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We estimate the fraction of stars that form in compact clusters (bound andunbound), 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 thefraction of stars in clusters that survive to ages between t1 and t2, denotedby Gamma_S(t1,t2), and find Gamma_S(10,100)=4.6 +/- 2.5% andGamma_S(100,400)=2.4 +/- 1.1 %, significantly lower than Gamma_F for the samegalaxies. We do not find any systematic trends in Gamma_F or Gamma_S with thestar formation rate (SFR), the SFR per unit area (Sigma_SFR), or the surfacedensity of molecular gas (Sigma_H2) within the host galaxy. Our results areconsistent with those found previously from the CMF/SFR statistic (where CMF isthe cluster mass function), and with the quasi-universal model in whichclusters in different galaxies form and disrupt in similar ways. Our results,however, contradict many previous claims that the fraction of stars in boundclusters increases strongly with Sigma_SFR and Sigma_H_2. We find that thepreviously 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 systematicallyused for galaxies with higher Sigma_SFR and Sigma_H2, and Gamma_S(10,100) forgalaxies with lower Sigma_SFR and Sigma_H_2.

The Fraction of Stars That Form in Clusters in Different Galaxies