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In this paper we analyze the X-ray, UV and optical data of the Seyfert 1.5galaxy 1H0419-577, with the aim of detecting and studying an ionized-gasoutflow. The source was observed simultaneously in the X-rays with XMM and inthe UV with HST-COS. Optical data were also acquired with the XMM OpticalMonitor. We detected a thin, lowly ionized warm absorber (log xi ~ 0.03, log NH~19.9 cm^-2) in the X-ray spectrum, consistent to be produced by the sameoutflow already detected in the UV. Provided the gas density estimated in theUV, the outflow is consistent to be located in the host galaxy, at ~ kpc scale.Narrow emission lines were detected in the X-rays, in the UV and also in theoptical spectrum. A single photoionized-gas model cannot account for all thenarrow lines emission, indicating that the narrow line region is probably astratified environment, differing in density and ionization. X-ray lines areunambiguously produced in a more highly ionized gas phase than the one emittingthe UV lines. The analysis suggests also that the X-ray emitter may be just adeeper portion of the same gas layer producing the UV lines. Optical lines areprobably produced in another, disconnected gas system. The different ionizationcondition, and the ~ pc scale location suggested by the line width for thenarrow lines emitters, argue against a connection between the warm absorber andthe narrow line region in this source.

Simultaneous XMM-Newton and HST-COS observation of 1H0419-577: the absorbing and emitting ionized gas