We have conducted millimeter interferometric observations of the Orion Molecular Cloud-2 ( OMC-2 ) FIR 6 region at an angular resolution of \sim 4 \arcsec - 7 \arcsec with the Nobeyama Millimeter Array ( NMA ) .
In the 3.3 mm continuum emission we detected dusty core counterparts of the previously identified FIR sources ( FIR 6a , 6b , 6c , and 6d ) , and moreover , resolved FIR 6a into three dusty cores .
The size and mass of these cores are estimated to be 1100-5900 AU and 0.19-5.5 M _ { \odot } , respectively .
We found that in the ^ { 12 } CO ( J =1–0 ) emission FIR 6b , 6c , and 6d eject the molecular outflow and that the FIR 6c outflow also exhibits at least two collimated jet-like components in the SiO ( J =2–1 ) emission .
At the tip of one of the SiO components there appears abrupt increase of the SiO line width ( \sim 15 km s ^ { -1 } ) , where the three resolved cores in FIR 6a seem to delineate the tip .
These results imply the presence of the interaction and the bowshock front between the FIR 6c molecular outflow and FIR 6a . If the interaction occurred after the formation of the FIR 6a cores the influence of the FIR 6c outflow on the FIR 6a cores is minimal , since the total gravitational force in the FIR 6a cores ( 1.0 - 7.7 \times 10 ^ { -4 } M _ { \odot } km s ^ { { } ^ { 1 } } yr ^ { -1 } ) is much larger than the outflow momentum flux ( 2.4 \times 10 ^ { -5 } M _ { \odot } km s ^ { { } ^ { 1 } } yr ^ { -1 } ) .
On the other hand , it is also possible that the interaction caused the gravitational instability in FIR 6a , and triggered the fragmentation into three cores , since the separation among these cores ( \sim 2.0 \times 10 ^ { 3 } AU ) is on the same order of the Jeans length ( \sim 5.0 - 8.4 \times 10 ^ { 3 } AU ) .
In either case , FIR 6a cores , with a mass of 0.18 - 1.6 M _ { \odot } and a density of 0.2 - 5.8 \times 10 ^ { 7 } cm ^ { -3 } , might be potential formation sites of the next generation of cluster members .