Revealing the drivers of galaxy formation in the densest cosmic environments

揭示最密集的宇宙环境中星系形成的驱动因素

• 批准号: MR/X035166/1
• 负责人: Yannick Bahe
• 金额: $ 115.99万
• 依托单位: Liverpool John Moores University
• 依托单位国家: 英国
• 项目类别: Fellowship
• 财政年份: 2024
• 资助国家: 英国
• 起止时间: 2024 至 无数据
• 项目状态: 未结题
• 来源: https://gtr.ukri.org/projects?ref=MR%2FX035166%2F1
• 关键词: Revealing; drivers; galaxy; formation; densest

One of the most perplexing aspects of our Universe is the huge variety of galaxy shapes and colours, from blue (star-forming) spiral discs to red (no longer star-forming) ellipticals. These differences are thought to be due to changing in- and outflows of gas (the "baryon cycle"), a process that can be investigated particularly cleanly when galaxies fall towards densely inhabited cosmic environments such as galaxy clusters. But we do not understand well how and why these changes occur, especially in the early Universe and for low-mass "dwarf" galaxies, and which other processes might be important, especially tidal stripping of stars into the diffuse "intra-cluster light".I will solve this problem by creating state-of-the-art defining computer simulations of galaxy clusters to interpret major new observations with ground- and space-based telescopes, including by the recently launched James Webb Space Telescope and with the new WEAVE spectrograph on the William Herschel Telescope. Exploiting extensive development work by myself and others, these simulations will realistically model the star forming gas in cluster galaxies for the first time. Spanning the full range from small "groups" to the most massive observed clusters, they will also include close analogues of four well-studied clusters in the local Universe.From these simulations, I will create synthetic observations, mimicking what they would look like in different wavelengths from X-rays through optical to radio. Comparing these with real observations, I will perform stringent tests of the simulation model and our understanding of galaxy formation encoded within it. In parallel, I will analyse the simulation outputs in detail, tracking individual galaxies through time to identify which physical processes emerge from the imposed laws of fundamental physics. In combination, these two approaches will solve the mystery of how galaxies form and evolve in the most extreme cosmic environments, and what they can tell us about the role of gas in- and outflows for galaxy formation in general.

我们宇宙中最令人困惑的方面之一是各种各样的星系形状和颜色，从蓝色（星形）螺旋盘到红色（不再是星形）椭圆形。这些差异被认为是由于气体内和流出的变化（“重子循环”），当星系落入密集居住的宇宙环境（例如星系簇）时，该过程可以特别干净地进行研究。但是我们不太了解这些变化的发生方式，尤其是在早期的宇宙和低质量的“矮人”星系中，哪些过程可能很重要，尤其是潮汐剥离恒星进入弥漫性的“群体内群光”。我将通过建立新的观察者来解决这个问题，从而解决这个问题，从而使詹姆斯的杰出序列逐渐建立新的序列，并将其置于现场的范围内，并将其定为新的观察器，并将其置于新的观察器中，并将其设置为众所周知的空间。太空望远镜以及威廉·赫歇尔（William Herschel）望远镜的新编织光谱仪。这些模拟利用我自己和其他人的广泛开发工作，将首次在集群星系中现实地建模恒星形成的气体。跨越从小“组”到最庞大的观测簇的整个范围，它们还将包括本地宇宙中四个经过良好研究群集的紧密类似物。从这些模拟中，我将创建合成观测值，模仿它们在X射线通过光学到广播的不同波长中看起来的样子。将这些与实际观察结果进行比较，我将对模拟模型进行严格的测试以及我们对其中编码的星系形成的理解。同时，我将详细分析模拟输出，通过时间跟踪各个星系，以确定哪些物理过程从施加的基本物理定律中出现。结合起来，这两种方法将解决星系如何在最极端的宇宙环境中形成和发展的奥秘，以及他们可以告诉我们的关于气体内和流出的角色在一般而言的角色。