Hostname: page-component-8448b6f56d-gtxcr Total loading time: 0 Render date: 2024-04-20T03:32:32.854Z Has data issue: false hasContentIssue false
  • English
  • Français

Aperture Synthesis Observations of CS, NH3, and Continuum in the Bipolar Flow Source NGC2071-IRS

Published online by Cambridge University Press:  12 April 2016

R. Kawabe ,
M. Kitamura ,
M. Ishiguro ,
T. Hasegawa ,
Y. Chikada  and
S. K. Okumura
R. Kawabe
Affiliation:
NOBEYAMA RADIO OBSERVATORY, NATIONAL ASTRONOMICAL OBSERVATORY
M. Kitamura
Affiliation:
NOBEYAMA RADIO OBSERVATORY, NATIONAL ASTRONOMICAL OBSERVATORY
M. Ishiguro
Affiliation:
NOBEYAMA RADIO OBSERVATORY, NATIONAL ASTRONOMICAL OBSERVATORY
T. Hasegawa
Affiliation:
INSTITUTE OF ASTRONOMY, UNIVERSITY OF TOKYO
Y. Chikada
Affiliation:
NOBEYAMA RADIO OBSERVATORY, NATIONAL ASTRONOMICAL OBSERVATORY
S. K. Okumura
Affiliation:
NOBEYAMA RADIO OBSERVATORY, NATIONAL ASTRONOMICAL OBSERVATORY

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 observations of CS(J=l-0, 2-1) and NH3(1,1) lines and 49, 98, and 110 GHz continuum in NGC2071-1RS with the Nobeyama Millimeter Array. Wfe have obtained maps of these lines and continuum maps with 2”. 7-20” resolution, ffe have found that dense molecular gas has a disk structure with a radial scale ranging 0.01 pc - 0.1 pc and has a ring-like structure with expanding motion at the central 5000 AU region. We also have found that there exists double dust continuum sources which are separated by 2500 AU in projection and are apparently located at the inner edges of the ring. Our observational results suggest that the disk of molecular gas has a central hole formed by wind and UV radiation from a central young stellar object, the central part is expanding, and that dust continuum emission comes from tangential parts of the shock compressed ring (r~1300 AU, M(H2)~ 21-34 Mo, and n(H2)~ 109) at the most inner side of the disk structure. The other possible model of the dust continuum sources is a binary system of self-luminous young stellar objects.

Type
III. Discs, Outflows, Jets and HH Objects
Information
International Astronomical Union Colloquium , Volume 120: Structure and Dynamics of the Interstellar Medium , 1989 , pp. 254 - 259
Copyright
Copyright © Springer-Verlag 1989

References

Bally, J. 1982, Ap.J., 261, 261 Google Scholar
Chikada, Y. et al., 1987, Proc. of the IEEE, 75, No. 9. 1203 Google Scholar
Dent, W. R. F. et al. 1989, preprint.Google Scholar
Harvey, P.M., Campbell, M. F., Hoffmann, W. F., Thronson, H. A. Jr., and Gatley, I. 1979, Ap.J., 229, 990.Google Scholar
Hildebrand, R.H. 1983, Quant. J. R. A. S., 24, 1267.Google Scholar
Ishiguro, M. et al., 1984, in the proceedings of the International Synposium on Millimter and Submillimeter Wave Radio Astronomy, Granada, 11.Google Scholar
Ishiguro, M. et al., 1989, in preparation.Google Scholar
Kasuga, T., Kawabe, R., Ishiguro, , Yamada, K., Kurihara, H., Niori, H., and Hirachi, Y. 1987, Rev. Sci. Instrum., 58, 379.Google Scholar
Kawabe, R. et al. 1984, Ap. J. (Letters), L73. 1984.Google Scholar
Kawabe, R. et al. 1989, in preparation.Google Scholar
Kitamura, Y., Kawabe, R., Yamashita, T., and Hayashi, M., 1989, preprint.Google Scholar
Miyama, S. M., Hayashi, C., and Narita, S. 1984, Ap.J., 279, 621.Google Scholar
Persson, R. L., Geball, T. R., Simon, T. L., Lonsdale, C. J., and Baas, F. 1981, Ap. J. (Letters), 251, L85.Google Scholar
Plambeck, R. L., Wright, M. C. H., Bieging, J.H., Baud, B.. Ho, P. T. P., and Vogel, S.N. 1982, Ap.J. (Letters), 259, 617.Google Scholar
Rodriguez, L. F., Canto, J., Torrelles, J.M., and Ho, P. T. P. 1986, Ap. J. (Letters), 301, L25.Google Scholar
Sandel, Y., Nyman, L.A., Haschick, A., and Winnberg, A. 1984, in Lecture Notes in Physics (Nearby Molecular Clouds), 237, 234.Google Scholar
Scoville, N.Z., Sargent, A. I., Sanders, D. B., Claussen, M.J. Masson, C. R., Lo, K.Y., and Phillips, T. G. 1986, Ap.J., 303, 416.Google Scholar
Snell, R. and Bally, J., 1986. Ap.J., 303, 683.Google Scholar
Snell, R., Scoville, N. Z., Sanders, D. B., and Erickson, N.R. 1984. Ap.J., 284, 176.Google Scholar
Takano, T., Fukui, Y., Ogawa, H., Takaba, H., Kawabe, R., Fujimoto, Y., Sugitani, K., and Fujimoto, M. 1984, Ap. J. (Letters), 282, L69.Google Scholar
Takano, T., Stutzki, J., Fukui, Y., and Winnewissar, G. 1986, Astr.Ap., 167, 333.Google Scholar
Takano, T. 1986, Ap.J., 303, 349.Google Scholar
Wootten, A., Loren, R. B., Sandquist, A., Friberg, P.. and Hjalmarson, A. 1984, Ap.J., 279, 633.Google Scholar
Zhou, S., Evans II, N. J., and Mundy, L. C. 1989, preprint.Google Scholar