2014/01/30 by A. Manzotti, Alessandro Manzotti, Wayne Hu +2 · 3 citations
Mathematics · Physics and Astronomy · #Anisotropy #Astrophysics #Computational physics #Cosmic microwave background #Cosmology and Gravitation Theories #Galaxies: Formation, Evolution, Phenomena #Galaxy #Mathematics #Non-Gaussianity #Optics #Physics #Polarization (electrochemistry) #Radio Astronomy Observations and Technology #Redshift #Sky #Spectral density #Statistical physics #Statistics #Trispectrum #Weak gravitational lensing #astro-ph.CO
paper · pdf · doi:10.1103/physrevd.90.023003
published as Phys. Rev. D 90, 023003 (2014) · 6 pages, 2 figures
arxiv created 2014/01/30 · openalex publication_date 2014/07/01 · arxiv updated 2014/07/09 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Lensing of the cosmic microwave background by modes that are larger than the size of the survey dilates intrinsic scales in the temperature and polarization fields and coherently shifts their observed power spectra with respect to the ensemble or all-sky mean. The effect can be simply encapsulated as a contribution to the power spectrum covariance matrix in accordance with the lensing trispectrum or as an additional parameter, the mean convergence in the field, for parameter estimation. It should be included for upcoming surveys that precisely measure acoustic polarization features deep into the damping tail at multipoles of \ensuremathℓ\ensuremath\gtrsim1500 with less than 10% of the sky. Its omission may lead to seemingly conflicting values for the angular scale of the sound horizon, which may then provide erroneous cosmological parameters when compared to baryon acoustic oscillation measurements.