2018
DOI: 10.3389/fphy.2017.00070
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Status of Neutrino Properties and Future Prospects—Cosmological and Astrophysical Constraints

Abstract: Cosmological observations are a powerful probe of neutrino properties, and in particular of their mass. In this review, we first discuss the role of neutrinos in shaping the cosmological evolution at both the background and perturbation level, and describe their effects on cosmological observables such as the cosmic microwave background and the distribution of matter at large scale. We then present the state of the art concerning the constraints on neutrino masses from those observables, and also review the pr… Show more

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Cited by 127 publications
(67 citation statements)
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References 184 publications
(323 reference statements)
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“…3 Current CMB measurements on N eff and upcoming sensitivity Both the polarization and temperature CMB spectra are sensitive to the number of effective neutrino species in the early Universe [3,51,52]. The most obvious effect of a change in N eff is to modify the time of matter-radiation equality which is of pivotal importance for structure formation [53].…”
Section: Numericsmentioning
confidence: 99%
“…3 Current CMB measurements on N eff and upcoming sensitivity Both the polarization and temperature CMB spectra are sensitive to the number of effective neutrino species in the early Universe [3,51,52]. The most obvious effect of a change in N eff is to modify the time of matter-radiation equality which is of pivotal importance for structure formation [53].…”
Section: Numericsmentioning
confidence: 99%
“…Neutrino oscillation experiments have measured with very good precision the three leptonic flavor mixing angles {θ 12 , θ 13 , θ 23 } and two independent neutrino mass-squared differences ∆m 2 21 ≡ m 2 2 − m 2 1 and |∆m 2 31 | ≡ |m 2 3 − m 2 1 |. The absolute scale of neutrino masses, however, has to be determined from non-oscillation approaches, using beta decay [1], neutrinoless double-beta decay [2], or cosmological observations [3]. Once the neutrino mass scale is established, one knows the lightest neutrino mass, which is m 1 in the case of normal neutrino mass ordering (NO) with m 1 < m 2 < m 3 , or m 3 in the case of inverted neutrino mass ordering (IO) with m 3 < m 1 < m 2 .…”
Section: Introductionmentioning
confidence: 99%
“…The posterior distributions of the effective neutrino mass and its variants are calculated in Sec. 3, where the present experimental information from neutrino oscillations, neutrinoless double beta decays and cosmology are included. Finally, we summarize our main results in Sec.…”
Section: Introductionmentioning
confidence: 99%
“…In order to demonstrate the validity and robustness of this method, we shall illustrate a particular case and consider the sum of the neutrino mass Σm ν (see Refs. [8][9][10] for its key signatures on cosmology). Focusing exclusively on bounds from Cosmic Microwave Background (CMB) measurements, the final analyses from the Planck satellite set a 95% CL limit of Σm ν < 0.24 eV [11] after considering CMB temperature, polarization and lensing at all scales.…”
mentioning
confidence: 99%