The hot phase of the ISM

Abstract

In this thesis I present a quantitative solution of the soft X-ray radiation transfer through the Galactic interstellar medium. I focus on the Galactic Halo emission because its intensity distribution is thought to trace the shape of the Milky Way's Dark Matter gravitational potential. The best fit model for the soft X-ray background allows to identify areas in the sky which deviate significantly from the this solution. These areas are associated with high-velocity cloud (HVC) complexes or possibly with the warm/hot intergalactic medium. Moreover, it is feasible to estimate lower distance limits to the HVC complexes.