We present cosmological simulations that closely mimic the real uiverse within ～100 Mpc of the Local Group. The simulations, called constrained simulations, reproduce the large-scale density field with major nearby structures, including the Local Group, the Coma and Virgo Clusters, the Great Attractor, the Perseus-Pisces Supercluster, and the Local Supercluster, in approximately correct locations. The MARK III survey of peculiar velocities of the observed structures inside an 80 h~(-1) Mpc sphere is used to constrain the initial conditions. Fourier modes on scales larger than a (Gaussian) resolution of ≈R_g = 5 h~(-1) Mpc are dominated by the constraints, while small-scale waves are essentially random. The main aim of this paper is the structure of the Local Supercluster region (LSC; ～30 h~(-1) Mpc around the Virgo Cluster) and the Local Group environment. We find that at the current epoch most of the mass (≈7.5 x 10~(14) h~(-1) solar mass) of the LSC is located in a filament roughly centered on the Virgo Cluster and extending over ～40 h~(-1) Mpc. The simulated Local Group (LG) is located in an adjacent smaller filament, which is not a part of the main body of the LSC and has a peculiar velocity of ≈250 km s~(-1) toward the Virgo Cluster. The peculiar velocity field in the LSC region is complicated and is drastically different from the field assumed in the Virgocentric infall models. We find that the peculiar velocity flow in the vicinity of the LG in the simulation is relatively "cold ": the peculiar line-of-sight velocity dispersion within 7 h~(-1) Mpc of the LG is approx< 60 km s~(-1), comparable to the observed velocity dispersion of nearby galaxies.
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机译：我们提出了宇宙模拟，它们紧密地模拟了本地群在约100 Mpc之内的真实宇宙。这些模拟称为约束模拟，它在近似正确的位置上重现了具有附近主要结构的大规模密度场，包括本地群，昏迷和处女座星团，伟大的吸引者，英仙座-双鱼座超级集群和本地超级集群。 MARK III对80 h〜（-1）Mpc球内观察到的结构的特殊速度进行了调查，以约束初始条件。尺度大于（高斯）分辨率≈R_g= 5 h〜（-1）Mpc的尺度上的傅立叶模式受约束条件支配，而小尺度波本质上是随机的。本文的主要目的是局部超级集群区域（LSC;处女座星团周围的〜30 h〜（-1）Mpc）的结构和局部群环境。我们发现，在当前时期，LSC的大部分质量（≈7.5x 10〜（14）h〜（-1）太阳质量）位于大约处在处女座星团中心且延伸约40h〜的细丝中。 （-1）Mpc。模拟的本地群（LG）位于相邻的较小细丝中，该细丝不是LSC主体的一部分，并且朝向处女座星团的速度约为≈250 km s〜（-1）。 LSC区域中的特殊速度场非常复杂，并且与处女座落入模型中假定的场完全不同。我们发现，在模拟中LG附近的特殊速度流是相对“冷”的：LG 7 h〜（-1）Mpc内的特殊视线速度弥散约为<60 km s〜 （-1），与附近星系的观测速度色散相当。
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