In this paper we analyze the X-ray , UV and optical data of the Seyfert 1.5 galaxy 1H0419-577 , with the aim of detecting and studying an ionized-gas outflow .
The source was observed simultaneously in the X-rays with XMM- Newton and in the UV with HST-COS. Optical data were also acquired with the XMM- Newton Optical Monitor .
We detected a thin , lowly ionized warm absorber ( \log \xi \approx 0.03 , \log \hbox { $N { { } _ { H } } $ } \approx 19.9 cm ^ { -2 } ) in the X-ray spectrum , consistent to be produced by the same outflow already detected in the UV .
Provided the gas density estimated in the UV , the outflow is consistent to be located in the host galaxy , at \approx kpc scale .
Narrow emission lines were detected in the X-rays , in the UV and also in the optical spectrum .
A single photoionized-gas model can not account for all the narrow lines emission , indicating that the narrow line region is probably a stratified environment , differing in density and ionization .
X-ray lines are unambiguously produced in a more highly ionized gas phase than the one emitting the UV lines .
The analysis suggests also that the X-ray emitter may be just a deeper portion of the same gas layer producing the UV lines .
Optical lines are probably produced in another , disconnected gas system .
The different ionization condition , and the \approx pc scale location suggested by the line width for the narrow lines emitters , argue against a connection between the warm absorber and the narrow line region in this source .