Search

Your search keyword '"J. E. Tolan"' showing total 59 results
Start Over "J. E. Tolan" Publication Year Range Last 10 years
59 results on '"J. E. Tolan"'

1. BICEP/Keck. XVII. Line-of-sight Distortion Analysis: Estimates of Gravitational Lensing, Anisotropic Cosmic Birefringence, Patchy Reionization, and Systematic Errors

Author

P. A. R. Ade, Z. Ahmed, M. Amiri, D. Barkats, R. Basu Thakur, C. A. Bischoff, D. Beck, J. J. Bock, H. Boenish, E. Bullock, V. Buza, J. R. Cheshire IV, J. Connors, J. Cornelison, M. Crumrine, A. Cukierman, E. V. Denison, M. Dierickx, L. Duband, M. Eiben, S. Fatigoni, J. P. Filippini, S. Fliescher, C. Giannakopoulos, N. Goeckner-Wald, D. C. Goldfinger, J. Grayson, P. Grimes, G. Hall, G. Halal, M. Halpern, E. Hand, S. Harrison, S. Henderson, S. R. Hildebrandt, J. Hubmayr, H. Hui, K. D. Irwin, J. Kang, K. S. Karkare, E. Karpel, S. Kefeli, S. A. Kernasovskiy, J. M. Kovac, C. L. Kuo, K. Lau, E. M. Leitch, A. Lennox, K. G. Megerian, L. Minutolo, L. Moncelsi, Y. Nakato, T. Namikawa, H. T. Nguyen, R. O’Brient, R. W. Ogburn IV, S. Palladino, M. Petroff, T. Prouve, C. Pryke, B. Racine, C. D. Reintsema, S. Richter, A. Schillaci, R. Schwarz, B. L. Schmitt, C. D. Sheehy, B. Singari, A. Soliman, T. St. Germaine, B. Steinbach, R. V. Sudiwala, G. P. Teply, K. L. Thompson, J. E. Tolan, C. Tucker, A. D. Turner, C. Umiltà, C. Vergès, A. G. Vieregg, A. Wandui, A. C. Weber, D. V. Wiebe, J. Willmert, C. L. Wong, W. L. K. Wu, H. Yang, K. W. Yoon, E. Young, C. Yu, L. Zeng, C. Zhang, S. Zhang, and BICEP/Keck Collaboration

Subjects
Observational cosmology, Cosmic microwave background radiation, Weak gravitational lensing, Primordial magnetic fields, Reionization, Astrophysics, QB460-466
Abstract

We present estimates of line-of-sight distortion fields derived from the 95 and 150 GHz data taken by BICEP2, BICEP3, and the Keck Array up to the 2018 observing season, leading to cosmological constraints and a study of instrumental and astrophysical systematics. Cosmological constraints are derived from three of the distortion fields concerning gravitational lensing from large-scale structure, polarization rotation from magnetic fields or an axion-like field, and the screening effect of patchy reionization. We measure an amplitude of the lensing power spectrum ${A}_{L}^{\phi \phi }=0.95\pm 0.20$ . We constrain polarization rotation, expressed as the coupling constant of a Chern–Simons electromagnetic term g _a _γ ≤ 2.6 × 10 ^−2 / H _I , where H _I is the inflationary Hubble parameter, and an amplitude of primordial magnetic fields smoothed over 1 Mpc B _1Mpc ≤ 6.6 nG at 95 GHz. We constrain the rms of optical depth fluctuations in a simple “crinkly surface” model of patchy reionization, finding A ^τ < 0.19 (2 σ ) for the coherence scale of L _c = 100. We show that all of the distortion fields of the 95 and 150 GHz polarization maps are consistent with simulations including lensed ΛCDM, dust, and noise, with no evidence for instrumental systematics. In some cases, the EB and TB quadratic estimators presented here are more sensitive than our previous map-based null tests at identifying and rejecting spurious B -modes that might arise from instrumental effects. Finally, we verify that the standard deprojection filtering in the BICEP/Keck data processing is effective at removing temperature to polarization leakage.

Published
2023
Full Text
View/download PDF

2. BICEP/Keck. XVI. Characterizing Dust Polarization through Correlations with Neutral Hydrogen

Author

P. A. R. Ade, Z. Ahmed, M. Amiri, D. Barkats, R. Basu Thakur, C. A. Bischoff, D. Beck, J. J. Bock, H. Boenish, E. Bullock, V. Buza, J. R. Cheshire IV, S. E. Clark, J. Connors, J. Cornelison, M. Crumrine, A. Cukierman, E. V. Denison, M. Dierickx, L. Duband, M. Eiben, S. Fatigoni, J. P. Filippini, S. Fliescher, C. Giannakopoulos, N. Goeckner-Wald, D. C. Goldfinger, J. Grayson, P. Grimes, G. Hall, G. Halal, M. Halpern, E. Hand, S. Harrison, S. Henderson, S. R. Hildebrandt, J. Hubmayr, H. Hui, K. D. Irwin, J. Kang, K. S. Karkare, E. Karpel, S. Kefeli, S. A. Kernasovskiy, J. M. Kovac, C. L. Kuo, K. Lau, E. M. Leitch, A. Lennox, K. G. Megerian, L. Minutolo, L. Moncelsi, Y. Nakato, T. Namikawa, H. T. Nguyen, R. O’Brient, R. W. Ogburn IV, S. Palladino, M. A. Petroff, T. Prouve, C. Pryke, B. Racine, C. D. Reintsema, S. Richter, A. Schillaci, R. Schwarz, B. L. Schmitt, C. D. Sheehy, B. Singari, A. Soliman, T. St. Germaine, B. Steinbach, R. V. Sudiwala, G. P. Teply, K. L. Thompson, J. E. Tolan, C. Tucker, A. D. Turner, C. Umiltà, C. Vergès, A. G. Vieregg, A. Wandui, A. C. Weber, D. V. Wiebe, J. Willmert, C. L. Wong, W. L. K. Wu, H. Yang, K. W. Yoon, E. Young, C. Yu, L. Zeng, C. Zhang, S. Zhang, and BICEP/Keck Collaboration

Subjects
Interstellar dust, Interstellar filaments, Neutral hydrogen clouds, Cosmic microwave background radiation, Interstellar magnetic fields, Interstellar medium, Astrophysics, QB460-466
Abstract

We characterize Galactic dust filaments by correlating BICEP/Keck and Planck data with polarization templates based on neutral hydrogen (H i ) observations. Dust polarization is important for both our understanding of astrophysical processes in the interstellar medium (ISM) and the search for primordial gravitational waves in the cosmic microwave background (CMB). In the diffuse ISM, H i is strongly correlated with the dust and partly organized into filaments that are aligned with the local magnetic field. We analyze the deep BICEP/Keck data at 95, 150, and 220 GHz, over the low-column-density region of sky where BICEP/Keck has set the best limits on primordial gravitational waves. We separate the H i emission into distinct velocity components and detect dust polarization correlated with the local Galactic H i but not with the H i associated with Magellanic Stream i . We present a robust, multifrequency detection of polarized dust emission correlated with the filamentary H i morphology template down to 95 GHz. For assessing its utility for foreground cleaning, we report that the H i morphology template correlates in B modes at a ∼10%–65% level over the multipole range 20 < ℓ < 200 with the BICEP/Keck maps, which contain contributions from dust, CMB, and noise components. We measure the spectral index of the filamentary dust component spectral energy distribution to be β = 1.54 ± 0.13. We find no evidence for decorrelation in this region between the filaments and the rest of the dust field or from the inclusion of dust associated with the intermediate velocity H i . Finally, we explore the morphological parameter space in the H i -based filamentary model.

