Reconstruction of lensing from the cosmic microwave background polarization

By C. Hirata, Uros Seljak. 2003

261 citations recorded by the source corpus.

Gravitational lensing of the cosmic microwave background (CMB) polarization field has been recognized as a potentially valuable probe of the cosmological density field. We apply likelihood-based techniques to the problem of lensing of CMB polarization and show that if the B-mode polarization is mapped, then likelihood-based techniques allow significantly better lensing reconstruction than is possible using the previous quadratic estimator approach. With this method the ultimate limit to lensing reconstruction is not set by the lensed CMB power spectrum. Second-order corrections are known to produce a curl component of the lensing deflection field that cannot be described by a potential; we show that this does not significantly affect the reconstruction at noise levels greater than 0.25 μK arcmin. The reduction of the mean squared error in the lensing reconstruction relative to the quadratic method can be as much as a factor of two at noise levels of 1.4 μK arcmin to a factor of ten at 0.25 μK arcmin, depending on the angular scale of interest.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/debde2c9ba06d15c0eb616b53c69acc56a6743ed

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In Astronomy and Astrophysics

Citations in the corpus

Detection of large-scale intrinsic ellipticity—density correlation from the Sloan Digital Sky Survey and implications for weak lensing surveys (2005, methodology): “…PSF; Mandelbaum et al. (2005a) uses the PSF maps obtained from stellar images by the psp pipeline (Lupton et al. 2001), and corrects for these using the re-Gaussianization technique of Hirata & Seljak (2003a), which includes corrections for non-Gaussianity of both the galaxy profile and the PSF.”
Galaxy Bias and non-Linear Structure Formation in General Relativity (2011, methodology): “One could also use the anisotropies in the small scale power to de-lense the CMB along the lines considered in [37, 38].”
A MEASUREMENT OF GRAVITATIONAL LENSING OF THE MICROWAVE BACKGROUND USING SOUTH POLE TELESCOPE DATA (2012, methodology): “Alternative approaches involve formulating and maximizing a lensing likelihood function in pixel space (Hirata & Seljak 2003a,b; Anderes et al. 2011).”
DeepCMB: Lensing Reconstruction of the Cosmic Microwave Background with Deep Neural Networks (2018, background): “…scattering surface to us, their paths are deflected by the gradient of the gravitational potential φ, an effect called gravitational lensing: X̃±(n̂) = X±(n̂+∇φ(n̂)), (1) where X is the unlensed field and X̃ denotes the lensed field (e.g., Hu, 2000) and X± = Q ± iU . for the polarization fields.”
Phases of new physics in the CMB (2015, methodology): “For CMB-S4, the lensing reconstruction noise was computed using the iterated delensing method described in [54] (based on [55–57]).”
Gravitational lensing (2010, methodology): “This demonstrates one example for the recovery of the lensing effects on the CMB (see also [194, 373]).”
CMB-S4 Science Case, Reference Design, and Project Plan (2019, methodology): “The TT , TE, EE, and φφ spectra were included, with the lensing reconstruction noise calculated using the minimum variance combination of quadratic estimators [543, 544], including the improvement from iterative EB reconstruction [575, 562].”
Delensing CMB polarization with external datasets (2010, methodology): “1 Polarization delensing A B-mode measurement which extends to small angular scales (` ∼ > 200) can be used to estimate the lensing potential, by means of lens reconstruction estimators which cross-correlate E and B-modes [17, 18, 19, 20].”