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The evolution of a galaxy is driven by the state of its interstellar medium. Dense molecular gas serves as the site for the formation of young massive stars, which in turn heat the gas and may drive outflows of material. Understanding the evolution of galaxies, therefore, requires quantitative measurements of the interstellar medium in wide range of galaxies from puny dwarf galaxies to mighty LIRGs. In this talk, I argue that developing wide-field, moderately high resolution, spectral line capabilities are key to this understanding using recent GBT 4mm observations of dense molecular gas as an example. These, and other observations, are already uncovering differences in the relationship of dense molecular gas to star formation in other nearby galaxies.
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