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The Suzaku Results of the Galactic Center X-rays

The Suzaku Results of the Galactic Center X-rays - Collisinal Excitation or Charge Exchange ? - Katusji Koyama, Kyoto University. ASTROE2 Launch: 2005/7/10. Nickname Suzaku An Ancient Oriental mythology. ３ Main Instrumnets on Suzaku ：　 HXD, XRS, XIS. 1s2p 1 P 1.

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The Suzaku Results of the Galactic Center X-rays

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  1. The Suzaku Results of the Galactic Center X-rays - Collisinal Excitation or Charge Exchange ? - Katusji Koyama, Kyoto University ASTROE2 Launch: 2005/7/10 Nickname Suzaku An Ancient Oriental mythology

  2. ３ Main Instrumnets on Suzaku：　HXD, XRS, XIS

  3. 1s2p1P1 1s2p3P0,1,2 Resonance (r) 6.703keV 1s2s 3S1 Δl=1,Δs=0 Forbidden(f) 6.639keV Δl=0,Δs=1 1s21S0 Fine Structure of Fe24+ The XRS Spectrum on Orbit • 60 mK, 7.0 eV @5.9 keV: • World (Universe) Records. But! Name TransitionEnergy (eV) --------------------------------------------------------- Resonance (r)1s2s１S0-1s2p 1P16700.5 Intercombination line (x) 1s2p1S0-1s2p 3P26682.4 (y)1s2p1S0-1s2p 3P016667.6 Forbidden line (f)1s2 1S0-1s2s 3S16636.7

  4. ASCA320 ksec (Koyama et al. 1996) Suzaku:180 ksec S XV Kβ S XVI Kα S XV Kα Si XIII Kβ Si XIV Kα Si XIII Kα Chandra600ksec (Muno et al.2004) XMM 50 ksec (Tanaka) XIS: The Best Performance as an X-ray CCD

  5. S14+Kα Si12+Kα Ar16+Kα Ca18+Kα Si13+Kα S15+Kα Ar16+Kβ S14+Kβ Ca19+Kα Si12+Kβ Ar17+Kα FeKα Fe24+Kα Ni26+Kα Fe25+Kα Ni27+Kα FeKβ Is the 6.7 keV line Collisional Excitation or Charge Exchange ? Fe24+Kβ Fe25+Kβ Ni Kα 6 7 8 6.4 keV 6.7 keV 2.46 keV

  6. 6685eV Name Observed Lab ⊿ (eV) ----------------------------- S Lya 2622.4+3.6-2.7 2621.6 0.8 FeLya 6969.5+2.8-2.1 6965.7 3.8 Mn Ka 5899.6+1.7-0.4 5895.1 4.5 He-like Fe Ka = 6679 eV Close to 6685eV(d =6eV) Width (s) = 38 eV (Triplet, not Velocity) Collisional Excitation Electron Capture = 6666eV Collisional Excitation= 6685 eV f r i r i f l l 6666eV Wargelin, Beiersdorfer et al. 2005, ApJ, 634,687 FeXXV FeXXIV G-ratio = r / (i+f)

  7. Ec= 6679 eV +/- 1 eV ( systematic error~ +- 5 eV): TheG-ratio decreases as decreasing plasma temperature. It also decreases with temperature due to the contribution of satellite line. Thus we can constrain the plasma temperature kT using the center energy. The results are: kT = 3.2 keV +3 -1 keV　（Vapec) kT = 7.5keV +∞ -3keV　（VMEKAL) This is just the XRS science, hence our GC study make more clear strategy for the NeXT, the corner stone project in Japan.

  8. Ionization Temperature Fe Ka H-like/He-like: kTi=6.5 keV +/- 0.1keV Fe Kb H-like/He-like: kTi=5.1 keV + 1.5 -1.0 keV Ni Ka H-like/He-like : kTi= 9.3 keV +1.6 -2.5 keV Electron Temperature He-like Fe Kb/Ka : kTe=6.2 keV +3 -1keV H-like Fe Kb/Ka: kTe> 6.5 keV (lower limiｔ) All the results are consitent if the Plasma is kTi ~ kTe=6.5 keV. This methodology to determine the electron temperature (kTe) at the Fe energy is possible only with Suzaku. Our new method constrains the Continuum shape, hence can separate the Non-thermal components.

  9. Temperatures are • nearly Constant at • l=-0.4～+0.1 deg , • while decrease • at the 6.4 keV Cloud • 6.7 keV Flux is smooth over the • GC Region • GC Background can be reliably estimated Sgr A East

  10. New SNR Sgr A East CEI NEI Ec=6663 (6661-6664) eV (6685 eV) Width= 47 (44-51) eV 2-temperature CEI Model kTH = 4.9 keV kTL = 1.2 keV NEI Model kTH = 13 keV kTL = 1.2keV nt = 2x1010sec May be Multi-temperature NEI

  11. The West of the Radio Arc We found not only neutral Fe Ka but also Fe Kb and Ni Ka Ni Ka Neutral Fe (Fluorescence) Neutral Ni(Fluorescence) He/H-like Fe (GC-plasma: BG) Fe Ka, Kb

  12. 6.7 keV , 2.46 keV Line Map • Discovery of New SNR Candidates • Related to the GC plasma ? • Cosmic Ray Acceleration ? • 6.4keV Line Map • Discovery of New XRNs • Past History of the Sgr A* Activity (Echo)？ • Related to the HEESS-TeV Emission ?

  13. New Sourcesin the Sgr B & C Regions 6.4 keV 2.46keV 6.7 keV

  14. The Galactic Center Observed with Suzaku 6.70keV-Map 2.46keV-Map Sgr A* 6.40keV-MaP １０８K Plasma 　 １０７K Plasma ● Black Hole Molecular Cloud 30 pc

  15. 明月記 客星出現例 一條院寛弘三年四月二日 葵酉 夜以降騎官中有大客星 朱雀 飛鳥時代のキトラ 古墳の壁画 Suzaku The wall painting of “Suzaku” in the ancient tomb “Kitora” built in the Asuka Era Meigetsuki :Records of guest stars In the 1-st May 1006, a large guest star appeared within the Kikan (Lupus) Constellation

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