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We have observed the young protostellar system NGC 2264 CMM3 in the 1.3 mmand 2.0 mm bands at a resolution of about 0.1$"$ (70 au) with ALMA. Thestructures of two distinct components, CMM3A and CMM3B, are resolved in thecontinuum images of both bands. CMM3A has an elliptical structure extendingalong the direction almost perpendicular to the known outflow, while CMM3Breveals a round shape. We have fitted two 2D-Gaussian components to theelliptical structure of CMM3A and CMM3B, and have separated the disk andenvelope components for each source. The spectral index $\alpha$ between 2.0 mmand 0.8 mm is derived to be 2.4-2.7 and 2.4-2.6 for CMM3A and CMM3B,respectively, indicating the optically thick dust emission and/or the graingrowth. A velocity gradient in the disk/envelope direction is detected forCMM3A in the CH$_3$CN, CH$_3$OH, and $^{13}$CH$_3$OH lines detected in the 1.3mm band, which can be interpreted as the rotation of the disk/envelope system.From this result, the protostellar mass of CMM3A is roughly evaluated to be$0.1- 0.5$ $M_\odot$ by assuming Keplerian rotation. The mass accretion rate isthus estimated to be $5\times10^{-5}$ - 4 $\times$ $10^{-3}$ $M_\odot$yr$^{-1}$, which is higher than typical mass accretion rate of low-massprotostars. The OCS emission line shows a velocity gradient in both outflowdirection and disk/envelope direction. A hint of outflow rotation is found, andthe specific angular momentum of the outflow is estimated to be comparable tothat of the disk. These results provide us with novel information on theinitial stage of a binary/multiple system.

Exploring the 100 au Scale Structure of the Protobinary System NGC 2264 CMM3 with ALMA