The morphology-density relation, ram-pressure stripping and ultra-diffuse galaxies in extra high resolution galaxy cluster zoom-in simulations

超高分辨率星系团放大模拟中的形态-密度关系、冲压压力剥离和超扩散星系

• 批准号: 516355818
• 负责人: Privatdozent Dr. Klaus Dolag
• 金额: --
• 依托单位: Lehrstuhl für beobachtende und experimentelle Astrophysik
• 依托单位国家: 德国
• 项目类别: Research Grants
• 资助国家: 德国
• 项目状态: 未结题
• 来源: https://gepris.dfg.de/gepris/projekt/516355818?language=en
• 关键词: morphology; density; relation; ram; pressure

Galaxy clusters and their impact via star-formation reduction, i.e. quenching, on individual satellite galaxies has been the focus of extensive observational research in recent years. As all satellite galaxies are processed in galaxy clusters, an opportunity arises to study the environmental dependence of galaxy evolution. The primary goal of this proposal is to understand the following question: How and to what extent does ram-pressure stripping in galaxy clusters contribute to the build-up of the morphology-density relation (an observational relation between environmental density and morphological galaxy type)? This is closely related to the second focus of the proposal, namely the evaluation and weighting of environmental quenching mechanisms in galaxy clusters. This, in turn, is connected to a third question: What are possible evolutionary pathways in galaxy clusters for the formation of the recently discovered ultra-diffuse galaxies (UDGs)? To understand these connections, we will perform extremely high resolution zoom-in simulations based on the treatment of physical processes used for the cosmological hydrodynamical simulation set \textit{Magneticum Pathfinder}, which have proven to successfully reproduce various properties of galaxies and galaxy clusters. Our dedicated goal is to resolve both ram-pressure stripping and the formation mechanism(s) of UDGs with an unprecedented level of detail. To this end, we aim at simulating 24 galaxy clusters with halo mass M_halo > 1e15 M_sol, resolved with almost 1e9 particles within the virial radius, giving a dark matter particle mass of m_dm~4e6 M_sol/h and a gas particle mass of $m_gas ~ 7e5 M_sol/h, resulting in a spatial resolution of the star particles of ~240 pc/h. With the proposed extreme high resolution we will be able to spatially resolve all necessary physical processes (especially turbulent mixing) involved in satellite galaxy quenching and UDG formation. In addition, we also plan to push the resolution for at least one cluster to ten times better mass resolution, increasing the spacial resolution to ~100 pc/h. As such, this project offers the unique opportunity to profoundly increase our understanding of how galaxy clusters transform their satellite galaxies.

星系团及其通过恒星形成减少（即猝灭）对单个卫星星系的影响一直是近年来广泛观测研究的焦点。 由于所有卫星星系都在星系团中进行处理，因此有机会研究星系演化的环境依赖性。该提案的主要目标是理解以下问题：星系团中的冲压压力剥离如何以及在多大程度上有助于形态密度关系（环境密度和形态星系类型之间的观测关系）的建立？这与该提案的第二个重点，即星系团环境猝灭机制的评估和加权密切相关。这又与第三个问题相关：最近发现的超弥散星系（UDG）的形成在星系团中可能有哪些进化途径？为了理解这些联系，我们将基于用于宇宙流体动力学模拟集 \textit{Magneticum Pathfinder} 的物理过程的处理来执行极高分辨率的放大模拟，该模拟集已被证明可以成功地再现星系和星系团的各种属性。我们的目标是以前所未有的详细程度解决冲压压力剥离和 UDG 的形成机制。为此，我们的目标是模拟 24 个晕质量 M_halo > 1e15 M_sol 的星系团，用维里半径内的近 1e9 个粒子进行解析，给出 m_dm~4e6 M_sol/h 的暗物质粒子质量和 $m_gas ~ 7e5 M_sol/h 的气体粒子质量，从而得到~240 pc/h 的恒星粒子空间分辨率。凭借所提出的极高分辨率，我们将能够在空间上解析卫星星系猝灭和 UDG 形成所涉及的所有必要的物理过程（尤其是湍流混合）。此外，我们还计划将至少一个簇的分辨率提高到质量分辨率的十倍，将空间分辨率提高到约 100 pc/h。因此，该项目提供了独特的机会来深刻地增进我们对星系团如何改造其卫星星系的理解。