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We present a framework for characterizing the large scale movement of baryonsrelative to dark matter in cosmological simulations, requiring only the initialconditions and final state of the simulation. This is performed using thespread metric which quantifies the distance in the final conditions betweeninitially neighbouring particles, and by analysing the baryonic content offinal haloes relative to that of the initial Lagrangian regions defined bytheir dark matter component. Applying this framework to the SIMBA cosmologicalsimulations, we show that 40% (10%) of cosmological baryons have moved $>1h^{-1}~ {\rm Mpc}^{-1}$ ($3h^{-1}~ {\rm Mpc}^{-1}$) by $z=0$, due primarily toentrainment of gas by jets powered by AGN, with baryons moving up to $12h^{-1}~{\rm Mpc}^{-1}$ away in extreme cases. Baryons decouple from the dynamics ofthe dark matter component due to hydrodynamic forces, radiative cooling, andfeedback processes. As a result, only 60% of the gas content in a given halo at$z=0$ originates from its Lagrangian region, roughly independent of halo mass.A typical halo in the mass range $M_{\rm vir} = 10^{12}$--$10^{13}{\rmM}_\odot$ only retains 20% of the gas originally contained in its Lagrangianregion. We show that up to 20% of the gas content in a typical Milky Way masshalo may originate in the region defined by the dark matter of another halo.This inter-Lagrangian baryon transfer may have important implications for theorigin of gas and metals in the circumgalactic medium of galaxies, as well asfor semi-analytic models of galaxy formation and "zoom-in" simulations.

Cosmological baryon transfer in the SIMBA simulations