Title: Distortions of the Hubble diagram: Line-of-sight signatures of local galaxy clusters Show Chinese title

Title: 哈勃图的畸变：本地星系团的视线特征

Abstract: The Universe expansion rate is modulated around local inhomogeneities due to their gravitational potential. Velocity waves are then observed around galaxy clusters in the Hubble diagram. This paper studies them in a ~738 Mpc wide, with 2048^3 particles, cosmological simulation of our cosmic environment (a.k.a. CLONE: Constrained LOcal \& Nesting Environment simulation). For the first time, the simulation shows that velocity waves that arise in the lines-of-sight of the most massive dark matter halos agree with those observed in local galaxy velocity catalogs in the lines-of-sight of Coma and several other local (Abell) clusters. For the best-constrained clusters such as Virgo and Centaurus, i.e. those closest to us, secondary waves caused by galaxy groups, further into the non-linear regime, also stand out. This match is not utterly expected given that before being evolved into a fully non-linear z=0 state, assuming {\Lambda}CDM, CLONE initial conditions are constrained with solely linear theory, power spectrum and highly uncertain and sparse local peculiar velocities. Additionally, Gaussian fits to velocity wave envelopes show that wave properties are tightly tangled with cluster masses. This link is complex though and involves the environment and formation history of the clusters. A proposed metric, measuring the distance between the observed and several re-centered simulated lines-of-sight, waves included, is shown to be capable of providing a tight mass range estimate for massive local clusters. Using machine learning techniques to grasp more thoroughly the complex wave-mass relation, velocity waves could in the near future be used to provide additional and independent mass estimates from galaxy dynamics within large cluster radii. Show Chinese abstract

Abstract: 宇宙的膨胀率由于局部不均匀性自身的引力势而被调制。 然后在哈勃图中观测到星系团周围的速度波。 本文研究了一个约738 Mpc宽，包含2048^3个粒子的宇宙环境的数值模拟（即CLONE：受限局部与嵌套环境模拟）。 首次显示，在最 massive 暗物质晕的视线方向产生的速度波，与在Coma和其他几个本地（Abell）团的视线方向观测到的速度波一致。 对于约束最好的团，如Virgo和Centaurus，即离我们最近的团，由星系团引起的次级波，在更深入非线性区域时也明显可见。 考虑到在演化为完全非线性z=0状态之前，假设{\Lambda }CDM，CLONE初始条件仅通过线性理论、功率谱以及高度不确定且稀疏的本地特殊速度进行约束，这种匹配并不完全出乎意料。 此外，对速度波包络的高斯拟合表明，波的特性与团的质量紧密纠缠。 尽管这种联系很复杂，涉及团的环境和形成历史。 提出了一种度量标准，用于测量观测到的和几个重新中心化的模拟视线方向之间的距离，包括波在内，该度量标准被证明能够为本地大质量团提供一个紧致的质量范围估计。 使用机器学习技术更全面地掌握复杂的波-质量关系，未来速度波可用于提供额外的、独立的从大团半径内的星系动力学得出的质量估计。