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Suzaku First Results on Galactic Diffuse Objects

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 Satellite. Japan 5 th X-ray Satellite Launched July 10, 2005.

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Suzaku First Results on Galactic Diffuse Objects

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  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. 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 XRT+XIS Best for diffuse and dim objects! Poster 18.24 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 6.3-6.5 keV (Fe I Kα) 5min Cool Material (～10K) Galactic center. 6.6-6.8 keV (He-like Fe Kα) What is the origin? Collisional excitation, or charge exchange?

  7. Plasma Diagnostic Collisional excitation Charge exchange High res. High res. r Low res. (CCD) Low res. (CCD) i r f f i 6666±5eV 6680-6685eV 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)

  8. 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

  9. XIS Images HESSJ1808 Center of HESSJ1808 2-10 keV HESSJ1616 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! We see hadronic process? Matsumoto et al. 2006 PASJ in print; astro-ph/0608475 Bamba et al. 2006 PASJ in print; astro-ph/0608310

  11. 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

  12. 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)?

  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.) http://www-cr.scphys.kyoto-u.ac.jp/conference/suzaku2006/

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