Most stars form in dense star clusters deeply embedded in residual gas. The populations of these objects range from small groups of stars with about a dozen binaries within a volume with a typical radius of r ≈ 0.3 pc through to objects formed in extreme star bursts containing N ≈ 108 stars within r ≈ 36 pc. Star clusters, or more generally dense stellar systems, must therefore be seen as the fundamental building blocks of galaxies. Differentiation of the term star cluster from a spheroidal dwarf galaxy becomes blurred near N ≈ 106. Both are mostly pressure-supported, that is, random stellar motions dominate any bulk streaming motions such as rotation.
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Kroupa, P. (2008). Initial Conditions for Star Clusters. In: Aarseth, S.J., Tout, C.A., Mardling, R.A. (eds) The Cambridge N-Body Lectures. Lecture Notes in Physics, vol 760. Springer, Dordrecht. https://doi.org/10.1007/978-1-4020-8431-7_8
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