Resolving cosmic neutrino structure: a hybrid neutrino<i>N</i>-body scheme

Brandbyge, Jacob; Hannestad, Steen

doi:10.1088/1475-7516/2010/01/021

Cited by 86 publications

(101 citation statements)

References 19 publications

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“…Since cosmological constraints can mainly be derived from moderate and large l-values it means that non-linear corrections must be under control at the percent level. For neutrinos this has already been achieved [70][71][72], but for example baryonic physics can contribute an uncertainty of 10% or more on scale which are relevant for cosmological parameter extraction [109].…”

Section: Weak Lensing Surveysmentioning

confidence: 99%

“…Simply treating neutrinos as particles is difficult because the thermal motion introduces noise which completely dominates the behaviour of neutrinos on small scales. However, it has been shown that the matter power spectrum can be computed at the 1% level of precision with neutrinos included, using Nbody techniques [70][71][72]61] (Fig. 4).…”

Section: Non-linear Evolutionmentioning

confidence: 99%

“…The numerical set-up was based on the code described in [72] and from the N-body simulations, halos were identified using the AMIGA halo finder [77].…”

Section: The Halo Mass Functionmentioning

confidence: 99%

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Neutrino physics from precision cosmology

Hannestad

2010

Progress in Particle and Nuclear Physics

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101

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Cosmology provides an excellent laboratory for testing various aspects of neutrino physics. Here, I review the current status of cosmological searches for neutrino mass, as well as other properties of neutrinos. Future cosmological probes of neutrino properties are also discussed in detail.Comment: 30 pages, 10 figures, Review article for Progress in Particle and Nuclear Physics, references update

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Section: Weak Lensing Surveysmentioning

confidence: 99%

Section: Non-linear Evolutionmentioning

confidence: 99%

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Neutrino physics from precision cosmology

Hannestad

2010

Progress in Particle and Nuclear Physics

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101

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“…Neutrinos are also responsible for dampening the matter power spectrum below their free-streaming scale; see e.g., [23] for a review. This effect, which amounts to a scale dependent power suppression, is straightforward to compute in linear theory [37] and in the non-linear regime via numerical simulations e.g., [38,39,40].…”

Section: Cosmology: Observational Constraints and Degeneraciesmentioning

confidence: 99%

Cosmology and Neutrino Physics

Jiménez¹

2018

Proceedings of XVII International Workshop on Neutrino Telescopes — PoS(NEUTEL2017)

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I review the current status of the cosmological standard model (LCDM) with a special focus on neutrino cosmology. In particular, I describe how the standard model of cosmology has, so far, passed all tests and thus is able to explain all current observations of the sky. Within this model, it is possible to infer properties of neutrinos. In particular, I show how current cosmological surveys constraint, robustly, the sum of neutrino masses < 0.13eV and that current cosmological data already favour strongly, in a Bayesian sense, the normal ordering of the neutrino masses. In the next five years, future cosmological surveys should be able to measure robustly the sum of neutrino masses and, further in the future, the individual masses of neutrinos. XVII International Workshop on Neutrino Telescopes

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“…[5,6]). At the same time, numerical predictions of the effect of neutrino masses on the clustering of small-scale structures are making a good deal of headway [7,8]. Within one decade, cosmological observations should be able to detect the absolute neutrino mass scale, even if the heaviest mass is close to 0.05 eV.…”

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confidence: 99%

Galaxies weigh in on neutrinos

Lesgourgues¹

2010

Physics

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A comparison between the density in surrounding galaxies today and a few billion years ago provides a new upper bound on neutrino mass. Neutrinos are infamously lightweight particles that are near impossible to detect, let alone place on a scale. Yet our most basic model for understanding the symmetries of matter and particles rests on an accurate measure of the neutrino masses.Over the past decade, observational cosmology has taken a leading position in providing an upper bound on these masses. Now, in a paper appearing in Physical Review Letters, Shaun Thomas, Filipe Abdalla, and Ofer Lahav at University College London in the UK [1] predict that the total neutrino mass, summed over the three neutrino families, is smaller than 0.28 eV-the tightest upper bound yet. Their prediction is based on a new mapping of the distribution of density of surrounding galaxies.Until recently, neutrinos were described in the standard model of particle physics as massless particles with three "flavor states": the electron, muon, and tau neutrino. The 1998 discovery at Japan's Super Kamiokande neutrino observatory that neutrinos oscillate between these flavor states brought the first direct experimental evidence for new physics beyond the standard model and lead to the picture that neutrino particles should be viewed as three "mass states," each of which is composed of a mixture of the three flavor states in fixed proportions that are parametrized by "mixing angles." Flavor oscillations depend on these angles, as well as on the differences between the squares of each mass. The details of this model are, however, still uncertain.In fact, because neutrino particles are so light and difficult to measure, they come saddled with a host of enigmas: Do neutrinos have the same mathematical structure as quarks and electrons (namely, "Dirac fermions") or a yet unobserved structure in which they would be their own antiparticle (referred to as "Majorana fermions")? Do their interactions violate chargeparity (CP) symmetry as is the case for quarks? What is the origin of their mass? What role did they play in the early evolution of the Universe that explains the excess of matter over antimatter that we now observe? Addressing these questions through all possible experimental techniques gives us an opportunity to probe new sectors of particle physics.Over time, experiments have yielded various bounds on neutrino masses. For example, the probability of flavor oscillation for solar or atmospheric neutrinos gives access to two mass square differences, but such results provide a lower bound on only two out of the three masses, and no upper bound on any of them. Currently, the lower bound on the largest neutrino mass is 0.05 eV. Tritium beta decay experiments are able to provide an upper bound on the sum over the three neutrino masses, M ν , but it is still on the order of 7 eV [2]. Germany's KA-TRIN experiment, a next generation tritium beta-decay experiment starting in 2012, could tighten this bound by another order of magnitude.Cosmological observ...

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Resolving cosmic neutrino structure: a hybrid neutrinoN-body scheme

Cited by 86 publications

References 19 publications

Neutrino physics from precision cosmology

Neutrino physics from precision cosmology

Cosmology and Neutrino Physics

Galaxies weigh in on neutrinos

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