The structure and dynamics of massive high-z cosmic-web filaments: three radial zones in filament cross-sections

Lu, Yue Samuel, Mandelker, Nir, Oh, Siang Peng, Dekel, Avishai, van den Bosch, Frank C., Springel, Volker, Nagai, Daisuke and van de Voort, Freeke ORCID: https://orcid.org/0000-0002-6301-638X 2024. The structure and dynamics of massive high-z cosmic-web filaments: three radial zones in filament cross-sections. Monthly Notices of the Royal Astronomical Society 527 (4) , 11256–11287. 10.1093/mnras/stad3779

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Abstract

We analyse the internal structure and dynamics of cosmic-web filaments connecting massive high-z haloes. Our analysis is based on a high-resolution AREPO cosmological simulation zooming-in on three Mpc-scale filaments feeding three massive haloes of at z ∼ 4, embedded in a large-scale sheet. Each filament is surrounded by a cylindrical accretion shock of radius ⁠. The post-shock gas is in virial equilibrium within the potential well set by an isothermal dark-matter filament. The filament line-mass is ⁠, the gas fraction within rshock is the universal baryon fraction, and the virial temperature is ∼7 × 105 K. These all match expectations from analytical models for filament properties as a function of halo mass and redshift. The filament cross-section has three radial zones. In the outer ‘thermal’ (T) zone, ⁠, inward gravity, and ram-pressure forces are overbalanced by outward thermal pressure forces, decelerating the inflowing gas and expanding the shock outwards. In the intermediate ‘vortex’ (V) zone, 0.25 ≤ r/rshock ≤ 0.65, the velocity field is dominated by a quadrupolar vortex structure due to offset inflow along the sheet through the post-shock gas. The outward force is dominated by centrifugal forces associated with these vortices, with additional contributions from global rotation and thermal pressure. Shear and turbulent forces associated with the vortices act inwards. The inner ‘stream’ (S) zone, ⁠, is a dense isothermal core, and ⁠, defining the cold streams that feed galaxies. The core is formed by an isobaric cooling flow and is associated with a decrease in outward forces, though exhibiting both inflows and outflows.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Publisher:	Oxford University Press
ISSN:	0035-8711
Date of First Compliant Deposit:	26 January 2024
Date of Acceptance:	1 December 2023
Last Modified:	30 Jan 2024 10:45
URI:	https://orca.cardiff.ac.uk/id/eprint/165863

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