ASTE银心CO J=3-2巡天：探测CMZ中的激波分子气体
The ASTE Galactic Center CO J=3-2 Survey: Probing Shocked Molecular Gas in the CMZ
摘要：
大规模的CO调查显示，我们银河系的中央分子区（CMZ）的特点是一些膨胀的壳/弧，并通过一个特殊的人口的致密云与大的速度宽度-高速致密云（HVCCs）。2005年至2008年，我们利用阿塔卡马亚毫米波望远镜实验（ASTE）对CMZ进行了大规模的CO J=3-2调查。数据几乎覆盖了CMZ和Clump 2的全部范围，网格间距为34弧秒。将CO J=3-2的数据与野边山射电天文台45米望远镜的CO J=1- 0的数据进行了比较。CMZ中的分子气体具有比银盘中的分子气体高的J=3-2/J=1-0强度比[R（3 - 2/1 - 0）= 0.7]。我们用R（3-2/1-0）>=1.5的标准提取了高激发的光学薄气体。高R（3-2/1-0）气体的团块在Sgr A和Sgr C区域中被发现，接近SNR G 0.9+0.1，以及具有高能HVCC的三个区域; CO 1.27+0.01、CO -0.41-0.23和CO -1.21-0.12。我们还发现了一些小斑点的高R（3-2/1-0）气体的CMZ。这些高R（3-2/1-0）团块和斑点中的许多具有大的速度宽度，并且一些明显地与HVCC一致，这表明它们是受冲击的分子气体的斑点。它们的起源应该是局部爆炸事件，可能是超新星爆炸。这表明高能HVCC与大质量致密星团有关，这些星团是由恒星形成的微暴形成的。从大尺度到小尺度的能量流的粗略估计表明，超新星冲击可以在CMZ的湍流激活和气体加热的显着贡献。
英文摘要：
Large-scale CO surveys have revealed that the central molecular zone (CMZ) of our Galaxy is characterized by a number of expanding shells/arcs, and by a peculiar population of compact clouds with large velocity widths -- high-velocity compact clouds (HVCCs). We have performed a large-scale CO J=3-2 survey of the CMZ from 2005 to 2008 with the Atacama Submillimeter-wave Telescope Experiment (ASTE). The data cover almost the full extent of the CMZ and the Clump 2 with a 34 arcsec grid spacing. The CO J=3-2 data were compared with the CO J=1--0 data taken with the Nobeyama Radio Observatory 45 m telescope. Molecular gas in the CMZ exhibits higher J=3-2/J=1-0 intensity ratios [R(3-2/1-0)=0.7] than that in the Galactic disk [R(3-2/1-0)=0.4]. We extracted highly excited, optically thin gas by the criterion, R(3-2/1-0)>=1.5. Clumps of high R(3-2/1-0) gas were found in the Sgr A and Sgr C regions, near SNR G 0.9+0.1, and three regions with energetic HVCCs; CO 1.27+0.01, CO -0.41-0.23, and CO -1.21-0.12. We also found a number of small spots of high R(3-2/1-0) gas over the CMZ. Many of these high R(3-2/1-0) clumps and spots have large velocity widths, and some apparently coincides with HVCCs, suggesting that they are spots of shocked molecular gas. Their origin should be local explosive events, possibly supernova explosions. These suggest that the energetic HVCCs are associated with massive compact clusters, which have been formed by microbursts of star formation. Rough estimates of the energy flow from large to small scale suggest that the supernova shocks can make a significant contribution to turbulence activation and gas heating in the CMZ.
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