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We present ALMA Band 9 observations of the [C II]158um emission for a sampleof 10 main-sequence galaxies at redshift z ~ 2, with typical stellar masses(log M*/Msun ~ 10.0 - 10.9) and star formation rates (~ 35 - 115 Msun/yr).Given the strong and well understood evolution of the interstellar medium fromthe present to z = 2, we investigate the behaviour of the [C II] emission andempirically identify its primary driver. We detect [C II] from six galaxies(four secure, two tentative) and estimate ensemble averages including nondetections. The [C II]-to-infrared luminosity ratio (L[C II]/LIR) of our sampleis similar to that of local main-sequence galaxies (~ 2 x 10^-3), and ~ 10times higher than that of starbursts. The [C II] emission has an averagespatial extent of 4 - 7 kpc, consistent with the optical size. Complementingour sample with literature data, we find that the [C II] luminosity correlateswith galaxies' molecular gas mass, with a mean absolute deviation of 0.2 dexand without evident systematics: the [C II]-to-H2 conversion factor (alpha_[CII] ~ 30 Msun/Lsun) is largely independent of galaxies' depletion time,metallicity, and redshift. [C II] seems therefore a convenient tracer toestimate galaxies' molecular gas content regardless of their starburst ormain-sequence nature, and extending to metal-poor galaxies at low and highredshifts. The dearth of [C II] emission reported for z > 6 - 7 galaxies mightsuggest either a high star formation efficiency or a small fraction of UV lightfrom star formation reprocessed by dust.

The [C II] emission as a molecular gas mass tracer in galaxies at low and high redshift