The Cosmic V-Web

Abstract

The network of filaments with embedded clusters surrounding voids seen in maps derived from redshift surveys and reproduced in simulations has been referred to as the cosmic web. A complementary description is provided by considering the shear in the velocity field of galaxies. The eigenvalues of the shear provide information on whether a region is collapsing in three dimensions, the condition for a knot, expanding in three-dimensions, the condition for a void, or in the intermediate condition of a filament or sheet. The structures that are quantitatively defined by the eigenvalues can be approximated by iso-contours that provide a visual representation of the cosmic velocity (V) web. The current application is based on radial peculiar velocities from the Cosmicflows-2 collection of distances. The three-dimensional velocity field is constructed using the Wiener filter methodology in the linear approximation. Eigenvalues of the velocity shear are calculated at each point on a grid. Here, knots and filaments are visualized across a local domain of diameter ~0.1c.

Accepted for publication in The Astrophysical Journal. Accompanied by a video and an interactive figure

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Cited by in corpus (21)

• Baryons in the CosmicWeb of IllustrisTNG - I: Gas in Knots, Filaments, Sheets and Voids
• Halo assembly bias and the tidal anisotropy of the local halo environment
• Action Dynamics of the Local Supercluster
• The Cosmic Ballet II: Spin alignment of galaxies and haloes with large-scale filaments in the EAGLE simulation
• Cosmicflows-3: Cosmography of the Local Void
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• The 2MASS redshift survey galaxy group catalogue derived from a graph-theory based friends-of-friends algorithm
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• Identification of Basins of Attraction in the Local Universe
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• Visualization in Astrophysics: Developing New Methods, Discovering Our Universe, and Educating the Earth
• A universal and physically motivated threshold for Hessian-based cosmic web identification: V-Web case