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The mass segregation of stellar clusters could be primordial rather thandynamical. Despite the abundance of studies of mass segregation for stellarclusters, those for stellar progenitors are still scarce, so the question onthe origin and evolution of mass segregation is still open. Our goal is tocharacterize the structure of the NGC 2264 molecular cloud and compare thepopulations of clumps and young stellar objects (YSOs) in this region whoserich YSO population has shown evidence of sequential star formation. Weseparated the Herschel column density map of NGC 2264 in three subregions andcompared their cloud power spectra using a multiscale segmentation technique.We identified in the whole NGC 2264 cloud a population of 256 clumps withtypical sizes of ~0.1 pc and masses ranging from 0.08 Msun to 53 Msun. Althoughclumps have been detected all over the cloud, the central subregion of NGC 2264concentrates most of the massive, bound clumps. The local surface density andthe mass segregation ratio indeed indicate a strong degree of mass segregationfor the 15 most massive clumps, with a median $\Sigma_6$ three time that of thewhole clumps population and $\Lambda_{MSR}$ about 8. We showed that thiscluster of massive clumps is forming within a high-density cloud ridge, itselfformed and probably still fed by the high concentration of gas observed onlarger scales in the central subregion. The time sequence obtained from thecombined study of the clump and YSO populations in NGC 2264 suggests that thestar formation started in the northern subregion, that it is now activelydeveloping at the center and will soon start in the southern subregion. Takentogether, the cloud structure and the clump and YSO populations in NGC 2264argue for a dynamical scenario of star formation.

Mass segregation and sequential star formation in NGC 2264 revealed by Herschel