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We present a simple model that explains the origin of warm diffuse gas seenprimarily as highly ionized absorption line systems in the spectra ofbackground sources. We predict the observed column densities of several highlyionized transitions such as OVI, OVIII, NeVIII, NV, and MgX; and present aunified comparison of the model predictions with absorption lines seen in theMilky Way disk, Milky Way halo,starburst galaxies, the circumgalactic mediumand the intergalactic medium at low and high redshifts. We show that diffusegas seen in such diverse environments can be simultaneously explained by asimple model of radiatively cooling gas. We show that most of such absorptionline systems are consistent with being collisionally ionized, and estimate themaximum likelihood temperature of the gas in each observation. This modelsatisfactorily explains why OVI is regularly observed around star-forming low-zL* galaxies, and why NV is rarely seen around the same galaxies. We furtherpresent some consequences of this model in quantifying the dynamics of thecooling gas around galaxies and predict the shock velocities associated withsuch flows. A unique strength of this model is that while it has only one free(but physically well-constrained) parameter, it nevertheless successfullyreproduces the available data on O VI absorbers in the interstellar,circumgalactic, intra-group, and intergalactic media, as well as the availabledata on other absorption-line from highly ionized species.

The formation and physical origin of highly ionized cooling gas