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Getting Around Cosmic Variance
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Getting Around Cosmic Variance
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Cosmic microwave background (CMB) anisotropies probe the primordial density field at the edge of the observable Universe. There is a limiting precision (``cosmic variance'') with which anisotropies can determine the amplitude of primordial mass fluctuations. This arises because the surface of last scatter (SLS) probes only a finite two-dimensional slice of the Universe. Probing other SLSs observed from different locations in the Universe would reduce the cosmic variance. In particular, the polarization of CMB photons scattered by the electron gas in a cluster of galaxies provides a measurement of the CMB quadrupole moment seen by the cluster. Therefore, CMB polarization measurements toward many clusters would probe the anisotropy on a variety of SLSs within the observable Universe, and hence reduce the cosmic-variance uncertainty.
Forward citations
Cited by 2 Pith papers
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Standard Reconstruction Shifts the Optimal Input Scale for CNN-Based Density-Field Reconstruction
Applying standard reconstruction before a CNN shifts the optimal input cube for z=10 density reconstruction from ~150-200 h^-1 Mpc to ~38-114 h^-1 Mpc, and a single post-reconstruction CNN beats dual-scale CNN inputs.
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