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When and how did galaxies form and their metals accumulate? Over the lastdecade, this has moved from an archeological question to a live investigation:there is now a broad picture of the evolution of galaxies in dark matter halos:their masses, stars, metals and supermassive blackholes. Galaxies have beenfound and studied in which these formation processes are taking place mostvigorously, all the way back in cosmic time to when the intergalactic medium(IGM) was still largely neutral. However, the details of how and why theinterstellar medium (ISM) in distant galaxies cools, is processed, recycled andenriched in metals by stars, and fuels active galactic nuclei (AGNs) remainuncertain. In particular, the cooling of gas to fuel star formation, and thechemistry and physics of the most intensely active regions is hidden from viewat optical wavelengths, but can be seen and diagnosed at mid- & far-infrared(IR) wavelengths. Rest-frame IR observations are important first to identifythe most luminous, interesting and important galaxies, secondly to quantifyaccurately their total luminosity, and finally to use spectroscopy to trace theconditions in the molecular and atomic gas out of which stars form. In order tomap out these processes over the full range of environments and large-scalestructures found in the universe - from the densest clusters of galaxies to theemptiest voids - we require tools for deep, large area surveys, of millions ofgalaxies out to z~5, and for detailed follow-up spectroscopy. The necessarytools can be realized technically. Here, we outline the requirements forgathering the crucial information to build, validate and challenge models ofgalaxy evolution.

A complete view of galaxy evolution: panchromatic luminosity functions and the generation of metals