The Effect of Massive Neutrinos on the Halo Spin Flip Phenomenon

Lee, Jounghun; Libeskind, Noam I; Ryu, Suho

doi:10.48550/arxiv.2004.02638

Cited by 4 publications

(11 citation statements)

References 16 publications

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“…The routine we go through for the investigation of the DE dependence of the halo spin transitions is similar to that described in Lee et al (2020), the summary of which is provided in the following.…”

Section: Data and Routinementioning

confidence: 99%

“…Instead of regarding the threshold mass at which cos θ 2 ∼ cos θ 3 as the transition mass of the halo spins, however, we adopt the more rigorous definition given by Lee et al (2020), according to which the spin transition occurs in a differential mass interval where the null hypothesis of p(cos θ 2 ) ∼ p(cos θ 3 ) is rejected by the KolmogorovSmirnov (KS) test at the confidence level lower than 99.9%. For the KS test of the null hypothesis of p(cos θ 2 ) ∼ p(cos θ 3 ) at each m h -interval, we evaluate two cumulative probability functions, P (cos θ 2 < cos θ) ≡ cos θ 0 p(cos θ 2 )d cos θ 2 and P (cos θ 3 < cos θ) ≡ cos θ 0 p(cos θ 3 )d cos θ 3 .…”

Section: Spin Transition Zonementioning

confidence: 99%

“…The same comparisons between the two cumulative distributions but for the wCDM and RPCDM cases are made in Figures 3 and 4, respectively. To show more clearly the differences between P (cos θ 2 < cos θ) and P (cos θ 3 < cos θ), we plot cos θ − P (cos θ i < cos θ) in lieu of P (cos θ i < cos θ) in Figures 2-4, as done in Lee et al (2020).…”

Section: Spin Transition Zonementioning

confidence: 99%

“…Very recently, Lee et al (2020) suggested a new near-field diagnostics based on the mass dependent transition of the halo spins, which refers to the numerically and observationally detected phenomenon that while the high-mass halos have their spins preferentially aligned with the directions perpendicular to the minor principal axes of the local tidal fields, the low-mass ones prefer the directions parallel to them in their spin orientations (e.g., Aragón-Calvo et al 2007;Hahn et al 2007b;Paz et al 2008;Codis et al 2012;Tempel & Libeskind 2013;Trowland et al 2013;Libeskind et al 2013;Aragon-Calvo & Yang 2014;Dubois et al 2014;Forero-Romero et al 2014;Codis et al 2015a,b;Hirv et al 2017;Codis et al 2018;Ganeshaiah Veena et al 2018;Ganeshaiah Veena et al 2019;Lee 2019;Kraljic et al 2020). What Lee et al (2020) newly found was that the critical mass at which the transition of the halo spin orientations occurs (transition mass of the halo spins) varies sensitively with the total neutrino mass, regardless of the smoothing scale of the tidal field.…”

Section: Introductionmentioning

confidence: 99%

“…In light of Lee et al (2020), we set off here to numerically explore if the transition mass of the halo spins can be used as a probe of DE with the help of N-body simulations. The contents of this Paper can be outlined as follows.…”

Section: Introductionmentioning

confidence: 99%

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The Halo Spin Transition as a Probe of Dark Energy

Lee,

Libeskind

2020

Preprint

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We present a numerical evidence supporting the claim that the massdependent transitions of the halo spin orientations from the intermediate to the minor principal directions of the local tidal fields can in principle be a useful discriminator of dark energy models. We first define a spin transition zone as the mass range of the halos, ∆m t , for which the intrinsic spin alignments with the minor tidal principal directions become as strong as that with the intermediate principal directions. Then, utilizing the halo samples from the DEUS simulations performed separately for the WMAP7 ΛCDM, phantom DE and quintessence models, we investigate if and how the three different dark energy models differ in ∆m t . It is shown that the differences in ∆m t among the three dark energy models are significant enough to discriminate the models from one another and robust against the variations of the smoothing scale of the tidal field and redshift. Noting that a narrower spin transition zone is more powerful as a probe of dark energy, we also show that the spin transition zones become narrower at higher redshifts, in the filamentary environments and for the case that the tidal fields are smoothed on the smaller scales. Our result is consistent with the scenario that ∆m t is mainly determined by how fast the nonlinear evolution of the tidal field proceeds, which in turn sensitively depends on the background cosmology.

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Section: Data and Routinementioning

confidence: 99%

Section: Spin Transition Zonementioning

confidence: 99%

Section: Spin Transition Zonementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Halo Spin Transition as a Probe of Dark Energy

Lee,

Libeskind

2020

Preprint

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Cosmic Ballet III: Halo spin evolution in the cosmic web

Veena

Cautun

Weygaert

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We explore the evolution of halo spins in the cosmic web using a very large sample of dark matter haloes in the ΛCDM Planck-Millennium N-body simulation. We use the nexus+ multiscale formalism to identify the hierarchy of filaments and sheets of the cosmic web at several redshifts. We find that at all times the magnitude of halo spins correlates with the web environment, being largest in filaments, and, for the first time, we show that it also correlates with filament thickness as well as the angle between spin-orientation and the spine of the host filament. For example, massive haloes in thick filaments spin faster than their counterparts in thin filaments, while for low-mass haloes the reverse is true. We also have studied the evolution of alignment between halo spin orientations and the preferential axes of filaments and sheets. The alignment varies with halo mass, with the spins of low-mass haloes being predominantly along the filament spine, while those of high-mass haloes being predominantly perpendicular to the filament spine. On average, for all halo masses, halo spins become more perpendicular to the filament spine at later times. At all redshifts, the spin alignment shows a considerable variation with filament thickness, with the halo mass corresponding to the transition from parallel to perpendicular alignment varying by more than one order of magnitude. The cosmic web environmental dependence of halo spin magnitude shows little evolution for z ≤ 2 and is likely a consequence of the correlations in the initial conditions or high redshift effects.

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The impact of massive neutrinos on halo assembly bias

Lazeyras,

Villaescusa-Navarro,

Viel

2020

Preprint

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Using the publicly available Quijote simulations, we present the first measurements of the assembly bias of dark matter halos in N-body simulations which include massive neutrinos. We focus on the dependence of the linear bias b 1 on three halo properties: 1) concentration c, 2) spin λ, and 3) ellipticity s. Although these simulations cover a large volume, superior to any future surveys, we do not detect any effect of neutrinos on the relations b 1 (c), b 1 (λ) and b 1 (s) at fixed halo mass. We further study the dependence of halo properties and environment on neutrinos, finding these quantities to be impacted by neutrino masses at the same level as assembly bias. We find that the effect of neutrinos on spin and shape can be largely attributed to the change in the cold dark matter σ 8 in neutrinos simulations, which is not the case for concentration.

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The Effect of Massive Neutrinos on the Halo Spin Flip Phenomenon

Cited by 4 publications

References 16 publications

The Halo Spin Transition as a Probe of Dark Energy

The Halo Spin Transition as a Probe of Dark Energy

Cosmic Ballet III: Halo spin evolution in the cosmic web

The impact of massive neutrinos on halo assembly bias

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