The Orion Molecular Cloud 2 (OMC-2) in the northern part of Orion A (d = 400 pc) is known as an embedded protocluster containing a large number of infrared sources (400 pc^{-2}; Lada & Lada 2003). In the OMC-2, fifteen young sources are clustering within three millimeter sources, FIR3, FIR4, and FIR5 (Chini et al. 1997, Farlan et al. 2016).
This poster introduces the results and discussions presented by Sato et al. (2023). Using the Atacama Large Millimeter/submillimeter Array (ALMA), we performed mosaic observations toward FIR3, FIR4, and FIR5, covering an area of 0.35 pc x 0.23 pc (~2’.9 × 1’.9), in the 1.3 mm continuum, CO(J = 2--1) line, and SiO(J = 5--4) line emissions. We identified 51 continuum sources, 36 of which are newly identified in Sato et al. (2023). Their dust masses, projected sizes, and H_2 gas number densities are estimated to be 3.8 × 10^{-5} -- 1.1 × 10^{-2} Msun, 290--2000 au, and 6.4 × 10^{6} -- 3.3 × 10^{8} cm^{-3}, respectively. The results of a Jeans analysis showed that, among the identified continuum sources, ~80% of the protostellar sources and ~15% of the prestellar sources are gravitationally bound. We identified 12 molecular outflows traced in the CO(J = 2--1) emission, six of which are newly detected. We identified shocked gas originating from outflows and other shocked regions traced by the SiO(J = 5--4) emission in this region. These results provide direct evidence of an interaction between a dust condensation, FIR4, and an energetic outflow driven by HOPS-370 within FIR3. In this poster, we also discuss how identified molecular outflows interact with other cluster members, and how the interaction might affect the consequential star formation within the embedded cluster at their earliest evolutionary stage.