Astrophys. J., 683, 255-266 (2008/August-2)
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.
SHIMAJIRI Y., TAKAHASHI S., TAKAKUWA S., SAITO M. and KAWABE R.
Abstract (from CDS):
We have observed the Orion Molecular Cloud-2 FIR 3/4 region in the H13CO+ (J=1-0), 12CO (J=1-0), SiO (v=0, J=2-1), and CS (J=2-1) lines and the 3.3 mm continuum emission with the Nobeyama Millimeter Array (NMA) and in the CO (J=3-2) and CH3 OH (JK=7K-6K) lines with Atacama Submillimeter Telescope Experiment (ASTE). Our NMA observations in the H13CO+ emission have revealed 0.07 pc scale dense gas associated with FIR 4 (FIR 4 clump). The 12CO (J=3-2,1-0) emission shows high-velocity blue- and redshifted components to both the northeast and southwest of FIR 3, suggesting an outflow from FIR 3 along the plane of the sky. The SiO and CH3 OH emission, known as shock tracers, are detected around the interface between the outflow and FIR 4 clump. Furthermore, the 12CO (J=1-0) emission shows an L-shaped structure in the PV diagram. These results suggest the presence of an interaction between the outflow and FIR 4 clump. Moreover, our interferometric 3.3 mm continuum observations have first found that FIR 4 consists of 11 dusty cores at a scale of ∼2000 AU. The separation among these cores (∼5x103 AU) is on the same order of the Jeans length (∼13x103 AU), and the estimated time scale of the fragmentation (∼3.8x104 yr) is similar to the time scale of the outflow interaction (∼1.4x104 yr). We suggest that the interaction triggered the fragmentation into these dusty cores, and hence the next generation of the cluster formation in FIR 4.
ISM: Clouds - ISM: Jets and Outflows - ISM: Molecules - Stars: Formation - stars: individual (OMC-2 FIR 3) - stars: individual (4) - stars: individual (5)
Fig.7, Table 4: [MWZ90] OMC-2 FIR 4a (Nos 4a-4k) added.
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