This page accompanies the paper Caustic Skeleton and the Local Cosmic Web: the Coma Cluster node and the Pisces Perseus ridge (2026). We provide additional video material for Figures [4] and [8] referenced in the Section [4] of the text.
Description: [This figure shows the caustic skeleton around the Coma Cluster in both Lagrangian space (top panels) and Eulerian space (bottom panels) in a \(L = 100\) Mpc box extracted from one example of a Universe re-simulation (refer to as \(M_1\)). We use the smoothing scale of \(\sigma =3\) Mpc. Left: \(A_3\) walls with \(A_4\) and \(D_4\) filaments. Middle: Both \(A_4\) and \(D_4\) filaments. Right: \(D_4\) filaments alone. The 3-dimensional first eigenvalue field of the deformation tensor is also included in the top Lagrangian-space panels, and the density field in the bottom Eulerian-space panels. The density is estimated with the Phase-Space Delaunay Tessellation Field Estimator (Feldbrugge 2024; Feldbrugge & Hertzsch 2025)]
Referenced in: Section [4.1] / Figure [4]
Rotating: rotate_box_coma.mp4
Zoom-in: zoom_in_coma.mp4
Description: [This figure shows the caustic skeleton of the Pisces-Perseus Supercluster in a \(60\) Mpc box for \(M_1\) Local Universe re-simulation. Coordinates are rotated so that the positive \(Z_R\)-direction is roughly along the line of sight and RA and DEC correspond to positive \(Y_R\) and negative \(X_R\) directions. Left: \(A_3\) walls with \(A_4\) and \(D_4\) filaments, Middle: \(A_4\) and \(D_4\) filaments, Right: Only \(D_4\) filaments. We use the smoothing scale of \(\sigma =3\) Mpc. The density is estimated with the Phase-Space Delaunay Tessellation Field Estimator (Feldbrugge 2024; Feldbrugge & Hertzsch 2025).]
Referenced in: Section [4.2] / Figure [8]
Rotating: rotate_box_pp.mp4
Zoom-in: zoom_in_pp.mp4