Public repository of the Cosmic Linear Anisotropy Solving System (master for the most recent version of the standard code; GW_CLASS to include Cosmic Gravitational Wave Background anisotropies; classnet branch for acceleration with neutral networks; ExoCLASS branch for exotic energy injection; class_matter branch for FFTlog)
The CMB temperature and polarisation fields gets affected via gravitational lensing, which leads to a damping of the acoustic peaks in their respective angular power spectrum. This can be seen by comparing the "raw" versus "lensed" TT, EE, and TE spectra outputted by CLASS.
I am however puzzled by the fact that I don't see any difference in the raw vs lensed T-phi cross-correlation spectra computed by CLASS: shouldn't there be some additional correlation when the lensed temperature field is cross-correlated with the lensing potential -- responsible for said lensing of the CMB?
Hi all,
The CMB temperature and polarisation fields gets affected via gravitational lensing, which leads to a damping of the acoustic peaks in their respective angular power spectrum. This can be seen by comparing the "raw" versus "lensed" TT, EE, and TE spectra outputted by CLASS.
I am however puzzled by the fact that I don't see any difference in the raw vs lensed T-phi cross-correlation spectra computed by CLASS: shouldn't there be some additional correlation when the lensed temperature field is cross-correlated with the lensing potential -- responsible for said lensing of the CMB?
Thanks in advance!