SAMI与TNG-Cluster：追踪星系自旋及环境转变在星团相空间和宇宙时间中的演化
SAMI and TNG-Cluster: tracing galaxy spin and environmental transformation across cluster phase-space and cosmic time
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中文总结 AI 辅助
本研究结合SAMI观测与TNG-Cluster模拟，发现星系团环境通过缓慢累积过程抑制卫星星系角动量，导致自旋参数在相空间中相关性微弱，需追踪个体轨道历史才能显现。
中文摘要 AI 辅助
星系团的致密环境通过气体剥离、潮汐相互作用、引力骚扰和饥饿机制抑制恒星形成，并改变内落卫星星系的运动学性质。投影相空间图将星系团星系的当前分布与其吸积历史联系起来。我们结合SAMI星系巡天的积分场光谱和TNG-Cluster模拟，研究恒星自旋参数（$\lambda_R$）、$(g-i)$颜色和sSFR如何在投影相空间内落区域中变化。在$z = 0$时，TNG-Cluster重现了SAMI观测到的相空间趋势的方向和大致强度，包括微弱但显著的$\lambda_R$-星系团中心距离相关性。利用这一一致性，我们将分析扩展到过去80亿年，追踪每个内落区域内星系性质的统计演化，并辅以代表性卫星的个体轨道历史。虽然颜色和sSFR在相空间位置和宇宙时间上均显示出清晰的单调梯度，但$\lambda_R$的行为不同：它在外部内落区域中基本保持均匀，只有维里化的核心区域表现出系统性较低的值，并且在所有区域中向当前时代呈现缓慢的单调下降。我们发现，由星系团环境驱动的角动量抑制是一个缓慢的累积过程，需要数Gyr的星系团核心暴露时间，并受轨道历史和恒星质量调制。这种渐进性质解释了为什么$\lambda_R$-环境相关性在统计样本的相空间区域中显得微弱；当追踪个体卫星历史时，这种效应显现出来，揭示了对长期星系团居留的持续动力学响应。
英文摘要
The dense environment of galaxy clusters suppresses star formation and alters the kinematic properties of infalling satellites through gas stripping, tidal interactions, gravitational harassment and starvation. Projected phase-space diagrams connect the present-day distribution of cluster galaxies to their accretion histories. We combine SAMI Galaxy Survey integral field spectroscopy with the TNG-Cluster simulation to investigate how the stellar spin parameter ($λ_R$), $(g-i)$ colour, and sSFR vary across projected phase-space infall regions. At $z = 0$, TNG-Cluster reproduces the direction and broad strength of the phase-space trends observed in SAMI, including the weak yet significant $λ_R$-clustercentric distance correlation. Leveraging this agreement, we extend the analysis across the last 8 Gyr, tracing the statistical evolution of galaxy properties within each infall region, and complement this with individual orbital histories of representative satellites. While colour and sSFR show clear monotonic gradients with both phase-space position and cosmic time, $λ_R$ behaves differently: it remains largely uniform across the outer infall regions, with only the virialised core exhibiting systematically lower values, and displays a slow monotonic decline toward the present day across all regions. We find that angular momentum suppression driven by the cluster environment is a slow, cumulative process requiring several Gyr of exposure to the cluster core, modulated by orbital history and stellar mass. This gradual nature explains why the $λ_R$-environment correlation appears weak across phase-space regions in statistical samples; the effect emerges when individual satellite histories are tracked, revealing a sustained dynamical response to prolonged cluster residence.
发表机构
- Universidade Tecnológica Federal do Paraná（帕拉纳联邦技术大学）
- European Southern Observatory（欧洲南方天文台）
- Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo（圣保罗大学天文、地球物理与大气科学研究所）
- University of Dodoma, College of Natural and Mathematical Sciences（多多马大学自然与数理科学学院）
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