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The past decade has seen an explosion of discoveries and new insights intothe diffuse gas within galaxies, galaxy clusters, and the filaments composingthe Cosmic Web. A new decade will bring fresh opportunities to further thisprogress towards developing a comprehensive view of the composition, thermalstate, and physical processes of diffuse gas in the Universe. Ultraviolet (UV)spectroscopy, probing diffuse 10^4-10^6 K gas at high spectral resolution, isuniquely poised to (1) witness environmental galaxy quenching processes inaction, such as strangulation and tidal- and ram-pressure stripping, (2)directly account for the baryon content of galaxy clusters in the cold-warm(T<10^6 K) gas, (3) determine the phase structure and kinematics of gasparticipating in the equilibrium-regulating exchange of energy at the cores ofgalaxy clusters, and (4) map cold streams and filaments of the Cosmic Web thatfeed galaxies and clusters. With a substantial UV undertaking beyond the HubbleSpace Telescope, all of the above would be achievable over the entire epoch ofgalaxy cluster formation. Such capabilities, coupled with already-plannedadvancements at other wavelengths, will transform extragalactic astronomy byrevealing the dominant formation and growth mechanisms of gaseous halos overthe mass spectrum, settling the debate between early- and late-time metalenrichment scenarios, and revealing how the ecosystems in which galaxies resideultimately facilitate their demise.

Ultraviolet Perspectives on Diffuse Gas in the Largest Cosmic Structures