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Using the largest mosaic of Hubble Space Telescope images around a galaxycluster, we map the distribution of dark matter throughout a $\sim$$6\times6$Mpc$^2$ area centred on the cluster MS 0451-03 ($z=0.54$,$M_{200}=1.65\times10^{15} \rm{M}_\odot$). Our joint strong- and weak-lensinganalysis shows three possible filaments extending from the cluster,encompassing six group-scale substructures. The dark-matter distribution in thecluster core is elongated, consists of two distinct components, and ischaracterized by a concentration parameter of $c_{200}=3.79\pm0.36$. Bycontrast, XMM-Newton observations show the gas distribution to be morespherical, with excess entropy near the core, and a lower concentration of$c_{200}=2.35^{+0.89}_{-0.70}$ (assuming hydrostatic equilibrium). Such aconfiguration is predicted in simulations of major mergers 2-7Gyr after thefirst core passage, when the two dark-matter halos approach second turnaround,and before their gas has relaxed. This post-merger scenario finds furthersupport in optical spectroscopy of the cluster's member galaxies, which showsthat star formation was abruptly quenched 5 Gyr ago. MS 0451-03 will be anideal target for future studies of the growth of structure along filaments,star-formation processes after a major merger, and the late-stage evolution ofcluster collisions.

The distribution of dark matter and gas spanning six megaparsecs around the post-merger galaxy cluster MS0451-03