CMB lensing beyond the power spectrum: Cosmological constraints from the one-point probability distribution function and peak counts

Liu, Jia; Hill, J. Colin; Sherwin, Blake D.; Petri, Andrea; Böhm, Vanessa; Haiman, Zoltán

doi:10.1103/physrevd.94.103501

Cited by 51 publications

(47 citation statements)

References 127 publications

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“…The lensing bispectrum is generated by the non-linear growth of the large-scale structure and the post-Born corrections. Since measurements of the lensing bispectrum will be useful to extract additional cosmological information in future CMB experiments [42][43][44][45], we will investigate the feasibility of the RD method for a lensing bispectrum measurement in our future work.…”

Section: Summary and Discussionmentioning

confidence: 99%

CMB internal delensing with general optimal estimator for higher-order correlations

Namikawa

2017

Phys. Rev. D

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We present a new method for delensing B modes of the cosmic microwave background (CMB) using a lensing potential reconstructed from the same realization of the CMB polarization (CMB internal delensing). The B-mode delensing is required to improve sensitivity to primary B modes generated by, e.g., the inflationary gravitational waves, axion-like particles, modified gravity, primordial magnetic fields, and topological defects such as cosmic strings. However, the CMB internal delensing suffers from substantial biases due to correlations between observed CMB maps to be delensed and that used for reconstructing a lensing potential. Since the bias depends on realizations, we construct a realization-dependent (RD) estimator for correcting these biases by deriving a general optimal estimator for higher-order correlations. The RD method is less sensitive to simulation uncertainties. Compared to the previous -splitting method, we find that the RD method corrects the biases without substantial degradation of the delensing efficiency.

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Section: Summary and Discussionmentioning

confidence: 99%

CMB internal delensing with general optimal estimator for higher-order correlations

Namikawa

2017

Phys. Rev. D

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“…Lensing signals have also been detected using CMB data alone from multiple CMB experiments (POLARBEAR Collaboration 2014; SPTpol Collaboration 2014; BICEP2/Keck Array Collaborations 2016; Planck Collaboration 2016b; ACTPol Collaboration 2017). In ongoing and near-future CMB experiments such as those reported by the Simons Observatory 8 , SPT-3G 9 , and CMB-S4 10 , the nonlinear growth of the large-scale structure and post-Born corrections become important in the lensing analysis Pratten & Lewis 2016) and are detectable by measuring the bispectrum (Namikawa 2016) and higher-order cumulants (Liu et al 2016). As these experiments will observe a wide area of CMB sky, a full-sky simulation including the effect of the nonlinear evolution will be required.…”

Section: Introductionmentioning

confidence: 99%

Full-sky Gravitational Lensing Simulation for Large-area Galaxy Surveys and Cosmic Microwave Background Experiments

Takahashi

Hamana

Shirasaki

et al. 2017

ApJ

181

248

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We present 108 full-sky gravitational lensing simulation data sets generated by performing multiplelens plane ray-tracing through high-resolution cosmological N -body simulations. The data sets include full-sky convergence and shear maps from redshifts z = 0.05 to 5.3 at intervals of 150 h −1 Mpc comoving radial distance (corresponding to a redshift interval of ∆z ≃ 0.05 at the nearby universe), enabling the construction of a mock shear catalog for an arbitrary source distribution up to z = 5.3. The dark matter halos are identified from the same N -body simulations with enough mass resolution to resolve the host halos of the Sloan Digital Sky Survey (SDSS) CMASS and luminous red galaxies (LRGs). Angular positions and redshifts of the halos are provided by a ray-tracing calculation, enabling the creation of a mock halo catalog to be used for galaxy-galaxy and cluster-galaxy lensing. The simulation also yields maps of gravitational lensing deflections for a source redshift at the last scattering surface, and we provide 108 realizations of lensed cosmic microwave background (CMB) maps in which the post-Born corrections caused by multiple light scattering are included. We present basic statistics of the simulation data, including the angular power spectra of cosmic shear, CMB temperature and polarization anisotropies, galaxy-galaxy lensing signals for halos, and their covariances. The angular power spectra of the cosmic shear and CMB anisotropies agree with theoretical predictions within 5% up to ℓ = 3000 (or at an angular scale θ > 0.5 arcmin). The simulation data sets are generated primarily for the ongoing Subaru Hyper Suprime-Cam survey, but are freely available for download at

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“…For example, for the fiducial CMB-S3 configuration assumed here, the temperature estimator contributes about 75% of the total S/N on the CMB lensing auto-power spectrum measurement [72]. The existence of the kSZ bias could thus motivate Stage-4 lensing survey designs that are optimized for depth (i.e., lower noise level) rather than large sky area, so that the polarization estimators dominate the lensing reconstruction S/N .…”

Section: A Polarization Reconstructionmentioning

confidence: 99%

Bias to CMB lensing reconstruction from temperature anisotropies due to large-scale galaxy motions

Ferraro

Hill

2018

Phys. Rev. D

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Gravitational lensing of the cosmic microwave background (CMB) is expected to be amongst the most powerful cosmological tools for ongoing and upcoming CMB experiments. In this work, we investigate a bias to CMB lensing reconstruction from temperature anisotropies due to the kinematic Sunyaev-Zel'dovich (kSZ) effect, that is, the Doppler shift of CMB photons induced by Compton-scattering off moving electrons. The kSZ signal yields biases due to both its own intrinsic non-Gaussianity and its non-zero cross-correlation with the CMB lensing field (and other fields that trace the large-scale structure). This kSZ-induced bias affects both the CMB lensing auto-power spectrum and its cross-correlation with low-redshift tracers. Furthermore, it cannot be removed by multifrequency foreground separation techniques because the kSZ effect preserves the blackbody spectrum of the CMB. While statistically negligible for current datasets, we show that it will be important for upcoming surveys, and failure to account for it can lead to large biases in constraints on neutrino masses or the properties of dark energy. For a Stage 4 CMB experiment, the bias can be as large as ≈ 15% or 12% in cross-correlation with LSST galaxy lensing convergence or galaxy overdensity maps, respectively, when the maximum temperature multipole used in the reconstruction is max = 4000, and about half of that when max = 3000. Similarly, we find that the CMB lensing auto-power spectrum can be biased by up to several percent. These biases are many times larger than the expected statistical errors. We validate our analytical predictions with cosmological simulations and present the first complete estimate of secondary-induced CMB lensing biases. The predicted bias is sensitive to the small-scale gas distribution, which is affected by pressure and feedback mechanisms, thus making removal via "bias-hardened" estimators challenging. Reducing max can significantly mitigate the bias at the cost of a decrease in the overall lensing reconstruction signal-tonoise. A bias 1% on large scales requires max 2000, which leads to a reduction in signal-to-noise by a factor of ≈ 3 − 5 for a Stage 4 CMB experiment. Polarization-only reconstruction may be the most robust mitigation strategy.

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CMB lensing beyond the power spectrum: Cosmological constraints from the one-point probability distribution function and peak counts

Cited by 51 publications

References 127 publications

CMB internal delensing with general optimal estimator for higher-order correlations

CMB internal delensing with general optimal estimator for higher-order correlations

Full-sky Gravitational Lensing Simulation for Large-area Galaxy Surveys and Cosmic Microwave Background Experiments

Bias to CMB lensing reconstruction from temperature anisotropies due to large-scale galaxy motions

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