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tokens: supported. The key features of each multiphase flow are summarized as follows. As rotation dominates over turbulent motions (Ta t v rot / v 1) in the massive galaxy, the condensation occurs along a conical helix, spinning up the gas which finally settles on to the equatorial region in a multiphase disc (Section 3 ). The disc is cylindrically stratified: the ionized (UV) gas envelops the neutral (optical/IR) layer which englobes the very thin molecular (radio) structure, dominating 95percent of the condensed mass. There is no major fragmentation observed, with the warm phase experiencing mild perturbations via pressure torques induced by condensation. The BHAR is suppressed by almost 2 dex compared with the cooling rate as most gas has found circularization. Accretion proceeds along a narrow polar funnel (10) or after reaching the inner equator through gas which condensed out of the plasma with low angular momentum. After 50Myr the disc has reached 1kpc extension. Extended molecular and warm discs with similar surface density have been observed in 1/3 of observed massive, typically quiescent, galaxies (Caon etal. 2000 ; Ocaa Flaquer etal. 2010 ; Young etal. 2011 ; Werner etal. 2014 ; Hamer etal. 2016 ). When rotation and turbulence are both inhibited, the hot plasma condenses radially, forming a compact multiphase cloud within the inner 100pc (Section 4 ). The inner multiphase density profiles are steep, following a free-fall slope ( r 3/2 within the SMBH influence region). The BHAR is almost identical to the cooling rate. Adiabatic, compressional heating inhibits the formation of the third molecular phase. The warm 8000K (optical/IR) gas dominates the condensed medium, albeit highly concentrated, with a very thin ionized UV layer. Similarly, a significant number of quiescent massive galaxies display a spherically symmetric warm H core (Caon etal. 2000 ; Werner etal. 2012 , 2014 ) and tend to lack cold gas, in particular when no AGN feedback or other major perturber are detected. In the more frequent, intermediate state the hot halo experiences both rotation and subsonic turbulent motions (160kms 1 ) leading to CCA (Section 5 ). The multiphase condensation occurs in the high density peaks via local runaway cooling. AGN heating prevents a global cooling inflow, facilitating the growth of multiphase structures. Initially, warm filaments condense out of the low-entropy plasma. The denser, perturbed regions further condense into molecular clouds, following a top-down rainfall. The CCA angular momentum transport is driven by pressure torques on 1kpc scale and dominated by chaotic inelastic collisions in the core (ram-pressure drag is secondary). The accretion rate can be modelled via quasi-spherical viscous accretion (Section 5.2 ), with an effective clump collisional viscosity c v c ; the mean free path is c 100pc with large scatter. The core cloud volume filling is a few per cent, rapidly declining beyond 1kpc. As ensemble, the multiphase clouds