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We study the core mass function (CMF) within 32 dense clumps in seveninfrared dark clouds (IRDCs) with the Atacama Large Millimeter/submillimeterArray (ALMA) via 1.3~mm continuum emission at a resolution of $\sim$1". We haveidentified 107 cores with the dendrogram algorithm, with a median radius ofabout 0.02 pc. Their masses range from 0.261 to 178 $M_{\odot}$. After applyingcompleteness corrections, we fit the combined IRDC CMF with a power law of theform $d N / d\:{\rm log} M \propto M^{-\alpha}$ and derive an index of$\alpha\simeq0.86\pm0.11$ for $M \geq 0.79\:M_\odot$ and$\alpha\simeq0.70\pm0.13$ for $M\geq 1.26\:M_\odot$, which is a significantlymore top-heavy distribution than the Salpeter stellar initial mass function(IMF) index of 1.35. We also make a direct comparison of these IRDC clump CMFresults to those measured in the more evolved protocluster G286 derived withsimilar methods, which have $\alpha\simeq1.29\pm0.19$ and $1.08\pm0.27$ inthese mass ranges, respectively. These results provide a hint that, especiallyfor the $M\geq 1.26\:M_\odot$ range where completeness corrections are modest,the CMF in high pressure, early-stage environments of IRDC clumps may betop-heavy compared to that in the more evolved, global environment of the G286protoclusters. However, larger samples of cores probing these differentenvironments are needed to better establish the robustness of this potentialCMF variation.

The Core Mass Function Across Galactic Environments. II. Infrared Dark Cloud Clumps