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The rotational lines of carbon monoxide and the fine structure lines of CIIand of the most abundant metals, emitted during the epoch of enhanced starformation in the universe, are redshifted in the frequency channels where thepresent-day and future CMB experiments are sensitive. We estimate thecontribution to the CMB angular power spectrum by the emission in such lines inmerging star-forming galaxies. We used the Lacey-Cole approach to characterizethe distribution of the merging halos, together with a parametrization for thestar formation rate in each of them. Using observational data from a sample oflocal, low-redshift, and high-redshift objects, we calibrated the luminosity ineach line as a function of the star formation rate. We show that thecorrelation term arising from CO line emission is a significant source offoreground for CMB in a broad range of frequencies (in particular in the 20-60GHz band) and for 1000<l<8000, corresponding to angular scales smaller than 10arcminutes. Moreover, we demonstrate that observing with different spectralresolutions will give the possibility of increasing the amplitude of the signalup to two orders of magnitude in C_l and will help separate the linecontribution from practically all other foreground sources and from the primaryfluctuations themselves, since these show no significant dependence on thespectral resolution. We propose to perform observations with varying spectralbandwidths as a new tool to construct a tomography of the universe, by probingdifferent redshift slices with varying thickness. (abridged)

Carbon monoxide line emission as a CMB foreground: tomography of the star-forming universe with different spectral resolutions