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Intensity mapping, which images a single spectral line from unresolvedgalaxies across cosmological volumes, is a promising technique for probing theearly universe. Here we present predictions for the intensity map and powerspectrum of the CO(1-0) line from galaxies at z ~ 2.4 -2.8, based on aparameterized model for the galaxy-halo connection, and demonstrate the extentto which properties of high-redshift galaxies can be directly inferred fromsuch observations. We find that our fiducial prediction should be detectable bya realistic experiment. Motivated by significant modeling uncertainties, wedemonstrate the effect on the power spectrum of varying each parameter in ourmodel. Using simulated observations, we infer constraints on our modelparameter space with an MCMC procedure, and show corresponding constraints onthe LIR-LCO relation and the CO luminosity function. These constraints would becomplementary to current high-redshift galaxy observations, which can detectthe brightest galaxies but not complete samples from the faint end of theluminosity function. By probing these populations in aggregate, CO intensitymapping could be a valuable tool for probing molecular gas and its relation tostar formation in high-redshift galaxies.

Connecting CO Intensity Mapping to Molecular Gas and Star Formation in the Epoch of Galaxy Assembly