CMB lensing reconstruction with point source masks

C. Sofia Carvalho; Ismael Tereno

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CMB lensing reconstruction with point source masks

C. Sofia Carvalho, Ismael Tereno

Cosmology and Nongalactic Astrophysics · Submitted 11 Mar 2011

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim We recover the lensing signal without significant loss of power or addition of spurious correlations, thus showing that masking defected pixels does not affect the reconstruction of the weak lensing convergence in real space.

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What the abstract itself states, as probabilities: claims first 0.02 · states limitation 0.31 · human participants 0.01 · controlled comparison 0.20 · randomized assignment 0.02 · states quantitative result 0.07 · compares with prior results 0.15 · mentions code or data availability 0.02.

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An incomplete sky coverage poses difficulties in the extraction of the weak lensing information from the CMB. We test the reconstruction of the weak lensing convergence from CMB maps to which masks of point sources have been applied. We use the quadratic estimator with a kernel with finite support acting in real space for a Planck simulation. We recover the lensing signal without significant loss of power or addition of spurious correlations, thus showing that masking defected pixels does not affect the reconstruction of the weak lensing convergence in real space.

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#	sentence	role	the authors' own work	states the main conclusion	strength
s0	An incomplete sky coverage poses difficulties in the extraction of the weak lensing information from the CMB.	background 1.00	0.05	0.02	asserted 0.99
s1	We test the reconstruction of the weak lensing convergence from CMB maps to which masks of point sources have been applied.	contribution 0.95	0.92	0.04	asserted 0.64
s2	We use the quadratic estimator with a kernel with finite support acting in real space for a Planck simulation.	method 1.00	0.90	0.02	asserted 0.93
s3	We recover the lensing signal without significant loss of power or addition of spurious correlations, thus showing that masking defected pixels does not affect the reconstruction of the weak lensing convergence in real space.	result 0.90	0.94	0.93	asserted 1.00

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Original abstract

An incomplete sky coverage poses difficulties in the extraction of the weak lensing information from the CMB. We test the reconstruction of the weak lensing convergence from CMB maps to which masks of point sources have been applied. We use the quadratic estimator with a kernel with finite support acting in real space for a Planck simulation. We recover the lensing signal without significant loss of power or addition of spurious correlations, thus showing that masking defected pixels does not affect the reconstruction of the weak lensing convergence in real space.

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3 arXiv papers cite this in 7 sentences

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Uses its method or tool 1 paper

Here we base our measurement on an estimator with demonstrated insensitivity to uncorrelated noise [ref] and good handling of excision of points [ref] , which makes it a reliable tool for the extraction of the lensing signal from the WMAP data.

CMB lensing reconstruction from the WMAP 7-year data · Introduction · 0.90

Compares with it 1 paper

This is in contrast with the results in Refs. [ref] , where the same method applied to simulations of the Planck experiment was able to retrieve the input signal.

CMB lensing reconstruction from the WMAP 7-year data · The convergence power spectrum · 0.98

What it cites · 21 sentences without a confident label

Uses the method or tool of 3 papers

Here we will use the real-space estimator introduced in Ref. [ref] , which is a real-space analog of the optimal estimator based on the convolution of the square of the lensed temperature map with a local kernel as follows κ̂_0(θ) =∫d^2θ^' T̃(θ^') ∫d^2θ^'' T̃(θ^'') Q(θ,θ^',θ^'').

Real space estimator for the weak lensing convergence from the CMB · Estimator of the weak lensing convergence · 1.00
In summary, we first compute the TT and the $ψψ$ power spectra generated by CAMB [ref] , on scales $ℓ≤4000$, for a fiducial flat $Λ$CDM cosmology consisting of $h=0.7, Ω_cdmh^2=0.112, Ω_bh^2=0.0226, n_s=0.96, σ_8=0.85, τ_rei=0.09, T_0=2.725 K$.

Efficient Computation of CMB anisotropies in closed FRW models · The point source mask · 0.98
In order to have the same noise amplitude in the maps, we adopt the so-called active incomplete sky-coverage strategy [ref] , which assumes the smaller coverage is compensated by longer observation times, reducing the noise per pixel as $=^fid(/^fid)^1/2.$ Alternatively, this can be seen as scaling the pixel size such as to cover the fiducial fraction of the sky.

Ideal scales for weighing the Universe · The estimated map · 0.96

Uses data or values from 2 papers

The value of $$ used for the cases of $Planck$ and $Designer$ is obtained from the total number of point sources detected on the full sky at the 143 GHz channel, as reported in the early results [ref] .

Planck Early Results. VII. The Early Release Compact Source Catalog · The point source mask · 1.00
For example, the analysis of the Atacama Cosmology Project (ACT) 2008 Survey used masks with $θ_s=5$ [ref] , for the $=0.35 ^-2$ point sources detected with a beam $≈2 arcmin$ [ref] .

The Atacama Cosmology Telescope: Extragalactic Sources at 148 GHz in the 2008 Survey · The point source mask · 0.86

Cites as background 7 papers

(See also Ref. [ref] for a study of its properties.) We also compare the results with those obtained from the conventional quadratic estimator defined in harmonic space.

CMB Lensing Reconstruction in Real Space · Introduction · 0.85
It was indirectly detected using WMAP data [ref] and recently direct detections in WMAP [ref] and ACT [ref] were reported.

Detection of Gravitational Lensing in the Cosmic Microwave Background · Introduction · 0.96
It was indirectly detected using WMAP data [ref] and recently direct detections in WMAP [ref] and ACT [ref] were reported.

Correlation of CMB with large-scale structure: II. Weak lensing · Introduction · 0.96

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