Multitracer CMB delensing maps from Planck and WISE data

Yu, Byeonghee; Hill, J. Colin; Sherwin, Blake D.

doi:10.1103/physrevd.96.123511

Cited by 52 publications

(43 citation statements)

References 86 publications

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“…In addition, we expect to achieve A lens of order 0.5 from external delensing (Sherwin and Schmittfull 2015) using CIB emission and other external matter tracers. Though practical delensing demonstrations have not yet achieved such low A lens directly (Larsen et al 2016;Man-zotti et al 2017;Carron et al 2017), recent work has shown the construction of multi-tracer maps with sufficient correlation with lensing to achieve A lens ≈ 0.5 (Yu et al 2017; Planck Collaboration 2018e).…”

Section: Delensing Efficiencymentioning

confidence: 99%

The Simons Observatory: science goals and forecasts

Ade

Aguirre

Ahmed

et al. 2019

J. Cosmol. Astropart. Phys.

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1,299

1,070

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The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro Toco in Chile, due to begin observations in the early 2020s. We describe the scientific goals of the experiment, motivate the design, and forecast its performance. SO will measure the temperature and polarization anisotropy of the cosmic microwave background in six frequency bands centered at: 27, 39, 93, 145, 225 and 280 GHz. The initial configuration of SO will have three small-aperture 0.5-m telescopes and one large-aperture 6-m telescope, with a total of 60,000 cryogenic bolometers. Our key science goals are to characterize the primordial perturbations, measure the number of relativistic species and the mass of neutrinos, test for deviations from a cosmological constant, improve our understanding of galaxy evolution, and constrain the duration of reionization. The small aperture telescopes will target the largest angular scales observable from Chile, mapping ≈ 10% of the sky to a white noise level of 2 µK-arcmin in combined 93 and 145 GHz bands, to measure the primordial tensor-to-scalar ratio, r, at a target level of σ(r) = 0.003. The large aperture telescope will map ≈ 40% of the sky at arcminute angular resolution to an expected white noise level of 6 µK-arcmin in combined 93 and 145 GHz bands, overlapping with the majority of the Large Synoptic Survey Telescope sky region and partially with the Dark Energy Spectroscopic Instrument. With up to an order of magnitude lower polarization noise than maps from the Planck satellite, the high-resolution sky maps will constrain cosmological parameters derived from the damping tail, gravitational lensing of the microwave background, the primordial bispectrum, and the thermal and kinematic Sunyaev-Zel'dovich effects, and will aid in delensing the large-angle polarization signal to measure the tensorto-scalar ratio. The survey will also provide a legacy catalog of 16,000 galaxy clusters and more than 20,000 extragalactic sources a .

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Section: Delensing Efficiencymentioning

confidence: 99%

The Simons Observatory: science goals and forecasts

Ade

Aguirre

Ahmed

et al. 2019

J. Cosmol. Astropart. Phys.

Self Cite

1,299

1,070

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show abstract

“…This suggests that a joint analysis could potentially give a substantial improvement to the lensing potential determination, and hence also improve the efficiency of delensing based on Planck data (Sherwin & Schmittfull 2015). A combined tracer map, including galaxy number counts from WISE in addition to the CIB and the 2015 Planck lensing map, has recently been presented over 43% of the sky by Yu et al (2017). Here we focus on the Planck-based combination of the CIB and lensing reconstructions on 60% of the sky, with similar maximum delensing efficiency, and use them to delens all four Planck CMB spectra.…”

