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Fig. 3.


Mass segregation ratio (ΛMSR; see Appendix D.3) as a function of the NMST (MST) most massive disks of GGD 27. ALMA 1 and ALMA 2, classified as Class II and Class III YSOs, respectively, are not included. The main deviation from a uniform behavior around unity is for NMST = 2, suggesting that the two most massive sources are closer to each other than the average distance between two random sources. The horizontal line at ΛMSR = 1 indicates the regime where sources show no evidence for mass segregation.

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