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We predict the space density of molecular gas reservoirs in the Universe, andplace a lower limit on the number counts of carbon monoxide (CO), hydrogencyanide (HCN) molecular and [CII] atomic emission lines in blind redshiftsurveys in the submillimeter-centimeter spectral regime. Our model uses: (a)recently available HCN Spectral Line Energy Distributions (SLEDs) of localLuminous Infrared Galaxies (LIRGs, L_IR>10^11 L_sun), (b) a value forepsilon=SFR/M_dense(H_2) provided by new developments in the study of starformation feedback on the interstellar medium and (c) a model for the evolutionof the infrared luminosity density. Minimal 'emergent' CO SLEDs from the densegas reservoirs expected in all star-forming systems in the Universe are thencomputed from the HCN SLEDs since warm, HCN-bright gas will necessarily beCO-bright, with the dense star-forming gas phase setting an obvious minimum tothe total molecular gas mass of any star-forming galaxy. We include [CII] asthe most important of the far-infrared cooling lines. Optimal blind surveyswith the Atacama Large Millimeter Array (ALMA) could potentially detect verydistant (z~10-12) [CII] emitters in the >ULIRG galaxy class at a rate of ~0.1-1per hour (although this prediction is strongly dependent on the star formationand enrichment history at this early epoch), whereas the (high-frequency)Square Kilometer Array (SKA) will be capable of blindly detecting z>3 low-J COemitters at a rate of ~40-70 per hour. The [CII] line holds special promise forthe detection of metal-poor systems with extensive reservoirs of CO-darkmolecular gas where detection rates with ALMA can reach up to 2-7 per hour inBands 4-6.

Molecular and atomic line surveys of galaxies I: the dense, star-forming phase as a beacon