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We have carried out the observations of the OMC-2 FIR 3/4 region with the NMAand ASTE in the H$^{13}$CO$^{+}$ (1--0), $^{12}$CO (3--2, 1--0), SiO ($v$=0,$J$=2--1), CS (2--1), and CH$_3$OH ($J_K$=7$_K$--6$_K$) lines and in the 3.3 mmcontinuum emission. Our NMA observations in the H$^{13}$CO$^{+}$ emission haverevealed 0.07 pc-scale dense gas associated with FIR 4. The $^{12}$CO(3--2,1--0) emission shows high-velocity blue and red shifted components at theboth north-east and south-west of FIR 3, suggesting a molecular outflow nearlyalong the plane of the sky driven by FIR 3. The SiO and the CH$_{3}$OH emissionare detected around the interface between the outflow and the dense gas.Furthermore, the $^{12}$CO (1--0) emission shows an L-shaped structure in theP-V diagram. These results imply presence of the shock due to the interactionbetween the molecular outflow driven by FIR 3 and the dense gas associated withFIR 4. Moreover, our high angular-resolution observations of FIR 4 in the 3.3mm continuum emission have first found that FIR 4 consists of eleven dustycores. The separation among these cores is on the same order of the Jeanslength, suggesting that the fragmentation into these cores has been caused bythe gravitational instability. The time scale of the fragmentation is similarto the time scale of the interaction between the molecular outflow and thedense gas. We suggest that the interaction between the molecular outflow fromFIR 3 and the dense gas associated with FIR 4 triggered the fragmentation intothese dusty cores, and hence the next generation the cluster formation.

astrophysical journal/the astrophysical journal

Millimeter- and Submillimeter-Wave Observations of the OMC-2/3 Region.  II. Observational Evidence for Outflow-Triggered Star Formation in the OMC-2  FIR 3/4 Region