Gas surface density maps (top) and power spectra (bottom) for ramses simulations of isolated galaxies with different settings: Left: simulation with no Jeans polytrope pressure floor. Right: simulation with a more easily triggered refinement criterion that enables ≈15 pc resolution throughout the galactic disk (and without the Jeans polytrope). Removing the Jeans polytrope ensures that the power on scales ≳200 pc is similar in ramses and gasoline simulations. Enhancing the typical cell size in ramses leads to improved agreement between ramses and gasoline power spectra on scales ≲50 pc at the expense of a discrepancy at moderate scales of ≈50–200 pc (as well as additional computational cost).