Published
2023
Full Text
View/download PDF

3. BICEP/Keck XII: Constraints on axionlike polarization oscillations in the cosmic microwave background

Author

P. A. R. Ade, Z. Ahmed, M. Amiri, D. Barkats, R. Basu Thakur, C. A. Bischoff, J. J. Bock, H. Boenish, E. Bullock, V. Buza, J. R. Cheshire, J. Connors, J. Cornelison, M. Crumrine, A. Cukierman, M. Dierickx, L. Duband, S. Fatigoni, J. P. Filippini, S. Fliescher, N. Goeckner-Wald, J. Grayson, G. Hall, M. Halpern, S. Harrison, S. Henderson, S. R. Hildebrandt, G. C. Hilton, J. Hubmayr, H. Hui, K. D. Irwin, J. Kang, K. S. Karkare, E. Karpel, B. G. Keating, S. Kefeli, S. A. Kernasovskiy, J. M. Kovac, C. L. Kuo, K. Lau, E. M. Leitch, K. G. Megerian, L. Moncelsi, T. Namikawa, C. B. Netterfield, H. T. Nguyen, R. O’Brient, R. W. Ogburn, S. Palladino, T. Prouve, C. Pryke, B. Racine, C. D. Reintsema, S. Richter, A. Schillaci, B. L. Schmitt, R. Schwarz, C. D. Sheehy, A. Soliman, T. St. Germaine, B. Steinbach, R. V. Sudiwala, G. Teply, K. L. Thompson, J. E. Tolan, C. Tucker, A. D. Turner, C. Umilta, A. G. Vieregg, A. Wandui, A. C. Weber, D. V. Wiebe, J. Willmert, C. L. Wong, W. L. K. Wu, H. Yang, K. W. Yoon, E. Young, C. Yu, L. Zeng, and C. Zhang

Published
2021
Full Text
View/download PDF

4. A demonstration of improved constraints on primordial gravitational waves with delensing

Author

P. A. R. Ade, Z. Ahmed, M. Amiri, A. J. Anderson, J. E. Austermann, J. S. Avva, D. Barkats, R. Basu Thakur, J. A. Beall, A. N. Bender, B. A. Benson, F. Bianchini, C. A. Bischoff, L. E. Bleem, J. J. Bock, H. Boenish, E. Bullock, V. Buza, J. E. Carlstrom, C. L. Chang, J. R. Cheshire, H. C. Chiang, T-L. Chou, R. Citron, J. Connors, C. Corbett Moran, J. Cornelison, T. M. Crawford, A. T. Crites, M. Crumrine, A. Cukierman, T. de Haan, M. Dierickx, M. A. Dobbs, L. Duband, W. Everett, S. Fatigoni, J. P. Filippini, S. Fliescher, J. Gallicchio, E. M. George, T. St. Germaine, N. Goeckner-Wald, D. C. Goldfinger, J. Grayson, N. Gupta, G. Hall, M. Halpern, N. W. Halverson, S. Harrison, S. Henderson, J. W. Henning, S. R. Hildebrandt, G. C. Hilton, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, N. Huang, J. Hubmayr, H. Hui, K. D. Irwin, J. Kang, K. S. Karkare, E. Karpel, S. Kefeli, S. A. Kernasovskiy, L. Knox, J. M. Kovac, C. L. Kuo, K. Lau, A. T. Lee, E. M. Leitch, D. Li, A. Lowitz, A. Manzotti, J. J. McMahon, K. G. Megerian, S. S. Meyer, M. Millea, L. M. Mocanu, L. Moncelsi, J. Montgomery, A. Nadolski, T. Namikawa, T. Natoli, C. B. Netterfield, H. T. Nguyen, J. P. Nibarger, G. Noble, V. Novosad, R. O’Brient, R. W. Ogburn, Y. Omori, S. Padin, S. Palladino, S. Patil, T. Prouve, C. Pryke, B. Racine, C. L. Reichardt, C. D. Reintsema, S. Richter, J. E. Ruhl, B. R. Saliwanchik, K. K. Schaffer, A. Schillaci, B. L. Schmitt, R. Schwarz, C. D. Sheehy, C. Sievers, G. Smecher, A. Soliman, A. A. Stark, B. Steinbach, R. V. Sudiwala, G. P. Teply, K. L. Thompson, J. E. Tolan, C. Tucker, A. D. Turner, C. Umiltà, T. Veach, J. D. Vieira, A. G. Vieregg, A. Wandui, G. Wang, A. C. Weber, N. Whitehorn, D. V. Wiebe, J. Willmert, C. L. Wong, W. L. K. Wu, H. Yang, V. Yefremenko, K. W. Yoon, E. Young, C. Yu, L. Zeng, and C. Zhang

Published
2021
Full Text
View/download PDF

5. Constraints on Primordial Gravitational Waves Using Planck , WMAP, and New BICEP2/ Keck Observations through the 2015 Season

Author

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

Published
2018
Full Text
View/download PDF

6. Bicep/Keck XV: The Bicep3 Cosmic Microwave Background Polarimeter and the First Three-year Data Set

Author

P. A. R. Ade, Z. Ahmed, M. Amiri, D. Barkats, R. Basu Thakur, C. A. Bischoff, D. Beck, J. J. Bock, H. Boenish, E. Bullock, V. Buza, J. R. Cheshire IV, J. Connors, J. Cornelison, M. Crumrine, A. Cukierman, E. V. Denison, M. Dierickx, L. Duband, M. Eiben, S. Fatigoni, J. P. Filippini, S. Fliescher, N. Goeckner-Wald, D. C. Goldfinger, J. Grayson, P. Grimes, G. Hall, G. Halal, M. Halpern, E. Hand, S. Harrison, S. Henderson, S. R. Hildebrandt, G. C. Hilton, J. Hubmayr, H. Hui, K. D. Irwin, J. Kang, K. S. Karkare, E. Karpel, S. Kefeli, S. A. Kernasovskiy, J. M. Kovac, C. L. Kuo, K. Lau, E. M. Leitch, A. Lennox, K. G. Megerian, L. Minutolo, L. Moncelsi, Y. Nakato, T. Namikawa, H. T. Nguyen, R. O’Brient, R. W. Ogburn IV, S. Palladino, T. Prouve, C. Pryke, B. Racine, C. D. Reintsema, S. Richter, A. Schillaci, R. Schwarz, B. L. Schmitt, C. D. Sheehy, A. Soliman, T. St. Germaine, B. Steinbach, R. V. Sudiwala, G. P. Teply, K. L. Thompson, J. E. Tolan, C. Tucker, A. D. Turner, C. Umiltà, C. Vergès, A. G. Vieregg, A. Wandui, A. C. Weber, D. V. Wiebe, J. Willmert, C. L. Wong, W. L. K. Wu, H. Yang, K. W. Yoon, E. Young, C. Yu, L. Zeng, C. Zhang, S. Zhang, Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Bicep/Keck

Subjects
polarization, noise, pole, temperature, Astronomy and Astrophysics, cosmic background radiation, optics, width, bolometer, Space and Planetary Science, infrared, optical, beam, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], performance
Abstract

We report on the design and performance of the Bicep3 instrument and its first three-year data set collected from 2016 to 2018. Bicep3 is a 52 cm aperture refracting telescope designed to observe the polarization of the cosmic microwave background (CMB) on degree angular scales at 95 GHz. It started science observation at the South Pole in 2016 with 2400 antenna-coupled transition-edge sensor bolometers. The receiver first demonstrated new technologies such as large-diameter alumina optics, Zotefoam infrared filters, and flux-activated SQUIDs, allowing ∼10× higher optical throughput compared to the Keck design. Bicep3 achieved instrument noise equivalent temperatures of 9.2, 6.8, and 7.1 μ K CMB s and reached Stokes Q and U map depths of 5.9, 4.4, and 4.4 μK arcmin in 2016, 2017, and 2018, respectively. The combined three-year data set achieved a polarization map depth of 2.8 μK arcmin over an effective area of 585 square degrees, which is the deepest CMB polarization map made to date at 95 GHz.

Published
2022

7. BICEP2 / Keck Array IX: New bounds on anisotropies of CMB polarization rotation and implications for axionlike particles and primordial magnetic fields

Author

P. A. R. Ade, Z. Ahmed, R. W. Aikin, K. D. Alexander, D. Barkats, S. J. Benton, C. A. Bischoff, J. J. Bock, R. Bowens-Rubin, J. A. Brevik, I. Buder, E. Bullock, V. Buza, J. Connors, B. P. Crill, L. Duband, C. Dvorkin, J. P. Filippini, S. Fliescher, T. St. Germaine, T. Ghosh, J. Grayson, S. Harrison, S. R. Hildebrandt, G. C. Hilton, H. Hui, K. D. Irwin, J. Kang, K. S. Karkare, E. Karpel, J. P. Kaufman, B. G. Keating, S. Kefeli, S. A. Kernasovskiy, J. M. Kovac, C. L. Kuo, N. Larson, E. M. Leitch, K. G. Megerian, L. Moncelsi, T. Namikawa, C. B. Netterfield, H. T. Nguyen, R. O’Brient, R. W. Ogburn, C. Pryke, S. Richter, A. Schillaci, R. Schwarz, C. D. Sheehy, Z. K. Staniszewski, B. Steinbach, R. V. Sudiwala, G. P. Teply, K. L. Thompson, J. E. Tolan, C. Tucker, A. D. Turner, A. G. Vieregg, A. C. Weber, D. V. Wiebe, J. Willmert, C. L. Wong, W. L. K. Wu, and K. W. Yoon

