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We study the core mass function (CMF) of the massive protoclusterG286.21+0.17 with the Atacama Large Millimeter/submillimeter Array via 1.3~mmcontinuum emission at a resolution of 1.0\arcsec\ (2500~au). We have mapped afield of 5.3\arcmin$\times$5.3\arcmin\ centered on the protocluster clump. Wemeasure the CMF in the central region, exploring various core detectionalgorithms, which give source numbers ranging from 60 to 125, depending onparameter selection. We estimate completeness corrections due to imperfect fluxrecovery and core identification via artificial core insertion experiments. Formasses $M\gtrsim1\:M_\odot$, the fiducial dendrogram-identified CMF can be fitwith a power law of the form${\rm{d}}N/{\rm{d}}{\rm{log}}M\propto{M}^{-\alpha}$ with $\alpha\simeq1.24\pm0.17$, slightly shallower than, but still consistent with, theindex of the Salpeter stellar initial mass function of 1.35.Clumpfind-identified CMFs are significantly shallower with$\alpha\simeq0.64\pm0.13$. While raw CMFs show a peak near $1\:M_\odot$,completeness-corrected CMFs are consistent with a single power law extendingdown to $\sim 0.5\:M_\odot$, with only a tentative indication of a shallowingof the slope around $\sim1\:M_\odot$. We discuss the implications of theseresults for star and star cluster formation theories.

The Core Mass Function in the Massive Protocluster G286.21+0.17 revealed by ALMA