The Cosmic Ballet: spin and shape alignments of haloes in the cosmic web

Veena, Punyakoti Ganeshaiah; Cautun, Marius; Weygaert, Rien van de; Tempel, Elmo; Jones, Bernard J. T.; Rieder, Steven; Frenk, Carlos S.

doi:10.1093/mnras/sty2270

Cited by 83 publications

(49 citation statements)

References 102 publications

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“…Our results for halos' spin showing a flip in spin orientation from low to high masses, and the corresponding transition mass, are in a good agreement with trends seen in both dark matter only simulations (e.g. Aragón-Calvo et al 2007;Codis et al 2012;Ganeshaiah Veena et al 2018), and most hydrodynamical simulations (e.g. Codis et al 2018;Ganeshaiah Veena et al 2019).…”

Section: Summary and Discussionsupporting

confidence: 88%

“…This conditional tidal torque theory agrees with findings seen in halos from cosmological N-body simulations (e.g. Aragón-Calvo et al 2007;Hahn et al 2007;Codis et al 2012;Trowland et al 2013;Wang & Kang 2017;Ganeshaiah Veena et al 2018).…”

Section: Introductionsupporting

confidence: 89%

“…The spin of massive halos is found to be preferentially perpendicular to filaments' direction and walls, while at the low mass end, halos' spin tend to be aligned with their host filaments and walls, in both pure DM-only (e.g. Aragón-Calvo et al 2007;Hahn et al 2007;Sousbie et al 2008;Codis et al 2012;Ganeshaiah Veena et al 2018) and simulations containing baryons Codis et al 2018).…”

Section: Halo Spin Alignmentmentioning

confidence: 95%

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And yet it flips: connecting galactic spin and the cosmic web

Kraljic

Davé

Pichon

2020

Monthly Notices of the Royal Astronomical Society

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We study the spin alignment of galaxies and halos with respect to filaments and walls of the cosmic web, identified with DISPERSE, using the SIMBA simulation from z = 0 − 2. Massive halos' spins are oriented perpendicularly to their closest filament's axis and walls, while low mass halos tend to have their spins parallel to filaments and in the plane of walls. A similar mass-dependent spin flip is found for galaxies, albeit with a weaker signal particularly at low mass and low-z, suggesting that galaxies' spins retain memory of their larger-scale environment. Low-z star-forming and rotation-dominated galaxies tend to have spins parallel to nearby filaments, while quiescent and dispersion-dominated galaxies show preferentially perpendicular orientation; the star formation trend can be fully explained by the stellar mass correlation, but the morphology trend cannot. There is a strong dependence on HI mass, such that high-HI galaxies tend to have parallel spins while low-HI galaxies are perpendicular, which persists even when matching samples in stellar mass, suggesting that HI content traces anisotropic infall more faithfully than the stellar component. Finally, at fixed stellar mass, the strength of spin alignments correlates with the filament's density, with parallel alignment for galaxies in high density environments. These findings are consistent with conditional tidal torque theory, and highlight a significant correlation between galactic spin and the larger scale tides that are important e.g. for interpreting weak lensing studies. SIMBA allows us to rule out numerical grid locking as the cause of previously-seen low mass alignment.

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Section: Summary and Discussionsupporting

confidence: 88%

Section: Introductionsupporting

confidence: 89%

Section: Halo Spin Alignmentmentioning

confidence: 95%

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And yet it flips: connecting galactic spin and the cosmic web

Kraljic

Davé

Pichon

2020

Monthly Notices of the Royal Astronomical Society

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“…The present study extends the analysis of Ganeshaiah Veena et al (2018) of the alignment of haloes with respect to cosmic web filaments. To this end, we explore whether the systematic alignment between the dark halo spins and their host filaments found in that study is preserved when studying the alignments of galaxy spins, and, in particular, we assess which factors may introduce differences in the spin-filament alignment of haloes and galaxies.…”

Section: Introductionsupporting

confidence: 70%

The Cosmic Ballet II: spin alignment of galaxies and haloes with large-scale filaments in the EAGLE simulation

Veena

Cautun

Tempel

et al. 2019

Monthly Notices of the Royal Astronomical Society

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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 web finders 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 spin 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 haloes, with the host haloes of elliptical galaxies having a larger degree of orthogonal alignment than the host haloes of spirals. 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.

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“…In terms of mass, the filaments are the most important environment, containing over half of the mass budget but filling only 6% of the cosmic volume (Cautun et al 2014). Most of the massive haloes, with M200 5 × 10 13 h −1 M , are found in nodes, while filaments contain the majority of lower mass haloes with mass M200 10 11 h −1 M (Ganeshaiah Veena et al 2018). In contrast, sheets and especially voids correspond to below average densities and are mostly devoid of haloes with masses above 10 12 h −1 M .…”

Section: Generic Behaviours Of the Fifth Forcementioning

confidence: 99%

Screening maps of the local Universe I – Methodology

Shao

Cautun

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We introduce the LOCal Universe Screening Test Suite (LOCUSTS) project, an effort to create 'screening maps' in the nearby Universe to identify regions in our neighbourhood which are screened, i.e., regions where deviations from General Relativity (GR) are suppressed, in various modified gravity (MG) models. In these models, deviations from the GR force law are often stronger for smaller astrophysical objects, making them ideal test beds of gravity in the local Universe. However, the actual behaviour of the modified gravity force also depends on the environment of the objects, and to make accurate predictions one has to take the latter into account. This can be done approximately using luminous objects in the local Universe as tracers of the underlying dark matter field. Here, we propose a new approach that takes advantage of state-of-the-art Bayesian reconstruction of the mass distribution in the Universe, which allows us to solve the modified gravity equations and predict the screening effect more accurately. This is the first of a series of works, in which we present our methodology and some qualitative results of screening for a specific MG model, f (R) gravity. Applications to test models using observations and extensions to other classes of models will be studied in future works. The screening maps of this work can be found at this link †.

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The Cosmic Ballet: spin and shape alignments of haloes in the cosmic web

Cited by 83 publications

References 102 publications

And yet it flips: connecting galactic spin and the cosmic web

And yet it flips: connecting galactic spin and the cosmic web

The Cosmic Ballet II: spin alignment of galaxies and haloes with large-scale filaments in the EAGLE simulation

Screening maps of the local Universe I – Methodology

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