Measurement of the Cosmic Microwave Background Polarization Lensing Power Spectrum with the POLARBEAR Experiment

Ade, Peter A. R.; Akiba, Y.; Anthony, A. E.; Arnold, K.; Atlas, M.; Barron, Darcy; Boettger, D.; Borrill, J.; Chapman, Scott; Chinone, Yuji; Dobbs, M.; Elleflot, T.; Errard, Josquin; Fabbian, Giulio; Feng, Chang; Flanigan, D.; Gilbert, A.; Grainger, W.; Halverson, N. W.; Hasegawa, M.; Hattori, K.; Hazumi, M.; Holzapfel, W. L.; Hori, Y.; Howard, J.; Hyland, P.; Inoue, Yuki; Jaehnig, Greg; Jaffe, A. H.; Keating, Brian; Kermish, Z.; Keskitalo, R.; Kisner, T. S.; Jeune, M. Le; Lee, A. T.; Linder, Eric V.; Leitch, E. M.; Lungu, Marius; Matsuda, Frederick; Matsumura, Tomotake; Meng, Xiaofan; Miller, Nathan J.; Morii, H.; Moyerman, S.; Myers, Mike; Navaroli, M.; Nishino, Hitoshi; Paar, H. P.; Peloton, J.; Quealy, E.; Rebeiz, Gabriel M.; Reichardt, Christian; Richards, P. L.; Ross, C.; Schanning, I.; Schenck, D. E.; Sherwin, Blake D.; Shimizu, A.; Shimmin, C. O.; Shimon, Meir; Siritanasak, P.; Smecher, G.; Spieler, H.; Stebor, N.; Steinbach, B.; Stompor, R.; Suzuki, Aritoki; Takakura, S.; Tomaru, T.; Wilson, B.; Yadav, Amit; Zahn, O.

doi:10.1103/physrevlett.113.021301

Cited by 161 publications

(111 citation statements)

References 33 publications

Supporting

Mentioning

111

Contrasting

Order By: Relevance

“…For low noise levels the large-scale lensing modes are all reconstructed with high signal to noise, even by the quadratic estimator, so the cosmological information is limited by cosmic variance. The main information gain from the iterative estimator comes on smaller scales where the quadratic estimator 4 http://pla.esac.esa.int. 5 Note that both references show the cross-correlation coefficient ρ L , while we show the efficiency ρ reconstruction noise starts to be substantial.…”

Section: Discussionmentioning

confidence: 99%

“…Ratios calculated using a lens multipole cut at L min ¼ 100 instead of L min ¼ 40 are shown in parentheses. Figure 4 also shows the delensing efficiency reachable using the publicly available 4 GNILC Cosmic Infrared Background (CIB) map [38] as an external tracer of the lensing map (purple points). We used the GNILC reconstruction at 545 GHz, covering 60% of the sky, and Planck 2015 lensing potential map to build these points.…”

Section: Delensing Efficiencymentioning

confidence: 99%

“…Lensing estimators use these higher-order statistics to construct an integrated measure of the linear mass fluctuations in the Universe that cross-correlates to all traditional large-scale structure tracers. After the first direct detection of lensing in the CMB by the ACT team [2], the SPT [3], POLARBEAR [4], SPTpol [5], BICEP2-KECK [6] and Planck [7] collaborations have also reported the detection of the lensing signal and published band-powers. The most decisive detection yet was by the Planck satellite [8]: its full-sky coverage comes with a statistical power that simply cannot be matched at the present time.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Maximum a posteriori CMB lensing reconstruction

2017

View full text Add to dashboard Cite

Gravitational lensing of the cosmic microwave background (CMB) is a valuable cosmological signal that correlates to tracers of large-scale structure and acts as a important source of confusion for primordial B-mode polarization. State-of-the-art lensing reconstruction analyses use quadratic estimators, which are easily applicable to data. However, these estimators are known to be suboptimal, in particular for polarization, and large improvements are expected to be possible for high signal-to-noise polarization experiments. We develop a method and numerical code, LensIt, that is able to find efficiently the most probable lensing map, introducing no significant approximations to the lensed CMB likelihood, and applicable to beamed and masked data with inhomogeneous noise. It works by iteratively reconstructing the primordial unlensed CMB using a deflection estimate and its inverse, and removing residual lensing from these maps with quadratic estimator techniques. Roughly linear computational cost is maintained due to fast convergence of iterative searches, combined with the local nature of lensing. The method achieves the maximal improvement in signal to noise expected from analytical considerations on the unmasked parts of the sky. Delensing with this optimal map leads to forecast tensor-to-scalar ratio parameter errors improved by a factor ≃2 compared to the quadratic estimator in a CMB stage IV configuration.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: Delensing Efficiencymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Maximum a posteriori CMB lensing reconstruction

