原星团云G0.253+0.016（`the Brick'）的模拟与观测辐射图中的复杂多尺度结构
The complex multi-scale structure in simulated and observed emission maps of the proto-cluster cloud G0.253+0.016 (`the Brick')
AI总结：
本文对比了原星团云the Brick的流体动力学模拟与ALMA观测，通过合成分子谱线图和结构分析发现，模拟在功率谱和分形维数上与观测一致，但密度PDF和惯性矩的差异表明需引入磁场等额外物理过程以完全解释气体结构。
摘要：
中央分子区（CMZ；银河系中心约500 pc的区域）处于强剪切、高气压和密度以及复杂化学的极端环境中，孕育了分子云。G0.253+0.016，也被称为`the Brick'，是这些云中最致密、最紧凑且最宁静的。阿塔卡马大型毫米波/亚毫米波阵列（ALMA）的高分辨率观测揭示了其复杂的层级结构。本文将近期关于the Brick的流体动力学模拟性质与ALMA观测结果进行了比较。为便于比较，我们对模拟进行后处理，并根据八种分子创建了分子谱线辐射的合成ALMA图。我们将谱线辐射图相互关联，并与质量柱密度进行相关分析，发现HNCO是模拟中八条辐射线里最佳的质量示踪剂。此外，我们利用密度概率分布函数（PDF）、空间功率谱、分形维数和惯性矩表征了观测和模拟云的空间结构。尽管在功率谱和分形维数方面，观测与模拟数据有很好的一致性，但在密度PDF和惯性矩上存在关键差异，我们将其归因于模拟中忽略了磁场。这表明银河系势场的存在可以重现许多云的性质，但需要额外的物理过程才能完全解释气体结构。
英文摘要：
The Central Molecular Zone (CMZ; the central ~ 500 pc of the Milky Way) hosts molecular clouds in an extreme environment of strong shear, high gas pressure and density, and complex chemistry. G0.253+0.016, also known as `the Brick', is the densest, most compact and quiescent of these clouds. High-resolution observations with the Atacama Large Millimeter/submillimeter Array (ALMA) have revealed its complex, hierarchical structure. In this paper we compare the properties of recent hydrodynamical simulations of the Brick to those of the ALMA observations. To facilitate the comparison, we post-process the simulations and create synthetic ALMA maps of molecular line emission from eight molecules. We correlate the line emission maps to each other and to the mass column density, and find that HNCO is the best mass tracer of the eight emission lines within the simulations. Additionally, we characterise the spatial structure of the observed and simulated cloud using the density probability distribution function (PDF), spatial power spectrum, fractal dimension, and moments of inertia. While we find good agreement between the observed and simulated data in terms of power spectra and fractal dimensions, there are key differences in the density PDFs and moments of inertia, which we attribute to the omission of magnetic fields in the simulations. This demonstrates that the presence of the Galactic potential can reproduce many cloud properties, but additional physical processes are needed to fully explain the gas structure.
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