We present the results of a recent ( March 2011 ) 160 ks Chandra -LETGS observation of the Seyfert galaxy NGC 4593 , and the analysis of archival X-ray and UV spectra taken with XMM- Newton and HST/STIS in 2002 .
We find evidence of a multi-component warm absorber ( WA ) in the X-rays with four distinct ionisation degrees ( \log \xi = 1.0 , \log \xi = 1.7 , \log \xi = 2.4 , and \log \xi = 3.0 ) outflowing at several hundreds of km s ^ { -1 } .
In the UV we detect 15 kinematic components in the absorbers , blueshifted with respect to the systemic velocity of the source , ranging from -60 km s ^ { -1 } to -1520 km s ^ { -1 } .
Although the predicted C iv and N v column densities from the low-ionisation X-ray outflow are in agreement with those measured for some components in the STIS spectrum , there are kinematic discrepancies that may prevent both the X-ray and UV absorbers from originating in the same intervening gas .
We derive upper limits on the location of the absorbers finding that the high-ionisation gas lie within \sim 6 - 29 pc from the central ionising source , while the low-ionisation gas is located at several hundreds of pc .
This is consistent with our line of sight passing through different parts of a stratified wind .
The total kinetic energy of the outflows injected into the surroundings of the host galaxy only accounts for a tiny fraction of the bolometric luminosity of the source and it is therefore unlikely that they may cause a significant impact in the interstellar medium of NGC 4593 in a given single episode of activity .