Hostname: page-component-76fb5796d-5g6vh Total loading time: 0 Render date: 2024-04-27T00:01:10.219Z Has data issue: false hasContentIssue false
  • English
  • Français

Aperture Synthesis Observations of NH3 and CS in Orion-KL

Published online by Cambridge University Press:  12 April 2016

Y. Murata ,
R. Kawabe ,
M. Ishiguro ,
T. Hasegawa ,
T. Takano ,
T. Kasuga ,
K.-I. Morita  and
M. Hayashi
Y. Murata
Affiliation:
Department of Astronomy, Faculty of Science, The University of Tokyo
R. Kawabe
Affiliation:
Nobeyama Radio Observatory, National Astronomical Observatory
M. Ishiguro
Affiliation:
Nobeyama Radio Observatory, National Astronomical Observatory
T. Hasegawa
Affiliation:
Institute of Astronomy, Faculty of Science, The University of Tokyo
T. Takano
Affiliation:
Nobeyama Radio Observatory, National Astronomical Observatory
T. Kasuga
Affiliation:
Nobeyama Radio Observatory, National Astronomical Observatory
K.-I. Morita
Affiliation:
Nobeyama Radio Observatory, National Astronomical Observatory
M. Hayashi
Affiliation:
Department of Astronomy, Faculty of Science, The University of Tokyo

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.

We have made aperture synthesis maps of Orion-KL in NH3(1,1),(2,2) and CS(J=l-0) emissions using the Nobeyama Millimeter Array. Both NH3 and CS maps show new detailed structures that have not been recognized before. Two NH3 filaments in the size of ~0.45 pc x0.04 pc are found extending to the northwest direction of Orion-KL. These filaments are associated with the HH objects and the finger-like H2 emissions; they are probably formed through the interaction with high velocity, highly channeled winds from the KL region. The CS maps show, on the other hand, shell structures around IRc2 as well as the well-known rotating disk. These shells coincide with the two lobes of the shock-excited H2 emission, being interpreted as the shock-compressed shells of ambient molecular gas interacting with the outflow from IRc2.

Type
IV. The Orion Nebula
Information
International Astronomical Union Colloquium , Volume 120: Structure and Dynamics of the Interstellar Medium , 1989 , pp. 327 - 332
Copyright
Copyright © Springer-Verlag 1989

References

Axon, D.J., and Taylor, K. 1984, Monthly Notices R.Astron.Soc, 270, 241.CrossRefGoogle Scholar
Bally, J. and Lada, C.,J. 1983, Astrophys.J., 265, 824.CrossRefGoogle Scholar
Batrla, W., Wilson, T.L., Bastien, P., and Ruf, K. 1983, Astron.Astrophys., 128, 279.Google Scholar
Beckwith, S., Persson, S.E., Neugebauer, G., and Becklin, E.E. 1978, Astrophys.J., 223,464.CrossRefGoogle Scholar
Chikada, Y. et al. 1987, Proc. of the IEEE, 75, No.9, 1203.CrossRefGoogle Scholar
Downes, D., Genzel, R., Becklin, E.E., and Wynn-Williams, C.G. 1981, Astrophys.J., 244, 869.CrossRefGoogle Scholar
Erickson, N.R., Goldsmith, P.F., Snell, R.L. Berson, R.L. Huguenin, G.R.,Ulich, B.L. and Lada, C.J. 1982, Astrophys. J.(Letters), 261, L103.CrossRefGoogle Scholar
Genzel, R., Reid, M.J., Moian, J.M., and Dowens, D. 1981, Astrophys.J., 244, 884.CrossRefGoogle Scholar
Hasegawa, T. et al. 1984, Astrophys.J., 283, 117.CrossRefGoogle Scholar
Hasegawa, T. et al. 1989, in preparationGoogle Scholar
Ishiguro, M. et al. 1984, in the proceedings Int. Symp. Milli-meter and Submillimeter Wave Radio Astronomy, Granada, 75 Google Scholar
Jones, B.F., and Walker, M.F. 1985, Astron.J., 90, 1320.CrossRefGoogle Scholar
Kasnga, T., Kawabe, R., Ishiguro, M., Yamada, K., Kurihara, H., Niori, M., and Hirachi, Y. 1987, Rev. Sci. Instrum., 58, 379 Google Scholar
Kawabe, R., et al. 1989, in preparationGoogle Scholar
Königl, A. 1982, Astrophys.J., 261, 155.CrossRefGoogle Scholar
Masson, C.R., Lo, K.Y., Phillips, , Sargent, A.I., Scoville, N.Z., and Woody, D.P. 1987, Astrophys.J., 319, 446.CrossRefGoogle Scholar
Mundy, L.G., Cornwell, T.J., Masson, C.R., Scoville, N.Z., Baath, L.B., and Johanssen, E.B. 1988, Astrophys.J., 325, 382.CrossRefGoogle Scholar
Okuda, T. and Ikeuchi, S. 1986 Publ.Astron.Soc. Japan, 38, 199.Google Scholar
Olofsson, J., Ellder, ,Hjalmarson, A., and Rydbeck, G., 1982, Astron.Astrophys., 113, L18.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.(Letters), 259, 617.CrossRefGoogle Scholar
Rudolph, A. and Welch, W.J. 1988, Astrophys. J.(Letters), 326, L31.CrossRefGoogle Scholar
Taylor, K.N.R., Storey, J.W.V., Sandell, G., Williams, P.M., and Zealey, W.J. 1984, Nature, 311, 236.CrossRefGoogle Scholar
Vogel, S.N., Bieging, J.H., Plambeck, R.L., Welch, W.J., Wright, M.C.H. 1985, Astrophys.J., 296, 600.CrossRefGoogle Scholar
Wright, M.C.H., Plambeck, R.L., Vogel, S.N., Ho, P.T.P., and Welch, W.J. 1983, Astrophys. J.(Letters), 267, L41.CrossRefGoogle Scholar
Wynn-Williams, C.G., Genzel, R., Becklin, E.E., and Downes, D. 1984, Astrophys.J., 281, 172.CrossRefGoogle Scholar