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This code was originally developed to modify the standard CMB (cosmic microwave background) lensing quadratic estimator (QE) used to reconstruct the lensing of the CMB by galaxy clusters --inpainted gradient QE--. Reference: arXiv: 1904.13392.
QE recontructs the underlying lensing potential using the correlation between large- and small-scale CMB at a given location on the sky. This is achieved using two maps (or a single map) filtered optimally to extract the large- and small-sclae informations. In an ideal world, in the absence of foregrounds and other non-primordial Gaussianites, lensing is the only process that introduces such a correlation between large- and small-scales. However, in the real world foregrounds, especially cluster Sunyaev Zeldovich (SZ), both thermal (tSZ) and kinematic (kSZ), also induce a similar correlation which contaminates the lensing reconstruction.
Inpainting the CMB at the cluster location in the map filtered to extract the large-scale CMB gradient removes the SZ contamination in that map and hence eliminates SZ-induced lensing bias. More details can be found in arXiv: 1904.13392.
