2010MNRAS.406.1609B -
Mon. Not. R. Astron. Soc., 406, 1609-1628 (2010/August-2)
Crawling the cosmic network: exploring the morphology of structure in the galaxy distribution.
BOND N.A., STRAUSS M.A. and CEN R.
Abstract (from CDS):
Although coherent large-scale structures such as filaments and walls are apparent to the eye in galaxy redshift surveys, they have so far proven difficult to characterize with computer algorithms. This paper presents a procedure that uses the eigenvalues and eigenvectors of the Hessian matrix of the galaxy density field to characterize the morphology of large-scale structure. By analysing the smoothed density field and its Hessian matrix, we can determine the types of structure - walls, filaments or clumps - that dominate the large-scale distribution of galaxies as a function of scale. We have run the algorithm on mock galaxy distributions in a Λcold dark matter cosmological N-body simulation and the observed galaxy distributions in the Sloan Digital Sky Survey. The morphology of structure is similar between the two catalogues, both being filament-dominated on 10-20h–1 Mpc smoothing scales and clump-dominated on 5h–1 Mpc scales. There is evidence for walls in both distributions, but walls are not the dominant structures on scales smaller than ∼ 25 h–1 Mpc. Analysis of the simulation suggests that, on a given comoving smoothing scale, structures evolve with time from walls to filaments to clumps, where those found on smaller smoothing scales are further in this progression at a given time.
Abstract Copyright:
© 2010 The Authors. Journal compilation © 2010 RAS
Journal keyword(s):
methods: data analysis - surveys - cosmology: observations - large-scale structure of Universe
Simbad objects:
1
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