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Without additional heating, radiative cooling of gas in the halos of massivegalaxies (Milky Way and above) produces cold gas or stars in excess of thatobserved. Previous work suggested that AGN jets are likely required, but theform of jet energy required to quench remains unclear. This is particularlychallenging for galaxy simulations, in which the resolution is orders ofmagnitude coarser than necessary to form and evolve the jet. On such scales,the uncertain parameters include: jet energy form (kinetic, thermal, and cosmicray (CR) energy), energy, momentum, and mass flux, magnetic field strength andgeometry, jet precession angle and period, opening-angle, and duty cycle. Weinvestigate all of these parameters in a $10^{14}\,{\rm M}_{\odot}$ halo usinghigh-resolution non-cosmological MHD simulations with the FIRE-2 (Feedback InRealistic Environments) stellar feedback model, conduction, and viscosity. Weexplore which scenarios match observational constraints and show thatCR-dominated jets can most efficiently quench the central galaxy through acombination of CR pressure support and a modification of the thermalinstability. Jets with most energy in mildly relativistic ($\sim$ MeV or$\sim10^{10}$ K) thermal plasma work, but require a factor $\sim 10$ largerenergy input. For a fixed energy flux, jets with higher specific energy (longercooling times) quench more effectively. For this halo size, kinetic jets areless efficient in quenching unless they have wide opening or precession angles.Magnetic fields play a minor role except when the magnetic flux reaches$\gtrsim 10^{44}$ erg s$^{-1}$ in a kinetic jet model, which causes the jetcocoon to significantly widen, and the quenching to become explosive. Weconclude that the criteria for a successful jet model are an optimal energyflux and a sufficiently wide jet cocoon with long enough cooling time at thecooling radius.

Which AGN Jets Quench Star Formation in Massive Galaxies?