2003/11/30 by Somnath Bharadwaj, Suketu Bhavsar, Suketu P. Bhavsar +1 · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Cosmology and Gravitation Theories #Galaxies: Formation, Evolution, Phenomena #astro-ph
paper · pdf · doi:10.1086/382140
published as Astrophys.J.606:25-31,2004 · 16 preprint pages, 4 figures, Replaced with accepted version in ApJ. Improved discussion and added references
arxiv created 2003/12/19 · openalex publication_date 2004/04/20 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We analyze the filamentarity in the Las Campanas redshift survey (LCRS) and determine the length scale at which filaments are statistically significant. The largest length scale at which filaments are statistically significant, real objects is between 70 and 80 h -1 Mpc for the LCRS -3° slice. Filamentary features longer than 80 h -1 Mpc, although identified, are not statistically significant; they arise from chance alignments. For the five other LCRS slices, filaments of lengths 50-70 h -1 Mpc are statistically significant, but not beyond. These results indicate that while individual filaments up to 80 h -1 Mpc are statistically significant, the impression of structure on larger scales is a visual effect. On scales larger than 80 h -1 Mpc, the filaments interconnect by statistical chance to form the filament-void network. The reality of the 80 h -1 Mpc features in the -3° slice makes them the longest coherent features in the LCRS. While filaments are a natural outcome of gravitational instability, any numerical model that attempts to describe the formation of large-scale structure in the universe must produce coherent structures on scales that match these observations.