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A comprehensive study of interstellar medium phases and the nature of theirboundaries or connections requires comparing abundances and velocity profilesfrom tracers of the different phases. In the UV, studies of a wealth ofabsorption features appearing in the spectra of hot stars yield fundamentalinsights into the composition and physical characteristics of all phases of theISM along with the processes that influence them. They also inform us on thenature of boundaries between them. However no single instrument has as yetgiven access to species in all ISM phases at the same high spectral resolution:from the molecular bands of CO and H2 in the far-UV, to the cold neutral mediumtracers C I and S I and the warm medium tracers like C II, NI, OI, Mg II, FeII, Si II etc, and to the high ions of the hot ionized medium C IV, Si IV inthe UV, as well as O VI in the far UV. We have yet to design the spectrometerthat will enable observing the full UV domain at resolving power R>200 000 andsignal-to-noise ratio SNR>500. The line FWHM being governed by turbulence,temperature, and species mass, such a resolution is necessary to resolve linesfrom both the cold molecular hydrogen and the warm metal ions with a turbulenceof ~1 km/s, and to differentiate distinct velocity components, typicallyseparated by less than 2 km/s.

Far to near UV spectroscopy of the interstellar medium at very high resolution and very high signal-to-noise ratio