Context : AGN outflows are thought to influence the evolution of their host galaxies and their super massive black holes .
To better understand these outflows , we executed a deep multiwavelength campaign on NGC 7469 .
The resulting data , combined with those of earlier epochs , allowed us to construct a comprehensive physical , spatial , and temporal picture for this AGN wind .

Aims : Our aim is to determine the distance of the UV outflow components from the central source , their abundances and total column-density , and the mechanism responsible for their observed absorption variability .

Methods : We studied the UV spectra acquired during the campaign as well as from three previous epochs ( 2002-2010 ) .
Our main analysis tools are ionic column-density extraction techniques and photoionization models ( both equilibrium and time-dependent models ) based on the code Cloudy .

Results : For component 1 ( at –600 km s ^ { -1 } ) our findings include the following : metallicity that is roughly twice solar ; a simple model based on a fixed total column-density absorber , reacting to changes in ionizing illumination that matches the different ionic column densities derived from four spectroscopic epochs spanning 13 years ; and a distance of R= 6 ^ { +2.5 } _ { -1.5 } pc from the central source .
Component 2 ( at –1430 km s ^ { -1 } ) has shallow troughs and is at a much larger R .
For component 3 ( at –1880 km s ^ { -1 } ) our findings include : a similar metallicity to component 1 ; a photoionization-based model can explain the major features of its complicated absorption trough variability and an upper limit of 60 or 150 pc on R .
This upper limit is consistent and complementary to the X-ray derived lower limit of 12 or 31 pc for R .
The total column density of the UV phase is roughly 1 % and 0.1 % of the lower and upper ionization components of the warm absorber , respectively .

Conclusions : The NGC 7469 outflow shows super-solar metallicity similar to the outflow in Mrk 279 , carbon and nitrogen are twice and four times more abundant than their solar values , respectively .
Similar to the NGC 5548 case , a simple model can explain the physical characteristics and the variability observed in the outflow .