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S. Park (NASA/GSFC, USRA)
The diffuse X-ray background emission (DXB) near the Galactic plane (l, b ~ 25.6o, 0.78o) is observed with ASCA. The observed region is toward a Galactic molecular cloud which is recently reported to cast a deep ``X-ray shadow'' in the Galactic DXB in the 0.5 - 2.0 keV band. The selection of this particular region is intended to provide a useful constraint for the spatial distribution of the DXB emission along the line of sight: i.e., the molecular cloud is optically thick at <2 keV that the bulk of the soft X-rays must originate in the foreground of the cloud which is at ~3 kpc from the Sun. In the 0.8 - 9.0 keV band, the observed spectrum is primarily from thermal plasmas and K emission lines from He-like Si and Fe ions are detected. The detailed nature of the spectrum is however complicated and most likely comprised of multiple components of hot thermal plasmas. The preliminary results from the GIS data imply the existence of a hot plasma (T > 106.9 K) within ~ 3 kpc from the Sun.
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