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Neutrino Halos in Clusters of Galaxies and their Weak Lensing Signature
Cosmology and Nongalactic Astrophysics · Submitted 25 Apr 2011
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim However, correctly modeling the distribution of mass in baryons and cold dark matter and suppressing any systematic errors to the accuracy required for detecting this neutrino perturbation is severely challenging.
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The abstract, sentence by sentence
We study whether non-linear gravitational effects of relic neutrinos on the development of clustering and large-scale structure may be observable by weak gravitational lensing. We compute the density profile of relic massive neutrinos in a spherical model of a cluster of galaxies, for several neutrino mass schemes and cluster masses. Relic neutrinos add a small perturbation to the mass profile, making it more extended in the outer parts. In principle, this non-linear neutrino perturbation is detectable in an all-sky weak lensing survey such as EUCLID by averaging the shear profile of a large fraction of the visible massive clusters in the universe, or from its signature in the general weak lensing power spectrum or its cross-spectrum with galaxies. However, correctly modeling the distribution of mass in baryons and cold dark matter and suppressing any systematic errors to the accuracy required for detecting this neutrino perturbation is severely challenging.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We study whether non-linear gravitational effects of relic neutrinos on the development of clustering and large-scale structure may be observable by weak gravitational lensing. | contribution 0.91 | 0.51 | 0.06 | hedged possibility 0.92 |
| s1 | We compute the density profile of relic massive neutrinos in a spherical model of a cluster of galaxies, for several neutrino mass schemes and cluster masses. | method 0.74 | 0.95 | 0.04 | asserted 0.98 |
| s2 | Relic neutrinos add a small perturbation to the mass profile, making it more extended in the outer parts. | result 0.99 | 0.77 | 0.24 | asserted 1.00 |
| s3 | In principle, this non-linear neutrino perturbation is detectable in an all-sky weak lensing survey such as EUCLID by averaging the shear profile of a large fraction of the visible massive clusters in the universe, or from its signature in the general weak lensing power spectrum or its cross-spectrum with galaxies. | interpretation 0.85 | 0.12 | 0.37 | hedged possibility 0.91 |
| s4 | However, correctly modeling the distribution of mass in baryons and cold dark matter and suppressing any systematic errors to the accuracy required for detecting this neutrino perturbation is severely challenging. | limitation 0.95 | 0.12 | 0.40 | asserted 0.99 |
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The paper
Original abstract
We study whether non-linear gravitational effects of relic neutrinos on the development of clustering and large-scale structure may be observable by weak gravitational lensing. We compute the density profile of relic massive neutrinos in a spherical model of a cluster of galaxies, for several neutrino mass schemes and cluster masses. Relic neutrinos add a small perturbation to the mass profile, making it more extended in the outer parts. In principle, this non-linear neutrino perturbation is detectable in an all-sky weak lensing survey such as EUCLID by averaging the shear profile of a large fraction of the visible massive clusters in the universe, or from its signature in the general weak lensing power spectrum or its cross-spectrum with galaxies. However, correctly modeling the distribution of mass in baryons and cold dark matter and suppressing any systematic errors to the accuracy required for detecting this neutrino perturbation is severely challenging.
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References
How the literature uses it
17 arXiv papers cite this in 29 sentences
Papers citing it · 15 sentences without a confident label
Compares with it 1 paper
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We also find a reasonable agreement with the neutrino overdensity profiles computed through the N-one-body method described in [ref] .
Non-linear evolution of the cosmic neutrino background · The neutrino halo · 0.99
Cites it as support 4 papers
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Such assumption is supported by different studies [ref] which have shown that the contribution of massive neutrinos to the total mass of dark matter haloes is below the percent level for the neutrino mass range relevant for this paper.
Cosmology with massive neutrinos III: the halo mass function and an application to galaxy clusters · The halo mass function · 1.00
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However, as $N$-body simulations show [ref] , the neutrino halo of each object is always much more extended than the one of dark matter, due to the high neutrino thermal velocities.
