  We present the results from our 140 ks XMM-Newton and 500 ks Chandra
observation of NGC 5548. The velocity structure of the X-ray absorber is
consistent with the velocity structure measured in the simultaneous UV spectra.
In the X-rays we can separate the highest outflow velocity component, -1040
km/s, from the other velocity components. This velocity component spans at
least three orders of magnitude in ionization parameter, producing both highly
ionized X-ray absorption lines (Mg XII, Si XIV) and UV absorption lines. A
similar conclusion is very probable for the other four velocity components. We
show that the lower ionized absorbers are not in pressure equilibrium with the
rest of the absorbers. Instead, a model with a continuous distribution of
column density versus ionization parameter gives an excellent fit to our data.
