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The Galactic Center Diffuse X-Rays Katsuji Koyama , Kyoto University

The Galactic Center Diffuse X-Rays Katsuji Koyama , Kyoto University. (1) FeXXV-Ka Line (6.7 keV) Diffuse or Point Sources ? How much is the fraction ? (2) FeI-Ka Line (6.4 keV) 3-D Distribution Time Variability. 0.0° 1.0° 2.0° 3.0°. Image. Divided to many

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The Galactic Center Diffuse X-Rays Katsuji Koyama , Kyoto University

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  1. The Galactic Center Diffuse X-Rays Katsuji Koyama , Kyoto University (1) FeXXV-Ka Line (6.7 keV) Diffuse or Point Sources ? How much is the fraction ? (2) FeI-Ka Line (6.4 keV) 3-D Distribution Time Variability

  2. 0.0° 1.0° 2.0° 3.0° Image Divided to many segments Fit the individual spectrum with a Power-law + Gaussians. Image Fluxes (F) F6.9 : 6.9 keV line F6.7 : 6.7 keV line

  3. F6.7: FeXXV-Ka l-distribution ~ 17exp(l/0.42) +exp(l/30) GRDX GCDX We have separatedthe GCDX and GRDX F6.9: FeXXVI-La

  4. b-distribution of F6.7 2 scale-heights in the GC Region Small=GCDX Large=GBDX ~ 7exp(b/0.16) +exp (b/1.2) We have separatedthe GCDX and GBDX 1) GCDX: Ellipse of +-(50pc, 20pc) 2) GBDX and GRDX Out side of the GC Region

  5. GCDX Divided 2 x 16 regions Fit the spectra with a Power-law + Gaussians. Gamma , Fluxes (F) and Equivalent width (EW) F5-10 : 5-10 keV band F6.4 , EW6.4 : 6.4 keV line F6.7 , EW6.7 : 6.7 keV line

  6. 100F6.7 About 2/3 (~1/1.5) of the 5-10 keV flux is associated to the 6.7 keV line and the other 1/3 (~0.5/1.5) is associated to the 6.4 keV line. 10F6.4 F6.7 + 0.5F6.4 F5-10

  7. 2 scale-heights of 6.7 keV line Image ~1/7 Point sources Revnivtsev Point Sources

  8. GBDX (A—G) & GRDX (1—5) Fit the spectra with a Power-law + Gaussians Fluxes (F) F5-10 : 5-10 keV band F6.4 : 6.4 keV line F6.7 : 6.7 keV line

  9. F6.7∝Fc F6.4 ∝ Fc

  10. F6.7+0.5F6.4 Deviation is found in the low flux side (GRDX and GBDX) Large fraction of the GRDX and GBDX is point sources ? In order to separate the 6.4 and 6.7 keV components , we need deep exposure off the GCDX.

  11. Time Variable l-distribution of the 6.4 keV lines Sgr A (Radio Arc)

  12. ~1keV ~5*1023

  13. Equivalent width and the origin X-ray origin electron origin Nobukawa: Nex Talk

  14. 3-D Cloud Positions： Face-onView (Ryu et al. 2009, PASJ 61 and this conference) Parabola x2+y2= (300-y)2 (Unit is light-year)

  15. 1994年 2004年 2000年 2005年 X-ray front

  16. Conclusions of the analysis of spatially divided X-ray spectra; 1 We have separated the GCDX, GRDX and GBDX. 2 We have determined 3-D distribution of the 6.4 keV line clumps. 3 Some of the 6.4 keV line clumps are time variable. The origin is X-ray reflection of a Past (~300 years) flare of Sgr A* with a time scale of ~10 years.

  17. Thank you for your attention

  18. Suzaku:180 ksec Best Spectrum of GC FeI FeXXV FeXXVI

  19. EW6.7+0.5EW6.4 = 600eV ~1 keV

  20. Blue: neutral Red: plasma Fe Mn S Ar Cr Ca Ni without S, Ar, Ca, Cr, Mn lines with S, Ar, Ca, Cr, Mn lines

  21. 4.0-6.0 keVband image Fe:EW=1 keV Fe:EW=0.2keV 10-3 2 0 χ -2 2 2 Energy(keV) Energy(keV) 5 5 10 10 Clump B Clump A

  22. Revnivtsev et al. 2009 b = -1.4 ° Muno et al. 2004 diffuse b = -0.0 ° point source

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