• Journal of The Korean Astronomical Society
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• v.26 no.1
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• pp.73-78
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• 1993

We have mapped the $C_3H_2\;2_{12}-1_{01}$ transition line toward the Sgr A molecular cloud on a 1' grid spacing and derived $C_3H_2$ column densities of $3\~7\times10^{14}\;cm^{-2}$ for molecular clouds of Sgr A. The fractional abundances of $C_3H_2$ relative to $H_2$ are obtained to be $3\~6\times10^{-9}$, 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 $C_3H_2$ column densities total masses of $\~10^6\; M_\bigodot$ 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 $C_3H_2$ in Sgr A may be partly due to the activities of the Galactic center.

• Journal of Astronomy and Space Sciences
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• v.21 no.4
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• pp.233-242
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• 2004

The $HCO^+$ 1-0 transition line was observed toward the Sgr B2 region in our Galactic center. We found that there exist two large-scale velocity structures of $v_{lsr}\;{\sim}50\;and\;{\sim}100kms^{-1}$, which are thought to interact with each other. A new gas clump 'OF28 Cloud'('Odenwald & Fazio FIR 38' Cloud), showing different chemical and kinematical properties with the Sgr B2(M) cloud, was found in the $50kms^{-1}$ gas component. Toward the core of this component, we derive the $HCO^+$ total column density, $N(HCO^+)=(2-5){\times}10^{14}cm^{-2}$ and the mass $M=1{\times}10^6M_{\odot}$, by estimating its size, ${\sim}15pc$, from the half-power width of this component. We also found that there is a highly turbulent component in this region in the velocity range of about $100kms^{-1}$. The column density of this component is $N(HCO^+)=1{\times}10^{13}cm^{-2}$. The $HCO^+$ in this region may form effectively by the reaction between $C^+$ and OH, which are the elements whose abundances increase rapidly in shocked region.