Grid based linear neutrino perturbations in cosmological<i>N</i>-body simulations

Brandbyge, Jacob; Hannestad, Steen

doi:10.1088/1475-7516/2009/05/002

Cited by 139 publications

(186 citation statements)

References 22 publications

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“…The widely used phenomenological calculation of the nonlinear matter power spectrum called the HALOFIT (Smith et al 2003) has not been calibrated for models with massive neutrinos. Consistent treatments of massive neutrinos in the nonlinear structure formation using cosmological perturbation theory (Saito et al 2008(Saito et al , 2009Wong 2008;Lesgourgues et al 2009;Shoji & Komatsu 2009) and numerical simulations (Brandbyge et al 2008;Brandbyge & Hannestad 2009) have just begun to be explored. More work along these lines would be necessary to exploit the information on the growth structure to constrain the mass of neutrinos.…”

Section: Neutrino Massmentioning

confidence: 99%

SEVEN-YEARWILKINSON MICROWAVE ANISOTROPY PROBE(WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION

Komatsu¹,

Smith²,

Dunkley³

et al. 2011

ApJS

7,710

472

6,429

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The combination of seven-year data from WMAP and improved astrophysical data rigorously tests the standard cosmological model and places new constraints on its basic parameters and extensions. By combining the WMAP data with the latest distance measurements from the baryon acoustic oscillations (BAO) in the distribution of galaxies and the Hubble constant (H 0 ) measurement, we determine the parameters of the simplest six-parameter ΛCDM model. The power-law index of the primordial power spectrum is n s = 0.968 ± 0.012 (68% CL) for this data combination, a measurement that excludes the Harrison-Zel'dovich-Peebles spectrum by 99.5% CL. The other parameters, including those beyond the minimal set, are also consistent with, and improved from, the five-year results. We find no convincing deviations from the minimal model. The seven-year temperature power spectrum gives a better determination of the third acoustic peak, which results in a better determination of the redshift of the matter-radiation equality epoch. Notable examples of improved parameters are the total mass of neutrinos, m ν < 0.58 eV (95% CL), and the effective number of neutrino species, N eff = 4.34 +0.86 −0.88 (68% CL), which benefit from better determinations of the third peak and H 0 . The limit on a constant dark energy equation of state parameter from WMAP+BAO+H 0 , without high-redshift Type Ia supernovae, is w = −1.10 ± 0.14 (68% CL). We detect the effect of primordial helium on the temperature power spectrum and provide a new test of big bang nucleosynthesis by measuring Y p = 0.326 ± 0.075 (68% CL). We detect, and show on the map for the first time, the tangential and radial polarization patterns around hot and cold spots of temperature fluctuations, an important test of physical processes at z = 1090 and the dominance of adiabatic scalar fluctuations. The seven-year polarization data have significantly improved: we now detect the temperature-E-mode polarization cross power spectrum at 21σ , compared with 13σ from the five-year data. With the seven-year temperature-B-mode cross power spectrum, the limit on a rotation of the polarization plane due to potential parity-violating effects has improved by 38% to Δα = −1.• 1 ± 1.• 4(statistical) ± 1.• 5(systematic) (68% CL). We report significant detections of the Sunyaev-Zel'dovich (SZ) effect at the locations of known clusters of galaxies. The measured SZ signal agrees well with the expected signal from the X-ray data on a cluster-by-cluster basis. However, it is a factor of 0.5-0.7 times the predictions from "universal profile" of Arnaud et al., analytical models, and hydrodynamical simulations. We find, for the first time in the SZ effect, a significant difference between the cooling-flow and non-cooling-flow clusters (or relaxed and non-relaxed clusters), which can explain some of the discrepancy. This lower amplitude is consistent with the lower-than-theoretically expected SZ power spectrum recently measured by the South Pole Telescope Collaboration.

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Section: Neutrino Massmentioning

confidence: 99%

SEVEN-YEARWILKINSON MICROWAVE ANISOTROPY PROBE(WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION

Komatsu¹,

Smith²,

Dunkley³

et al. 2011

ApJS

7,710

472

6,429

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“…Saito et al 2008Saito et al , 2009Wong 2008;Brandbyge et al 2008;Brandbyge & Hannestad 2009;Viel et al 2010;Marulli et al 2011;Bird et al 2012;Carbone et al 2012;Hou et al 2014;Lesgourgues & Pastor 2012). The renewed interest is mainly driven by the large amount of cosmological data available today, which allow placing competitive limits on the neutrino mass-scale and hierarchy.…”

Section: Revival Of Neutrino Sciencementioning

confidence: 99%

“…More recently, Brandbyge et al (2008) described a simple method for including the effect of massive neutrinos in large-scale N-body simulations, using a hybrid TreePM approach, but neglecting all the hydrodynamics; their findings already showed that the suppression of power due to the presence of massive neutrinos is increased by nonlinear effects. Subsequently, Brandbyge & Hannestad (2009) modeled neutrinos as a fluid with a grid method, and pointed out the relative benefits and drawbacks of implementing the effects of neutrinos in the form of particles versus a grid-based implementation. In their code, the gravitational force due to neutrinos is calculated using the linearly evolved density distribution of the neutrinos in Fourier space.…”

