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Star formation and accretion onto supermassive black holes in the nuclei ofgalaxies are the two most energetic processes in the Universe, producing thebulk of the observed emission throughout its history. We simulated theluminosity functions of star-forming and active galaxies for spectral linesthat are thought to be good spectroscopic tracers of either phenomenon, as afunction of redshift. We focused on the infrared (IR) and sub-millimeterdomains, where the effects of dust obscuration are minimal. Using threedifferent and independent theoretical models for galaxy formation andevolution, constrained by multi-wavelength luminosity functions, we computedthe number of star-forming and active galaxies per IR luminosity and redshiftbin. We converted the continuum luminosity counts into spectral line countsusing relationships that we calibrated on mid- and far-IR spectroscopic surveysof galaxies in the local universe. Our results demonstrate that futurefacilities optimized for survey-mode observations, i.e., the Space InfraredTelescope for Cosmology and Astrophysics (SPICA) and the Cerro ChajnantorAtacama Telescope (CCAT), will be able to observe thousands of z>1 galaxies inkey fine-structure lines, e.g., [SiII], [OI], [OIII], [CII], in ahalf-square-degree survey, with one hour integration time per field of view.Fainter lines such as [OIV], [NeV] and H_2 (0-0)S1 will be observed in severaltens of bright galaxies at 1<z<2, while diagnostic diagrams of active-nucleusvs star-formation activity will be feasible even for normal z~1 galaxies. Wediscuss the new parameter space that these future telescopes will cover andthat strongly motivate their construction.

Far-IR/Submillimeter Spectroscopic Cosmological Surveys: Predictions of Infrared Line Luminosity Functions for z<4 Galaxies