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We re-analyzed the 9 observations performed on 2006 by XMM-Newton and Chandrain the 0.3 to 10 keV energy band of NGC 3516 (Seyfert 1.5). The best fit modelof these observations consists of a continuum emission absorbed by four ionizedcomponents and ten narrow emission lines. Three ionized absorbing componentsproduce features in the soft X-ray band. The fourth ionization componentproduces FeXXV-XXVI in the hard- energy band. We study the absorbers timeresponse to well detect changes in the X-ray luminosity of this source, onlytwo components show clear opacity changes consistent with gas close tophotoionization equilibrium. The other two components do not seem to respond tocontinuum variations. This response time allows us to constrain their location.One outflowing component must be located within the obscuring torus, at adistance 2.7X10^17 cm from the central engine, likely originated in theaccretion disk. The three remaining outflowing components are at distanceslarger than 10^{16-17} cm. Two of them have similar outflow velocities andlocations, these may be in pressure equilibrium, forming a multi-phase medium,if the gas has metallicity larger than the solar one (5 times). We find nocorrelation between the change in covering factor of the absorbers and the fluxof the source. This, in connection with the observed variability of the ionizedabsorbers, suggests that the changes in flux are not produced by this material.If the variations are indeed produced by obscuring clumps of gas, these must belocated much closer in to the central source.

A detailed analysis of the high resolution X-ray spectra of NGC 3516: Variability of the ionized absorbers