Neutrino clustering in the Milky Way and beyond · Other objects: Virgo & Andromeda · 0.99
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The emerging picture shows neutrinos with masses in the currently viable range playing a minor role in the nonlinear collapse of cold DM structures: even though a fraction of them do cluster inside CDM halos, their contribution to the total mass of a halo is negligible [ref] .
Cosmology with massive neutrinos II: on the universality of the halo mass function and bias · Conclusions · 0.96
Cites it as background 9 papers
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[ref] , for neutrino masses ranging from 50 to 300 meV.
Calculation of the local density of relic neutrinos · Minimal neutrino masses · 0.91
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The clustering of neutrinos within the gravitational potential wells of CDM haloes has already been studied using semi-analytic models [ref] and N-body simulations [ref] .
Non-linear evolution of the cosmic neutrino background · The neutrino halo · 0.99
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Massive neutrinos also impact on the fully non-linear regime in many different ways and on different observables like for example: the matter power spectrum at small scales [ref] , the halo-matter bias [ref] , the clustering within dark matter halos [ref] , the evolution of cosmic voids [ref] , the halo mass function [ref] , redshift-space distortions [ref] , Ly$α$ forest statistical properties of the transmitted flux [ref] , Sunyaev-Zeld́ovich effects in galaxy cluster surveys [ref] , galaxy clustering [ref] .
The halo model in a massive neutrino cosmology · Introduction · 0.82
What it cites · 7 sentences without a confident label
Contests 1 paper
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As we have shown, the NFW halo profile extrapolated to large radius that is used by [ref] underestimates the neutrino contribution to the profile at large radius.
Gravitational clustering of relic neutrinos and implications for their detection · Neutrino density profiles · contest 0.76
Uses the method or tool of 3 papers
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We use the empirical formula of [ref] , obtained from a numerical fit to the results of N-body cosmological simulations, to calculate the mass and concentration parameter of the most massive progenitor of our halo of mass $M_f$ at the final redshift $z_f$, for each earlier epoch at redshift $z>z_f$.
Accurate universal models for the mass accretion histories and concentrations of dark matter halos · Dark matter halo evolution · 0.95
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The first piece is the NFW profile [ref] , valid inside the virial radius.
The Structure of Cold Dark Matter Halos · Mass density profile · 0.80
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The second piece is obtained starting from the average initial density perturbation around a halo in a Gaussian random field, and evolving it in the non-linear regime by assuming spherical gravitational collapse without shell-crossing [ref] .
Probing Early Clustering with Lyman-Alpha Absorption Lines Beyond the Quasar Redshift · Mass density profile · 0.97
Compares with 2 papers
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Comparing our calculations with previously published results, we find that we reproduce the results by [ref] when using their dark matter halo (NFW) density profile and halo evolution model, but we do not reproduce those of [ref] (see [ref] for a discussion of this difference).
Neutrino Clustering in Cold Dark Matter Halos : Implications for Ultra High Energy Cosmic Rays · Neutrino density profiles · 1.00
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Comparing our calculations with previously published results, we find that we reproduce the results by [ref] when using their dark matter halo (NFW) density profile and halo evolution model, but we do not reproduce those of [ref] (see [ref] for a discussion of this difference).
Gravitational clustering of relic neutrinos and implications for their detection · Neutrino density profiles · 1.00
Cites as background 6 papers
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Previous work has studied this non-linear neutrino clustering [ref] .
Grid Based Linear Neutrino Perturbations in Cosmological N-body Simulations · Introduction · 0.95
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Previous work has studied this non-linear neutrino clustering [ref] .
The effect of neutrinos on the matter distribution as probed by the Intergalactic Medium · Introduction · 0.95
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Previous work has studied this non-linear neutrino clustering [ref] .
Neutrinos in Non-linear Structure Formation - The Effect on Halo Properties · Introduction · 0.95
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