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CS(J = 2-1) Observations of B335

Published online by Cambridge University Press:  04 August 2017

Osamu Kameya ,
Tatsuhiko Hasegawa ,
Naomi Hirano ,
Keiya Takakubo  and
Munezo Seki
Osamu Kameya
Affiliation:
Astronomical Institute, Faculty of Science, Tohoku University, Sendai, Japan
Tatsuhiko Hasegawa
Affiliation:
Astronomical Institute, Faculty of Science, Tohoku University, Sendai, Japan
Naomi Hirano
Affiliation:
Astronomical Institute, Faculty of Science, Tohoku University, Sendai, Japan
Keiya Takakubo
Affiliation:
Astronomical Institute, Faculty of Science, Tohoku University, Sendai, Japan
Munezo Seki
Affiliation:
College of General Education, Tohoku University, Sendai, Japan

Extract

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CS(J = 2-1) observations of B335 are carried out using the NRO 45-m telescope with a 16″ beam. We get many self-reversed profiles with good S/N ratio. Assuming that this region consists of a core and a halo, we get the molecular hydrogen density and the CS relative abundance in the halo. The CS wings are located within the cavity of the CO wing (Goldsmith et al. 1984).

Type
I. Star Forming Processes in the Solar Neighborhood
Information
Symposium - International Astronomical Union , Volume 115: Star Forming Regions , 1987 , pp. 366 - 367
Copyright
Copyright © Reidel 1987 

References

Goldsmith, P.F., Snell, R.L., Hemeon-Heyer, M., and Langer, W.D.: 1984, Astrophys. J. 286, 599.Google Scholar
Hasegawa, T., Hirano, N., Kameya, O., Taniguchi, Y., Tosa, M., Takakubo, K., and Seki, M.: 1986, Publ. Astron. Soc. Japan 38, No. 3, in press.Google Scholar
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Menten, K.M., Walmsley, C.M., and Ungerechts, H.: 1984, Astron. Astrophys. 137, 108.Google Scholar
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