Published
2017
Full Text
View/download PDF

8. Optical Characterization of the Keck Array and BICEP3 CMB Polarimeters from 2016 to 2019

Author

R. Basu Thakur, P. A. R. Ade, Mark Halpern, Sarah M. Harrison, S. Fliescher, Howard Hui, A. D. Turner, E. Bullock, E. Karpel, C. Tucker, B. Racine, Bryan Steinbach, S. A. Kernasovskiy, Lorenzo Moncelsi, Mandana Amiri, Victor Buza, T. St. Germaine, H. T. Nguyen, K. L. Thompson, E. M. Leitch, J. R. Cheshire, Chao Zhang, C. L. Kuo, J. J. Bock, H. Boenish, S. Fatigoni, L. Duband, S. R. Hildebrandt, King Tong Lau, E. Young, Roger O'Brient, John M Kovac, Kirit Karkare, Abigail G. Vieregg, Toshiya Namikawa, Zeeshan Ahmed, D. V. Wiebe, R. Schwarz, C. Pryke, Alessandro Schillaci, C. D. Sheehy, E. Yang, Kent D. Irwin, Stefan Richter, R. V. Sudiwala, S. Kefeli, S. Palladino, W. L. K. Wu, J. Cornelison, A. Wandui, Marion Dierickx, Carl D. Reintsema, C. L. Wong, J. Willmert, J. E. Tolan, G. Hall, K. G. Megerian, Gene C. Hilton, Denis Barkats, C. Yu, A. Cukierman, Jake Connors, R. W. Ogburn, J. A. Grayson, M. Crumrine, K. W. Yoon, C. Umilta, A. C. Weber, Colin A. Bischoff, J. Kang, Calvin B. Netterfield, Jeffrey P. Filippini, Ahmed Soliman, Namikawa, Toshiya [0000-0003-3070-9240], and Apollo - University of Cambridge Repository

Subjects
Transition-edge sensor, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, BICEP3, Radio spectrum, 010305 fluids & plasmas, Optics, Polarization, 0103 physical sciences, General Materials Science, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Gravitational wave, business.industry, Detector, Condensed Matter Physics, Polarization (waves), Inflation, Astrophysics - Astrophysics of Galaxies, Atomic and Molecular Physics, and Optics, Astrophysics of Galaxies (astro-ph.GA), Refracting telescope, Keck Array, Transition edge sensor, Astrophysics - Instrumentation and Methods for Astrophysics, business, Beam (structure)
Abstract

The BICEP/Keck experiment (BK) is a series of small-aperture refracting telescopes observing degree-scale Cosmic Microwave Background (CMB) polarization from the South Pole in search of a primordial $B$-mode signature. This $B$-mode signal arises from primordial gravitational waves interacting with the CMB, and has amplitude parametrized by the tensor-to-scalar ratio $r$. Since 2016, BICEP3 and the Keck Array have been observing with 4800 total antenna-coupled transition-edge sensor detectors, with frequency bands spanning 95, 150, 220, and 270 GHz. Here we present the optical performance of these receivers from 2016 to 2019, including far-field beams measured in situ with an improved chopped thermal source and instrument spectral response measured with a field-deployable Fourier Transform Spectrometer. As a pair differencing experiment, an important systematic that must be controlled is the differential beam response between the co-located, orthogonally polarized detectors. We generate per-detector far-field beam maps and the corresponding differential beam mismatch that is used to estimate the temperature-to-polarization leakage in our CMB maps and to give feedback on detector and optics fabrication. The differential beam parameters presented here were estimated using improved low-level beam map analysis techniques, including efficient removal of non-Gaussian noise as well as improved spatial masking. These techniques help minimize systematic uncertainty in the beam analysis, with the goal of constraining the bias on $r$ induced by temperature-to-polarization leakage to be subdominant to the statistical uncertainty. This is essential as we progress to higher detector counts in the next generation of CMB experiments., 8 pages, 3 figures. Accepted by the Journal of Low Temperature Physics (Proceedings of the 18th International Workshop on Low Temperature Detectors)

Published
2020

9. Improved Constraints on Cosmology and Foregrounds from BICEP2 and Keck Array Cosmic Microwave Background Data with Inclusion of 95 GHz Band

Author

P. A. R. Ade, Z. Ahmed, R. W. Aikin, K. D. Alexander, D. Barkats, S. J. Benton, C. A. Bischoff, J. J. Bock, R. Bowens-Rubin, J. A. Brevik, I. Buder, E. Bullock, V. Buza, J. Connors, B. P. Crill, L. Duband, C. Dvorkin, J. P. Filippini, S. Fliescher, J. Grayson, M. Halpern, S. Harrison, G. C. Hilton, H. Hui, K. D. Irwin, K. S. Karkare, E. Karpel, J. P. Kaufman, B. G. Keating, S. Kefeli, S. A. Kernasovskiy, J. M. Kovac, C. L. Kuo, E. M. Leitch, M. Lueker, K. G. Megerian, C. B. Netterfield, H. T. Nguyen, R. O’Brient, R. W. Ogburn, A. Orlando, C. Pryke, S. Richter, R. Schwarz, C. D. Sheehy, Z. K. Staniszewski, B. Steinbach, R. V. Sudiwala, G. P. Teply, K. L. Thompson, J. E. Tolan, C. Tucker, A. D. Turner, A. G. Vieregg, A. C. Weber, D. V. Wiebe, J. Willmert, C. L. Wong, W. L. K. Wu, and K. W. Yoon

Published
2016
Full Text
View/download PDF

10. Joint Analysis of BICEP2/Keck ArrayandPlanckData

Author

P. A. R. Ade, N. Aghanim, Z. Ahmed, R. W. Aikin, K. D. Alexander, M. Arnaud, J. Aumont, C. Baccigalupi, A. J. Banday, D. Barkats, R. B. Barreiro, J. G. Bartlett, N. Bartolo, E. Battaner, K. Benabed, A. Benoît, A. Benoit-Lévy, S. J. Benton, J.-P. Bernard, M. Bersanelli, P. Bielewicz, C. A. Bischoff, J. J. Bock, A. Bonaldi, L. Bonavera, J. R. Bond, J. Borrill, F. R. Bouchet, F. Boulanger, J. A. Brevik, M. Bucher, I. Buder, E. Bullock, C. Burigana, R. C. Butler, V. Buza, E. Calabrese, J.-F. Cardoso, A. Catalano, A. Challinor, R.-R. Chary, H. C. Chiang, P. R. Christensen, L. P. L. Colombo, C. Combet, J. Connors, F. Couchot, A. Coulais, B. P. Crill, A. Curto, F. Cuttaia, L. Danese, R. D. Davies, R. J. Davis, P. de Bernardis, A. de Rosa, G. de Zotti, J. Delabrouille, J.-M. Delouis, F.-X. Désert, C. Dickinson, J. M. Diego, H. Dole, S. Donzelli, O. Doré, M. Douspis, C. D. Dowell, L. Duband, A. Ducout, J. Dunkley, X. Dupac, C. Dvorkin, G. Efstathiou, F. Elsner, T. A. Enßlin, H. K. Eriksen, E. Falgarone, J. P. Filippini, F. Finelli, S. Fliescher, O. Forni, M. Frailis, A. A. Fraisse, E. Franceschi, A. Frejsel, S. Galeotta, S. Galli, K. Ganga, T. Ghosh, M. Giard, E. Gjerløw, S. R. Golwala, J. González-Nuevo, K. M. Górski, S. Gratton, A. Gregorio, A. Gruppuso, J. E. Gudmundsson, M. Halpern, F. K. Hansen, D. Hanson, D. L. Harrison, M. Hasselfield, G. Helou, S. Henrot-Versillé, D. Herranz, S. R. Hildebrandt, G. C. Hilton, E. Hivon, M. Hobson, W. A. Holmes, W. Hovest, V. V. Hristov, K. M. Huffenberger, H. Hui, G. Hurier, K. D. Irwin, A. H. Jaffe, T. R. Jaffe, J. Jewell, W. C. Jones, M. Juvela, A. Karakci, K. S. Karkare, J. P. Kaufman, B. G. Keating, S. Kefeli, E. Keihänen, S. A. Kernasovskiy, R. Keskitalo, T. S. Kisner, R. Kneissl, J. Knoche, L. Knox, J. M. Kovac, N. Krachmalnicoff, M. Kunz, C. L. Kuo, H. Kurki-Suonio, G. Lagache, A. Lähteenmäki, J.-M. Lamarre, A. Lasenby, M. Lattanzi, C. R. Lawrence, E. M. Leitch, R. Leonardi, F. Levrier, A. Lewis, M. Liguori, P. B. Lilje, M. Linden-Vørnle, M. López-Caniego, P. M. Lubin, M. Lueker, J. F. Macías-Pérez, B. Maffei, D. Maino, N. Mandolesi, A. Mangilli, M. Maris, P. G. Martin, E. Martínez-González, S. Masi, P. Mason, S. Matarrese, K. G. Megerian, P. R. Meinhold, A. Melchiorri, L. Mendes, A. Mennella, M. Migliaccio, S. Mitra, M.-A. Miville-Deschênes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, A. Moss, D. Munshi, J. A. Murphy, P. Naselsky, F. Nati, P. Natoli, C. B. Netterfield, H. T. Nguyen, H. U. Nørgaard-Nielsen, F. Noviello, D. Novikov, I. Novikov, R. O’Brient, R. W. Ogburn, A. Orlando, L. Pagano, F. Pajot, R. Paladini, D. Paoletti, B. Partridge, F. Pasian, G. Patanchon, T. J. Pearson, O. Perdereau, L. Perotto, V. Pettorino, F. Piacentini, M. Piat, D. Pietrobon, S. Plaszczynski, E. Pointecouteau, G. Polenta, N. Ponthieu, G. W. Pratt, S. Prunet, C. Pryke, J.-L. Puget, J. P. Rachen, W. T. Reach, R. Rebolo, M. Reinecke, M. Remazeilles, C. Renault, A. Renzi, S. Richter, I. Ristorcelli, G. Rocha, M. Rossetti, G. Roudier, M. Rowan-Robinson, J. A. Rubiño-Martín, B. Rusholme, M. Sandri, D. Santos, M. Savelainen, G. Savini, R. Schwarz, D. Scott, M. D. Seiffert, C. D. Sheehy, L. D. Spencer, Z. K. Staniszewski, V. Stolyarov, R. Sudiwala, R. Sunyaev, D. Sutton, A.-S. Suur-Uski, J.-F. Sygnet, J. A. Tauber, G. P. Teply, L. Terenzi, K. L. Thompson, L. Toffolatti, J. E. Tolan, M. Tomasi, M. Tristram, M. Tucci, A. D. Turner, L. Valenziano, J. Valiviita, B. Van Tent, L. Vibert, P. Vielva, A. G. Vieregg, F. Villa, L. A. Wade, B. D. Wandelt, R. Watson, A. C. Weber, I. K. Wehus, M. White, S. D. M. White, J. Willmert, C. L. Wong, K. W. Yoon, D. Yvon, A. Zacchei, and A. Zonca

