  We have developed a new X-ray absorption model, called {\tt IONeq}, which
computes the optical depth $\tau(E)$ simultaneously for ions of all abundant
elements, assuming ionization equilibrium and taking into account turbulent
broadening. We use this model to analyze the interstellar medium (ISM)
absorption features in the Milky Way for a sample of 18 galactic (LMXBs) and 42
extragalactic sources (mainly Blazars). The absorbing ISM was modeled as a
combination of three components/phases - neutral ($T\lesssim1\times10^{4}$ K),
warm ($T\sim5\times 10^{4}$ K) and hot ($T\sim2\times10^{6}$ K). We found that
the spatial distribution of both, neutral and warm components, are difficult to
describe using smooth profiles due to nonuniform distribution of the column
densities over the sky. For the hot phase we used a combination of a flattened
disk and a halo, finding comparable column densities for both spatial
components, in the order of $\sim 6-7\times10^{18}\;{\rm cm^{-2}}$, although
this conclusion depends on the adopted parametrization. If the halo component
has sub-solar abundance $Z$, then the column density has be scaled up by a
factor $\frac{Z_\odot}{Z}$. The vertically integrated column densities of the
disk components suggests the following mass fractions for these three ISM
phases in the Galactic disk: neutral $\sim~89\%$, warm $\sim 8\%$ and hot $\sim
3\%$ components, respectively. The constraints on the radial distribution of
the halo component of the hot component are weak.
