Galaxy cluster growth as a probe of dark matter

星系团的生长作为暗物质的探针

• 批准号: 2569611
• 金额: --
• 依托单位: Durham University
• 依托单位国家: 英国
• 项目类别: Studentship
• 财政年份: 2021
• 资助国家: 英国
• 起止时间: 2021 至 无数据
• 项目状态: 未结题
• 来源: https://gtr.ukri.org/projects?ref=studentship-2569611
• 关键词: Galaxy; cluster; growth; probe; dark

Dark matter is one of the most mysterious constituents of our Universe, and constitutes up to 80% of its matter content. Most particle physics theories predict dark matter to interact so weakly with standard model particles that it will remain fundamentally undetectable in terrestrial experiments. If correct, dark matter can only be studied where it gathers in sufficient quantities for its gravity to affect things around it we can see. With this PhD project, we will track the behaviour of dark matter in galaxy clusters (the most massive structures in the universe), to constrain its particle nature. Different dark matter models make different testable predictions for the rate at which structures, assemble compared to the standard cold dark matter (CDM). For example, warm dark matter inhibits the initial seeding of dark matter structures in the early Universe, while self-interacting dark matter (SIDM) predicts interactions between dark matter particles at late times that prevent the densest regions from growing. Galaxy clusters are ideal laboratories in which to study its properties because they are still forming through mergers of smaller clusters and galaxy groups, commonly called substructures, and every merger acts like a gigantic particle collider. The decoupling of baryons (stars and gas) and dark matter during mergers in massive substructures provides an important constraint on the non-gravitational forces acting on dark matter particle. If SIDM, we expect variation of a few percent (between 3 and 5%) of substructures' stellar and gas density compared to CDM, as well as frictional forces that cause dark matter to gradually separate from stars and gas. With this project, one will independently 'follow' the dark matter, stellar and gas contents in massive clusters, by mapping their distributions, weighing them, and identifying any differences/similarities (distribution peaks, quantities, etc). For this one will exploit observations obtained by the Hubble Space Telescope in the context of the large treasury programme, BUFFALO (https://buffalo.ipac.caltech.edu/), and follow-up spectroscopy from the largest telescope on Earth (VLT). BUFFALO observations were designed to map clusters' dark matter via the eject of 'gravitational lensing', which distorts and magnifies objects behind the cluster. The results obtained will be interpreted within the theoretical framework of state-of-the-art Durham's simulations of our universe.

暗物质是我们宇宙中最神秘的组成部分之一，占其物质含量的80%。大多数粒子物理理论预测暗物质与标准模型粒子的相互作用非常弱，以至于在地球实验中基本上仍然无法检测到它。如果是正确的，只有在暗物质聚集到足够的数量，使其引力足以影响我们可以看到的周围事物的情况下，才能研究暗物质。通过这个博士项目，我们将跟踪星系团(宇宙中最大质量的结构)中暗物质的行为，以限制其粒子性质。与标准冷暗物质(CDM)相比，不同的暗物质模型对结构的组装速度做出了不同的可测试预测。例如，热暗物质抑制了早期宇宙中暗物质结构的初始播种，而自相互作用暗物质(SIDM)预测了暗物质粒子之间的相互作用，从而阻止了最密集区域的增长。星系团是研究其性质的理想实验室，因为它们仍然是通过较小星系团和星系群(通常称为子结构)的合并形成的，而每一次合并都像一个巨大的粒子对撞机。重子(恒星和气体)和暗物质在大质量子结构合并过程中的解耦为作用于暗物质粒子的非引力提供了重要的约束。如果是SIDM，我们预计与CDM相比，子结构的恒星和气体密度会有几个百分点(在3%到5%之间)的变化，以及导致暗物质逐渐从恒星和气体中分离的摩擦力。通过这个项目，人们将独立地跟踪大质量星系团中的暗物质、恒星和气体的含量，方法是绘制它们的分布图，对它们进行加权，并确定任何不同/相似之处(分布峰值、数量等)。这一次将利用哈勃太空望远镜在大型国库方案布法罗(https://buffalo.ipac.caltech.edu/)，)和地球上最大望远镜的后续光谱学的背景下获得的观测结果。布法罗天文台的设计初衷是通过抛出“引力透镜”来绘制星系团的暗物质图，引力透镜会扭曲和放大星系团背后的物体。所获得的结果将在最先进的达勒姆对我们宇宙的模拟的理论框架内进行解释。