BICEP Array: a multi-frequency degree-scale CMB polarimeter

Hui, H.; Ade, Peter A. R.; Ahmed, Zeeshan; Aikin, R. W.; Alexander, K. D.; Barkats, D.; Benton, S. J.; Bischoff, C. A.; Bock, J. J.; Bowens-Rubin, R.; Brevik, J. A.; Buder, I.; Bullock, E.; Buza, V.; Connors, J.; Cornelison, J.; Crill, B. P.; Crumrine, M.; Dierickx, M.; Duband, L.; Dvorkin, Cora; Filippini, J. P.; Fliescher, S.; Grayson, J.; Hall, G.; Halpern, M.; Harrison, S.; Hildebrandt, S. R.; Hilton, G. C.; Irwin, K. D.; Kang, J.; Karkare, K. S.; Karpel, E.; Kaufman, Jon; Keating, Brian; Kefeli, S.; Kernasovskiy, S. A.; Kovac, J. M.; Kuo, Chao-Lin; Lau, K.; Larsen, N. A.; Leitch, E. M.; Lueker, M.; Megerian, K. G.; Moncelsi, L.; Namikawa, Toshiya; Netterfield, C. B.; Nguyen, Hien; O’Brient, R.; Ogburn, R. W.; Palladino, S.; Pryke, C.; Racine, B.; Richter, Sonja; Schwarz, R.; Schillaci, A.; Sheehy, C. D.; Soliman, A.; Germaine, T. St.; Staniszewski, Z.; Steinbach, B.; Sudiwala, R.; Teply, G. P.; Thompson, K. L.; Tolan, J. E.; Tucker, C.; Turner, Anthony; Umiltà, Caterina; Vieregg, A. G.; Wandui, A.; Weber, A. C.; Wiebe, Donald; Willmert, J.; Wong, C. L.; Wu, W. L. K.; Yang, Eui-Hyeok; Yoon, K. W.; Zhang, C.

doi:10.1117/12.2311725

Cited by 84 publications

(73 citation statements)

References 11 publications

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“…While we have based our reach estimates here on Planck results, searches for the AC effect are of course possible with time-series data from any of the existing or proposed ground-based, polarization-sensitive CMB experiments [158] (e.g., BICEP and the Keck Array [159][160][161], ACTpol [162], SPTpol [163], POLARBEAR-2 [164], Simons Observatory [165], etc.). A dedicated experiment built to search for oscillating CMB polarization could also potentially have a significantly greater sensitivity to the AC effect than we plot in Fig.…”

Section: B Ac Oscillation Of Polarizationmentioning

confidence: 99%

Axion dark matter detection with CMB polarization

2019

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We point out two ways to search for low-mass axion dark matter using cosmic microwave background (CMB) polarization measurements. These appear, in particular, to be some of the most promising ways to directly detect fuzzy dark matter. Axion dark matter causes rotation of the polarization of light passing through it. This gives rise to two novel phenomena in the CMB. First, the late-time oscillations of the axion field today cause the CMB polarization to oscillate in phase across the entire sky. Second, the early-time oscillations of the axion field wash out the polarization produced at last scattering, reducing the polarized fraction (TE and EE power spectra) compared to the standard prediction. Since the axion field is oscillating, the common (static) 'cosmic birefringence' search is not appropriate for axion dark matter. These two phenomena can be used to search for axion dark matter at the lighter end of the mass range, with a reach several orders of magnitude beyond current constraints. We set a limit from the washout effect using existing Planck results, and find significant future discovery potential for CMB detectors searching in particular for the oscillating effect.

