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(Abridged) In this paper, we investigate the physical conditions of[CI]-traced gas in high-mass star-forming regions by analyzing APEX [CI] 492GHz single-pointing observations of the ATLASGAL Top100 sources along withother multi-wavelength data. Our 98 sources are clearly detected in [CI] 492GHz emission, and the observed integrated intensities and line widths tend toincrease toward evolved stages of star formation. In addition to these "main"components that are associated with the Top100 sample, 41 emission and twoabsorption features are identified by their velocities toward 28 and two linesof sight respectively as "secondary" components. The secondary components havesystematically smaller integrated intensities and line widths than the maincomponents. We found that [CI] 492 GHz and 13CO(2-1) are well correlated withthe 13CO(2-1)-to-[CI] 492 GHz integrated intensity ratio varying from 0.2 to5.3. In addition, we derived the H2-to-[CI] conversion factor, X(CI), bydividing 870 micron-based H2 column densities by the observed [CI] 492 GHzintegrated intensities and found that X(CI) ranges from 2.3e20 to 1.3e22 with amedian of 1.7e21. In contrast to the strong correlation with 13CO(2-1), [CI]492 GHz has a scattered relation with the 870 micron-traced molecular gas.Finally, we performed LTE and non-LTE analyses of the [CI] 492 GHz and 809 GHzdata for a subset of the Top100 sample and inferred that [CI] emission likelyoriginates from warm (kinetic temperature > 60 K), optically thin (opacity <0.5), and highly pressurized (thermal pressure ~ e5 to e8 K/cm3) regions.

ATLASGAL-selected massive clumps in the inner Galaxy. X. Observations of atomic carbon at 492 GHz