Published
2015
Full Text
View/download PDF

11. BICEP/Keck XII: Constraints on axionlike polarization oscillations in the cosmic microwave background

Author

S. R. Hildebrandt, H. Boenish, D. V. Wiebe, P. A. R. Ade, K. G. Megerian, J. Kang, C. D. Sheehy, Bryan Steinbach, D. Barkats, S. Palladino, J. E. Tolan, J. Cheshire, J. J. Bock, C. L. Kuo, Edward D. Young, C. D. Reintsema, Tyler St. Germaine, Marion Dierickx, C. Yu, Colin A. Bischoff, Stefan Richter, S. Kefeli, A. C. Weber, Jake Connors, Ahmed Soliman, Lorenzo Moncelsi, A. Schillaci, R. W. Ogburn, Jeffrey P. Filippini, Roger O'Brient, M. Crumrine, K. W. Yoon, G. Hall, C. L. Wong, Abigail G. Vieregg, C. Umilta, Brian Keating, S. Henderson, R. Schwarz, Lingzhen Zeng, John M Kovac, Kirit Karkare, Mark Halpern, J. Hubmayr, Kei May Lau, Calvin B. Netterfield, S. Fatigoni, M. Amiri, Kent D. Irwin, A. Cukierman, E. Bullock, J. A. Grayson, Victor Buza, Howard Hui, Neil Goeckner-Wald, Grant Teply, C. Tucker, S. Fliescher, R. V. Sudiwala, W. L. K. Wu, Toshiya Namikawa, H. Yang, J. Cornelison, Z. Ahmed, S. A. Kernasovskiy, B. L. Schmitt, T. Prouve, C. Pryke, B. Racine, H. T. Nguyen, E. M. Leitch, Bicep, Chao Zhang, A. Wandui, A. D. Turner, E. Karpel, L. Duband, K. L. Thompson, Sarah M. Harrison, J. Willmert, Gene C. Hilton, and R. Basu Thakur

Subjects
Coupling constant, Physics, 010308 nuclear & particles physics, Oscillation, Cosmic microwave background, Dark matter, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Parameter space, Polarization (waves), 01 natural sciences, Amplitude, 0103 physical sciences, 010306 general physics, Axion
Abstract

We present an improved search for axion-like polarization oscillations in the cosmic microwave background (CMB) with observations from the Keck Array. An all-sky, temporally sinusoidal rotation of CMB polarization, equivalent to a time-variable cosmic birefringence, is an observable manifestation of a local axion field and potentially allows a CMB polarimeter to detect axion-like dark matter directly. We describe improvements to the method presented in previous work, and we demonstrate the updated method with an expanded dataset consisting of the 2012-2015 observing seasons. We set limits on the axion-photon coupling constant for mass $m$ in the range $10^{-23}$-$10^{-18}~\mathrm{eV}$, which corresponds to oscillation periods on the order of hours to years. Our results are consistent with the background model. For periods between $1$ and $30~\mathrm{d}$ ($1.6 \times 10^{-21} \leq m \leq 4.8 \times 10^{-20}~\mathrm{eV}$), the $95\%$-confidence upper limits on rotation amplitude are approximately constant with a median of $0.27^\circ$, which constrains the axion-photon coupling constant to $g_{\phi\gamma} < (4.5 \times 10^{-12}~\mathrm{GeV}^{-1}) m/(10^{-21}~\mathrm{eV}$), if axion-like particles constitute all of the dark matter. More than half of the collected BICEP dataset has yet to be analyzed, and several current and future CMB polarimetry experiments can apply the methods presented here to achieve comparable or superior constraints. In the coming years, oscillation measurements can achieve the sensitivity to rule out unexplored regions of the axion parameter space.

Published
2021

12. Improved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season

Author

J. J. Bock, M. Amiri, B. Steinbach, Kent D. Irwin, S. Kefeli, B. Racine, E. Hand, J. E. Tolan, Abigail G. Vieregg, C. Tucker, J. Willmert, N. Goeckner-Wald, S. Richter, A. Turner, H. Hui, B. L. Schmitt, T. Namikawa, G. Halal, P. A. R. Ade, K. G. Megerian, L. Zeng, R. Schwarz, Victor Buza, L. Minutolo, T. St. Germaine, C. D. Sheehy, Jake Connors, R. Basu Thakur, S. Fliescher, C. Pryke, M. Crumrine, Bicep, Mark Halpern, C. Umilta, Sarah M. Harrison, H. Yang, Chao-Lin Kuo, Che-Hang Yu, K. Lau, Shengyu Zhang, C. Bischoff, C. Verges, S. R. Hildebrandt, S. Fatigoni, R. O'Brient, Denis Barkats, Chao Zhang, Jeffrey P. Filippini, A. Cukierman, H. Boenish, H. T. Nguyen, D. V. Wiebe, K. S. Karkare, Gene C. Hilton, E. Young, J. Grayson, M. Eiben, Y. Nakato, Z. Ahmed, D. C. Goldfinger, A. C. Weber, J. R. Cheshire, L. Duband, C. D. Reintsema, S. Henderson, T. Prouve, A. Wandui, P. Grimes, K. L. Thompson, G. P. Teply, J. Cornelison, S. Palladino, J. Kang, E. V. Denison, Marion Dierickx, A. Lennox, A. Soliman, R. W. Ogburn, R. V. Sudiwala, E. Bullock, D. Beck, C. L. Wong, A. Schillaci, E. Karpel, J. Hubmayr, G. Hall, W. L. K. Wu, L. Moncelsi, K. W. Yoon, E. M. Leitch, S. A. Kernasovskiy, J. M. Kovac, Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), BICEP, and Keck

