The Large- and Small-Scale Structures of Dust in the Star-forming Perseus Molecular Cloud
The Large- and Small-Scale Structures of Dust in the Star-forming Perseus Molecular Cloud
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DOI：
10.1086/503193
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发表时间：
2006-02
期刊：
影响因子：
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通讯作者：
H. Kirk;D. Johnstone;J. di Francesco
中科院分区：
文献类型：
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作者：
H. Kirk;D. Johnstone;J. di Francesco
我们提出了一个分析~3.5度2的亚毫米波连续谱和消光数据的英仙座分子云。我们在亚毫米图中识别出58个团块，在灭绝图中识别出39个结构（“核心”）和11个结构关联（“超级核心”）。亚毫米团块和消光核的累积质量分布具有较陡的斜率（α ~ 2和1.5-2），比Salpeter初始质量函数（IMF; α = 1.35）更陡，而消光超核的累积质量分布具有较浅的斜率（α ~ 1）。大多数亚毫米团块与10 K 5-7 mag的稳定Bonnor-Ebert球体很好地拟合，尽管Bonnor-Ebert模型表明，如果它们存在，我们应该能够在较低的柱密度下检测到它们。这些观测结果为灭绝阈值提供了一个比分析蛇夫座分子云的不太敏感的观测结果（Johnstone等人）更强的理由。分析了次毫米团块与其母消光核的关系。亚毫米波段的团块倾向于偏离较大的消光峰，这表明团块是通过外部触发事件形成的，与以前的观测结果一致。
We present an analysis of ~3.5 deg2 of submillimeter continuum and extinction data of the Perseus molecular cloud. We identify 58 clumps in the submillimeter map, and we identify 39 structures ("cores") and 11 associations of structures ("super cores") in the extinction map. The cumulative mass distributions of the submillimeter clumps and extinction cores have steep slopes (α ~ 2 and 1.5-2, respectively), steeper than the Salpeter initial mass function (IMF; α = 1.35), while the distribution of extinction super cores has a shallow slope (α ~ 1). Most of the submillimeter clumps are well fit by stable Bonnor-Ebert spheres with 10 K 5-7 mag), although Bonnor-Ebert models suggest that we should have been able to detect them at lower column densities if they exist. These observations provide a stronger case for an extinction threshold than that found in analysis of less sensitive observations of the Ophiuchus molecular cloud (Johnstone et al.). The relationship between submillimeter clumps and their parent extinction core has been analyzed. The submillimeter clumps tend to lie offset from the larger extinction peaks, suggesting that the clumps formed via an external triggering event, consistent with previous observations.