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Section: B Ac Oscillation Of Polarizationmentioning

confidence: 99%

Axion dark matter detection with CMB polarization

2019

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“…At present the error bars for the B-mode detection are too large to come to any conclusion in this respect, σðrÞ ∼ 0.02 [2]. But during the next 5-10 years it will become σðrÞ ∼ 0.005, or even σðrÞ ∼ 0.003, depending on the level of delensing that can be achieved in the future [1,2]. Therefore, the future missions will be needed to clarify any results of the current B-mode experiments.…”

Section: Introductionmentioning

confidence: 91%

“…Current and future cosmic microwave background radiation (CMB) missions, such as BICEP2/Keck [1,2], CMB-S4 [3][4][5], SO [6], LiteBIRD [7], and PICO [8], may potentially detect the tensor to scalar ratio at a level r ¼ 5 × 10 −4 ð5σÞ and improve constraints on n s by a factor of 3 relative to Planck, to achieve σðn s Þ ¼ 0.0015 [8]. A thorough investigation of all phenomenologically viable inflationary models that can explain the future CMB data is necessary for a correct interpretation of the meaning of a detection/nondetection of the primordial gravitational waves.…”

Section: Introductionmentioning

confidence: 99%

CMB targets after the latest Planck data release

Каллош

Linde

2019

Phys. Rev. D

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We show that a combination of the simplest α attractors and KKLT inflation models related to Dp-brane inflation covers most of the area in the (n s , r) space favored by Planck 2018. For α-attractor models, there are discrete targets 3α ¼ 1; 2; …; 7, predicting seven different values of r ¼ 12α=N 2 in the range 10 −2 ≳ r ≳ 10 −3 . In the small r limit, α-attractors and Dp-brane inflation models describe vertical β stripes in the (n s , r) space, with n s ¼ 1 − β=N, β ¼ 2; 5 3 ; 8 5 ; 3 2 ; 4 3 . A phenomenological description of these models and their generalizations can be achieved in the context of pole inflation. Most of the 1σ area in the (n s , r) space favored by Planck 2018 can be covered models with β ¼ 2 and β ¼ 5=3. Future precision data on n s may help to discriminate between these models even if the precision of the measurement of r is insufficient for the discovery of gravitational waves produced during inflation.

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“…Here we consider only the polarisation fields, as CMB polarisation is the focus of many current and future experiments searching for evidence of inflation (e.g. Hui et al 2018;Ade et al 2019;Abazajian et al 2016;Hazumi et al 2019). However, our formalism naturally extends to include the temperature field, as well as including cross-correlation between fields observed by different detectors.…”

Section: Cmb Pseudoa M Covariancementioning

confidence: 99%

Exact joint likelihood of pseudo-Cℓ estimates from correlated Gaussian cosmological fields

Upham

Whittaker

Brown

2019

Monthly Notices of the Royal Astronomical Society

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We present the exact joint likelihood of pseudo-C power spectrum estimates measured from an arbitrary number of Gaussian cosmological fields. Our method is applicable to both spin-0 fields and spin-2 fields, including a mixture of the two, and is relevant to Cosmic Microwave Background, weak lensing and galaxy clustering analyses. We show that Gaussian cosmological fields are mixed by a mask in such a way that retains their Gaussianity, without making any assumptions about the mask geometry. We then show that each auto-or cross-pseudo-C estimator can be written as a quadratic form, and apply the known joint distribution of quadratic forms to obtain the exact joint likelihood of a set of pseudo-C estimates in the presence of an arbitrary mask. Considering the polarisation of the Cosmic Microwave Background as an example, we show using simulations that our likelihood recovers the full, exact multivariate distribution of E E, BB and E B pseudo-C power spectra. Our method provides a route to robust cosmological constraints from future Cosmic Microwave Background and large-scale structure surveys in an era of ever-increasing statistical precision.

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BICEP Array: a multi-frequency degree-scale CMB polarimeter

Cited by 84 publications

References 11 publications

Axion dark matter detection with CMB polarization

Axion dark matter detection with CMB polarization

CMB targets after the latest Planck data release

Exact joint likelihood of pseudo-Cℓ estimates from correlated Gaussian cosmological fields

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