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The Millimeter-wave Intensity Mapping Experiment (mmIME) recently reported adetection of excess spatial fluctuations at a wavelength of 3 mm, which can beattributed to unresolved emission of several CO rotational transitions between$z\sim1-5$. We study the implications of this data for the high-redshiftinterstellar medium using a suite of state-of-the-art semianalytic simulationswhich have successfully reproduced many other sub-millimeter line observationsacross the relevant redshift range. We find that the semianalytic predictionsare mildly in tension with the mmIME result, with a predicted CO power$\sim3.5\sigma$ below what was observed. We explore some simple modificationsto the models which could resolve this tension. Increasing the molecular gasabundance at the relevant redshifts to $\sim10^8\ M_\odot\ \rm{Mpc}^{-3}$, avalue well above that obtained from directly imaged sources, would resolve thediscrepancy, as would assuming a CO-$H_2$ conversion factor $\alpha_{\rm{CO}}$of $\sim1.5\ M_{\odot}$ K$^{-1}$ $(\rm{km}/\rm{s})^{-1}$ pc$^{2}$, a valuesomewhat lower than is commonly assumed. We go on to demonstrate that theseconclusions are quite sensitive to the detailed assumptions of our simulations,highlighting the need for more careful modeling efforts as more intensitymapping data become available.

On estimating the cosmic molecular gas density from CO Line Intensity Mapping observations