A CO J = 3–2 Survey of the Galactic Center
A CO J = 3–2 Survey of the Galactic Center
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DOI：
10.1093/pasj/59.1.15
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发表时间：
2007-01
影响因子：
2.3
通讯作者：
T. Oka;M. Nagai;K. Kamegai;Kunihiko Tanaka;Nobuyuki Kuboi
中科院分区：
文献类型：
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作者：
T. Oka;M. Nagai;K. Kamegai;Kunihiko Tanaka;Nobuyuki Kuboi
利用阿塔卡玛亚毫米波望远镜实验（ASTE）在CO J=3-2线上观测了银河系中心分子带（CMZ）。银河系中心的分子气体显示出高的J=3-2/J=1-0强度比（~ 0.9），而银河系盘中旋臂中的气体显示出较低的强度比（~ 0.5）。高速致密云CO 0.02-0.02和高能壳层CO 1.27+0.01，以及Sgr A区的气体都表现出超过1.5的高J=3-2/J=1-0强度比。我们还发现了一些高比率气体的小斑点。这些高比率的斑点中的一些具有大的速度宽度，并且一些似乎与非热的线或细丝相关联。这些可能是被未知超新星冲击的热分子气体点，这些超新星在CMZ中可能很丰富。
We have surveyed the central molecular zone (CMZ) of our Galaxy in the CO J=3-2 line with the Atacama Submillimeter-wave Telescope Experiment (ASTE). Molecular gas in the Galactic center shows high J=3-2/J=1-0 intensity ratio (~ 0.9) while gas in the spiral arms in the Galactic disk shows the lower ratio (~ 0.5). The high-velocity compact cloud CO 0.02-0.02 and the hyperenergetic shell CO 1.27+0.01, as well as gas in the Sgr A region exhibit high J=3-2/J=1-0 intensity ratio exceeding 1.5. We also found a number of small spots of high ratio gas. Some of these high ratio spots have large velocity widths and some seem to associate with nonthermal threads or filaments. These could be spots of hot molecular gas shocked by unidentified supernovae which may be abundant in the CMZ.