A new life for sterile neutrinos: resolving inconsistencies using hot dark matter

Hamann, Jan; Hasenkamp, Jasper

doi:10.1088/1475-7516/2013/10/044

Cited by 115 publications

(159 citation statements)

References 66 publications

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“…The tension between this measurement and the Planck temperature power spectrum has been discussed in Ade et al (2013b) (see also Hamann & Hasenkamp 2013;Battye & Moss 2013); and including a large value for the sum of the neutrino masses is mentioned as one possibility to relieve this tension. However, Costanzi et al (2013) showed that in the case of mν = 0.4 eV there is up to 30% uncertainty on the predicted cluster count depending on whether the r.m.s.…”

Section: The Reliability Of Low Redshift Growth Of Structure Constraintsmentioning

confidence: 77%

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: signs of neutrino mass in current cosmological data sets

Beutler

Saito

Brownstein

et al. 2014

Monthly Notices of the Royal Astronomical Society

125

143

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We investigate the cosmological implications of the latest growth of structure measurement from the Baryon Oscillation Spectroscopic Survey (BOSS) CMASS Data Release 11 with particular focus on the sum of the neutrino masses, m ν . We examine the robustness of the cosmological constraints from the Baryon Acoustic Oscillation (BAO) scale, the Alcock-Paczynski effect and redshift-space distortions (D V /r s , F AP , f σ 8 ) of Beutler et al. (2013), when introducing a neutrino mass in the power spectrum template. We then discuss how the neutrino mass relaxes discrepancies between the Cosmic Microwave Background (CMB) and other low-redshift measurements within ΛCDM. Combining our cosmological constraints with WMAP9 yields m ν = 0.36 ± 0.14 eV (68% c.l.), which represents a 2.6σ preference for non-zero neutrino mass. The significance can be increased to 3.3σ when including weak lensing results and other BAO constraints, yielding m ν = 0.35 ± 0.10 eV (68% c.l.). However, combining CMASS with Planck data reduces the preference for neutrino mass to ∼ 2σ. When removing the CMB lensing effect in the Planck temperature power spectrum (by marginalising over A L ), we see shifts of ∼ 1σ in σ 8 and Ω m , which have a significant effect on the neutrino mass constraints. In case of CMASS plus Planck without the A L -lensing signal, we find a preference for a neutrino mass of m ν = 0.34 ± 0.14 eV (68% c.l.), in excellent agreement with the WMAP9+CMASS value. The constraint can be tightened to 3.4σ yielding m ν = 0.36 ± 0.10 eV (68% c.l.) when weak lensing data and other BAO constraints are included.

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Section: The Reliability Of Low Redshift Growth Of Structure Constraintsmentioning

confidence: 77%

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: signs of neutrino mass in current cosmological data sets

Beutler

Saito

Brownstein

et al. 2014

Monthly Notices of the Royal Astronomical Society

125

143

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“…These results arise from the fact that the free-streaming of massive neutrinos can reduce the tension between the values of σ 8 obtained with CMB and LSS data [279][280][281][282][283][284][285][286][287][288][289][290]. For the light sterile neutrinos, similar analyses were performed in the ΛCDM +N eff +m eff s model by several authors [291,[328][329][330][331][332][333], in spite of some tension between different datasets [334]. Figure 7(b), adapted from Ref.…”

Section: Current Bounds From Cosmologymentioning

confidence: 80%

Light sterile neutrinos

Gariazzo

Giunti

Laveder

et al. 2015

J. Phys. G: Nucl. Part. Phys.

224

336

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Abstract. The theory and phenomenology of light sterile neutrinos at the eV mass scale is reviewed. The reactor, Gallium and LSND anomalies are briefly described and interpreted as indications of the existence of short-baseline oscillations which require the existence of light sterile neutrinos. The global fits of short-baseline oscillation data in 3+1 and 3+2 schemes are discussed, together with the implications for β-decay and neutrinoless double-β decay. The cosmological effects of light sterile neutrinos are briefly reviewed and the implications of existing cosmological data are discussed. The review concludes with a summary of future perspectives.

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“…H 0 from CMB data and direct measurements of H 0 (see also [41,[64][65][66][67]). We therefore now include N eff as a free parameter and examine the constraints on its value, 4 as well as the effect on the neutrino mass bound.…”

Section: E Joint Constraints On Neutrino Mass and Number Of Speciesmentioning

confidence: 99%

Inflationary freedom and cosmological neutrino constraints

2014

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The most stringent bounds on the absolute neutrino mass scale come from cosmological data. These bounds are made possible because massive relic neutrinos affect the expansion history of the universe and lead to a suppression of matter clustering on scales smaller than the associated free streaming length. However, the resulting effect on cosmological perturbations is relative to the primordial power spectrum of density perturbations from inflation, so freedom in the primordial power spectrum affects neutrino mass constraints. Using measurements of the cosmic microwave background (CMB), the galaxy power spectrum and the Hubble constant, we constrain neutrino mass and number of species for a modelindependent primordial power spectrum. Describing the primordial power spectrum by a 20-node spline, we find that the neutrino mass upper limit is a factor 3 weaker than when a power law form is imposed, if only CMB data are used. The primordial power spectrum itself is constrained to better than 10% in the wave vector range k ≈ 0.01 − 0.25 Mpc −1 . Galaxy clustering data and a determination of the Hubble constant play a key role in reining in the effects of inflationary freedom on neutrino constraints. The inclusion of both eliminates the inflationary freedom degradation of the neutrino mass bound, giving for the sum of neutrino masses Σm ν < 0.18 eV (at 95% confidence level, Planck þ BOSS þ H 0 ), approximately independent of the assumed primordial power spectrum model. When allowing for a free effective number of species, N eff , the joint constraints on Σm ν and N eff are loosened by a factor 1.7 when the power law form of the primordial power spectrum is abandoned in favor of the spline parametrization.

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A new life for sterile neutrinos: resolving inconsistencies using hot dark matter

Cited by 115 publications

References 66 publications

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: signs of neutrino mass in current cosmological data sets

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: signs of neutrino mass in current cosmological data sets

Light sterile neutrinos

Inflationary freedom and cosmological neutrino constraints

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