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 ^ { -1 } , 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 .