Section: Particle Implementation Of Massive Neutrinosmentioning

confidence: 99%

Suite of hydrodynamical simulations for the Lyman-αforest with massive neutrinos

Rossi

Palanque-Delabrouille

Borde

et al. 2014

A&A

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The signature left in quasar spectra by neutral hydrogen in the Universe allows constraining the sum of the neutrino masses with a better sensitivity than laboratory experiments and may shed new light on the neutrino mass hierarchy and the absolute mass-scale of neutrinos. Constraints on cosmological parameters and on the dark energy equation of state can also be derived from a joint parameter estimation procedure. However, this requires a detailed modeling of the line-of-sight power spectrum of the transmitted flux in the Lyman-α (Lyα) forest on scales ranging from a few to hundreds of megaparsecs, which in turn demands the inclusion and careful treatment of cosmological neutrinos. To this end, we present here a suite of state-of-the-art hydrodynamical simulations with cold dark matter (CDM), baryons and massive neutrinos, specifically targeted for modeling the low-density regions of the intergalactic medium (IGM) as probed by the Lyα forest at high-redshift. The simulations span volumes ranging from (25 h −1 Mpc) 3 to (100 h −1 Mpc) 3 , and were made using either 3 × 192 3 21 million or 3 × 768 3 1.4 billion particles. The resolution of the various runs was further enhanced, so that we reached the equivalent of 3 × 3072 3 87 billion particles in a (100 h −1 Mpc) 3 box size. The chosen cosmological parameters are compatible with the latest Planck 2013 results, although we also explored the effect of slight variations in the main cosmological and astrophysical parameters. We adopted a particle-type implementation of massive neutrinos, and consider three degenerate species with masses m ν = 0.1, 0.2, 0.3, 0.4, and 0.8 eV, respectively. We improved on previous studies in several ways, in particular with updated routines for IGM radiative cooling and heating processes, and initial conditions based on second-order Lagrangian perturbation theory (2LPT) rather than the Zel'dovich approximation. This allowed us to safely start our runs at relatively low redshift (z = 30), which reduced the shot-noise contamination in the neutrino component and the CPU consumption. In addition to providing technical details on the simulations, we present the first analysis of the nonlinear three-and one-dimensional matter and flux power spectra from these models, and characterize the statistics of the transmitted flux in the Lyα forest including the effect of massive neutrinos. In synergy with recent data from the Baryon Acoustic Spectroscopic Survey (BOSS) and the Planck satellite, and with a grid of corresponding neutrino-less simulations, our realizations will allow us to constrain cosmological parameters and neutrino masses directly from the Lyα forest with improved sensitivity. In addition, our simulations can be useful for a broader variety of cosmological and astrophysical applications, ranging from the three-dimensional modeling of the Lyα forest to cross-correlations between different probes, studying the expansion history of the Universe including massive neutrinos, and particle-physics related topics. Moreover, while ...

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“…Let the rms mass fluctuation within a sphere of radius r be σ M (r). The average linear overdensity δ 2 = ν 2 σ M (r 2 ) within a radius r 2 , under the condition that the mean linear overdensity within the smaller radius r 1 is equal to δ 1 = ν 1 σ M (r 1 ), can be calculated as ν 2 = γ 12 ν 1 , where 6) where j 1 is the spherical Bessel function. We use this equation to obtain the average linear overdensity profile around a halo.…”

Section: Mass Density Profilementioning

confidence: 99%

“…Apart from this linear effect, massive neutrinos are also expected to cluster around gravitationally collapsed dark matter haloes as their streaming velocities are reduced and become comparable to the velocity dispersions of the halos, thereby modifying the dark matter halo total mass density profile. Previous work has studied this non-linear neutrino clustering [4][5][6][7][8][9]. Here, we present a new calculation with updated parameters and a more realistic halo model.…”

Section: Introductionmentioning

confidence: 99%

Neutrino halos in clusters of galaxies and their weak lensing signature

Villaescusa-Navarro

Miralda-Escudé

Peña-Garay

et al. 2011

J. Cosmol. Astropart. Phys.

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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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Grid based linear neutrino perturbations in cosmologicalN-body simulations

Cited by 139 publications

References 22 publications

SEVEN-YEARWILKINSON MICROWAVE ANISOTROPY PROBE(WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION

SEVEN-YEARWILKINSON MICROWAVE ANISOTROPY PROBE(WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION

Suite of hydrodynamical simulations for the Lyman-αforest with massive neutrinos

Neutrino halos in clusters of galaxies and their weak lensing signature

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