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We propose observations of the molecular gas distribution during the era ofreionization. At $z \sim $ 6 to 8, $^{12}$CO$(J=1-0)$ line intensity results ina mean brightness temperature of about 0.5 $\mu$K with rms fluctuations of 0.1$\mu$K at 1 to 10 Mpc spatial scales, corresponding to 30 arcminute angularscales. This intensity fluctuations can be mapped with an interferometer,similar to existing and planned 21-cm background experiments, but operating at$\sim$ 12 to 17 GHz. We discuss the feasibility of detecting thecross-correlation between HI and CO molecular gas since such across-correlation has the advantage that it will be independent of systematicsand most foregrounds in each of the 21-cm and CO$(1-0)$ line experiments.Additional instruments tuned to higher-order transitions of the CO molecule oran instrument operating with high spectral resolution at mm-wavelengthstargeting 158 $\mu$m CII could further improve the reionization studies withmolecular gas. The combined 21-cm and CO line observations has the potential toestablish the relative distribution of gas in the inter-galactic medium andmolecular gas that are clumped in individual first-light galaxies that areclosely connected to the formation of massive stars in these galaxies.

Probing Reionization with Intensity Mapping of Molecular and Fine Structure Lines