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The cosmic ballet II : spin alignment of galaxies and haloes with large-scale filaments in the EAGLE simulation.

Ganeshaiah Veena, Punyakoti and Cautun, Marius and Tempel, Elmo and van de Weygaert, Rien and Frenk, Carlos S (2019) 'The cosmic ballet II : spin alignment of galaxies and haloes with large-scale filaments in the EAGLE simulation.', Monthly notices of the royal astronomical society., 487 (2). pp. 1607-1625.

Abstract

We investigate the alignment of galaxies and haloes relative to cosmic web filaments using the EAGLE hydrodynamical simulation. We identify filaments by applying the nexus+ method to the mass distribution and the Bisous formalism to the galaxy distribution. Both return similar filamentary structures that are well aligned and that contain comparable galaxy populations. EAGLE haloes have an identical spin alignment with filaments as their counterparts in dark-matter-only simulations: a complex mass-dependent trend with low-mass haloes spinning preferentially parallel to and high-mass haloes spinning preferentially perpendicular to filaments. In contrast, galaxy spins do not show such a transition and have a propensity for perpendicular alignments at all masses, with the degree of alignment being largest for massive galaxies. This result is valid for both nexus+ and Bisous filaments. When splitting by morphology, we find that elliptical galaxies show a stronger orthogonal spin–filament alignment than spiral galaxies of similar mass. The same is true of their host haloes. Due to the misalignment between galaxy shape and spin, galaxy minor axes are oriented differently with filaments than galaxy spins. We find that the galaxies whose minor axis is perpendicular to a filament are much better aligned with their host haloes. This suggests that many of the same physical processes determine both the galaxy–filament and the galaxy–halo alignments. The volume of the EAGLE simulation is relatively small and many of the alignments we have found are weak; validation of our conclusions will require hydrodynamical simulations of significantly larger volumes.

Item Type:Article
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Status:Peer-reviewed
Publisher Web site:https://doi.org/10.1093/mnras/stz1343
Publisher statement:This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Date accepted:03 May 2019
Date deposited:30 July 2019
Date of first online publication:16 May 2019
Date first made open access:30 July 2019

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