Feedback reshapes the baryon distribution within haloes, in halo outskirts, and beyond: the closure radius from dwarfs to massive clusters

We explore three sets of cosmological hydrodynamical simulations, IllustrisTNG, EAGLE, and SIMBA, to investigate the physical processes impacting distribution baryons in around haloes across an unprecedented mass range $10^8<M_{\rm 200c}/{\rm M_{\odot}}<10^{15}$, from halo centre out scales as large $30\,R_{\rm 200c}$. demonstrate that baryonic feedback mechanisms significantly redistribute gas, lowering baryon fractions inside while simultaneously accumulating this material outside virial radius. To understand large-scale redistribution identify dominant responsible, we examine several variants TNG selectively exclude stellar AGN feedback, cooling, radiation. find heating UV background low-mass haloes, intermediate-mass groups ($10^{12} \leq M_{\rm M_{\odot}}<10^{14}$) are processes. Galaxy clusters least influenced by these on scales. introduce a new mass-dependent characteristic scale, closure radius $R_{\rm c}$, within which all associated with found. For clusters, universal relation between scale fraction: c}/R_{\rm 200c,500c}-1=\beta(z)(1-f_{\rm b}(<R_{\rm 200c,500c})/f_{\rm b,cosmic})$, where $\beta(z)=\alpha\,(1+z)^\gamma$, $\alpha$ $\gamma$ free parameters fit using simulations. Accordingly, predict observed X-ray can be found c}\sim 1.5-2.5 R_{\rm Our results used constrain theoretical models, particularly physics supernova well their interplay environmental processes, through comparison current future SZ observations.