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The Cosmic Neutrino Background
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The cosmic neutrino background is like the cosmic microwave background, but less photon-y and more neutrino-ey. The CNB is also less talked about than the CMB, mostly because it's nearly impossible to detect directly. But if it could be detected, it would be interesting in several ways that are discussed.
Forward citations
Cited by 3 Pith papers
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Sensitivity of Next-Generation CMB Surveys to Neutrinos and Other Light Relics
CMB-S4 forecasts: the two-site design reaches sigma(Neff)=0.029 in seven years, the Chile-only revised design reaches 0.030 in nine, and a cosmic-variance-limited survey would reach 0.0073.
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Lorentz Transformation of the Energy Spectrum of the Equilibrium State of Massive Free Fields
Massive free-field spectra in moving frames cannot be represented by a scalar temperature with dipole anisotropy, forcing the use of a four-vector temperature.
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Neutrino masses from large-scale structures: future sensitivity and theory dependence
Forecasted 1-sigma sensitivity to the sum of neutrino masses is 15 meV for Planck+DESI and 7 meV for CMB-S4+MegaMapper, with the one-loop bispectrum providing 10% and 30% of the constraining power.
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