Weak gravitational lensing of the CMB

By A. Lewis, A. Challinor. 2006

904 citations recorded by the source corpus.

Weak gravitational lensing has several important effects on the cosmic microwave background (CMB): it changes the CMB power spectra, induces non-Gaussianities, and generates a B-mode polarization signal that is an important source of confusion for the signal from primordial gravitational waves. The lensing signal can also be used to help constrain cosmological parameters and lensing mass distributions. We review the origin and calculation of these effects. Topics include: lensing in General Relativity, the lensing potential, lensed temperature and polarization power spectra, implications for constraining inflation, non-Gaussian structure, reconstruction of the lensing potential, delensing, sky curvature corrections, simulations, cosmological parameter estimation, cluster mass reconstruction, and moving lenses/dipole lensing.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/3cbe6c38b9f8659c699269861216dbdb1f264914

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In Astronomy and Astrophysics

Citations in the corpus

Planck2018 results (2018, methodology): “…theoretical predictions for the mixed adiabatic and isocurvature models by first calculating the total unlensed CMB spectra as a sum of adiabatic, isocurvature, and correlation C`’s, and performing a similar summation for the lensing potential power spectrum (Seljak 1996; Lewis & Challinor 2006).”
Delensing CMB polarization with external datasets (2010, background): “Gravitational lensing by large-scale structure preserves surface brightness, and therefore remaps the temperature anisotropy and polarization of the CMB (for recent reviews see [27, 28]).”
The Atacama Cosmology Telescope: DR6 Gravitational Lensing Map and Cosmological Parameters (2023, methodology): “Thus, for the CMB lensing mass maps produced here, we have (Lewis & Challinor 2006) WκCMB(z) = 3 2 ΩmH 2 0 (1 + z) H(z) χ(z) c [ χ(z?)”
Status of Neutrino Properties and Future Prospects—Cosmological and Astrophysical Constraints (2017, background): “Note that non-linear corrections (see next section for further details) to the lensing potential are important in this case to get accurate large-scale BB spectrum coefficients [54].”
REVISING THE HALOFIT MODEL FOR THE NONLINEAR MATTER POWER SPECTRUM (2012, background): “Gravitational lensing by foreground matter distributions is known to affect the light path of CMB photons coming from the last scattering surface (e.g., Lewis & Challinor 2006).”
Gravitational lensing (2010, background): “This subject has been comprehensively reviewed by [273].”
COrE (Cosmic Origins Explorer) A White Paper (2011, background): “7 arcmin and degree-scale correlations, is a sensitive probe of the growth of structure over a range of redshifts peaking around z ≈ 2 (see [39] for an extensive review).”
FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2008, neutral): “As for the estimation of the cosmological parameters from these spectra, we now include the weak gravitational lensing effect of CMB due to the intervening matter fluctuations (see Lewis & Challinor 2006, for a review), which was not included in the 3- year analysis.”
Improved constraints on dark energy from Chandra X-ray observations of the largest relaxed galaxy clusters (2007, background): “…the small contribution to the TT data expected to arise from the Sunyaev-Z’eldovich (SZ) effect in clusters and groups (e.g. Komatsu & Seljak 2002) and do not account for gravitational lensing of the CMB (Lewis & Challinor 2006), which has a negligible effect on the derived cosmological parameters.”
A MEASUREMENT OF THE DAMPING TAIL OF THE COSMIC MICROWAVE BACKGROUND POWER SPECTRUM WITH THE SOUTH POLE TELESCOPE (2011, methodology): “The effect of lensing on the CMB temperature power spectrum is largely captured by considering large-scale structure in the linear regime (Lewis & Challinor 2006).”
Using the Full Power of the Cosmic Microwave Background to Probe Axion Dark Matter (2017, background): “In the range of ` covered by Planck, non-linear corrections can be safely neglected (e.g. Lewis & Challinor 2006).”
SIMULATIONS OF THE MICROWAVE SKY (2009, background): “Lensing of the Primary CMB Gravitational lensing is a secondary anisotropy of the microwave background caused by the deflection of primary microwave background photons by intervening large-scalestructure potentials (see Lewis & Challinor 2006, for a recent review).”