Multiscale phenomenology of the cosmic web

By Miguel Angel Aragon-Calvo, Rien van de Weygaert, Bernard J.T. Jones Dept. PhysicsAstronomy, T. J. H. University, Baltimore., U.S.A., K. Institute, U. Groningen, The Netherlands.. 2010

208 citations recorded by the source corpus.

We analyze the structure and connectivity of the distinct morphologies that define the Cosmic Web. With the help of our Multiscale Morphology Filter (MMF), we dissect the matter distribution of a cosmologicalCDM N-body computer simulation into cluster, filaments and walls. The MMF is ideally suited to adress both the anisotropic morphological character of filaments and sheets, as well as the multiscale nature of the hierarchically evolved cosmic matter distribution. The results of our study may be summarized as follows: i).- While all morphologies occupy a roughly well defined range in density, this alone is not sufficient to differentiate between t given their overlap. Environment defined only in terms of density fails to incorporate the intrinsic dynamics of each morphology. This plays an important role in both linear and non lin- ear interactions between haloes. ii).- Most of the mass in the Universe is concentrated in filaments, narrowly followed by clusters. In terms of volume, clusters only represent a minute fraction, and filaments not more than 9%. Walls are relatively inconspicous in terms of mass and volume. iii).- On average, massive clusters are connected to more filaments than low mass clusters. Clusters with M � 10 14 Mh −1 have on average two connecting filaments, while clusters with M > 10 15 Mh −1 have on average five connecting filaments. iv).- Density profiles indicate that the typical width of filaments is 2 h −1 Mpc. Walls have less well defined boundaries with widths between 5-8 Mpc h −1 . In their interior, filaments have a power-law density profile with slope � − 1, corresponding to an isothermal density profile.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/40b337eceaf5d86283dfa955e94ce5b656a2e4eb

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Citations in the corpus

Detecting filamentary pattern in the cosmic web: a catalogue of filaments for the SDSS (2013, methodology): “This is expected since filaments are the bridges between clusters and large clusters are in intersection of many filaments (Aragón-Calvo et al. 2010a).”
Evolution of the cosmic web (2014, methodology): “Our results on the density segregation are in agreement with the previous findings of Hahn et al. (2007a) and Aragón-Calvo et al. (2010a).”
Tracing the cosmic web (2017, methodology): “…all except knots particles Scale-Space, Hessian Aragón-Calvo et al. (2007a) Aragón-Calvo & Yang (2014) Spineweb all except knots particles Topology Aragón-Calvo et al. (2010c) DisPerSE all except knots particles Topology Sousbie (2011) ORIGAMI all particles Phase-Space Falck et al. (2012); Falck…”
The persistent cosmic web and its filamentary structure I: Theory and implementation (2010, methodology): “…been the subject of less attention, there still exist a large number of references describing their features and introducing numerical void finders, such as, for instance, Neyrinck (2008), Platen, van de Weygaert & Jones (2007) and Aragón-Calvo et al. (2010a) (see also the references therein).”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, background): “These are in agreement with the prediction that massive filaments can be as heavy as small galaxy clusters [71].”