Massive neutrinos and cosmology

By Julien Lesgourgues, S. Pastor. 2005

1,022 citations recorded by the source corpus.

The present experimental results on neutrino flavour oscillations provide evidence for non-zero neutrino masses, but give no hint on their absolute mass scale, which is the target of beta decay and neutrinoless double-beta decay experiments. Crucial complementary information on neutrino masses can be obtained from the analysis of data on cosmological observables, such as the anisotropies of the cosmic microwave background or the distribution of large-scale structure. In this review we describe in detail how free-streaming massive neutrinos affect the evolution of cosmological perturbations. We summarize the current bounds on the sum of neutrino masses that can be derived from various combinations of cosmological data, including the most recent analysis by the WMAP team. We also discuss how future cosmological experiments are expected to be sensitive to neutrino masses well into the sub-eV range.

Subfields: Nuclear and High Energy Physics, Radiation

View Paper: https://www.semanticscholar.org/paper/c653d1bc81d6158c11d9a8bb26952f4fa77767ea

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Citations in the corpus

Updated results on neutrino mass and mass hierarchy from cosmology with Planck 2018 likelihoods (2019, background): “Effects of massive neutrinos on cosmological observables have been extensively studied in the literature [16–22] and these effects help in constraining the sum of neutrino masses.”
Lensing is Low: Cosmology, Galaxy Formation, or New Physics? (2016, background): “Finite-mass neutrinos have large velocity dispersion and suppress the growth of LSS below the neutrino free-streaming scale (e.g. Lesgourgues & Pastor 2006; Saito, Takada & Taruya 2008, 2009) and could therefore impact the amplitude of the g-g lensing signal.”
Cosmological Parameters from Observations of Galaxy Clusters (2011, background): “…structure, since any particle with non-zero mass at some point cools from a relativistic state, in which it effectively suppresses structure formation, to a non-relativistic state, in which it actively participates in the growth of structure (details are reviewed in Lesgourgues & Pastor 2006).”
CMB-S4 Science Case, Reference Design, and Project Plan (2019, background): “The scale separating these two regimes is the neutrino free-streaming scale, defined by [222, 223] kfs(a) ≡ √ 3 2aH(a)/vν(a) ≈ 0.”
Cosmology with massive neutrinos I: towards a realistic modeling of the relation between matter, haloes and galaxies (2013, background): “Although the impact of neutrino masses on cosmology is very well understood at the linear order [5, 24], their impact on the fully non-linear regime has not been extensively studied.”
Cosmology with massive neutrinos II: on the universality of the halo mass function and bias (2013, background): “2) is fixed, then the total matter power spectrum in a massive neutrino model, Pmm(k; fν), is reduced by a constant factor on scales k knr and small values of fν [28, 31] Pmm(k; fν) Pmm(k; fν = 0) ' 1− 8fν .”
SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2010, background): “…2007; Yamamoto et al. 2007; Chiba & Takahashi 2007; Bean et al. 2007; Hu & Sawicki 2007; Song et al. 2007; Starobinsky 2007; Daniel et al. 2008; Jain & Zhang 2008; Bertschinger & Zukin 2008; Amin et al. 2008; Hu 2008) and determine the mass of neutrinos (Hu et al. 1998; Lesgourgues & Pastor 2006).”
Global constraints on absolute neutrino masses and their ordering (2017, background): “[16, 63–67]), letting cosmology to strongly bound the neutrino mass scale, indeed providing the current strongest (albeit model dependent) bounds on Σ.”
Robust forecasts on fundamental physics from the foreground-obscured, gravitationally-lensed CMB polarization (2015, methodology): “As an integrated measure of the geometry and growth of structure in the Universe, the measurement of lensing B modes provides both insight into late-time physics, such as the damping of structure formation by massive neutrinos [4, 5] and the influence of dark energy [6–8], and an opportunity to brea”