Atomic Carbon in the AFGL 333 Cloud
Atomic Carbon in the AFGL 333 Cloud
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DOI：
10.1086/504861
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发表时间：
2006-09
期刊：
影响因子：
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通讯作者：
T. Sakai;T. Oka;S. Yamamoto
中科院分区：
文献类型：
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作者：
T. Sakai;T. Oka;S. Yamamoto
我们用富士山亚毫米波望远镜在C 0 3 P1 - 3 P0（[CI] 492 GHz）和12 CO J = 3-2发射谱线上绘制了W3巨分子云。[C I]分布在分子云上延伸，在三个形成云的星星W3 Main、W3（OH）和AFGL 333处有峰值。AFGL 333云的[C I]发射较强，而12 CO J = 3-2发射相对较弱。为了表征AFGL 333云的物理和化学状态，我们还用野边山射电天文台45米望远镜观测了CO J = 1-0同位素谱线和CCS和N_2H ~+谱线。AFGL 333云的[C 0]/[CO]和[CCS]/[N2 H +]丰度比高于W3（OH）云，表明AFGL 333云比W3（OH）云年轻。在AFGL 333云中，我们发现了两个巨大的核心，没有任何活跃的星星形成的迹象。它们被高度引力束缚，被认为是巨大星前核的良好候选者。
We have mapped the W3 giant molecular cloud in the C0 3P1-3P0 ([C I] 492 GHz) and 12CO J = 3-2 emission lines with the Mount Fuji Submillimeter-wave Telescope. The [C I] distribution is extended over the molecular cloud, having peaks at three star forming clouds, W3 Main, W3(OH), and AFGL 333. The [C I] emission is found to be strong in the AFGL 333 cloud, where the 12CO J = 3-2 emission is relatively weak. In order to characterize the physical and chemical states of the AFGL 333 cloud, we have also observed the CO J = 1-0 isotopomer lines and the CCS and N2H+ lines with the Nobeyama Radio Observatory 45 m Telescope. The [C0]/[CO] and [CCS]/[N2H+] abundance ratios are found to be higher in the AFGL 333 cloud than in the W3(OH) cloud, suggesting that the AFGL 333 cloud is younger than the W3(OH) cloud. In the AFGL 333 cloud we have found two massive cores without any sign of active star formation. They are highly gravitationally bound and are regarded as good candidates for a massive prestellar core.