星系形态与暗物质晕结构之间的联系 I：薄盘的运行阈值与来自暗物质侧的尺寸预测因子
Connection between galaxy morphology and dark-matter halo structure I: a running threshold for thin discs and size predictors from the dark sector
AI总结：
本研究利用TNG50模拟，通过新的运动学分解方法揭示星系盘尺寸与暗物质晕自旋、浓度及吸积率的相关性，并发现盘形成需稳定晕条件与持续物质供应。
摘要：
我们利用宇宙学模拟研究星系形态与宿主暗物质（DM）晕结构之间的联系。引入一种新的运动学分解方案，我们稳健地将薄盘和厚盘分离，并测量晕的性质，包括宇宙网位置、内部结构和组装历史。在TNG50模拟中，我们发现用于盘区分的轨道圆度阈值随星系质量和红移系统地变化。类似地，恒星晕与内部星系之间的能量阈值依赖于质量和红移，在亚银河晕质量处达到最小，而圆度阈值在此处接近其峰值。重新审视星系尺寸预测因子，我们表明TNG50中的盘尺寸与超越维里质量和红移的三个结构参数相关：1）与晕自旋λ在红移范围内呈正相关——比先前在zoom-in模拟中报告的更强，但仍弱于简单的r_{1/2}/R_vir ∝ λ标度关系；2）与DM浓度c呈反相关；3）在更活跃吸积的晕中盘更大。盘质量分数在更圆的晕以及宇宙节点和纤维中更高，暗示盘的发展需要稳定的晕条件和持续的物质供应。我们的方法公开且适用于其他模拟。
英文摘要：
We study the connection between galaxy morphology and host dark matter (DM) halo structure using cosmological simulations. Introducing a new kinematic decomposition scheme, we robustly separate thin and thick discs and measure halo properties, including cosmic web locations, internal structures, and assembly histories. In the TNG50 simulation, we find that the orbital-circularity threshold for disc differentiation varies systematically with galaxy mass and redshift. Similarly, the energy threshold between stellar halos and inner galaxies depends on mass and redshift, minimizing at sub-Galactic halo mass where the circularity threshold approaches its peak. Revisiting galaxy size predictors, we show that disc sizes in TNG50 correlate with three structural parameters beyond virial mass and redshift: 1) a positive correlation with halo spin $λ$ across redshifts -- stronger than previously reported for zoom-in simulations but still weaker than the simple $r_{1/2}/R_{\rm vir} \propto λ$ scaling; 2) an anti-correlation with DM concentration $c$; 3) larger discs in more actively accreting haloes. Disc mass fraction is higher in rounder haloes and in cosmic knots and filaments, implying that disc development needs both stable halo conditions and continuous material supply. Our methodology is public and adaptable to other simulations.
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