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Most stars form in dense star clusters deeply embedded in residual gas. Theseobjects must therefore be seen as the fundamental building blocks of galaxies.With this contribution some physical processes that act in the very early andalso later dynamical evolution of dense stellar systems in terms of shapingtheir later appearance and properties, and the impact they have on their hostgalaxies, are highlighted. Considering dense systems with increasing mass, itturns out that near 10^6 Msol their properties change fundamentally: stellarpopulations become complex, a galaxial mass--radius relation emerges and themedian two-body relaxation time becomes longer than a Hubble time.Intriguingly, only systems with a two-body relaxation time longer than a Hubbletime show weak evidence for dark matter, whereby dSph galaxies form totaloutliers.

The formation, disruption and properties of pressure-supported stellar systems and implications for the astrophysics of galaxies