Section: Joint Cib-cmb Lensing Potential Reconstructionmentioning

confidence: 99%

Planck2018 results

Aghanim¹,

Akrami²,

Ashdown³

et al. 2020

A&A

565

170

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We present measurements of the cosmic microwave background (CMB) lensing potential using the final Planck 2018 temperature and polarization data. Using polarization maps filtered to account for the noise anisotropy, we increase the significance of the detection of lensing in the polarization maps from 5σ to 9σ. Combined with temperature, lensing is detected at 40σ. We present an extensive set of tests of the robustness of the lensing-potential power spectrum, and construct a minimum-variance estimator likelihood over lensing multipoles 8 ≤ L ≤ 400 (extending the range to lower L compared to 2015), which we use to constrain cosmological parameters. We find good consistency between lensing constraints and the results from the Planck CMB power spectra within the ΛCDM model. Combined with baryon density and other weak priors, the lensing analysis alone constrains σ8Ωm0.25 = 0.589 ± 0.020 (1σ errors). Also combining with baryon acoustic oscillation data, we find tight individual parameter constraints, σ8 = 0.811 ± 0.019, H0 = 67.9−1.3+1.2 km s−1 Mpc−1, and Ωm = 0.303−0.018+0.016. Combining with Planck CMB power spectrum data, we measure σ8 to better than 1% precision, finding σ8 = 0.811 ± 0.006. CMB lensing reconstruction data are complementary to galaxy lensing data at lower redshift, having a different degeneracy direction in σ8 − Ωm space; we find consistency with the lensing results from the Dark Energy Survey, and give combined lensing-only parameter constraints that are tighter than joint results using galaxy clustering. Using the Planck cosmic infrared background (CIB) maps as an additional tracer of high-redshift matter, we make a combined Planck-only estimate of the lensing potential over 60% of the sky with considerably more small-scale signal. We additionally demonstrate delensing of the Planck power spectra using the joint and individual lensing potential estimates, detecting a maximum removal of 40% of the lensing-induced power in all spectra. The improvement in the sharpening of the acoustic peaks by including both CIB and the quadratic lensing reconstruction is detected at high significance.

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“…A lens indicates the residual lensing amplitude after delensing the lensing signal. In our analysis, we have taken A lens = 0.5 which is possible to achieve using several delensing algorithms (Simard et al 2015;Sherwin & Schmittfull 2015;Carron et al 2017;Yu et al 2017;Manzotti et al 2017;Millea et al 2017). Aτ denotes the normalization chosen to include or exclude the patchy reionization signal.…”

Section: Contamination To Tensor To Scalar Ratio and Tensor Spectral mentioning

confidence: 99%

Is patchy reionization an obstacle in detecting the primordial gravitational wave signal?

Mukherjee

Paul

Choudhury

2019

Monthly Notices of the Royal Astronomical Society

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The large-scale CMB B-mode polarization is the direct probe to the low frequency primordial gravitational wave signal. However, unambiguous measurement of this signal requires a precise understanding of the possible contamination. One such potential contamination arises from the patchiness in the spatial distribution of free electrons during the epoch of reionization. We estimate the B-mode power spectrum due to patchy reionization using a combination of photon-conserving semi-numerical simulation and analytical calculation, and compare its amplitude with the primordial B-mode signal. For a reionization history which is in agreement with several latest observations, we find that a stronger secondary B-mode polarization signal is produced when the reionization is driven by the sources in massive halos and its amplitude can be comparable to the recombination bump for tensor to scalar ratio (r) 5 × 10 −4 . If contamination from patchy reionization is neglected in the analysis of B-mode polarization data, then for the models of reionization considered in this analysis, we find a maximum bias of about 30% in the value of r = 10 −3 when spatial modes between ∈ [50, 200] are used with a delensing efficiency of 50%. The inferred bias from patchy reionization is not a severe issue for the upcoming ground-based CMB experiment Simons Observatory, but can be a potential source of confusion for proposed CMB experiments which target to detect the value of r < 10 −3 . However, this obstacle can be removed by utilizing the difference in the shape of the power spectrum from the primordial signal. 1 This value changes by about 1-σ with change in the reionization model (Planck Collaboration et al. 2018).

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Multitracer CMB delensing maps from Planck and WISE data

Cited by 52 publications

References 86 publications

The Simons Observatory: science goals and forecasts

The Simons Observatory: science goals and forecasts

Planck2018 results

Is patchy reionization an obstacle in detecting the primordial gravitational wave signal?

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