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We present a novel approach to estimating the intensity mapping signal of anyCO rotational line emitted during the Epoch of Reionization (EoR). Our approachis based on large velocity gradient (LVG) modeling, a radiative transfermodeling technique that generates the full CO spectral line energy distribution(SLED) for a specified gas kinetic temperature, volume density, velocitygradient, molecular abundance, and column density. These parameters, whichdrive the physics of CO transitions and ultimately dictate the shape andamplitude of the CO SLED, can be linked to the global properties of the hostgalaxy, mainly the star formation rate (SFR) and the SFR surface density. Byfurther employing an empirically derived SFR-M relation for high redshiftgalaxies, we can express the LVG parameters, and thus the specific intensity ofany CO rotational transition, as functions of the host halo mass M and redshiftz. Integrating over the range of halo masses expected to host CO-luminousgalaxies, we predict a mean CO(1-0) brightness temperature ranging from ~0.6{\mu}K at z= 6 to ~0.03 {\mu} at z= 10 with brightness temperature fluctuationsof $\Delta_{CO}^2$ ~ 0.1 and 0.005 {\mu}K respectively, at k = 0.1 Mpc$^{-1}$.In this model, the CO emission signal remains strong for higher rotationallevels at z = 6, with <T$_{CO}$>~ 0.3 and 0.05 {\mu}K for the CO J = 6->5 andCO J = 10->9 transitions respectively. Including the effects of COphotodissociation in these molecular clouds, especially at low metallicities,results in the overall reduction in the amplitude of the CO signal, with thelow- and high-J lines weakening by 2-20% and 10-45%, respectively, over theredshift range 4 < z < 10.

Predicting the intensity mapping signal for multi-$J$ CO lines