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Using the SWIFT simulation code we study different forms of active galacticnuclei (AGN) feedback in idealized galaxy groups and clusters. We first presenta physically motivated model of black hole (BH) spin evolution and a numericalimplementation of thermal isotropic feedback (representing the effects ofenergy-driven winds) and collimated kinetic jets that they launch at differentaccretion rates. We find that kinetic jet feedback is more efficient atquenching star formation in the brightest cluster galaxies (BCGs) than thermalisotropic feedback, while simultaneously yielding cooler cores in theintracluster medium (ICM). A hybrid model with both types of AGN feedbackyields moderate star formation rates, while having the coolest cores. We thenconsider a simplified implementation of AGN feedback by fixing the feedbackefficiencies and the jet direction, finding that the same general conclusionshold. We vary the feedback energetics (the kick velocity and the heatingtemperature), the fixed efficiencies and the type of energy (kinetic versusthermal) in both the isotropic and the jet case. The isotropic case is largelyinsensitive to these variations. In particular, we highlight that kineticisotropic feedback (used e.g. in IllustrisTNG) is similar in its effects to itsthermal counterpart (used e.g. in EAGLE). On the other hand, jet feedback mustbe kinetic in order to be efficient at quenching. We also find that it is muchmore sensitive to the choice of energy per feedback event (the jet velocity),as well as the efficiency. The former indicates that jet velocities need to becarefully chosen in cosmological simulations, while the latter motivates theuse of BH spin evolution models.

Winds versus jets: a comparison between black hole feedback modes in simulations of idealized galaxy groups and clusters