Cloud Structure and Physical Conditions in Star-forming Regions from Optical Observations. I. Data and Component Structure
Cloud Structure and Physical Conditions in Star-forming Regions from Optical Observations. I. Data and Component Structure
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光学观测中恒星形成区域的云结构和物理条件。
DOI：
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发表时间：
2004
期刊：
影响因子：
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通讯作者：
D. Welty
中科院分区：
文献类型：
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作者：
K. Pan;S. Federman;K. Cunha;V. Smith;D. Welty
我们展示了三个恒星形成区域 ρ Oph、Cep OB2 和 Cep OB3 中 29 条视线的星际 CN、CH、CH+、Ca I、K I 和 Ca II 吸收的高分辨率光谱（在~0.6-1.8 km s-1）。描述了观察结果和数据缩减。早期测量的总等效宽度与我们的结果之间的一致性非常好。然而，我们更高分辨率的光谱揭示了大多数视线中的复杂结构和紧密混合的成分。每个物种的速度分量结构是通过一起分析给定视线的六种物种的光谱来获得的。表格中的列密度和各个分量的多普勒参数是通过使用轮廓拟合方法来确定的。沿视线的总柱密度是通过对各个组件的轮廓拟合结果求和来计算的，并与表观光学深度方法的柱密度进行比较。对这些数据及其影响的更详细分析将在另一篇论文中介绍。
We present high-resolution optical spectra (at ∼0.6-1.8 km s-1) of interstellar CN, CH, CH+, Ca I, K I, and Ca II absorption toward 29 lines of sight in three star-forming regions, ρ Oph, Cep OB2, and Cep OB3. The observations and data reduction are described. The agreement between earlier measurements of the total equivalent widths and our results is quite good. However, our higher resolution spectra reveal complex structure and closely blended components in most lines of sight. The velocity component structure of each species is obtained by analyzing the spectra of the six species for a given sight line together. The tabulated column densities and Doppler parameters of individual components are determined by using the method of profile fitting. Total column densities along lines of sight are computed by summing results from profile fitting for individual components and are compared with column densities from the apparent optical depth method. A more detailed analysis of these data and their implications will be presented in a companion paper.