Density and metallicity of the Milky-Way circumgalactic gas
  The halo of the Milky-Way circumgalactic gas extends up to the virial radius
of the Galaxy, ~250 kpc. The halo properties may be deduced from X-ray
spectroscopic observations and from studies of the ram-pressure stripping of
satellite dwarf galaxies. The former method is more precise but its results
depend crucially on the assumed metallicity of the circumgalactic gas; the
latter one does not need these assumptions. Here, the information from both
approaches is combined to constrain observationally the gas metallicity and
density as functions of the galactocentric distance. It is demonstrated that
the two kinds of data could be reconciled if the metallicity decreased to
Z~0.1Z_Sun in the outer parts of the extended halo. The corresponding gas
density profile is rather flat, falling as r^{-(0.45...0.75)} at large
galactocentric distances r.
