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Galaxy evolution models require feedback from AGN to suppress star-formation in massive galaxies. However comma the mechanisms that enable AGN feedback to reach galactic scales are hotly debated. Two key models aredoublePoint (1) direct radiation pressure on dust and (2) ISM entrainment in hot winds. Measurements of the presence and properties of any hot wind component of AGN outflows thus represent a critical means of identifying dominant AGN feedback mechanisms. Sensitive and spatially resolved UV diagnostics from highly ionized emission go beyond differentiating AGN photoionized gas and shocks to serve as barometers that enable estimates of any hot wind pressure. These highly ionized UV line diagnostics (O VI-N V) were recently used to demonstrate that the dynamics of the UV emitting comma outflowing clouds from a prototypical superwind driven by a radio-quiet AGN are dominated by radiation pressure with negligible compression by a hot wind. These observations indicate that this AGN outflow is driven by radiation pressure or was driven by a hot wind that has since dissipated despite ongoing AGN activity. On the other hand comma AGN outflows driven along the jets of radio-loud systems are thought to be ISM entrained in a hot wind associated with the jets. To test this prediction comma we propose the first spatially resolved UV spectroscopy and complementary high-resolution VLA data of a known 5-30 kpc outflow of a recently rejuvenated radio-loud AGN. This will enable unique insights into the wind driving mechanisms comma the physical conditions-properties of the outflow comma and a detailed study of the jet and cool outflow morphology compared to a radio-quiet case.