Abstract

Forming new generations of stars in galaxies critically depends on both feeding and feedback processes that fuel and regulate their gas supply.  The circumgalactic medium (CGM) serves as both a gas reservoir and mediator of all interactions between galaxies and their environments.  Not only do matter and energy transport in or out of a galaxy occur in the CGM, but larger scale effects such as ram-pressure or tidal stripping in groups and clusters must first impact the CGM.  On even larger scales, the total gas budget that must feed these reservoirs is distributed among the filaments, sheets, nodes, and voids of the Cosmic Web.  I will present observations at each of these scales demonstrating 1) feedback caught in the act via a 40 kpc scale outflow mapped in emission, 2) the suppression of cold halo gas reservoirs in groups and clusters, and 3) how gas in the intergalactic medium is distributed with respect to the Cosmic Web traced by galaxies and is shock-heated in the centers of filaments.  Toward this final point, I will present a new Cosmic Web reconstruction method inspired by the Physarum polycephalum slime mold, which recovers the environmental dependencies of galaxy properties with high fidelity.