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The Galactic X-ray Halo

Published online by Cambridge University Press:  12 April 2016

J. Pietz ,
J. Kerp ,
P.M.W. Kalberla ,
W.B. Burton ,
Dap Hartmann  and
U. Mebold
J. Pietz
Affiliation:
Radioastronomisches Institut der Universitaät Bonn, Germany
J. Kerp
Affiliation:
Radioastronomisches Institut der Universitaät Bonn, Germany
P.M.W. Kalberla
Affiliation:
Radioastronomisches Institut der Universitaät Bonn, Germany
W.B. Burton
Affiliation:
Sterrewacht Leiden, The Netherlands
Dap Hartmann
Affiliation:
Sterrewacht Leiden, The Netherlands Harvard-Smithsonian Center for Astrophysics, USA
U. Mebold
Affiliation:
Radioastronomisches Institut der Universitaät Bonn, Germany

Abstract

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We analyzed the soft X-ray background (SXRB) source intensity distribution of the ¾ keV and ¼ keV photons by correlating the public ROSAT PSPC All-Sky Survey data with the new Leiden/Dwingeloo HI Survey. We found that the ¾ keV and ¼ keV distant background source intensity distribution can be modelled by an isothermal (T = 1.5.106 K) disk-like (scale length A1 = 15 kpc) X-ray halo in addition to the radiation of the extragalactic X-ray background.

Type
Part VIII High-Velocity Clouds, Galactic Halo Models, Observations of the LMC
Information
International Astronomical Union Colloquium , Volume 166: The Local Bubble and Beyond , 1997 , pp. 471 - 474
Copyright
Copyright © Springer-Verlag 1998

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