Subjects
noise, satellite: Planck, statistical analysis: confidence limit, media_common.quotation_subject, Cosmic microwave background, General Physics and Astronomy, cosmic background radiation: polarization, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, power spectrum, 01 natural sciences, symbols.namesake, gravitation: lens, cosmological model: parameter space, 0103 physical sciences, synchrotron, Planck, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, Spectral index, 010308 nuclear & particles physics, Gravitational wave, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation: primordial, cosmological model: dust, Polarization (waves), BICEP, CMB cold spot, Sky, WMAP, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Noise (radio)
Abstract

International audience; We present results from an analysis of all data taken by the BICEP2, Keck Array, and BICEP3 CMB polarization experiments up to and including the 2018 observing season. We add additional Keck Array observations at 220 GHz and BICEP3 observations at 95 GHz to the previous 95/150/220 GHz dataset. The Q/U maps now reach depths of 2.8, 2.8, and 8.8 μKCMB arcmin at 95, 150, and 220 GHz, respectively, over an effective area of ≈600 square degrees at 95 GHz and ≈400 square degrees at 150 and 220 GHz. The 220 GHz maps now achieve a signal-to-noise ratio on polarized dust emission exceeding that of Planck at 353 GHz. We take auto- and cross-spectra between these maps and publicly available WMAP and Planck maps at frequencies from 23 to 353 GHz and evaluate the joint likelihood of the spectra versus a multicomponent model of lensed ΛCDM+r+dust+synchrotron+noise. The foreground model has seven parameters, and no longer requires a prior on the frequency spectral index of the dust emission taken from measurements on other regions of the sky. This model is an adequate description of the data at the current noise levels. The likelihood analysis yields the constraint r0.05<0.036 at 95% confidence. Running maximum likelihood search on simulations we obtain unbiased results and find that σ(r)=0.009. These are the strongest constraints to date on primordial gravitational waves.

Published
2021

13. Observing low elevation sky and the CMB Cold Spot with BICEP3 at the South Pole

Author

Lingzhen Zeng, Paul K. Grimes, Denis Barkats, G. Hall, J. Cornelison, P. A. R. Ade, Jeffrey P. Filippini, E. V. Denison, Ki Won Yoon, S. Henderson, S. Richter, Edward D. Young, R. Schwarz, Y. Nakato, N. Precup, Shengyu Zhang, Sarah M. Harrison, Lorenzo Moncelsi, Che-Hang Yu, Lionel Duband, C. Pryke, Rashmikant V. Sudiwala, G. P. Teply, J. Kang, S. Fliescher, C. Umiltà, A. Wandui, Abigail G. Vieregg, A. C. Weber, Kent D. Irwin, J. Willmert, Gene C. Hilton, H. Boenish, Bryan Steinbach, A. Cukierman, John M Kovac, H. T. Nguyen, Donald V. Wiebe, Kirit Karkare, E. M. Leitch, King Tong Lau, J. Cheshire, Colin A. Bischoff, Toshiya Namikawa, Ahmed Soliman, S. Kefeli, Benjamin L. Schmitt, Eui-Hyeok Yang, E. Bullock, Johannes Hubmayr, W. L. K. Wu, Mark Halpern, Roger O'Brient, D. C. Goldfinger, Anthony D. Turner, T. Prouve, E. Karpel, C. L. Wong, J. E. Tolan, Keith L. Thompson, Sergi R. Hildebrandt, Alessandro Schillaci, Chao-Lin Kuo, Jake Connors, Victor Buza, S. Fatigoni, S. A. Kernasovskiy, James J. Bock, S. Palladino, Carl D. Reintsema, C. D. Sheehy, T. St. Germaine, Marion Dierickx, M. Crumrine, R. W. Ogburn, Zeeshan Ahmed, R. Basu Thakur, M. Eiben, J. A. Grayson, Carole Tucker, B. Racine, Howard Hui, K. G. Megerian, Neil Goeckner-Wald, L. Minutolo, Chao Zhang, Mandana Amiri, Institut Laue-Langevin (ILL), Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Zmuidzinas, Jonas, Gao, Jian-Rong, ILL, and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)

Subjects
gravitational radiation: polarization, detector: performance, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Cosmic microwave background, cosmic background radiation: polarization, anomaly, FOS: Physical sciences, 02 engineering and technology, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, BICEP3, 010309 optics, 0103 physical sciences, Cosmic Microwave Background, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], mirror, Instrumentation and Methods for Astrophysics (astro-ph.IM), media_common, Gravitational Waves, Beam diameter, polarization, Cold spot, Gravitational wave, beam: width, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, 021001 nanoscience & nanotechnology, Polarization (waves), BICEP, Flat mirror, Inflation, B-mode, Sky, Refracting telescope, power spectrum: angular dependence, Cold Spot, 0210 nano-technology, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, Geology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

BICEP3 is a 520 mm aperture on-axis refracting telescope at the South Pole, which observes the polarization of the cosmic microwave background (CMB) at 95 GHz to search for the B-mode signal from inflationary gravitational waves. In addition to this main target, we have developed a low-elevation observation strategy to extend coverage of the Southern sky at the South Pole, where BICEP3 can quickly achieve degree-scale E-mode measurements over a large area. An interesting E-mode measurement is probing a potential polarization anomaly around the CMB Cold Spot. During the austral summer seasons of 2018-19 and 2019-20, BICEP3 observed the sky with a flat mirror to redirect the beams to various low elevation ranges. The preliminary data analysis shows degree-scale E-modes measured with high signal-to-noise ratio., 12 pages, 10 figures; Figure 7 shows the correct file

Published
2020

14. Polarization Calibration of the BICEP3 CMB polarimeter at the South Pole

Author

K. G. Megerian, L. Minutolo, Y. Nakato, John M Kovac, Kirit Karkare, H. Boenish, D. C. Goldfinger, Roger O'Brient, A. D. Turner, C. D. Sheehy, Stefan Richter, Kent D. Irwin, E. Karpel, E. Bullock, Lingzhen Zeng, K. L. Thompson, S. Fliescher, M. Crumrine, K. W. Yoon, G. Hall, H. Hui, J. Kang, P. A. R. Ade, C. Yu, C. Umilta, S. Henderson, Zeeshan Ahmed, A. Cukierman, J. Hubmayr, B. L. Schmitt, N. Precup, D. V. Wiebe, S. Kefeli, Kei May Lau, E. Young, R. Basu Thakur, A. Wandui, Denis Barkats, Victor Buza, Neil Goeckner-Wald, Paul K. Grimes, Jeffrey P. Filippini, Marion Dierickx, J. J. Bock, Mark Halpern, E. Yang, R. V. Sudiwala, W. L. K. Wu, C. D. Reintsema, S. A. Kernasovkiy, R. Schwarz, C. Tucker, Lorenzo Moncelsi, G. Halal, J. R. Cheshire, J. A. Grayson, Abigail G. Vieregg, S. R. Hildebrandt, Bryan Steinbach, S. Zhang, J. Willmert, Gene C. Hilton, Chao Zhang, Mandana Amiri, A. C. Weber, Toshiya Namikawa, Chao-Lin Kuo, J. Cornelison, S. Fatigoni, S. Palladino, T. Prouve, C. Pryke, Colin A. Bischoff, B. Racine, H. T. Nguyen, E. M. Leitch, E. V. Denison, A. Schillaci, J. E. Tolan, L. Duband, J. Connors, R. W. Ogburn, M. Eiben, C. L. Wong, Ahmed Soliman, Sarah M. Harrison, G. P. Teply, T. St. Germaine, Institut Laue-Langevin (ILL), ILL, Service des Basses Températures (SBT ), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Zmuidzinas, Jonas, and Gao, Jian-Rong

Subjects
Cosmic microwave background, FOS: Physical sciences, 02 engineering and technology, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, 010309 optics, Telescope, Optics, law, Polarization, 0103 physical sciences, Cosmic Microwave Background, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Birefringence, business.industry, Gravitational wave, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Polarimeter, 021001 nanoscience & nanotechnology, Polarization (waves), Cosmology, Refracting telescope, Calibration, Transition edge sensor, Astrophysics - Instrumentation and Methods for Astrophysics, 0210 nano-technology, business
Abstract

The BICEP3 CMB Polarimeter is a small-aperture refracting telescope located at the South Pole and is specifically designed to search for the possible signature of inflationary gravitational waves in the Cosmic Microwave Background (CMB). The experiment measures polarization on the sky by differencing the signal of co-located, orthogonally polarized antennas coupled to Transition Edge Sensor (TES) detectors. We present precise measurements of the absolute polarization response angles and polarization efficiencies for nearly all of BICEP3s $\sim800$ functioning polarization-sensitive detector pairs from calibration data taken in January 2018. Using a Rotating Polarized Source (RPS), we mapped polarization response for each detector over a full 360 degrees of source rotation and at multiple telescope boresight rotations from which per-pair polarization properties were estimated. In future work, these results will be used to constrain signals predicted by exotic physical models such as Cosmic Birefringence., Comment: Proceedings submitted to SPIE 2020 (AS111). 12 pages, 5 figures, 2 tables

