We have mapped the C 3 H 2 2 12 − 1 01 transition line toward the Sgr A molecular cloud on a 1' grid spacing and derived C 3 H 2 column densities of 3 \~ 7 × 10 14 c m − 2 for molecular clouds of Sgr A. The fractional abundances of C 3 H 2 relative to H 2 are obtained to be 3 \~ 6 × 10 − 9 , which are slightly lower than that for the cold dark cloud TMC-1 but are enhanced by factors of 5-60 compared to those for Sgr B2 and the Orion extended ridge. We also estimate from the C 3 H 2 column densities total masses of \~ 10 6 M ⨀ for two clouds (M - 0.13 - 0.08 and M - 0.02 - 0.07), which are thought to be close to the virial equilibrium. We suggest that the large abundance of C 3 H 2 in Sgr A may be partly due to the activities of the Galactic center.

ABSTRACT
Ⅰ. INTRODUCTION
Ⅱ. OBSERVATIONS
Ⅲ. RESULTS
Ⅳ. DISCUSSION
ACKNOWLEDGEMENTS
REFERENCES

• C. W. LEE(Department of Earth Science, Pusan National University)
• Y. C. MINH(Daeduk Radio Astronomy Observatory, KAO))
• W. M. IRVINE(Five College Astronomy Observatory and Department of Physics and Astronomy, University of Massachusetts)