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The present work explores the origin of the formation of star clusters in ourGalaxy and in Small Magellanic Cloud (SMC) through simulated H-R diagrams andcompare those with observed star clusters. The simulation study producessynthetic H-R diagrams by Markov Chain Monte Carlo (MCMC) technique using starformation history (SFH), luminosity function (LF), abundance of heavy metal (Z)and a big library of isochrones as basic inputs and compares them with observedH-R diagrams of various star clusters. The distance based comparison betweenthose two diagrams is carried out through two dimensional matching of points inColor-Magnitude Diagram (CMD) after optimal choice of bin size and appropriatedistance function. It is found that a poor medium of heavy elements (Z =0.0004), Gaia LF along with mixture of multiple Gaussian distributions of SFHmay be the origin of formation of globular clusters (GCs). On the contrary,enriched medium (Z = 0.019) is favoured with Gaia LF along with double powerlaw (i.e. unimodal) SFH. For SMC clusters, the choice of exponential LF andexponential SFH is a proper combination for poor medium whereas Gaia LF withBeta type SFH is preferred in an enriched medium for the formation of starclusters.

Exploration about the origin of galactic and extragalactic star clusters through simulated H-R diagrams