Neutrino Mass from Cosmology

By Julien Lesgourgues, S. Pastor. 2012

254 citations recorded by the source corpus.

Neutrinos can play an important role in the evolution of the Universe, modifying some of the cosmological observables. In this contribution we summarize the main aspects of cosmological relic neutrinos and we describe how the precision of present cosmological data can be used to learn about neutrino properties, in particular their mass, providing complementary information to beta decay and neutrinoless double-beta decay experiments. We show how the analysis of current cosmological observations, such as the anisotropies of the cosmic microwave background or the distribution of large-scale structure, provides an upper bound on the sum of neutrino masses of order 1 eV or less, with very good perspectives from future cosmological measurements which are expected to be sensitive to neutrino masses well into the sub-eV range.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/063103f0a6c93ef8578342f6dd5b88d4447718dc

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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.”
Constraint on neutrino masses from SDSS-III/BOSS Lyα forest and other cosmological probes (2014, background): “The transition from the relativistic to non-relativistic regime of the heaviest neutrinos may have left a small signature in the CMB temperature anisotropy spectrum, on intermediate scales, through the early integrated Sachs-Wolfe effect [8–10].”
On Effective Degrees of Freedom in the Early Universe (2016, background): “The collision rate between neutrinos and electrons (and its antiparticle), Γν, is given by [6,17]:”
Core Cosmology Library: Precision Cosmological Predictions for LSST (2018, methodology): “The relevant known quantity which has been determined via particle physics experiments is the square of the difference of neutrino masses (up to a sign for one of the differences, hence the two possible hierarchies, see Lesgourgues & Pastor 2012b; Lattanzi & Gerbino 2017).”
The Phenomenology of Right Handed Neutrinos (2013, background): “59See [438] and references therein for a detailed account of this issue.”
The effects of QCD equation of state on the relic density of WIMP dark matter (2015, methodology): “For 50 keV < T < 1 MeV we use numerical results from figure 1 of [51] to determine the evolution of Tν with respect to Tγ .”
Current Direct Neutrino Mass Experiments (2013, background): “The temperature of the cosmicmicrowave background photons together with the different decoupling times of the relic photons and the relic neutrinos after the big bang yields a relic neutrino density of 336/cm(3) [6].”
Constraints on neutrino masses from Lyman-alpha forest power spectrum with BOSS and XQ-100 (2017, background): “sive neutrinos is a – 1 – step-like suppression of power by a factor of order 1 8( = m), where the present neutrino energy density relative to the critical density is given by = P m =(93:14h2 eV2) [10,11]. Cosmic Microwave Background (CMB) data can also constrain P m . In the standard thermal histor”
DESI and other Dark Energy experiments in the era of neutrino mass measurements (2013, background): “interested in neutrino mass (see [133] for a review).”