The Benefits of CMB Delensing

Hotinli, Selim C.; Meyers, Joel; Trendafilova, Cynthia; Green, Daniel; van Engelen, Alexander

doi:10.48550/arxiv.2111.15036

Cited by 2 publications

(2 citation statements)

References 132 publications

(170 reference statements)

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“…Note however that the contribution from halo lensing could in principle be mitigated by CMB delensing, the procedure of reversing the effects on lensing on the CMB, which has a variety of benefits for cosmological inference [see e.g. 57,58]. The coherence of unlensed CMB gradient at small scales makes the measurement of small-scale CMB lensing due to halos feasible [see e.g.…”

Section: Jcap06(2024)076 6 Discussion and Conclusionmentioning

confidence: 99%

On the detectability of the moving lens signal in CMB experiments

Hotinli,

Pierpaoli

2024

J. Cosmol. Astropart. Phys.

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Upcoming cosmic microwave background (CMB) experiments are expected to detect new signals probing interaction of CMB photons with intervening large-scale structure. Among these the moving-lens effect, the CMB temperature anisotropy induced by cosmological structures moving transverse to our line of sight, is anticipated to be measured to high significance in the near future. In this paper, we investigate two possible strategies for the detection of this signal: pairwise transverse-velocity estimation and oriented stacking. We expand on previous studies by including in the analysis realistic simulations of competing signals and foregrounds. We confirm that the moving lens effect can be detected at ≥ 10σ level by a combination of CMB-S4 and LSST surveys. We show that the limiting factors in the detection depend on the strategy: for the stacking analysis, correlated extragalactic foregrounds, namely the cosmic infrared background and thermal Sunyaev Zel'dovich effect, play the most important role. The addition of foregrounds make the signal-to-noise ratio be most influenced by large and nearby objects. As for the pairwise detection, halo lensing and pair number counts are the main issues. In light of our findings, we elaborate on possible strategies to improve the analysis approach for the moving lens detection with upcoming experiments. We also deliver to the community all the simulations and tools we developed for this study.

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Section: Jcap06(2024)076 6 Discussion and Conclusionmentioning

confidence: 99%

On the detectability of the moving lens signal in CMB experiments

Hotinli,

Pierpaoli

2024

J. Cosmol. Astropart. Phys.

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“…For both, we include the delensed TT, TE, and EE power spectra, including lensing reconstruction. The lensing reconstruction noise is determined from iterative delensing of both the temperature and polarization maps (Hotinli et al 2021). We restrict CMB-S3 and CMB-S4 to ℓ > 30, and include Planck TT data for ℓ < 30.…”

Section: Constraints On ∑M νmentioning

confidence: 99%

Constraints on the Optical Depth to Reionization from Balloon-borne Cosmic Microwave Background Measurements

Errard

Remazeilles

Aumont

et al. 2022

ApJ

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We assess the uncertainty with which a balloon-borne experiment, nominally called Tau Surveyor (τS), can measure the optical depth to reionization σ(τ) with given realistic constraints of instrument noise and foreground emissions. Using a τS fiducial design with six frequency bands between 150 and 380 GHz, with white and uniform map noise of 7 μK arcmin, achievable with a single midlatitude flight, and including Planck's 30 and 44 GHz data, we assess the error σ(τ) obtained with three foreground models and as a function of sky fraction f sky between 40% and 54%. We carry out the analysis using both parametric and blind foreground separation techniques. We compare the σ(τ) values to those obtained with low-frequency and high-frequency versions of the experiment called τS-lf and τS-hf, which have only four and up to eight frequency bands with narrower and wider frequency coverage, respectively. We find that with τS, the lowest constraint is σ(τ) = 0.0034, obtained for one of the foreground models with f sky = 54%. σ(τ) is larger, in some cases by more than a factor of 2, for smaller sky fractions, with τS-lf, or as a function of foreground model. The τS-hf configuration does not lead to significantly tighter constraints. The exclusion of the 30 and 44 GHz data, which give information about synchrotron emission, leads to significant τ misestimates. Decreasing noise by an ambitious factor of 10, while keeping f sky = 40%, gives σ(τ) = 0.0031. The combination of σ(τ) = 0.0034, baryon acoustic oscillation data from DESI, and future cosmic microwave background B-mode lensing data from the CMB-S3/CMB-S4 experiments could give σ(∑m ν ) = 17 meV.

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The Benefits of CMB Delensing

Cited by 2 publications

References 132 publications

On the detectability of the moving lens signal in CMB experiments

On the detectability of the moving lens signal in CMB experiments

Constraints on the Optical Depth to Reionization from Balloon-borne Cosmic Microwave Background Measurements

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