Left panel: density PDFs for runs with varied γ₀ and magnetization. The same time steps as used for the mass spectra are shown with decreasing line width. The density PDF is almost invariant in time. The high-density end merely changes from one run to another. A power law of n^−1.5 is shown for comparison. The low-density end is narrower in run T10G07 because of the increasing thermal pressure with decreasing density. More magnetized runs have less low-density gas as well, due to similar effects. Right panel: density PDF of model A (lower initial density) without and with magnetic field. The magnetic field does not affect the PDF in the density range where stars are actively forming.