Without additional heating radiative cooling of gas in the halos of massive galaxies Milky Way and above produces cold gas or stars in excess of that observed Previous work suggested that AGN jets are likely required but the form of jet energy required to quench remains unclear This is particularly challenging for galaxy simulations in which the resolution is orders of magnitude coarser than necessary to form and evolve the jet On such scales the uncertain parameters include jet energy form kinetic thermal and cosmic ray CR energy energy momentum and mass flux magnetic field strength and geometry jet precession angle and period openingangle and duty cycle We investigate all of these parameters in a 1014M⊙ halo using highresolution noncosmological MHD simulations with the FIRE2 Feedback In Realistic Environments stellar feedback model conduction and viscosity We explore which scenarios match observational constraints and show that CRdominated jets can most efficiently quench the central galaxy through a combination of CR pressure support and a modification of the thermal instability Jets with most energy in mildly relativistic ∼ MeV or ∼1010 K thermal plasma work but require a factor ∼10 larger energy input For a fixed energy flux jets with higher specific energy longer cooling times quench more effectively For this halo size kinetic jets are less efficient in quenching unless they have wide opening or precession angles Magnetic fields play a minor role except when the magnetic flux reaches ≳1044 erg s−1 in a kinetic jet model which causes the jet cocoon to significantly widen and the quenching to become explosive We conclude that the criteria for a successful jet model are an optimal energy flux and a sufficiently wide jet cocoon with long enough cooling time at the cooling radius