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In this paper, we investigate the relevance of using the  12 CO‐line emissions as indicators of star formation rates (SFRs). For the first time, we present this study for a relatively large number of  12 CO transitions (12) as well as over a large interval in redshift (from   z ∼ 0  to 6). For the nearby sources  ( D ≤ 10 Mpc) , we have used our previously published homogeneous sample of  12 CO data, mixing observational and modelled line intensities. For higher  z  sources  ( z ≥ 1) , we have collected  12 CO observations from various papers and completed the data set of line intensities with model predictions which we also present in this paper. Finally, for increasing the statistics, we have included recent  12 CO(1–0) and  12 CO(3–2) observations of intermediate‐ z  sources. Linear regressions have been calculated for identifying the tightest SFR– 12 CO‐line luminosity relationships. We show that the  total  12 CO, the  12 CO(5–4), the  12 CO(6–5) and the  12 CO(7–6) luminosities are the best indicators of SFRs (as measured by the far‐infrared luminosity). Comparisons with theoretical approaches from Krumholz &amp; Thompson and Narayanan et al. are also performed in this paper. Although in general agreement, the predictions made by these authors and the observational results we present here show small and interesting discrepancies. In particular, the slope of the linear regressions for   J  upper ≥ 4  12 CO  lines is not similar between theoretical studies and observations. On the one hand, a larger high‐ J  12 CO data set of observations might help to better agree with models, increasing the statistics. On the other hand, theoretical studies extended to high‐redshift sources might also reduce such discrepancies.

Are 12 CO lines good indicators of the star formation rate in galaxies?