Low-end mass function of the Quintuplet cluster

TL;DR

This study applies a novel pixel intensity histogram method to estimate the low-mass end of the initial mass function in the Quintuplet cluster, revealing similarities with the Arches cluster and suggesting a universal IMF in the Galactic Center region.

Contribution

The paper introduces the PIH method to analyze the low-end IMF of the Quintuplet cluster, extending previous work on the Arches cluster and providing new insights into star formation in the Galactic Center.

Findings

Low-end IMF of Quintuplet is consistent with Kroupa MF.

Significant number of stars below 1 solar mass.

Clusters are likely about 100 pc from the Galactic Center.

Abstract

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