Fig. 1.
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Plummer-like power law density profiles of stellar clusters for q = 3, 4, 5, and of the corresponding initial gas, with p = 2, 2.6, 3.3. The density profiles of the initial gas were recovered according to the star cluster formation model of Parmentier & Pfalzner (2013), alike in Shukirgaliyev et al. (2017), for ϵff = 0.05, and tSF = 3 Myr.
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