Published
2020

15. Analysis of Temperature-to-Polarization Leakage in BICEP3 and Keck CMB Data from 2016 to 2018

Author

Y. Nakato, S. Palladino, J. Kang, H. Boenish, A. D. Turner, E. Karpel, D. C. Goldfinger, K. L. Thompson, C. L. Wong, P. A. R. Ade, E. V. Denison, S. Kefeli, Bicep, Jeffrey P. Filippini, M. Crumrine, K. W. Yoon, J. Hubmayr, G. Hall, A. C. Weber, C. Umilta, A. Wandui, S. Fliescher, A. Cukierman, Victor Buza, Chao Zhang, J. A. Grayson, Lingzhen Zeng, E. Bullock, J. Willmert, Kei May Lau, Gene C. Hilton, Denis Barkats, John M Kovac, C. D. Sheehy, Kirit Karkare, Colin A. Bischoff, K. G. Megerian, Kent D. Irwin, L. Minutolo, P. Grimes, R. V. Sudiwala, C. Yu, W. L. K. Wu, N. Precup, T. Namikawa, Bryan Steinbach, Eui-Hyeok Yang, J. Cheshire, J. J. Bock, Roger O'Brient, Lorenzo Moncelsi, Mark Halpern, R. Schwarz, S. Henderson, Ahmed Soliman, Shengyu Zhang, Abigail G. Vieregg, B. L. Schmitt, C. D. Reintsema, Stefan Richter, Marion Dierickx, Z. Ahmed, S. A. Kernasovskiy, A. Schillaci, S. R. Hildebrandt, Edward D. Young, T. Prouve, C. Pryke, B. Racine, H. T. Nguyen, E. M. Leitch, C. L. Kuo, M. Amiri, D. V. Wiebe, J. E. Tolan, Jake Connors, R. W. Ogburn, Sarah M. Harrison, Grant Teply, L. Duband, T. St. Germaine, M. Eiben, R. Basu Thakur, Howard Hui, Neil Goeckner-Wald, C. Tucker, J. Cornelison, S. Fatigoni, Institut Laue-Langevin (ILL), ILL, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), and BICEP/Keck

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, cosmic background radiation: polarization, 02 engineering and technology, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Residual, 01 natural sciences, B-mode: primordial, 010309 optics, Optics, 0103 physical sciences, Cosmic Microwave Background, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], numerical calculations, Instrumentation and Methods for Astrophysics (astro-ph.IM), Leakage (electronics), media_common, Physics, Gravitational Waves, polarization, business.industry, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation, 021001 nanoscience & nanotechnology, Polarization (waves), BICEP, Inflation, cosmic background radiation: temperature, B-mode, Sky, Refracting telescope, Keck Array, Physics::Accelerator Physics, Astrophysics - Instrumentation and Methods for Astrophysics, 0210 nano-technology, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Beam (structure), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The BICEP/Keck Array experiment is a series of small-aperture refracting telescopes observing degree-scale Cosmic Microwave Background polarization from the South Pole in search of a primordial $B$-mode signature. As a pair differencing experiment, an important systematic that must be controlled is the differential beam response between the co-located, orthogonally polarized detectors. We use high-fidelity, in-situ measurements of the beam response to estimate the temperature-to-polarization (T $\rightarrow$ P) leakage in our latest data including observations from 2016 through 2018. This includes three years of BICEP3 observing at 95 GHz, and multifrequency data from Keck Array. Here we present band-averaged far-field beam maps, differential beam mismatch, and residual beam power (after filtering out the leading difference modes via deprojection) for these receivers. We show preliminary results of "beam map simulations," which use these beam maps to observe a simulated temperature (no $Q/U$) sky to estimate T $\rightarrow$ P leakage in our real data., Comment: 9 pages, 4 figures

Published
2020

16. A Demonstration of Improved Constraints on Primordial Gravitational Waves with Delensing

Author

Roger O'Brient, John M Kovac, Kirit Karkare, T. Natoli, Kent D. Irwin, A. E. Lowitz, N. Huang, Y. Omori, Victor Buza, Robert I. Citron, S. A. Kernasovskiy, W. L. Holzapfel, Ahmed Soliman, Jeff McMahon, C. Corbett Moran, P. A. R. Ade, Lingzhen Zeng, S. Henderson, W. B. Everett, J. D. Hrubes, Jessica Avva, C. Yu, Calvin B. Netterfield, Lorenzo Moncelsi, J. R. Cheshire, Jason W. Henning, J. A. Grayson, S. Patil, K. K. Schaffer, Elizabeth George, Abigail G. Vieregg, Denis Barkats, V. G. Yefremenko, Jason E. Austermann, N. W. Halverson, A. Cukierman, H. Boenish, B. L. Schmitt, Marion Dierickx, M. Crumrine, K. W. Yoon, Joaquin Vieira, E. Young, G. Hall, Stefan Richter, C. Sievers, Toshiya Namikawa, Graeme Smecher, C. Umilta, D. V. Wiebe, S. Fliescher, T.-L. Chou, H. C. Chiang, Johannes Hubmayr, H. Yang, C. D. Sheehy, Chao-Lin Kuo, Mark Halpern, Christian L. Reichardt, Marius Millea, Joshua Montgomery, S. Kefeli, J. Cornelison, J. J. Bock, Bryan Steinbach, Howard Hui, Gensheng Wang, Andreas Bender, Neil Goeckner-Wald, J. E. Ruhl, Dale Li, C. Tucker, K. G. Megerian, T. M. Crawford, M. A. Dobbs, Mandana Amiri, V. Novosad, R. Schwarz, S. Fatigoni, S. R. Hildebrandt, S. Padin, John E. Carlstrom, E. Bullock, Chao Zhang, T. de Haan, D. C. Goldfinger, John P. Nibarger, Andrew Nadolski, J. Willmert, Carl D. Reintsema, Gene C. Hilton, N. Whitehorn, B. Racine, H. T. Nguyen, A. A. Stark, E. M. Leitch, Alessandro Schillaci, A. D. Turner, E. Karpel, T. Veach, R. Basu Thakur, K. L. Thompson, T. Prouve, A. T. Crites, C. Pryke, C. L. Wong, C. L. Chang, J. Kang, Adam Anderson, Grant Teply, Benjamin Saliwanchik, A. Wandui, Gilbert Holder, A. Manzotti, A. C. Weber, G. I. Noble, Federico Bianchini, Nikhel Gupta, Jeffrey P. Filippini, R. V. Sudiwala, Adrian T. Lee, Bradford Benson, Lloyd Knox, W. L. K. Wu, Colin A. Bischoff, S. S. Meyer, Jason Gallicchio, T. St. Germaine, S. Palladino, L. Duband, J. E. Tolan, Zeeshan Ahmed, L. M. Mocanu, Jake Connors, Kei May Lau, Sarah M. Harrison, Lindsey Bleem, R. W. Ogburn, J. A. Beall, Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), SPTpol, BICEP/Keck, BICEP, and Keck

Subjects
data analysis method, satellite: Planck, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, Cosmic background radiation, cosmic background radiation: polarization, FOS: Physical sciences, cosmic background radiation, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, cosmic rays, gravitation: lens, statistical analysis, Cosmic infrared background, 0103 physical sciences, Experiments in gravity, Sample variance, Planck, numerical calculations, 010306 general physics, Astrophysics::Galaxy Astrophysics, Physics, polarization, background, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: primordial, BICEP, South Pole Telescope, Gravitational lens, B-mode, infrared, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a constraint on the tensor-to-scalar ratio, $r$, derived from measurements of cosmic microwave background (CMB) polarization $B$-modes with "delensing," whereby the uncertainty on $r$ contributed by the sample variance of the gravitational lensing $B$-modes is reduced by cross-correlating against a lensing $B$-mode template. This template is constructed by combining an estimate of the polarized CMB with a tracer of the projected large-scale structure. The large-scale-structure tracer used is a map of the cosmic infrared background derived from Planck satellite data, while the polarized CMB map comes from a combination of South Pole Telescope, BICEP/Keck, and Planck data. We expand the BICEP/Keck likelihood analysis framework to accept a lensing template and apply it to the BICEP/Keck data set collected through 2014 using the same parametric foreground modelling as in the previous analysis. From simulations, we find that the uncertainty on $r$ is reduced by $\sim10\%$, from $��(r)$= 0.024 to 0.022, which can be compared with a $\sim26\%$ reduction obtained when using a perfect lensing template. Applying the technique to the real data, the constraint on $r$ is improved from $r_{0.05} < 0.090$ to $r_{0.05} < 0.082$ (95\% C.L.). This is the first demonstration of improvement in an $r$ constraint through delensing., 23 pages, 11 figures; match published version

