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The Quintuplet and Arches clusters, which were formed in the harshenvironment of the Galactic Center (GC) a few million years ago, have beenexcellent targets for studying the effects of a star-forming environment on theinitial mass function (IMF). In order to estimate the shape of the low-end IMFof the Arches cluster, Shin & Kim devised a novel photometric method thatutilizes pixel intensity histograms (PIHs) of the observed images. Here, weapply the PIH method to the Quintuplet cluster and estimate the shape of itslow-end IMF below the magnitude of completeness limit as set by conventionalphotometry. We found that the low-end IMF of the Quintuplet is consistent withthat found for the Arches cluster--Kroupa MF, with a significant number oflow-mass stars below 1 $M_{\odot}$. We conclude that the most likely IMFs ofthe Quintuplet and the Arches clusters are not too different from the IMFsfound in the Galactic disc. We also find that the observed PIHs and stellarnumber density profiles of both clusters are best reproduced when the clustersare assumed to be at three-dimensional distances of approximately 100 pc fromthe GC.

Low-end mass function of the Quintuplet cluster