A kinematic classification of the cosmic web

By Y. Hoffman, Ofer Metuki, G. Yepes, S. Gottlober, J. Forero-Romero, N. Libeskind, A. Knebe. 2012

152 citations recorded by the source corpus.

A new approach for the classification of the cosmic web is presented. In extension of the previous work of Hahn et al. and Forero-Romero et al., the new algorithm is based on the analysis of the velocity shear tensor rather than the gravitational tidal tensor. The procedure consists of the construction of the shear tensor at each (grid) point in space and the evaluation of its three eigenvectors. A given point is classified to be either a void, sheet, filament or a knot according to the number of eigenvalues above a certain threshold, 0, 1, 2 or 3, respectively. The threshold is treated as a free parameter that defines the web. The algorithm has been applied to a dark matter only simulation of a box of side length 64 h−1 Mpc and N = 10243 particles within the framework of the 5-year Wilkinson and Microwave Anisotropy Probe/Λ cold dark matter (ΛCDM) model. The resulting velocity-based cosmic web resolves structures down to ≲0.1 h−1 Mpc scales, as opposed to the ≈1 h−1 Mpc scale of the tidal-based web. The underdense regions are made of extended voids bisected by planar sheets, whose density is also below the mean. The overdense regions are vastly dominated by the linear filaments and knots. The resolution achieved by the velocity-based cosmic web provides a platform for studying the formation of haloes and galaxies within the framework of the cosmic web.

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

View Paper: https://www.semanticscholar.org/paper/b9eb69ddfb9d6756de0dc55d0418acb6a90b48e0

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Citations in the corpus

Tracing the cosmic web (2017, methodology): “• The Hessian methods (NEXUS+, T-web, V-web and CLASSIC) have a mix of knots, filaments and sheets, with voids dominating the under dense volume.”
Evolution of the cosmic web (2014, background): “It suggests that approaches based on the tidal field (Hahn et al. 2007a; Forero-Romero et al. 2009) or velocity shear field (Hoffman et al. 2012) are not very sensitive to the more tenuous structures.”
Detecting filamentary pattern in the cosmic web: a catalogue of filaments for the SDSS (2013, methodology): “…(Hahn et al. 2007; Lee & Lee 2008; Forero-Romero et al. 2009; Bond, Strauss & Cen 2010a,b; Wang et al. 2012), on the velocity field (Shandarin 2011; Hoffman et al. 2012; Wang et al. 2013), skeleton analysis (Novikov, Colombi & Doré 2006; Sousbie et al. 2008), watershed segmentation (Platen, van…”