Key points are not available for this paper at this time.
The large--scale structure (LSS) in the Universe comprises a complicated filamentary network of matter. We study this network using a high--resolution simulation of structure formation of a Λ Cold Dark Matter cosmology. We investigate the distribution of matter between neighbouring large haloes whose masses are comparable to massive clusters of galaxies. We identify a total of 228 filaments between neighbouring clusters. Roughly half of the filaments are either warped or lie off the cluster--cluster axis. We find that straight filaments on the average are shorter than warped ones. More massive clusters are connected to more filaments than less massive ones on average. This finding indicates that the most massive clusters form at the intersections of the filamentary backbone of LSS. For straight filaments, we compute mass profiles. Radial profiles show a fairly well--defined radius, rₛ, beyond which the profiles follow an r^-2 power law fairly closely. For the majority of filaments, rₛ lies between 1. 5 h^-1 Mpc and 2. 0 h^-1 Mpc. The enclosed overdensity inside rₛ varies between a few times up to 25 times mean density, independent of the length of the filaments. Along the filaments' axes, material is not distributed uniformly. Towards the clusters, the density rises, indicating the presence of the cluster infall regions. In addition, we also find some sheet--like connections between clusters. In roughly a fifth of all cluster--cluster connections where we could not identify a filament or sheet, projection effects lead to filamentary structures in the projected mass distribution. (abridged)
Colberg et al. (Wed,) studied this question.
Synapse has enriched 5 closely related papers on similar clinical questions. Consider them for comparative context: