HIGH ATOMIC CARBON ABUNDANCE IN MOLECULAR CLOUDS IN THE GALACTIC CENTER REGION
HIGH ATOMIC CARBON ABUNDANCE IN MOLECULAR CLOUDS IN THE GALACTIC CENTER REGION
复制标题
银河系中心区域分子云中的高原子碳丰度
DOI:
10.1088/2041-8205/743/2/l39
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发表时间:
2011
期刊:
影响因子:
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通讯作者:
K. Kamegai
中科院分区:
文献类型:
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作者:
Kunihiko Tanaka;T. Oka;S. Matsumura;M. Nagai;K. Kamegai
This Letter presents a Nyquist-sampled, high-resolution [C i] 3P1–3P0 map of the −0.°2 < l < 1.°2 × −0.°1 < b < 0° region in the Central Molecular Zone (CMZ) taken with the Atacama Submillimeter Telescope Experiment 10 m telescope. We have found that molecular clouds in the CMZ can be classified into two groups according to their [C i]/13CO intensity ratios: a bulk component consisting of clouds with a low, uniform [C i]/13CO ratio (0.45) and another component consisting of clouds with high [C i]/13CO ratios (>0.8). The [C i]-enhanced regions appear in M−0.02−0.07, the circumnuclear disk, the 180 pc ring, and the high-velocity compact cloud CO+0.02−0.02. We have carried out a large velocity gradient analysis and have derived the C0/CO column density ratio for M−0.02−0.07 as 0.47, which is approximately twice that of the bulk component of the CMZ (0.26). We propose several hypotheses on the origin of high C0 abundance in M−0.02−0.07, including cosmic-ray/X-ray dissociation and mechanical dissociation of CO in the pre-existing molecular clouds. We also suggest the possibility that M−0.02−0.07 is a cloud at an early stage of chemical evolution from diffuse gas, which was possibly formed by the bar-induced mass inflow in the Galactic center region.