Published
2020
Full Text
View/download PDF

17. Constraints on Primordial Gravitational Waves Using Planck , WMAP, and New BICEP2/ Keck Observations through the 2015 Season

Author

Peter A. R. Ade, Lorenzo Moncelsi, N. A. Larsen, Abigail G. Vieregg, S. Kefeli, J. A. Grayson, Justus A. Brevik, Randol W. Aikin, King Tong Lau, Toshiya Namikawa, John M Kovac, Z. K. Staniszewski, Stefan Richter, Kirit Karkare, S. Palladino, K. G. Megerian, C. D. Sheehy, Chao-Lin Kuo, Denis Barkats, A. Wandui, J. J. Bock, Kent D. Irwin, Victor Buza, A. D. Turner, E. Karpel, L. Duband, R. Bowens-Rubin, M. Lueker, J. Cornelison, J. Kang, Cora Dvorkin, K. L. Thompson, Colin A. Bischoff, Howard Hui, Calvin B. Netterfield, J. P. Kaufman, J. E. Tolan, C. Tucker, R. Schwarz, Alessandro Schillaci, Marion Dierickx, T. St. Germaine, D. V. Wiebe, M. Crumrine, A. C. Weber, R. V. Sudiwala, Jake Connors, G. Hall, Brian Keating, J. Willmert, W. L. K. Wu, S. Fliescher, Ahmed Soliman, C. Umilta, Ki Won Yoon, Kate D. Alexander, Gene C. Hilton, Jeffrey P. Filippini, Steven J. Benton, R. W. Ogburn, B. P. Crill, Chao Zhang, C. Pryke, Grant Teply, Hyunsoo Yang, B. Racine, C. L. Wong, Sarah M. Harrison, H. T. Nguyen, E. M. Leitch, I. Buder, Bryan Steinbach, E. Bullock, Roger O'Brient, Mark Halpern, Z. Ahmed, S. A. Kernasovskiy, and S. R. Hildebrandt

Subjects
Physics, 010308 nuclear & particles physics, Gravitational wave, media_common.quotation_subject, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, General Physics and Astronomy, Planck temperature, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Polarization (waves), 01 natural sciences, 7. Clean energy, CMB cold spot, Spectral line, symbols.namesake, 13. Climate action, Sky, 0103 physical sciences, symbols, Astrophysics::Earth and Planetary Astrophysics, Planck, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common
Abstract

We present results from an analysis of all data taken by the bicep2/Keck CMB polarization experiments up to and including the 2015 observing season. This includes the first Keck Array observations at 220 GHz and additional observations at 95 and 150 GHz. The Q and U maps reach depths of 5.2, 2.9, and 26 μKCMB arcmin at 95, 150, and 220 GHz, respectively, over an effective area of ≈400 square degrees. The 220 GHz maps achieve a signal to noise on polarized dust emission approximately equal to that of Planck at 353 GHz. We take auto and cross spectra between these maps and publicly available WMAP and Planck maps at frequencies from 23 to 353 GHz. We evaluate the joint likelihood of the spectra versus a multicomponent model of lensed-ΛCDM+r+dust+synchrotron+noise. The foreground model has seven parameters, and we impose priors on some of these using external information from Planck and WMAP derived from larger regions of sky. The model is shown to be an adequate description of the data at the current noise levels. The likelihood analysis yields the constraint r0.05

Published
2018

18. Ultra-thin large-aperture vacuum windows for millimeter wavelengths receivers

Author

R. W. Ogburn, E. Bullock, Mark Halpern, B. Racine, Grant Teply, M. Lueker, K. Lau, J. Willmert, S. J. Benton, G. Hall, H. T. Nguyen, I. Buder, Peter A. R. Ade, Lorenzo Moncelsi, Bryan Steinbach, J. Kang, R. Bowens-Rubin, Hong Yang, Abigail G. Vieregg, Randol W. Aikin, M. Crumrine, J. Connors, K. L. Thompson, B. G. Keating, Howard Hui, J. P. Kaufman, K. G. Megerian, C. L. Kuo, S. A. Harrison, S. Palladino, Marion Dierickx, Justus A. Brevik, Carole Tucker, S. Fliescher, Chris Pentacoff, N. A. Larsen, Zeeshan Ahmed, S. A. Kernasovskiy, S. R. Hildebrandt, Victor Buza, A. Wandui, J. E. Tolan, Denis Barkats, C. L. Wong, Kate D. Alexander, Roger O'Brient, E. Karpel, C. Pryke, Jeffrey P. Filippini, J. J. Bock, R. V. Sudiwala, S. Kefeli, W. L. K. Wu, C. D. Sheehy, K. W. Yoon, D. V. Wiebe, Cora Dvorkin, R. Schwarz, E. M. Leitch, J. Cornelison, C. Umiltà, A. C. Weber, John M Kovac, G. C. Hilton, Kirit Karkare, Kent D. Irwin, S. Richter, Colin A. Bischoff, B. P. Crill, Alessandro Schillaci, T. St. Germaine, Ahmed Soliman, J. A. Grayson, C. Zhang, A. D. Turner, L. Duband, T. Namikawa, Z. K. Staniszewski, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Zmuidzinas, Jonas, and Gao, Jian-Rong

Subjects
Cryostat, Materials science, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Transmission loss, polymer, Cosmic microwave background, FOS: Physical sciences, cosmic background radiation: polarization, fabrication, 7. Clean energy, 01 natural sciences, microwaves, 010309 optics, Optics, Vacuum Windows, Polarization, 0103 physical sciences, Cosmic Microwave Background, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), attenuation, Primordial Gravitational Waves, business.industry, Attenuation, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation: primordial, Polymer Materials, Polarization (waves), sensitivity, BICEP, vacuum system, Wavelength, Millimeter Wavelengths, cryogenics, Keck Array, Millimeter, atmosphere: pressure, business, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Microwave, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Targeting faint polarization patterns arising from Primordial Gravitational Waves in the Cosmic Microwave Background requires excellent observational sensitivity. Optical elements in small aperture experiments such as Bicep3 and Keck Array are designed to optimize throughput and minimize losses from transmission, reflection and scattering at millimeter wavelengths. As aperture size increases, cryostat vacuum windows must withstand larger forces from atmospheric pressure and the solution has often led to a thicker window at the expense of larger transmission loss. We have identified a new candidate material for the fabrication of vacuum windows: with a tensile strength two orders of magnitude larger than previously used materials, woven high-modulus polyethylene could allow for dramatically thinner windows, and therefore significantly reduced losses and higher sensitivity. In these proceedings we investigate the suitability of high-modulus polyethylene windows for ground-based CMB experiments, such as current and future receivers in the Bicep/Keck Array program. This includes characterizing their optical transmission as well as their mechanical behavior under atmospheric pressure. We find that such ultra-thin materials are promising candidates to improve the performance of large-aperture instruments at millimeter wavelengths, and outline a plan for further tests ahead of a possible upcoming field deployment of such a science-grade window., Comment: Published in Proc. SPIE. Presented at SPIE Astronomical Telescopes and Instrumentation Conference 10708: Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy XI, June 2018. 14 pages, 7 figures

