Neutrino halos in clusters of galaxies and their weak lensing signature

Villaescusa-Navarro, Francisco; Miralda-Escudé, Jordi; Peña-Garay, Carlos; Quilis, Vicent

doi:10.1088/1475-7516/2011/06/027

Cited by 35 publications

(37 citation statements)

References 30 publications

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“…However, it is now well established that while massive neutrinos contribute to the expansion rate of the Universe their non-linear clustering is negligible [43,44,[47][48][49][50][51]55] for reasonable neutrino masses. One of the consequences of this is that the halo mass function and halo bias in a cosmology with massive neutrinos can be described in terms of the CDM plus baryons density field (instead of the total matter density field) [50,51,55,65].…”

Section: Pinocchio and Methods Implementationmentioning

confidence: 99%

Simulating cosmologies beyond ΛCDM with PINOCCHIO

Rizzo

Villaescusa-Navarro

Monaco

et al. 2017

J. Cosmol. Astropart. Phys.

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We present a method that extends the capabilities of the PINpointing Orbit-Crossing Collapsed HIerarchical Objects (PINOCCHIO) code, allowing it to generate accurate dark matter halo mock catalogues in cosmological models where the linear growth factor and the growth rate depend on scale. Such cosmologies comprise, among others, models with massive neutrinos and some classes of modified gravity theories. We validate the code by comparing the halo properties from PINOCCHIO against N-body simulations, focusing on cosmologies with massive neutrinos: νΛCDM. We analyse the halo mass function, halo two-point correlation function, halo power spectrum and the moments of the halo density field, showing that PINOCCHIO reproduces the results from simulations with the same level of precision as the original code (∼ 5 − 10%). We demonstrate that the abundance of halos in cosmologies with massless and massive neutrinos from PINOCCHIO matches very well the outcome of simulations, and point out that PINOCCHIO can reproduce the Ω ν − σ 8 degeneracy that affects the halo mass function. We show that the clustering properties of the halos from PINOCCHIO matches accurately those from simulations both in real and redshift-space, in the latter case up to k = 0.3 h Mpc −1 . We finally point out that the first moments of the halo density field from simulations are precisely reproduced by PINOCCHIO. We emphasize that the computational time required by PINOCCHIO to generate mock halo catalogues is orders of magnitude lower than the one needed for N-body simulations. This makes this tool ideal for applications like covariance matrix studies within the standard ΛCDM model but also in cosmologies with massive neutrinos or some modified gravity theories.

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Section: Pinocchio and Methods Implementationmentioning

confidence: 99%

Simulating cosmologies beyond ΛCDM with PINOCCHIO

Rizzo

Villaescusa-Navarro

Monaco

et al. 2017

J. Cosmol. Astropart. Phys.

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“…We can note that Virgo is much bigger and distant than Andromeda. However, as N -body simulations show [41], the neutrino halo of each object is always much more extended than the one of dark matter, due to the high neutrino thermal velocities. Thus, despite its high distance from the Milky Way, we expect that Virgo will also contribute to the neutrino overdensity at the Earth location.…”

Section: Other Objects: Virgo and Andromedamentioning

confidence: 99%

Neutrino clustering in the Milky Way and beyond

Mertsch

Parimbelli

Salas

et al. 2020

J. Cosmol. Astropart. Phys.

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The standard cosmological model predicts the existence of a Cosmic Neutrino Background, which has not yet been observed directly. Some experiments aiming at its detection are currently under development, despite the tiny kinetic energy of the cosmological relic neutrinos, which makes this task incredibly challenging. Since massive neutrinos are attracted by the gravitational potential of our Galaxy, they can cluster locally. Neutrinos should be more abundant at the Earth position than at an average point in the Universe. This fact may enhance the expected event rate in any future experiment. Past calculations of the local neutrino clustering factor only considered a spherical distribution of matter in the Milky Way and neglected the influence of other nearby objects like the Virgo cluster, although recent N -body simulations suggest that the latter may actually be important. In this paper, we adopt a back-tracking technique, well established in the calculation of cosmic rays fluxes, to perform the first three-dimensional calculation of the number density of relic neutrinos at the Solar System, taking into account not only the matter composition of the Milky Way, but also the contribution of the Andromeda galaxy and the Virgo cluster. The effect of Virgo is indeed found to be relevant and to depend non-trivially on the value of the neutrino mass. Our results show that the local neutrino density is enhanced by 0.53% for a neutrino mass of 10 meV, 12% for 50 meV, 50% for 100 meV or 500% for 300 meV.

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“…Dark matter halos are identified by employing the Friends-of-Friends algorithm (Davis et al 1985) by setting the linking length parameter b = 0.2. The group-finder is run only on top of the CDM+baryon distribution, as the contribution of neutrino to the masses of halos has been shown to be negligible (Villaescusa-Navarro et al 2011, 2013aBrandbyge et al 2010;Ichiki & Takada 2012;LoVerde 2014b;Castorina et al 2014). Only halos that contain more than 20 particles are identified, although for the main analysis we only consider halos with masses above 3.2× 10 13 h −1 M and 3 × 10 12 h −1 M for the low-and highresolution simulations, respectively.…”

Section: Numerical Simulationsmentioning

confidence: 99%

The Imprint of Neutrinos on Clustering in Redshift Space

Villaescusa-Navarro

Banerjee

Dalal

et al. 2018

ApJ

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We investigate the signatures left by the cosmic neutrino background on the clustering of matter, CDM+baryons and halos in redshift-space using the HADES simulations: a set of more than 1000 N-body and hydrodynamical simulations with massless and massive neutrinos. While on large scales the clustering of matter and CDM+baryons is very different in cosmologies with massive and massless neutrinos, we find that the effect neutrinos induce on the clustering of CDM+baryons in redshift-space on small scales is almost entirely due to the change in σ 8 . However, neutrinos do imprint a characteristic signature in the quadrupole of the total matter field (CDM+baryon+neutrinos) on small scales, that can be used to disentangle the effect of σ 8 and M ν . We show that the effect of neutrinos on the clustering of halos is very different, on all scales, to the effects induced by varying σ 8 . We find that the effects of neutrinos of the growth rate of CDM+baryons ranges from ∼ 0.3% to 2% on scales k ∈ [0.01, 0.5] hMpc −1 for neutrinos with masses M ν 0.15 eV. We compute the bias between the momentum of halos and the momentum of CDM+baryon and find it to be 1 on large scales for all models with massless and massive neutrinos considered. This point towards a velocity bias between halos and total matter on large scales that it is important to account for in order to extract unbiased neutrino information from velocity/momentum surveys such as kSZ observations. We show that, even on very large-scales, non-linear corrections are important to describe the clustering of halos in redshift-space in cosmologies with massless and massive neutrinos at low redshift. We show that baryonic effects can affect the clustering of matter and CDM+baryons in redshift-space by up to a few percent down to k = 0.5 hMpc −1 . We find that hydrodynamics and astrophysical processes, as implemented in our simulations, only distort the relative effect that neutrinos induce on the anisotropic clustering of matter, CDM+baryons and halos in redshift-space by less than 1%. Thus, the effect of neutrinos in the fully non-linear regime can be written as a transfer function with very weak dependence on astrophysics that can be studied through N-body simulations.

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Neutrino halos in clusters of galaxies and their weak lensing signature

Cited by 35 publications

References 30 publications

Simulating cosmologies beyond ΛCDM with PINOCCHIO

Simulating cosmologies beyond ΛCDM with PINOCCHIO

Neutrino clustering in the Milky Way and beyond

The Imprint of Neutrinos on Clustering in Redshift Space

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