The structure of the soft x-ray background in the galactic plane
Abstract
With mosaics of the ROSAT PSPC pointed observations, the structure of the 0.1−2.0 keV soft X-ray background in the Galactic plane (0° < l < 26°) is studied. In the [special characters omitted] keV flux. In the [special characters omitted] and 1.5 keV band (0.5–2.0 keV), several shadows in the diffuse X-ray background cast by distant molecular clouds are detected. These shadows indicate that 15%–60% of the observed diffuse X-ray emission originates from behind 0.1–3 kpc from the Sun. These deep shadows imply a highly enhanced X-ray emitting region around the Galactic center: the existence of a Galactic X-ray bulge. The estimated temperature of the Galactic X-ray bulge is 106.6 K. The foreground X-ray emission (originating in front of the molecular clouds) appears to have a harder spectrum than the X-ray bulge.
Degree
Ph.D.
Advisors
Finley, Purdue University.
Subject Area
Astronomy|Astrophysics
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