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During the transition phase from a prestellar to a protostellar cloud core,one or several protostars can form within a single gas core. The detailedphysical processes of this transition, however, still remain unclear. Wepresent 1.3 mm dust continuum and molecular line observations with the AtacamaLarge Millimeter/submillimeter Array (ALMA) toward 43 protostellar cores in theOrion Molecular Cloud Complex ($\lambda$ Orionis, Orion B, and Orion A) with anangular resolution of $\sim$ 0.35" ($\sim$ 140 au). In total, we detect 13binary/multiple systems. We derive an overall multiplicity frequency (MF) of28$\%$ $\pm$ 4$\%$ and a companion star fraction (CSF) of 51$\%$ $\pm$ 6$\%$,over a separation range of 300-8900 au. The median separation of companions isabout 2100 au. The occurrence of stellar multiplicity may depend on thephysical characteristics of the dense cores. Notably, those containingbinary/multiple systems tend to show higher gas density and Mach number thancores forming single stars. The integral-shaped filament (ISF) of Orion A giantmolecular cloud (GMC), which has the highest gas density and hosts high-massstar formation in its central region (the Orion Nebula cluster), shows thehighest MF and CSF among the Orion GMCs. In contrast, the $\lambda$ OrionisGiant Molecular Cloud (GMC) has a lower MF and CSF than the Orion B and Orion AGMCs, indicating that feedback from HII regions may suppress the formation ofmultiple systems. We also find that the protostars comprising a binary/multiplesystem are usually at different evolutionary stages.

ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): How do dense core properties affect the multiplicity of protostars?