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CS Lines and Dust Continuum Observations of the OMC2 Infrared Cluster

  • T. Umemoto (a1), N. Ohashi (a1), Y. Murata (a1), K. Tatematsu (a1) and M. Suzuki (a1)...

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It is known that stars in GMCs are often born as clusters. Recently, near infrared imaging has enabled us to study the young stars within molecular clouds (e.g., Lada & Lada 1991). Orion Molecular Cloud 2 (OMC2) is located 12' north of the Trapezium cluster in the Orion A cloud, and contains a cluster of about 20 near-IR sources and several FIR sources distributed within a diameter of 0.2 pc (Rayner et al... 1989; Johnson et al. 1990; Mezger, Wink, & Zylka 1990). By large scale mapping observations using the NRO 45 m telescope, this infrared cluster is found to be associated with a dense molecular core (Tatematsu et al. 1993, Umemoto et al. 1993). The region was observed using the Nobeyama Millimeter Array (NMA) to elucidate the structure and cluster formation process within a core.

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References

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Fischer, J., Sanders, D.B., Simon, M., & Solomon, M. 1985, ApJ, 293, 508
Johnson, J.J. et al., 1990, AJ, 100, 518
Lada, C.J. & Lada, E.A. 1991, in The Formation and Evolution of Star Clusters, A.S.P. Conference Series No.11, ed. James, K.A., (Chelsea: Michigan), p3
Mezger, P.G., Wink, J.E., & Zylka, R. 1990, A&A, 228, 95
Ohashi, N., Kawabe, R., Hayashi, M., Ishiguro, M. 1991, AJ, 102, 2054
Rayner, J., McLean, L., McCaughrean, M., & Aspin, C. 1989, MNRAS, 241, 469
Tatematsu, K. et al. 1993, ApJ, 404, 643
Umemoto, T. et al. 1993 in preparation
Wilking, B.A., Lada, C.J. & Young, E.T. 1989, ApJ, 340, 823

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