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High-mass stars are formed within massive molecular clumps, where a largenumber of stars form close together. The evolution of the clumps with differentmasses and luminosities is mainly regulated by its high-mass stellar contentand the formation of such objects is still not well understood. In this work,we characterise the mid-J CO emission in a statistical sample of 99 clumps(Top100) selected from the ATLASGAL survey that are representative of theGalactic proto-cluster population. High-spatial resolution APEX-CHAMP+ maps ofthe CO(6-5) and CO(7-6) transitions were obtained and combined with additionalsingle-pointing APEX-FLASH+ spectra of the CO(4-3) line. We study thecorrelations of the CO line luminosities and profiles for the three COtransitions with the clump properties and investigate if and how they change asa function of the evolution. All sources were detected above 3-$\sigma$ in allthree CO transitions and most of the sources exhibit broad CO emission likelyassociated with molecular outflows. We found that the extension of the mid-J COemission is correlated with the size of the dust emission traced by theHerschel-PACS 70 $\mu$m maps. The CO line luminosity is correlated with theluminosity and mass of the clumps. However, it does not correlate with the L/Mratio. The dependency of the CO luminosity with the properties of the clumps issteeper for higher-J transitions. Our data seem to exclude that this trend isbiased by self-absorption features in the CO emission, but rather suggest thatdifferent J transitions arise from different regions of the inner envelope.Moreover, high-mass clumps show similar trends in CO luminosity as lower massclumps, but are systematically offset towards larger values, suggesting thathigher column density and/or temperature (of unresolved) CO emitters are foundinside high-mass clumps.

ATLASGAL-selected high-mass clumps in the inner Galaxy. VII. Characterisation of mid-J CO emission