Relative differences between properties of GW progenitor events obtained with the on-the-fly and post-processing modes of AREPO-GW for a rerun of the MTNG46 simulation. Differences are expressed as percentages, with the post-processing mode taken as the reference case. Top row: Comoving rates as a function of time (left panel), delay time distribution (middle panel), and merger efficiency as a function of tabulated SEVN metallicity (right panel). Bottom row: Distribution of GW progenitor events as a function of the metallicity of the parent star particle (left panel), BBH (middle panel), and BHNS (right panel) mass functions.