Spin conservation of cosmic filaments

Abstract

Cosmic filaments are the largest collapsing structure in the Universe. Recently both observations and simulations inferred that cosmic filaments have coherent angular momenta (spins). Here we use filament finders to identify the filamentary structures in cosmological simulations and study their physical origins, which are well described by the primordial tidal torque of their Lagrangian counterpart regions -- protofilaments. This initial angular momenta statistically preserve their directions to low redshifts. We further show that a spin reconstruction method can predict the spins of filaments and potentially relate their spins to the initial conditions of the Universe. This correlation provides a new way of constraining and obtaining additional information of the initial perturbations of the Universe.

7 pages, 6 figures. Matches the accepted version in Physical Review D

References in corpus (7)

• Properties of Dark Matter Haloes in Clusters, Filaments, Sheets and Voids
• ELUCID - Exploring the Local Universe with reConstructed Initial Density field I: Hamiltonian Markov Chain Monte Carlo Method with Particle Mesh Dynamics
• ELUCID - Exploring the Local Universe with reConstructed Initial Density field III: Constrained Simulation in the SDSS Volume
• Possible observational evidence that cosmic filaments spin
• Spin Parity of Spiral Galaxies I -- Corroborative Evidence for Trailing Spirals
• Nonlinear $E$-mode clustering in Lagrangian space
• Spin Mode Reconstruction in Lagrangian Space

Cited by in corpus (4)

• Cosmic Filament Spin from Dark Matter Vortices
• Analysis of $\sim 10^6$ spiral galaxies from four telescopes shows large-scale patterns of asymmetry in galaxy spin directions
• Baryonic Effects on Lagrangian Clustering and Angular Momentum Reconstruction
• Measuring cosmic filament spin with the kinetic Sunyaev-Zel'dovich effect