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Molecular-Line Studies of the Bipolar Flow Source GL490∗

Published online by Cambridge University Press:  04 August 2017

R. Kawabe ,
N. Kaifu ,
S. S. Hayashi  and
T. Hasegawa
R. Kawabe
Affiliation:
Department of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113, Japan Department of Astrophysics, Nagoya University, Chikusa-ku, Nagoya 464, Japan
N. Kaifu
Affiliation:
Nobeyama Radio Observatory∗, Nobeyama, Minamisaku, Nagano 384-14, Japan
S. S. Hayashi
Affiliation:
Department of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113, Japan
T. Hasegawa
Affiliation:
Nobeyama Radio Observatory∗, Nobeyama, Minamisaku, Nagano 384-14, Japan

Extract

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We have made HCO+ (J = 1-0), HCN (J = 1-0) and CS (J = 2-1) observations of a bipolar flow source GL490 (Lada and Harvey 1981; Snell et al. 1984) using the Nobeyama 45-m telescope with 20″ resolution. A HCO+ spectrum obtained toward a central infrared source (Harvey et al. 1979) has prominent line wings extending up to 15-25 km s−1 from the line center (Figure 1). Figure 2 shows a map of HCO+ high velocity emission more than 8 km s−1 off the line center. The emission has “head-tail”-structures in both the blue- and the red-shifted sides; a “head” with stronger emission and a “tail” with weaker narrow ridge emission extending to the opposite side of the “head” through the center. The “head” emission has the same bipolar structure as the CO flow. Intermediate velocity emission at 38 km s−1 from the line center shows (1) a narrow ridge elongated in the NE-SW direction, at the blue-shifted side, and (2) a pair of shell-like structures symmetrically placed SW and NE of the center of the high velocity emission, at the red-shifted side (Figure 3).

Type
I. Star Forming Processes in the Solar Neighborhood
Information
Symposium - International Astronomical Union , Volume 115: Star Forming Regions , 1987 , pp. 352 - 354
Copyright
Copyright © Reidel 1987 

References

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