Satellite plane vs isotropic distribution Two-panel edge-on Milky Way comparison: ΛCDM predicts isotropically distributed satellite galaxies accreted from dark matter filaments, but observations show satellites confined to a thin kinematically coherent plane consistent with tidal origin. ΛCDM prediction Isotropic accretion from DM filaments Observed Thin kinematically coherent plane DM halo MW edge-on Satellites from random directions MW edge-on VPOS Phase-space correlated — tidal origin If most satellites are ancient TDGs, the substrate explains both: planar distribution (tidal origin) and high M/L ratios (MOND dynamics) Pawlowski & Kroupa 2020 — VPOS RMS height ~20 kpc, p ~ 0.04% in ΛCDM
Left: ΛCDM predicts satellite galaxies are accreted from random directions along dark matter filaments, producing an approximately isotropic distribution. The dashed circle indicates the predicted DM halo extent. Right: The observed Milky Way satellite system forms a thin, kinematically coherent plane — the "vast polar structure" (VPOS, Pawlowski & Kroupa 2020). Green arrows indicate coherent orbital motion within the plane. This is naturally explained if most satellites are ancient TDGs from a past interaction. The substrate framework explains both the planar distribution and the satellites' apparently high dark matter content: boundary parity physics produces MOND-enhanced dynamics in every baryonic system regardless of formation history.