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(abridged) The far-UV wavelength range (912-2000A) provides access to atomicand molecular transitions of many species the interstellar medium (ISM),circumgalactic medium (CGM), and intergalactic medium, within phases spanning awide range of ionization, density, temperature, and molecular gas fraction.Far-UV space telescopes have enabled detailed studies of the ISM in the MilkyWay thanks to absorption features appearing in the UV spectra of hot stars andyielding fundamental insights into the composition and physical characteristicsof all phases of the ISM along with the processes that influence them. However,we have yet to design a spectrometer able to observe the full UV domain atresolving power R>10^5 with a signal-to-noise ratio SNR>500. Such a resolutionis necessary to resolve lines from both the cold molecular hydrogen and thewarm metal ions with a turbulent velocity of about 1 km s-1, and todifferentiate distinct velocity components. Future UV spectroscopic studies ofthe Milky Way ISM must revolutionize our understanding of the ISM as adynamical, unstable, and magnetized medium, and rise to the challenge broughtforward by current theories. Another interesting prospect is to transpose thesame level of details that has been reached for the Milky Way to the ISM inexternal galaxies, in particular in metal-poor galaxies, where the ISM chemicalcomposition, physical conditions, and topology change dramatically, withsignificant consequences on the star-formation properties. Finally, we need tobe able to perform statistical analyses of background quasar lines of sightintersecting the CGM of galaxies at various redshifts and to comprehend therole of gas exchanges and flows for galaxy evolution.

ESA Voyage 2050 white paper: A complete census of the gas phases in and  around galaxies, far-UV spectropolarimetry as a prime tool for understanding  galaxy evolution and star formation