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To distinguish between the different theories proposed to explain massivestar formation, it is crucial to establish the distribution, the extinction,and the density of low-mass stars in massive star-forming regions. We analyzeddeep X-ray observations of the Orion massive star-forming region using theChandra Orion Ultradeep Project (COUP) catalog. We found that pre-main sequence(PMS) low-mass stars cluster toward the three massive star-forming regions: theTrapezium Cluster (TC), the Orion Hot Core (OHC), and OMC1-S. We derivedlow-mass stellar densities of 10^{5} stars pc^{-3} in the TC and OMC1-S, and of10^{6} stars pc^{-3} in the OHC. The close association between the low-massstar clusters with massive star cradles supports the role of these clusters inthe formation of massive stars. The X-ray observations show for the first timein the TC that low-mass stars with intermediate extinction are clustered towardthe position of the most massive star, which is surrounded by a ring ofnon-extincted low-mass stars. Our analysis suggests that at least two basicingredients are needed in massive star formation: the presence of dense gas anda cluster of low-mass stars. The scenario that better explains our findingsassumes high fragmentation in the parental core, accretion at subcore scalesthat forms a low-mass stellar cluster, and subsequent competitive accretion.

The role of low-mass star clusters in massive star formation in Orion