2014MNRAS.445L.124T

We use a high-resolution hydrodynamic simulation that tracks the non-equilibrium abundance of molecular hydrogen within a massive high-redshift galaxy to produce mock Atacama Large Millimeter Array (ALMA) maps of the fine-structure lines of atomic carbon, C i 1-0 and C i 2-1. Inspired by recent observational and theoretical work, we assume that C i is thoroughly mixed within giant molecular clouds and demonstrate that its emission is an excellent proxy for H2. Nearly all of the H2 associated with the galaxy can be detected at redshifts z < 4 using a compact interferometric configuration with a large synthesized beam (that does not resolve the target galaxy) in less than 4h of integration time. Low-resolution imaging of the C i lines (in which the target galaxy is resolved into three to four beams) will detect ∼ 80 per cent of the H2 in less than 12h of aperture synthesis. In this case, the resulting data cube also provides the crucial information necessary for determining the dynamical state of the galaxy. We conclude that ALMA observations of the C i 1-0 and 2-1 emission are well-suited for extending the interval of cosmic look-back time over which the H2 distributions, the dynamical masses, and the Tully-Fisher relation of galaxies can be robustly probed.