剖析猎户座B云的分子结构：来自主成分分析的见解
Dissecting the molecular structure of the Orion B cloud: Insight from Principal Component Analysis
摘要：
上下文目前在（亚）毫米观测站中可用的宽带接收器和光谱仪的组合提供了星际介质的宽视场高光谱成像。在大约50小时内，在度宽的视场内可以观察到数十条谱线。这些丰富的数据需要用统计学的术语来重新阐述有关星际介质的物理问题。目标。我们的目标是获得信息的物理结构的星际介质从统计分析的许多线从不同的物种在一个大的视野，而不需要详细的辐射转移或天体化学建模。方法.我们将数据的非线性重新缩放与最简单的多变量分析方法之一，即主成分分析相结合，将观测到的信号分解为我们首先定性解释的成分，然后根据我们对观测区域和天体化学的深入了解进行定量解释。结果我们确定了3个主成分，线性组成的线亮度温度，在不同的水平与列密度，体积密度和紫外辐射场。结论.当对物理参数的充分不同的混合物进行采样时，有可能分解分子发射，以便获得对所观察到的星际介质的物理见解。这为今后研究星际介质开辟了一条新的途径。
英文摘要：
Context. The combination of wideband receivers and spectrometers currently available in (sub-)millimeter observatories deliver wide- field hyperspectral imaging of the interstellar medium. Tens of spectral lines can be observed over degree wide fields in about fifty hours. This wealth of data calls for restating the physical questions about the interstellar medium in statistical terms. Aims. We aim at gaining information on the physical structure of the interstellar medium from a statistical analysis of many lines from different species over a large field of view, without requiring detailed radiative transfer or astrochemical modeling. Methods. We coupled a nonlinear rescaling of the data with one of the simplest multivariate analysis methods, namely the Principal Component Analysis, to decompose the observed signal into components that we interpret first qualitatively and then quantitatively based on our deep knowledge of the observed region and of the astrochemistry at play. Results. We identify 3 principal components, linear compositions of line brightness temperatures, that are correlated at various levels with the column density, the volume density and the UV radiation field. Conclusions. When sampling a sufficiently diverse mixture of physical parameters, it is possible to decompose the molecular emission in order to gain physical insight on the observed interstellar medium. This opens a new avenue for future studies of the interstellar medium.
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