The Structure of the Soft X-ray Background in the Galactic Plane

Details The Structure of the Soft X-ray Background in the Galactic Plane The Structure of the Soft X-ray Background in the Galactic Plane

May 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...192.1803p&link_type=abstract

American Astronomical Society, 192nd AAS Meeting, #18.03; Bulletin of the American Astronomical Society, Vol. 30, p.844

Astronomy and Astrophysics

Astronomy

Scientific paper

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(deg) < l < 26(deg) ) is studied. In the 0.25 keV band, degree scale X-ray intensity variations are detected at +/-10% level about the mean. This intensity variation implies a contribution from a relatively thin emission region such as a clumpy boundary shell of the Local Hot Bubble to the observed 0.25 keV flux. In the 0.75 and 1.5 keV band, several shadows in the diffuse X-ray background cast by 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: existence of a Galactic X-ray bulge.

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