Gravitational clustering of relic neutrinos and implications for their detection

Ringwald, Andreas; Wong, Yvonne Y. Y.

doi:10.1088/1475-7516/2004/12/005

Cited by 215 publications

(357 citation statements)

References 118 publications

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“…211802-2 of origin is about 10 ÿ4 eV 2 , 10 ÿ5 eV 2 , and 10 ÿ6 eV 2 for 8 B, 7 Be, and pp neutrinos, respectively. With our choice of jM 2 i j of O 10 ÿ5 ÿ 10 ÿ4 eV 2 at neutrino production, we expect nonstandard matter effects to be of the same order as standard matter effects.…”

Section: 211802 (2005) P H Y S I C a L R E V I E W L E T T E R S mentioning

confidence: 99%

Solar Mass-Varying Neutrino Oscillations

2005

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We propose that the solar neutrino deficit may be due to oscillations of mass-varying neutrinos (MaVaNs). This scenario elucidates solar neutrino data beautifully while remaining comfortably compatible with atmospheric neutrino and K2K data and with reactor antineutrino data at short and long baselines (from CHOOZ and KamLAND). We find that the survival probability of solar MaVaNs is independent of how the suppression of neutrino mass caused by the acceleron-matter couplings varies with density. Measurements of MeV and lower energy solar neutrinos will provide a rigorous test of the idea. DOI: 10.1103/PhysRevLett.95.211802 PACS numbers: 13.15.+g, 14.60.Pq, 14.60.St Introduction.-Neutrino oscillation experiments have conclusively demonstrated that neutrinos have mass. Also, evidence has mounted that the expansion of our Universe is in an accelerating phase caused by a negative pressure component called dark energy. While these two seemingly disparate advances are unequivocally among the most important of the last few years, our knowledge of both is woefully incomplete.Solar neutrino data provide the only evidence of matter effects on neutrino oscillations. The large mixing angle (LMA) solution, while favored by reactor antineutrino data, is somewhat discrepant with solar data, thus calling into question how well neutrino-matter interactions are understood. It is crucial that our understanding of neutrino-matter interactions be confirmed or modified.Dark energy is troubling because the acceleration of the Universe is a very recent phenomenon in its expansion history. This ''cosmic coincidence'' problem can be expressed as follows: Why are the dark matter and dark energy densities comparable today even though their ratio scales as 1=a 3 (where a is the scale factor)?The coincidence that the scale of dark energy 2 10 ÿ3 eV 4 is similar to the scale of neutrino mass-squared differences 0:01 eV 2 was exploited recently in Refs. [1,2] to solve the coincidence problem. The authors of Ref.[2] considered the possibility of coupling neutrinos to dark energy by supposing that the dark energy density is a function of neutrino mass and imposing the condition that the total energy density of neutrinos and dark energy remain stationary under variations in neutrino mass. Then neutrino masses vary in such a way that the neutrino energy density and the dark energy density are related over a wide range of a.A way to make the dark energy density neutrino-mass dependent is to introduce a Yukawa coupling between a sterile neutrino and a light scalar field (similar to quintessence) called the acceleron. At energy scales below the sterile neutrino mass, the effective potential of the acceleron at late times receives a contribution equal to m n , where m and n are the active neutrino mass and number

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Section: 211802 (2005) P H Y S I C a L R E V I E W L E T T E R S mentioning

confidence: 99%

Solar Mass-Varying Neutrino Oscillations

2005

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“…(10), does not consider clustering of neutrinos on CDM structures, which occurs when the neutrino thermal velocity drops below the velocity dispersion, v, of forming clusters; for instance, it takes place at z ∼ 2.3 for v ∼ 1000 km s −1 and m ν ∼ 0.5 eV. The corresponding neutrino halo profile is flatter in the centre than a pure CDM Navarro-Frenk-White (Ringwald & Wong 2004). Including it in the 1-halo term of the halo model, Abazajian et al (2005) showed that it decreases the non-linear matter power spectrum.…”

Section: Robustness Of the Constraintsmentioning

confidence: 99%

CFHTLS weak-lensing constraints on the neutrino masses

Tereno

Schimd

Uzan

et al. 2009

A&A

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Context. Oscillation experiments yield strong evidence that at least some neutrinos are massive. As a hot dark-matter component, massive neutrinos should modify the expansion history of the Universe as well as the evolution of cosmological perturbations, in a different way from cold dark matter or dark energy. Aims. We use the latest release of CFHTLS cosmic-shear data to constrain the sum of the masses m ν of neutrinos, assuming three degenerate mass states. We also consider a joint analysis including other cosmological observables, notably CMB anisotropies, baryonic acoustic oscillations, and distance modulus from type Ia supernovae. Methods. Combining CAMB with a lensing code, we compute the aperture mass variance using a suitable recipe to deal with matter perturbations in the non-linear regime. The statistical analysis is performed by sampling an 8-dimensional likelihood on a regular grid as well as using the importance sampling technique. Results. We obtain the first constraint on neutrino masses based on cosmic-shear data, and combine CFHTLS with WMAP, SDSS, 2dFGRS, Gold-set, and SNLS data. The joint analysis yields 0.03 eV < m ν < 0.54 eV at the 95% confidence level. The preference for massive neutrinos vanishes when systematics are included.

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“…Gravitational clustering is most significant for more massive neutrinos, since these became non-relativistic at earlier times. Simulations show that the local density of neutrinos could be enhanced over the cosmological average by an order of magnitude or more [8,9].…”

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confidence: 99%

Measuring anisotropies in the cosmic neutrino background

Lisanti

Tully

2014

Phys. Rev. D

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Neutrino capture on tritium has emerged as a promising method for detecting the cosmic neutrino background (CνB). We show that relic neutrinos are captured most readily when their spin vectors are anti-aligned with the polarization axis of the tritium nuclei and when they approach along the direction of polarization. As a result, CνB observatories may measure anisotropies in the cosmic neutrino velocity and spin distributions by polarizing the tritium targets. A small dipole anisotropy in the CνB is expected due to the peculiar velocity of the lab frame with respect to the cosmic frame and due to late-time gravitational effects. The PTOLEMY experiment, a tritium observatory currently under construction, should observe a nearly isotropic background. This would serve as a strong test of the cosmological origin of a potential signal. The polarized-target measurements may also constrain non-standard neutrino interactions that would induce larger anisotropies and help discriminate between Majorana versus Dirac neutrinos.

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Gravitational clustering of relic neutrinos and implications for their detection

Cited by 215 publications

References 118 publications

Solar Mass-Varying Neutrino Oscillations

Solar Mass-Varying Neutrino Oscillations

CFHTLS weak-lensing constraints on the neutrino masses

Measuring anisotropies in the cosmic neutrino background

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