Upper limits on neutrino masses from the 2dFGRS and WMAP: the role of priors

Elgarøy, Ø.; Lahav, O.

doi:10.1088/1475-7516/2003/04/004

Cited by 83 publications

(45 citation statements)

References 75 publications

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“…Still, the precise analysis of the recent microwave background anisotropy data and structure data at large red-shifts imply the necessity of some admixture of hot DM which can be naturally provided by light neutrinos with Σm ν f < 2.2 eV or m ν f < 0.73 eV (see for example [29,30]). Recent WMAP measurements (see [31]) together with the LSS analysis has improved the limit: Σm ν f < 0.69 eV and hence, m ν f < 0.23 eV.…”

Section: Large Scale Structure and Neutrinomentioning

confidence: 99%

Neutrino oscillations and the early universe

Kirilova¹

2004

Open Physics

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Abstract:The observational and theoretical status of neutrino oscillations in connection with solar and atmospheric neutrino anomalies is presented briefly. The effect of neutrino oscillations on the evolution of the early Universe is discussed in detail. A short review is given of the standard Big Bang Nucleosynthesis (BBN) and the influence of resonant and non-resonant neutrino oscillations on active neutrinos and on primordial synthesis of He-4. BBN cosmological constraints on neutrino oscillation parameters are discussed.

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Section: Large Scale Structure and Neutrinomentioning

confidence: 99%

Neutrino oscillations and the early universe

Kirilova¹

2004

Open Physics

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“…When m ν > 10 −3 eV neutrinos are non-relativistic today [11] and thus behave like a hot component of dark matter. The presence of even a small fraction of massive neutrinos (hot dark matter) f ν ≡ Ω ν /Ω M , of order 10-20 %, requires a smaller value for the cosmological constant in comparison to a pure ΛCDM model, while other cosmological parameters are largely unaffected [6]. This is because a smaller Ω Λ results in a larger Ω M and hence a faster fluctuation growth rate, which compensates for the reduction of small-and intermediate-scale power caused by the neutrinos.…”

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confidence: 99%

“…To compute P (k, z) we assume a close to scaleinvariant (Harrison-Peebles-Yu-Zeldovich) post-inflation energy density perturbation power spectrum P 0 (k) ∝ k n , with n ∼ 1, and we use a semi-analytical approximation for the transfer function T (k, z) in the ΛCDM model with three species of equal-mass neutrinos [41]. 6 For the 5 This is more consistent with estimates from WMAP data and from Big Bang nucleosynthesis using the mean of the primordial deuterium abundance measurements, but it is significantly larger than an estimate based on helium and lithium abundance measurements, see, e.g., Ref. [17].…”

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confidence: 99%

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Neutrino mass limit from galaxy cluster number density evolution

et al. 2005

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Measurements of the evolution with redshift of the number density of massive galaxy clusters are used to constrain the energy density of massive neutrinos and so the sum of neutrino masses mν . We consider a spatially-flat cosmological model with cosmological constant, cold dark matter, baryonic matter, and massive neutrinos. Accounting for the uncertainties in the measurements of the relevant cosmological parameters we obtain a limit of mν < 2.4 eV (95 % C.L.). Constraints on neutrino masses are of great interest for particle physics as well as for cosmology, and thus attract a lot of scientific attention (for recent reviews see Refs. [1, 2, 3,4]). Current upper limits on the sum of neutrino masses, m ν , from cosmological structure formation data [5,6], cosmic microwave background (CMB) fluctuation data [7,8], or combined CMB + large-scale structure data [9,10,11,12,13], are of order an eV [14] (for various limits see Table 1 of Ref. [4]). The number of neutrino species can be constrained from Big Bang nucleosynthesis or by using CMB and large-scale structure data [11,15].High energy physics experiments also constrain neutrino masses, and have measured the number of light neutrino species with high precision [3]. Direct searches for neutrino mass effects in beta decays yield limits in the region of several eV, but the sum over all neutrino masses is almost unconstrained by beta decay and other experiments, mainly due to the weak limit on the tauneutrino mass. The measurement of neutrino oscillations on the other hand constrains the differences between the squared masses of the neutrino mass eigenstates ∆m 2 . With the justified assumption that neutrino masses are non-negative and for mass splittings ∆m , we obtain m ν > 0.04 eV if the solar mass splitting is between the highest and second highest mass eigenstates ( m ν > 0.07 eV if the atmospheric mass splitting is between the two highest states). Results from the LSND collaboration yield a larger lower limit on m ν , and must be considered if confirmed by the MiniBooNE experiment [16], which is currently taking data.In this paper we use the dependence of galaxy cluster number density evolution on the massive neu- * Electronic address: tinatin@phys.ksu.edu † Electronic address: evt@phys.ksu.edu ‡ Electronic address: arna@lukash.asc.rssi.ru § Electronic address: ratra@phys.ksu.edu trino energy density parameter Ω ν to set a limit on m ν . We consider the standard spatially-flat ΛCDM Friedmann-Lemaître-Robertson-Walker cosmological spacetime model with baryons, cold dark matter (CDM), massive neutrinos, and a non-zero cosmological constant Λ (for a recent review see Ref.[17]). To compute the cluster number density as a function of redshift z we use the Press-Schechter approach [18,19] as modified by Sheth and Tormen (ST) [20].1 This approach makes use of the mass function N (M > M 0 ) of clusters (cluster number density as a function of cluster mass M greater than a fiducial mass M 0 ), which depends on cosmological model parameters [21,22,23,24]. In particular,...

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“…However, m 0 is constrained by WMAP data [10],3m 0 < 0.71 eV. When analyzed in conjunction with neutrino oscillation, it is found that mass eigenvalues are essentially degenerate with 3m 0 > 0.4 eV [11] The above limits put limits on ε : 7.9 × 10 −3 < ε < 2.5 × 10 −2 . It is pertinent to remark that in view of small mass differences involved [cf.…”

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confidence: 99%

Neutrino mass matrix with approximate flavor symmetry

Riazuddin

2003

J. High Energy Phys.

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Phenomenological implications of neutrino oscillations implied by recent experimental data on pattern of neutrino mass matrix are disscussed. It is shown that it is possible to have a neutrino mass matrix which shows approximate flavor symmetry; the neutrino mass differences arise from flavor violation in off-diagonal Yukawa couplings. Two modest extensions of the standard model, which can embed the resulting neutrino mass matix have also been discussed.

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Upper limits on neutrino masses from the 2dFGRS and WMAP: the role of priors

Cited by 83 publications

References 75 publications

Neutrino oscillations and the early universe

Neutrino oscillations and the early universe

Neutrino mass limit from galaxy cluster number density evolution

Neutrino mass matrix with approximate flavor symmetry

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