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We present HST/COS observations of highly ionized absorption lines associatedwith a radio-loud QSO at $z=1.1319$. The absorption system has multiplevelocity components, tracing gas that is largely outflowing from the QSO atvelocities of a few 100 km s$^{-1}$. There is an unprecedented range inionization, with detections of HI, NIII, NIV, NV, OIV, OIV*, OV, OVI, NeVIII,MgX, SV and ArVIII. We estimate the total hydrogen number density from thecolumn density ratio N(OIV*)/N(OIV) to be$\log(n_{\textrm{H}}/\textrm{cm}^3)\sim 3$. Assuming photoionizationequilibrium, we derive a distance to the absorbing complex of $2.3<R<6.0$ kpcfrom the centre of the QSO. A range in ionization parameter, covering $\sim 2$orders of magnitude, suggest absorption path lengths in the range$10^{-4.5}<l_{\textrm{abs}}<1$ pc. In addition, the absorbing gas onlypartially covers the background emission from the QSO continuum, which suggestsclouds with transverse sizes $l_{\textrm{trans}}<10^{-2.5}$ pc. Widelydiffering absorption path lengths, combined with covering fractions less thanunity across all ions pose a challenge to models involving simple cloudgeometries. These issues may be mitigated by the presence of non-equilibriumeffects, together with the possibility of multiple gas temperatures. Thedynamics and expected lifetimes of the gas clouds suggest that they do notoriginate from close to the AGN, but are instead formed close to their observedlocation. Their inferred distance, outflow velocities and gas densities arebroadly consistent with scenarios involving gas entrainment or condensations inwinds driven by either supernovae, or the supermassive black hole accretiondisc. In the case of the latter, the present data most likely does not tracethe bulk of the outflow by mass, which could instead manifest itself as anaccompanying warm absorber, detectable in X-rays.

A compact, metal-rich, kpc-scale outflow in FBQS J0209-0438: Detailed diagnostics from HST/COS extreme UV observations