Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996rftu.proc..335p&link_type=abstract
International Conference on X-ray Astronomy and Astrophysics: Röntgenstrahlung from the Universe, p. 335 - 336
Astronomy and Astrophysics
Astrophysics
X-Ray Background: Galactic Halo
Scientific paper
By analyzing ROSAT PSPC pointings and H I 21-cm line observations the authors investigate the soft X-ray background (SXRB) distribution towards (l,b) = (90°,60°). Comparing the SXRB intensity with the column density distribution of neutral absorbing matter they found evidence for a soft X-ray shadow. The soft X-ray radiation transport equation can be accurately solved by a two X-ray plasma component model which consists of a cooler plasma (T ≤ 106K) located between us and the bulk of the absorbing matter and a hotter plasma (T ≥ 106.2K) located beyond the neutral clouds casting the shadow. The authors use ROSAT spectra to check for absorbing column densities against observed H I column densities and find consistent numbers in the range NH I = (0.7-5.6)×1020cm-2. Fits of their two-component plasma model to the scatter diagrams of X-ray intensity versus NH I yield a foreground count rate of 5×10-4counts s-1arcmin-2 and an unabsorbed count rate of the distant plasma of about 9×10-4counts s-1arcmin-2. While the foreground count rate is typically for the Local Hot Bubble, the distant plasma is roughly 2.5 times fainter than detected at galactic latitudes of about 40°. This result indicates that the distant X-ray emission is not entirely produced by the superposition of extragalactic source because an intensity variation with galactic latitude is not expected. Thus, a significant fraction of the SXRB is caused by a hot plasma in the galactic halo.
Kerp Juergen
Mebold Ulrich
Pietz Jochen
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