Spatial Distribution of the Galactic Diffuse X-Rays and the Spectral/Timing Study of the 6.4-keV Clumps Katsuji Koyama Department of Physics, Graduate.

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Presentation transcript:

Spatial Distribution of the Galactic Diffuse X-Rays and the Spectral/Timing Study of the 6.4-keV Clumps Katsuji Koyama Department of Physics, Graduate school of Science, Kyoto University, Sakyo-ku, Kyoto Talk by T. Tsuru Posters B40, 44, 45

Suzaku X-ray Maps along the Galactic Center and Ridge (GC, GR) Origin of the 6.4 (Neutral Fe) 6.7 (He-like Fe) 6.96 (H-like Fe) - keV lines and Continuum flux 6.4 keV (Neutral Fe) 6.7 keV (He-like Fe) keV Diffuse ? or Integrated point sources ?

The Galactic Center X-Rays (GCX) map near Sgr A* East West Red: 6.7 keV (He-like Fe) Blue:6.4 keV (Neutral Fe) Green: 2.45 keV(He-like S) GC East-West asymmetry of the Flux and Spectrum

( ｂ ) The 6.7 keV line flux vs Integrated point source flux (Chandra deep exposure) Near GC ( |I| < 0.3 deg) l-distribution b-distribution Point source Flux (4.8-8 keV) 10 x 6.7 keV line (EW=0.5 keV) Sgr A*

The 6.7 and 6.96 keV lines in GC and GR 6.7 keV line : Exponential HWHM ~ 0.2 deg Temperature F 6.96 /F 6.7 ~ (GC) ~ (GR) 6.7keV lines 6.96/6.7 keV Point-sources: power-law index = 0.9 (Infrared star numbers, Chandra point sources)

Gamma is constant (~1.9) (independent of F 6.4 /F 6.7 ) F 6.4 /F 6.7 vs Gamma F 6.4 /F 6.7 Gamma Made 2 x 16 spectra and fit with a model of Power-law + Gaussian lines. Gamma, Fluxes (F) and Equivalent width (EW) F 5-10 : 5-10 keV band F 6.4, EW 6.4 : 6.4 keV line F 6.7, EW 6.7 : 6.7 keV line Keep this fact in your mind

EW EW 6.4 = Constant F 5-10 F F F F 6.4 Phenomenologically, about 2/3 (~1/1.57) 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.

F 5-10 ~ 2* 6.7 keV line + 1*6.4 keV line Gamma ~1.9 （ independent of F 6.4 /F 6.7 ) kT=6.5 keV gamma= keV Plasma (gamma ~ 2.4) = Power law (gamma ~ 1.4) F 6.4 ~ F keV plasma (gamma= 2.4) 6.7 Cont (gamma= 1.9) 6.4 Cont (gamma= 1.9) Power-law (gamma= 1.4) Point (gamma= 0.9) (2x )/3 = 1.9

diffuse point source Chandra (Muno et al.2004) 6.7keV 6.4keV Point Source Contribution Strong 6.7 keV line, ~ 1/6 of total (Minimum ) Gamma=0.9 Point source spectrum has an EW 6.7 ~ 0.4 keV, and EW 6.4 ~ 0.1 keV. < 20% of GCX Gamma=0.9 1/6

Point source spectrum (CV) has, and (Ezuka et al. 2002) Point source spectrum (GC) has EW 6.4 ~ 0.1 keV, and EW 6.7 ~ 0.4 keV. (Muno et al. 2004) EW 6.7 EW 6.4 Magnetic CVs If diffuse source has EW 6.7 ~ 1 keV (7 keV, 2-solar = Sgr A East SNR ). Then point source is ~ 2/3 of total (Maximum) Point source spectrum must have Gamma ~1.9 inconsistent with ~0.9 (Chandra, Muno et al.) Point sources EW 6.4 ~ keV EW 6. ７ ~ keV

Chandra (2002)Suzaku (2005) keV line * (10 -5 photons s -1 cm -2 ) * 4.7 sigma variability 6.4 keV Line is time variable. A Clump near Sgr A* Chandra (2002)Suzaku (2005) Sgr A* (1.5 sigma for the 6.7 keV line)

Half-decay life of the 6.4 keV flux ~15 ys ~10pc M 0.66G The Sgr B2 Cloud This flux change can not be explained by point sources

Conclusions of the analysis of spatially divided X-ray spectra; (1) Integrated flux of point sources contributes ~1/6 at least, but less than 2/3 of the total Galactic center X-rays (GCX). (2) Major fraction of the GCX is diffuse. (3) Plasma temperature of the GC is probably higher than that of the GR. (4) 6.4 keV line clumps are time variable, hence the origin is not point sources.