Notes. For each galaxy we computed the V-band total stellar luminosity L_V, the stellar mass M_⋆, the virial mass M₂₀₀, the virial radius R₂₀₀, the stellar line-of-sight velocity dispersion σ_LOS, and the mode of the stellar metallicity distribution function [Fe/H], all defined inside one virial radius. In the first row different PMF models are shown at a variety of magnetic spectral indices between −2.9 to −2.1 for constant B_λ = 0.05, and in the second row for a constant spectral index at n_B  =   − 2.9 and magnetic field strengths in the range B_λ  =  0.05 − 0.50 nG. ^(a)Halos that did not reach z = 0 crashed at the redshift specified here. The reason some simulations crashed at z >  0 is due to the high gas density coupled to a high stellar mass and strong stellar feedback. The simulation time steps in dense regions is dominated by the Courant condition Δt  ∼  Δx/c_s with c_s the sound speed and Δx the spatial resolution. As Δx  ∼  1/ρ^1/3, the time steps shrink with increasing density. In the presence of stellar feedback, which heats up the gas in dense regions and subsequently increases the sound speed, the time step shrinkage becomes worse. As the current version of our code uses a limit on the shortest time steps, simulations crash in extreme conditions (hot-dense gas). The problem mainly occurs for the most massive halos where the gas density is higher, triggering a stronger cooling and higher star formation, which leads to a significant gas heating. By removing the time step limit, we can avoid the simulation crash, however at the expense of running simulations for many more CPU-hours.