Coordinated time variability of multi-phase ultra-fast outflows in J132216.25 + 052446.3

We present a time variability analysis of broad absorption lines (BAL; spread over the velocity range 5800-29000 km/s) seen in spectrum J132216.25+052446.3 (z(em)= 2.04806) at ten different epochs spanning 19 years. The strongest component (BAL-A; 5800-9900 is made up several narrow components having separations close to C IV doublet splitting. IV, N V, and Si from BAL-A show correlated optical depth without significant changes structure. A very shallow (BAL-C; 15000-29000 emerged during our monitoring period coinciding with dimming episode J1322+0524. All identified equivalent widths increasing decreasing flux. This together emission-line consistent ionization being main driver variability. observed UV-continuum variations are weaker than what required by photo-ionization models. scatter iv width given continuum flux can be understood if ionizing photons much larger that UV continuum, photon fluxes not and/or covering factor flow varies continuously. suggest produced stable clumpy outflow located beyond emission line region BAL-C newly formed wind near accretion disk both respond continuum.