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Fig. 11.
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Star formation rate in the nuclear region (left) and at galactic scale (right) for qcrE, qcrC, and qcrNoFb simulations. Here, t = 0 corresponds to the initial condition with the spinning gaseous halo in hydrostatic equilibrium and t0 = 150 Myr (when AGN feedback is turned on) is marked with a gray vertical line.
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