Spatial Distribution of the Galactic Center Diffuse X-Rays and the Spectra of the Brightest 6.4keV Clumps

Details Spatial Distribution of the Galactic Center Diffuse X-Rays and the Spectra of the Brightest 6.4keV Clumps Spatial Distribution of the Galactic Center Diffuse X-Rays and the Spectra of the Brightest 6.4keV Clumps

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009pasj...61s.255k&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.61, No.SP1, pp.S255--S262

Astronomy and Astrophysics

Astronomy

19

Galaxy: Center, Ism: Supernova Remnants, X-Ray Spectra

Scientific paper

The high energy resolution and low background, particularly in the hard X-ray band, of the X-ray Imaging Spectrometer onboard Suzaku provide excellent spectra of the Galactic center diffuse X-rays (GCDX). This paper reports on the results of spatially resolved spectroscopy of the GCDX. The most pronounced features of the GCDX are the K-shell transition lines from neutral (FeI) and He-like (FeXXV) irons at energies of 6.4keV and 6.7keV, respectively. The fluxes of these lines are non-uniformly and asymmetrically distributed with respect to Sgr A*. The 6.4keV lines are particularly bright on the positive side of the Galactic longitude (east-side) with clumpy structures. A bright clump near the GC exhibits a time variability over a timescale of a few years. Neither the 6.4keV nor 6.7keV line flux shows close proportionality to the continuum flux (5--10keV band); the 6.4keV line shows excess on the high flux side, and vice versa for the 6.7keV line. On the other hand, the sum of the 6.4keV plus 6.7keV line fluxes with a ratio of 1:2 shows good proportionality to the continuum flux, and hence we phenomenologically decomposed the continuum flux of the GCDX into the 6.4keV- and 6.7keV-associated continuums with a flux ratio of 1:2. Based on these facts, we have tried to estimate the contribution of diffuse and integrated flux of point sources to the GCDX.

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