Reconstructing the Universe with secondary CMB anisotropies

The cosmic microwave background radiation has been an indispensable tool for learning about the origins and evolution of our Observable Universe. Satellites and ground based experiments measuring the temperature and polarization anisotropies with ever increasing angular resolution and sensitivity have established the standard cosmological model, LCDM, and constrained or ruled out a huge variety of theoretical models of the early Universe. Most of this cosmological information has thus far been derived from the primary CMB, anisotropies largely sourced during the epoch of recombination some 380,000 years after the Big Bang. However, experiments are achieving the sensitivity and resolution necessary to access a whole new treasure-trove of cosmological information: secondary temperature and polarization anisotropies induced by photons scattering from mass (CMB lensing) and free electrons (the Sunyaev Zel'dovich effect). Unlike the primary CMB, where cosmological information is contained in the pattern of fluctuations in statistically isotropic temperature/polarization anisotropies, the secondary CMB encodes cosmological information in the statistical anisotropies of non-gaussian temperature/polarization fields on the sky. In this talk, I will describe the possibilities for future CMB experiments, in concert with large galaxy surveys, to reconstruct the cosmological information contained in the statistics of the secondary CMB anisotropies. In particular, I will describe the information that can be reconstructed from kinetic/polarized Sunyaev Zel'dovich effect, CMB lensing, and the moving lens effect. I speculate on what we might learn from future measurements, and conclude by discussing several projects in progress.

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Wednesday, February 20, 2019 - 14:00 to 15:30
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