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We compare the existent methods including the minimum spanning tree basedmethod and the local stellar density based method, in measuring masssegregation of star clusters. We find that the minimum spanning tree methodreflects more the compactness, which represents the global spatial distributionof massive stars, while the local stellar density method reflects more thecrowdedness, which provides the local gravitational potential information. Itis suggested to measure the local and the global mass segregationsimultaneously. We also develop a hybrid method that takes both aspects intoaccount. This hybrid method balances the local and the global mass segregationin the sense that the predominant one is either caused either by dynamicalevolution or purely accidental, especially when such information is unknown apriori. In addition, we test our prescriptions with numerical models and showthe impact of binaries in estimating the mass segregation value. As anapplication, we use these methods on the Orion Nebula Cluster (ONC)observations and the Taurus cluster. We find that the ONC is significantly masssegregated down to the 20th most massive stars. In contrast, the massive starsof the Taurus cluster are sparsely distributed in many different subclusters,showing a low degree of compactness. The massive stars of Taurus are also foundto be distributed in the high-density region of the subclusters, showingsignificant mass segregation at subcluster scales. Meanwhile, we also applythese methods to discuss the possible mechanisms of the dynamical evolution ofthe simulated substructured star clusters.

Simulations of Fractal Star Cluster Formation: I. New Insights for Measuring Mass Segregation of Star Clusters with SubStructure