Hostname: page-component-78c5997874-xbtfd Total loading time: 0 Render date: 2024-11-05T03:37:56.019Z Has data issue: false hasContentIssue false
  • English
  • Français

The Orion Star-Forming Complex

Published online by Cambridge University Press:  04 August 2017

Tetsuo Hasegawa
Tetsuo Hasegawa*
Affiliation:
Nobeyama Radio Observatory, Tokyo Astronomical Observatory, University of Tokyo, Nobeyama, Minamisaku, Nagano 384-13, Japan

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

High resolution images of the Orion Nebula in the millimeter wave emission lines of CS and CO taken with the 45-m telescope at Nobeyama are presented. They cover a field approximately 400″ square with a 15″ – 34″ resolution and reveal a wealth of information on kinematic and density structures. The images of the J=1-0 (49 GHz) and J=2-1 (98 GHz) lines of CS show a long (>1 pc) and narrow (∼0.1 pc) N-S ridge of dense molecular gas. On the ridge, two major clumps are recognized; one is associated with the KL object and the other is 100″ south of it. The images of the J=1-0 (115 GHz) CO line indicate interaction between the molecular cloud and the H II region formed by the Trapezium stars. Bright CO emission is found towards the edges of the denser part of the H II region delineated by radio continuum emission. The CO emission coincides with the emission of vibrationally excited H2 and the 3.3 μm dust emission feature. The CO images reveal filamentary structures (“streamers”) stretching radially from the KL region. On the streamers there are Herbig-Haro objects moving away from the KL region. They may be tracers of weak interaction between the ambient molecular gas and mostly unseen, highly collimated, high-velocity (>200 km/s) jets.

Type
I. Star Forming Processes in the Solar Neighborhood
Information
Symposium - International Astronomical Union , Volume 115: Star Forming Regions , 1987 , pp. 123 - 137
Copyright
Copyright © Reidel 1987 

References

Axon, D. J., and Taylor, K. 1984, M. N. R. A. S., 207, 241.Google Scholar
Bastien, P., Batrla, W., Henkel, C., Pauls, T., Walmsley, C. M., and Wilson, T. L. 1985, Astron. Astrophys., 146, 86.Google Scholar
Batrla, W., Wilson, T. L., Bastien, P. and Ruf, K. 1983, Astron. Astrophys., 128, 279.Google Scholar
Evans, N. J. II, Zuckermann, B., Sato, T., and Morris, G. 1975, Astrophys. J. (Letters), 261, L103.Google Scholar
Gatley, I., and Kaifu, N. 1987, in Astrochemistry, IAU Symposium No. 120, ed. Vardya, M. S. and Tarafdar, S. P., to be published.Google Scholar
Goldsmith, P. F., Langer, W. D., Schloerb, F. P., and Scoville, N. Z. 1980, Astrophys. J., 240, 524.Google Scholar
Hasegawa, T. 1986, Astrophys. Sp. Sci., 118, 421.Google Scholar
Hasegawa, T., Kaifu, N., Inatani, J., Morimoto, M., Chikada, Y., Hirabayashi, H., Iwashita, Y., Morita., K.-I., Tojo, A., and Akabane, K. 1984, Astrophys. J., 283, 117.Google Scholar
Hayashi, M., Hasegawa, T., Gatley, I., Garden, R., and Kaifu, N. 1985, M. N. R. A. S., 215, 31P.CrossRefGoogle Scholar
Jaffe, D. T., Davidson, J. A., Dragovan, M., and Hildebrand, R. H. 1984, Astrophys. J., 284, 637.Google Scholar
Jones, B. F., and Walker, M. F. 1985, Astron. J., 90, 1320.Google Scholar
Johnston, K. J., Palmer, P., Wilson, T. L., and Bieging, J. 1983, Astrophys. J. (Letters), 271, L89.Google Scholar
Keene, J., Hildebrand, R. H., and Whitcomb, S. E. 1982, Astrophys. J. (Letters), 252, L11.Google Scholar
Kutner, M. L., Evans, N. J. II, and Tucker, K. D. 1976, Astrophys. J., 209, 452.Google Scholar
Kutner, M. L., Tucker, K. D., Chin, G., and Thaddeus, P. 1977, Astrophys. J., 215, 521.Google Scholar
Linke, R. A., and Wannier, P. G. 1974, Astrophys. J. (Letters), 193, L41.Google Scholar
Liszt, H. S., and Linke, R. A. 1975, Astrophys. J., 196. 709.CrossRefGoogle Scholar
Liszt, H. S., Wilson, R. W., Penzias, A. A., Jefferts, K. B., Wannier, P. G., and Solomon, P. M. 1974, Astrophys. J., 190, 557.Google Scholar
Münch, G. 1977, Astrophys. J. (Letters), 212, L77.Google Scholar
Olofsson, H., Elldér, J., Hjalmarson, A., and Rydbeck, G. 1982, Astron. Astrophys., 113, L18.Google Scholar
Omodaka, T., Hayashi, M., and Hasegawa, T. 1984, Astrophys. J. (Letters), 282, L77.Google Scholar
Omodaka, T. et al. 1987, these proceedings.Google Scholar
Plambeck, R. L., Wright, M. C. H., Welch, W. J., Bieging, J. H., Baud, B., Ho, P. T. P., and Vogel, S. N. 1982, Astrophys. J., 259, 617.Google Scholar
Schloerb, F. P., Goldsmith, P. F., and Scoville, N. Z. 1982, in Regions of Recent Star Formation, ed. Roger, R. S. and Dewdney, P. E. (Dordrecht: D. Reidel), p.439.CrossRefGoogle Scholar
Schloerb, F. P., and Loren, R. B. 1982, in Symposium on the Orion Nebula to Honor Henry Draper, ed. Glassgold, A. E., Huggins, P. J., and Schucking, E. L. (New York: New York Academy of Sciences), p. 32.Google Scholar
Sugitani, K., Fukui, Y., Ogawa, H., and Kawabata, K. 1986, Astrophys. J., in press.Google Scholar
Taylor, K. N. R., Storey, J. W. V., Sandell, G., Williams, P. M., and Zealey, W. J. 1984, Nature, 311, 236.Google Scholar
Tielens, A.G.G.M., and Hollenbach, D. 1985, Astrophys. J., 291, 722.Google Scholar
Vogel, S. N., Bieging, J. H., Plambeck, R. L., Welch, W. J., and Wright, M. C. H. 1985, Astrophys. J., 296, 600.Google Scholar