Abstract
We analyze the possibility of delensing cosmic microwave background (CMB) polarization maps using foreground weak lensing (WL) information. We build an estimator of the CMB lensing potential out of optimally combined projected-potential estimators to different source redshift bins. Our estimator is most sensitive to the redshift depth of the WL survey, less so to the shape noise level. Estimators built using galaxy surveys like the Large Synoptic Survey Telescope and the Supernova Acceleration Probe recover up to 80%–90% of the potential fluctuations power at but only of the small-angular-scale power (). This translates into a 30%–50% reduction in the lensing -mode power. We illustrate the potential advantages of a 21 cm survey by considering a fiducial WL survey for which we take the redshift depth and the effective angular concentration of sources as free parameters. For a noise level of in the polarization map itself, as projected for a CMBPol experiment, and a beam with , we find that going to at yields a delensing performance similar to that of a quadratic lensing potential estimator applied to small-scale CMB maps: the lensing -mode contamination is reduced by almost an order of magnitude. In this case, there is also a reduction by a factor of in the detectability threshold of the tensor -mode power. At this CMB noise level, the -mode detection threshold is only lower even for perfect delensing, so there is little gain from sources with . The delensing gains are lost if the CMB beam exceeds . The delensing gains and useful depend acutely on the CMB map noise level, but beam sizes below 10 arcmin do not help. Delensing via foreground sources does not require arc-minute-resolution CMB observations, a substantial practical advantage over the use of CMB observables for delensing.
- Received 2 July 2007
DOI:https://doi.org/10.1103/PhysRevD.76.123009
©2007 American Physical Society