Neutrino physics from the cosmic microwave background and large scale structure
Section snippets
Executive summary
The cosmological background of neutrinos thermally produced in the big bang has been definitively (albeit indirectly) detected. Measurements of the cosmic microwave background (CMB) alone have led to a constraint on the effective number of neutrino species of Ade et al. [1], a value away from zero and consistent with expectations. Experiments planned and underway are prepared to study this background in detail via its influence on distance-redshift relations and the growth of
Forecast sensitivity to and Σ
In this section, we present forecast sensitivity to cosmic neutrinos from future CMB and LSS experiments. Various complementary probes of neutrino mass are surveyed. However, we highlight a few methods considered to be least sensitive to systematic effects: an arcminute-scale CMB polarization survey from the Stage-IV CMB experiment CMB-S4 (described below and in Appendix A), galaxy clustering, and cosmic shear. The exact forecast of uncertainty depends on the cosmology and priors assumed. Our
Theoretical priors
The goal of constraining and potentially detecting neutrino mass and neutrino number density cosmologically is based within a rigorously constrained and well-tested model. However, that model has some inherent theoretical priors and simplifying assumptions. Almost all of the constraints on neutrino mass discussed here and in the literature are constraints on neutrinos as an extension to the standard cosmological model, minimally described by six parameters, but sometimes extended to up to 10
Conclusions
The experimental quantification of the cosmological neutrino background has achieved the robust detection of the neutrino background energy density through its effects on the CMB and LSS, and the measures of properties of neutrinos in the cosmological background have achieved unprecedented precision and accuracy. These measures compete in precision with laboratory probes of neutrino number and mass, albeit with the theoretical priors discussed in Section 3.1. The current generation of Planck
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