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The Universe expansion rate is modulated around local inhomogeneities due totheir gravitational potential. Velocity waves are then observed around galaxyclusters 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 thefirst time, the simulation shows that velocity waves that arise in thelines-of-sight of the most massive dark matter halos agree with those observedin local galaxy velocity catalogs in the lines-of-sight of Coma and severalother local (Abell) clusters. For the best-constrained clusters such as Virgoand Centaurus, i.e. those closest to us, secondary waves caused by galaxygroups, further into the non-linear regime, also stand out. This match is notutterly expected given that before being evolved into a fully non-linear z=0state, assuming {\Lambda}CDM, CLONE initial conditions are constrained withsolely linear theory, power spectrum and highly uncertain and sparse localpeculiar velocities. Additionally, Gaussian fits to velocity wave envelopesshow that wave properties are tightly tangled with cluster masses. This link iscomplex though and involves the environment and formation history of theclusters. A proposed metric, measuring the distance between the observed andseveral re-centered simulated lines-of-sight, waves included, is shown to becapable of providing a tight mass range estimate for massive local clusters.Using machine learning techniques to grasp more thoroughly the complexwave-mass relation, velocity waves could in the near future be used to provideadditional and independent mass estimates from galaxy dynamics within largecluster radii.

Distortions of the Hubble diagram: Line-of-sight signatures of local galaxy clusters