Quantifying the structure of the molecular interstellar medium with the G-virial method

分子气体构成了银河系星际介质（ISM）中最冷、密度最大的阶段，这是与恒星形成直接相关的阶段。然而，分子ISM的结构仅以有限的方式被量化，重力如何在ISM中起作用仍然不清楚。在博士期间，申请人开发了一种名为G-virial的新方法来量化分子ISM。新方法直接对模拟或观测数据起作用。它生成了引力在这个空间中的重要性图，可以直接与恒星形成联系起来，并用于推导引力相干气体凝聚的各种特性，包括质量半径和质量速度关系。在该项目中，我们计划综合现有的最先进的模拟和观测结果，从银河系尺度到单个恒星形成核心的g - viriv，并回答分子ISM研究中的几个基本问题：分子云中引力相干区域的结构是什么？是什么因素决定了它们？引力相干区域的性质与恒星形成有什么关系？这些地区有一个演化顺序吗？分子云的动力学是如何与银河系的动力学耦合的？此外，该项目将分子ISM的理论和观测研究联系起来，并将为未来ISM- spp优先项目的不同项目提供一个连接的接口。

Molecular gas constitutes the coldest and densest phase of the Milky Way interstellar medium (ISM), and this is the phase that is directly related to star formation. However, the structure of the molecular ISM has only been quantified in limited ways, and how gravity functions in the ISM is still not clear. During his PhD, the applicant developed a new method named G-virial to quantify the molecular ISM. The new method works directly on the simulated or observed data. It generate maps of the importance of gravity in this space, which can be directly linked to star formation and used to derive various properties of the gravitational-coherent gas condensations including mass-radius and mass-velocity relations. In the proposed project, we plan synthesize the available results from the state-of-the-art simulations and observations from the Galactic scale to the individual star-forming cores with the G-virial, and answer several fundamental questions in molecular ISM study: What are the structures of the gravitationally-coherent regions in molecular clouds? What factors determine them? How are the properties of the gravitationally-coherent regions related to star formation? It there an evolution sequence of the regions? How are the dynamics of molecular clouds coupled to the dynamics of the Milky Way? Moreover, the project links the theoretical and observational studies of the molecular ISM, and will offer an interface where different projects in the ISM-SPP priority project can be connected in the future.