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We make use of our 'minimal' cold interstellar medium (ISM) emission linemodel that predicts the molecular and atomic line emission per unit dense,star-forming gas mass (Geach & Papadopoulos 2012; Paper I) to examine theutility of key line ratios in surveys of the so-called star formation 'mode' astraced by xi_SF = M_dense(H_2)/M_total(H_2). We argue that xi_SF and itsproxies provide very sensitive, extinction-free discriminators of rapidstarburst/merger-driven versus secular quiescent/disk-like stellar massassembly, with the most promising diagnostic to be applied in the near-futurebeing CO(4-3)/[CI](1-0). These lines are accessible across nearly the fullrange 0<z<2 (thus covering the bulk of galaxy evolution) with the Atacama LargeMillimeter Array. In addition to their diagnostic power, another advantage ofthis combination is the similar observed frequencies (Delta nu_0 ~ 30 GHz) ofthe lines, resulting in nearly spatially-matched beams for a fixed aperture,thus mitigating the effects of resolution/morphology bias in the interpretationof galaxy-averaged line ratios. Finally we discuss the capability of deep blindredshift surveys with the high frequency component of the Square KilometerArrray (SKA) in discovering H_2-rich galaxies with very low xi_SF values. Thesecould be the progenitors of starburst galaxies seen prior to the onset of starformation; such galaxies could be a class of extreme outliers from local (gassurface density)-(star formation rate) scaling laws, which would exclude themfrom current star formatation or stellar mass selected samples. Ourconservative model suggests that SKA could detect such systems residing at z~3at a rate of 20-200 per hour.

Molecular and atomic line surveys of galaxies II: unbiased estimates of their star formation mode