804 ~10
Crab (PWN) 3e-3
RXJ1713 (SNR) ~0.06
We see hadronic process?
Real Dark Accelerator!
Matsumoto et al. 2006 PASJ in print; astro-ph/0608475Bamba et al. 2006 PASJ in print; astro-ph/0608310
SN1006O-band image
FIBI
ONe
Mg Si
SAr
Ca Fe
First detection of emission lines from S, Ar, Ca, Fe!
Center energy of Fe: 6.43 keV low nt ( ~ 109cm-
3s) plasma
Cygnus Loop
ROSAT HRI
XIS FOV
First detection of C & N lines!
C dominant (C : N : O ~ 5 : 2: 1) He burning origin (massive star)?
log
linear
XIS BI spectrum
(Miyata et al. 2006 PASJ in print)
Summary
1. Suzaku XRT+XIS is the best combination for studying diffuse emission.
2. The origin of He-like Fe Kα 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.
You can see many other results from Suzaku !
Distributed at the booth and other places.
Get CD-ROM!
Kyoto, Japan, Dec. 4 – 8, 2006
We still accept your registration.(Sorry, the call for papers had been closed.)
The Extreme Universe in the Suzaku Era
http://www-cr.scphys.kyoto-u.ac.jp/conference/suzaku2006/
Over 300 participants.~ 90 talks will be given.
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