The Fraction of Stars That Form in Clusters in Different Galaxies

TL;DR

This study estimates the fraction of stars forming in clusters across various galaxy types, finding a roughly universal value around 24%, with no strong correlation to galaxy star formation metrics, challenging previous assumptions.

Contribution

It provides the first comprehensive comparison of star cluster formation fractions across diverse galaxy types, demonstrating near-universality and correcting misconceptions about correlations with galaxy properties.

Findings

Gamma_F ~ 24% across galaxy types

Cluster survival fractions are significantly lower than formation fractions

No strong correlation between Gamma_F and galaxy SFR or gas density

Abstract

We estimate the fraction of stars that form in compact clusters (bound and unbound), Gamma_F, in a diverse sample of eight star-forming galaxies, including two irregulars, two dwarf starbursts, two spirals, and two mergers. The average value for our sample is Gamma_F ~ 24 +/- 9%. We also calculate the fraction of stars in clusters that survive to ages between t1 and t2, denoted by Gamma_S(t1,t2), and find Gamma_S(10,100)=4.6 +/- 2.5% and Gamma_S(100,400)=2.4 +/- 1.1 %, significantly lower than Gamma_F for the same galaxies. We do not find any systematic trends in Gamma_F or Gamma_S with the star formation rate (SFR), the SFR per unit area (Sigma_SFR), or the surface density of molecular gas (Sigma_H2) within the host galaxy. Our results are consistent with those found previously from the CMF/SFR statistic (where CMF is the cluster mass function), and with the quasi-universal model in which clusters in different galaxies form and disrupt in similar ways. Our results, however, contradict many previous claims that the fraction of stars in bound clusters increases strongly with Sigma_SFR and Sigma_H_2. We find that the previously reported trends are largely driven by comparisons that mixed Gamma_F ~ Gamma_S(0,10) and Gamma_S(10,100), where Gamma_S(0,10) was systematically used for galaxies with higher Sigma_SFR and Sigma_H2, and Gamma_S(10,100) for galaxies with lower Sigma_SFR and Sigma_H_2.