2017

View full text Add to dashboard Cite

show abstract

“…It is a practical example of real synergy between overlapping surveys, where combining probes leads to improved systematics and not just a marginally higher signal-tonoise ratio. CMB lensing has been measured by the WMAP satellite [39,40], the Atacama Cosmology Telescope (ACT) [41][42][43][44], the South Pole Telescope (SPT) [45][46][47], POLARBEAR [48], the Planck satellite [49,50], and the BICEP 2/Keck Array [51]. In the future, Advanced ACT [52], SPT-3G [53], and a stage 4 ground-based CMB experiment (CMB S4) [54,55], as well as the Simons Observatory [56], will provide high fidelity maps of the CMB lensing convergence over a large fraction of the sky.…”

Section: Introductionmentioning

confidence: 99%

Looking through the same lens: Shear calibration for LSST, Euclid, and WFIRST with stage 4 CMB lensing

et al. 2017

View full text Add to dashboard Cite

The next-generation weak lensing surveys (i.e., LSST, Euclid, and WFIRST) will require exquisite control over systematic effects. In this paper, we address shear calibration and present the most realistic forecast to date for LSST/Euclid/WFIRST and CMB lensing from a stage 4 CMB experiment ("CMB S4"). We use the COSMOLIKE code to simulate a joint analysis of all the two-point functions of galaxy density, galaxy shear, and CMB lensing convergence. We include the full Gaussian and non-Gaussian covariances and explore the resulting joint likelihood with Monte Carlo Markov chains. We constrain shear calibration biases while simultaneously varying cosmological parameters, galaxy biases, and photometric redshift uncertainties. We find that CMB lensing from CMB S4 enables the calibration of the shear biases down to 0.2%-3% in ten tomographic bins for LSST (below the ∼0.5% requirements in most tomographic bins), down to 0.4%-2.4% in ten bins for Euclid, and 0.6%-3.2% in ten bins for WFIRST. For a given lensing survey, the method works best at high redshift where shear calibration is otherwise most challenging. This self-calibration is robust to Gaussian photometric redshift uncertainties and to a reasonable level of intrinsic alignment. It is also robust to changes in the beam and the effectiveness of the component separation of the CMB experiment, and slowly dependent on its depth, making it possible with third-generation CMB experiments such as AdvACT and SPT-3G, as well as the Simons Observatory.

show abstract

“…Recently, initial measurements of the odd parity polarization pattern, B-mode, of the CMB were also reported. [2,3,4,5,6,7,8].…”

Section: Introductionmentioning

confidence: 99%

The Polarbear-2 and the Simons Array Experiments

et al. 2016

Self Cite

View full text Add to dashboard Cite

We present an overview of the design and status of the POLARBEAR-2 and the Simons Array experiments. POLARBEAR-2 is a Cosmic Microwave Background polarimetry experiment which aims to characterize the arc-minute angular scale B-mode signal from weak gravitational lensing and search for the degree angular scale B-mode signal from inflationary gravitational waves. The receiver has a 365 mm diameter focal plane cooled to 270 milli-Kelvin. The focal plane is filled with 7,588 dichroic lenslet-antenna coupled polarization sensitive Transition Edge Sensor (TES) bolometric pixels that are sensitive to 95 GHz and 150 GHz bands simultaneously. The TES bolometers are read-out by SQUIDs with 40 channel frequency domain multiplexing. Refractive optical elements are made with high purity alumina to achieve high optical throughput. The receiver is designed to achieve noise equivalent temperature of 5.8 µK CMB √ s in each frequency band. POLARBEAR-2 will deploy in 2016 in the Atacama desert in Chile. The Simons Array is a project to further increase sensitivity by deploying three POLARBEAR-2 type receivers. The Simons Array will cover 95 GHz, 150 GHz and 220 GHz frequency bands for foreground control. The Simons Array will be able to constrain tensor-to-scalar ratio and sum of neutrino masses to σ (r) = 6 × 10 −3 at r = 0.1 and ∑ m ν (σ = 1) to 40 meV.

show abstract

Measurement of the Cosmic Microwave Background Polarization Lensing Power Spectrum with the POLARBEAR Experiment

Cited by 161 publications

References 33 publications

Maximum a posteriori CMB lensing reconstruction

Maximum a posteriori CMB lensing reconstruction

Looking through the same lens: Shear calibration for LSST, Euclid, and WFIRST with stage 4 CMB lensing

The Polarbear-2 and the Simons Array Experiments

Contact Info

Product

Resources

About