Massive star cluster formation - I. High star formation efficiency while resolving feedback of individual stars

Open Access

Fig. B.1.

Fraction of the number of stars formed with agglomeration of stars below the mass on the x-axis over the total number of stars sampled by the IMF. We used $M_{agg} = 4 M_{⊙}$ $M_{\mathrm{agg}} = 4\rm\, M_\odot$ , which means the number of stars in the grid is 10% of the number that are formed by our IMF.

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