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Binary populations in young star clusters show multiplicity fractions bothlower and up to twice as high as those observed in the Galactic field. Wefollow the evolution of a population of binary stars in dense and loose starclusters starting with an invariant initial binary population and a formalmultiplicity fraction of unity, and demonstrate that these models can explainthe observed binary properties in Taurus, Rho-Ophiuchus, Chamaeleon, Orion, IC348, Upper Scorpius A, Praesepe, and the Pleiades. The model needs to considersolely different birth densities for these regions. The evolved theoreticalorbital-parameter distributions are highly probable parent distributions forthe observed ones. We constrain the birth conditions (stellar mass, M_ecl, andhalf-mass radius, r_h) for the derived progenitors of the star clusters and theoverall present-day binary fractions allowed by the present model. The resultscompare very well with properties of molecular cloud clumps on the verge ofstar formation. Combining these with previously and independently obtainedconstraints on the birth densities of globular clusters, we identify a weakstellar mass -- half-mass radius correlation for cluster-forming cloud clumps,r_h / pc ~ (M_ecl / M_sun)^(0.13+-0.04). The ability of the model to reproducethe binary properties in all the investigated young objects, coveringpresent-day densities from 1-10 stars pc^-3 (Taurus) to 2x10^4 stars pc^-3(Orion), suggests that environment-dependent dynamical evolution plays animportant role in shaping the present-day properties of binary populations instar clusters, and that the initial binary properties may not vary dramaticallybetween different environments.

Inverse dynamical population synthesis: Constraining the initial conditions of young stellar clusters by studying their binary populations