Collaborative Research: A Systematic and Comprehensive Study of Black Hole-Driven Turbulence in Massive Galactic Systems

为了防止星系的全部气体供应立即转化为恒星，必须存在一种反馈机制来减缓恒星的形成。一个很有希望的候选者是通过超大质量黑洞向星系的气体供应中注入湍流。这个研究小组已经开发了一种技术来测量拥有巨大中心黑洞的系统中的气体湍流，并将使用大量星系样本直接评估这种机制的可行性。该团队将与艺术家/平面设计师合作，将他们的作品整合到一系列免费提供的天文馆展览中，指导STEM研究中代表性不足的群体，支持博士后和研究生，并向本科生介绍天文学研究。该项目由MPS/AST和促进竞争研究的既定计划（EPSCoR）联合资助。这个项目将提供一个更完整的关于吸积的SMBHs所提供的“反馈”的视图，从而更好地理解黑洞与宿主星系的关系。更具体地说，它将直接探测大质量早期星系的星系团内、星系周围和星际介质的能量学。利用x射线（钱德拉）、可见光（VLT/MUSE）和亚毫米（ALMA）观测，通过这些系统在不同质量尺度下的气体运动学，揭示湍流的起源、冷热气体之间的耦合以及微观物理。研究多相细丝速度结构的创新技术有可能成为一种更直接、更准确的方法来探测湍流气体运动，对x射线表面亮度波动分析，共振散射分析，甚至直接用瞳测量x射线线宽。该项目将成为下一代基于热量计的x射线天文台的探路者，如XRISM，雅典娜-西福和猞猁。该奖项反映了美国国家科学基金会的法定使命，并通过使用基金会的知识价值和更广泛的影响审查标准进行评估，被认为值得支持。

In order to prevent the immediate conversion of a galaxy’s total gas supply into stars, a feedback mechanism must exist to slow down star formation. One promising candidate is the injection of turbulence into a galaxy’s supply of gas by a super-massive black hole. This research team has developed a technique to measure gas turbulence in systems hosting giant central black holes and will directly evaluate the viability of this mechanism using a large sample of galaxies. The team will work with artists/graphic designers to integrate their work into a series of freely available planetarium shows, mentor under-represented groups in STEM research, support a postdoc and a graduate student, and introduce undergraduates to astronomical research. This project is jointly funded by MPS/AST and the Established Program to Stimulate Competitive Research (EPSCoR). This project will deliver a more complete view of the “feedback” provided by accreting SMBHs, leading to a better understanding of the black hole-host galaxy relation. More specifically, it will directly probe the energetics of the intra-cluster, circum-galactic, and interstellar media of massive early-type galaxies. The origin of turbulence, the coupling between hot and cold gas, and the microscopic physics will be revealed through the gas kinematics of these systems at different mass scales using X-ray (Chandra), visible (VLT/MUSE), and sub-millimeter (ALMA) observations. The innovative technique of studying the velocity structure of multi-phase filaments has the potential to be a more direct and accurate way to probe turbulent gas motion, vis-a-vis X-ray surface brightness fluctuation analysis, resonant scattering analysis, and even the direct X-ray line width measurement with Hitomi. This project will be a pathfinder for the calorimeter-based X-ray observatories of the next generation such as XRISM, Athena-XIFU, and Lynx.This award reflects NSF's statutory mission and has been deemed worthy of support through evaluation using the Foundation's intellectual merit and broader impacts review criteria.