Published
2018

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

Author

Marion Dierickx, E. M. Leitch, John M Kovac, Kirit Karkare, Cora Dvorkin, R. Schwarz, Roger O'Brient, G. P. Teply, Kent D. Irwin, C. L. Kuo, Alessandro Schillaci, S. A. Kernasovskiy, E. Bullock, J. Willmert, Sarah M. Harrison, M. Lueker, Howard Hui, Ki Won Yoon, C. L. Wong, A. Wandui, B. P. Crill, Bryan Steinbach, Peter A. R. Ade, Lorenzo Moncelsi, I. Buder, B. Racine, Victor Buza, Abigail G. Vieregg, R. Bowens-Rubin, S. Palladino, T. St. Germaine, Donald V. Wiebe, James J. Bock, K. G. Megerian, S. Fliescher, Randol W. Aikin, H. T. Nguyen, A. C. Weber, C. Umiltà, Z. K. Staniszewski, Brian Keating, S. J. Benton, W. L. K. Wu, T. Namikawa, Eui-Hyeok Yang, M. Crumrine, S. Richter, A. D. Turner, L. Duband, Mark Halpern, Kam Y. Lau, K. L. Thompson, C. D. Sheehy, Colin A. Bischoff, Kate D. Alexander, C. Pryke, J. A. Grayson, Justus A. Brevik, Carole Tucker, J. Cornelison, Gene C. Hilton, N. A. Larsen, Zeeshan Ahmed, S. R. Hildebrandt, Denis Barkats, J. E. Tolan, Jake Connors, R. W. Ogburn, Rashmikant V. Sudiwala, J. P. Kaufman, Jeffrey P. Filippini, Ahmed Soliman, J. Kang, G. Hall, E. Karpel, S. Kefeli, C. Zhang, Calvin B. Netterfield, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Zmuidzinas, Jonas, and Gao, Jian-Rong

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), engineering, Cosmic microwave background, FOS: Physical sciences, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, shielding: design, Optics, Polarization, 0103 physical sciences, Cosmic Microwave Background, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Instrumentation, Astrophysics::Galaxy Astrophysics, activity report, detector: design, Physics, 010308 nuclear & particles physics, business.industry, shielding: magnetic, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Polarimeter, Polarization (waves), BICEP, optics, Cardinal point, South Pole Telescope, Electromagnetic shielding, Astrophysics - Instrumentation and Methods for Astrophysics, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

BICEP Array is the newest multi-frequency instrument in the BICEP/Keck Array program. It is comprised of four 550 mm aperture refractive telescopes observing the polarization of the cosmic microwave background (CMB) at 30/40, 95, 150 and 220/270 GHz with over 30,000 detectors. We present an overview of the receiver, detailing the optics, thermal, mechanical, and magnetic shielding design. BICEP Array follows BICEP3's modular focal plane concept, and upgrades to 6" wafer to reduce fabrication with higher detector count per module. The first receiver at 30/40 GHz is expected to start observing at the South Pole during the 2019-20 season. By the end of the planned BICEP Array program, we project $\sigma(r) \sim 0.003$, assuming current modeling of polarized Galactic foreground and depending on the level of delensing that can be achieved with higher resolution maps from the South Pole Telescope., Comment: 15 pages, 13 figures

Published
2018

20. BICEP2/Keck Array VIII: Measurement of gravitational lensing from large-scaleb-mode polarization

Author

Toshiya Namikawa, Cora Dvorkin, Chao-Lin Kuo, E. Karpel, R. Schwarz, Keck Array, M. Lueker, James J. Bock, K. L. Thompson, Zeeshan Ahmed, Roger O'Brient, J. Kang, K. G. Megerian, J. P. Kaufman, J. E. Tolan, Mark Halpern, E. Bullock, Bicep Collaborations, Angiola Orlando, Jeffrey P. Filippini, Howard Hui, I. Buder, Jake Connors, Bryan Steinbach, H. T. Nguyen, E. M. Leitch, Calvin B. Netterfield, Sarah M. Harrison, Peter A. R. Ade, R. V. Sudiwala, Z. K. Staniszewski, R. Bowens-Rubin, Brian Keating, W. L. K. Wu, Steven J. Benton, R. W. Ogburn, Abigail G. Vieregg, S. Fliescher, J. Willmert, Kate D. Alexander, Gene C. Hilton, C. Pryke, L. Duband, Randol W. Aikin, Victor Buza, Donald V. Wiebe, S. R. Hildebrandt, C. D. Sheehy, Grant Teply, S. Kefeli, Colin A. Bischoff, C. L. Wong, A. D. Turner, S. Richter, J. A. Grayson, Justus A. Brevik, Carole Tucker, Ki Won Yoon, B. P. Crill, John M Kovac, Kirit Karkare, Kent D. Irwin, S. A. Kernasovskiy, A. C. Weber, and Denis Barkats

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Cosmic microwave background, Cosmic background radiation, Spectral density, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), 01 natural sciences, Cosmology, symbols.namesake, Amplitude, Gravitational lens, Space and Planetary Science, 0103 physical sciences, symbols, Planck, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present measurements of polarization lensing using the 150 GHz maps which include all data taken by the BICEP2 & Keck Array CMB polarization experiments up to and including the 2014 observing season (BK14). Despite their modest angular resolution ($\sim 0.5^\circ$), the excellent sensitivity ($\sim 3\mu$K-arcmin) of these maps makes it possible to directly reconstruct the lensing potential using only information at larger angular scales ($\ell\leq 700$). From the auto-spectrum of the reconstructed potential we measure an amplitude of the spectrum to be $A^{\phi\phi}_{\rm L}=1.15\pm 0.36$ (Planck $\Lambda$CDM prediction corresponds to $A^{\phi\phi}_{\rm L}=1$), and reject the no-lensing hypothesis at 5.8$\sigma$, which is the highest significance achieved to date using an EB lensing estimator. Taking the cross-spectrum of the reconstructed potential with the Planck 2015 lensing map yields $A^{\phi\phi}_{\rm L}=1.13\pm 0.20$. These direct measurements of $A^{\phi\phi}_{\rm L}$ are consistent with the $\Lambda$CDM cosmology, and with that derived from the previously reported BK14 B-mode auto-spectrum ($A^{\rm BB}_{\rm L}=1.20\pm 0.17$). We perform a series of null tests and consistency checks to show that these results are robust against systematics and are insensitive to analysis choices. These results unambiguously demonstrate that the B-modes previously reported by BICEP / Keck at intermediate angular scales ($150\lesssim\ell\lesssim 350$) are dominated by gravitational lensing. The good agreement between the lensing amplitudes obtained from the lensing reconstruction and B-mode spectrum starts to place constraints on any alternative cosmological sources of B-modes at these angular scales., Comment: 12 pages, 8 figures

Published
2016

21. BICEP2/Keck Array XI: Beam Characterization and Temperature-to-Polarization Leakage in the BK15 Data Set

Author

Grant Teply, R. V. Sudiwala, Brian Keating, W. L. K. Wu, S. R. Hildebrandt, Howard Hui, S. A. Kernasovskiy, A. Wandui, S. Kefeli, Jeffrey P. Filippini, J. A. Grayson, D. V. Wiebe, Justus A. Brevik, Carole Tucker, King Tong Lau, John M Kovac, S. Palladino, Toshiya Namikawa, Tyler St. Germaine, Kirit Karkare, M. Lueker, Alessandro Schillaci, N. A. Larsen, Mark Halpern, Lionel Duband, Kent D. Irwin, H. Yang, C. D. Sheehy, Chao-Lin Kuo, J. Willmert, Gene C. Hilton, J. Cornelison, J. E. Tolan, Ki Won Yoon, Calvin B. Netterfield, Stefan Richter, Zeeshan Ahmed, A. C. Weber, R. Bowens-Rubin, B. P. Crill, S. Fliescher, Jake Connors, M. Crumrine, G. Hall, Steven J. Benton, R. W. Ogburn, Ahmed Soliman, C. Umilta, Colin A. Bischoff, J. J. Bock, J. Kang, C. Pryke, Peter A. R. Ade, Lorenzo Moncelsi, Denis Barkats, Chao Zhang, B. Racine, C. L. Wong, J. P. Kaufman, R. Schwarz, Abigail G. Vieregg, A. D. Turner, Randol W. Aikin, H. T. Nguyen, Victor Buza, E. M. Leitch, E. Bullock, E. Karpel, K. L. Thompson, Z. K. Staniszewski, Roger O'Brient, Marion Dierickx, I. Buder, Bryan Steinbach, Sarah M. Harrison, K. G. Megerian, Service des Basses Températures (SBT ), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), BICEP2, Keck Array, Institut Nanosciences et Cryogénie (INAC), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)

Subjects
Planck, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, scalar tensor, Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], inflation, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Leakage (electronics), Physics, Gravitational wave, Astrophysics::Instrumentation and Methods for Astrophysics, temperature, Astronomy and Astrophysics, BICEP, sensitivity, Polarization (waves), CMB cold spot, Computational physics, B-mode, WMAP, Space and Planetary Science, symbols, beam profile, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, statistical, Beam (structure), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Precision measurements of cosmic microwave background (CMB) polarization require extreme control of instrumental systematics. In a companion paper we have presented cosmological constraints from observations with the BICEP2 and Keck Array experiments up to and including the 2015 observing season (BK15), resulting in the deepest CMB polarization maps to date and a statistical sensitivity to the tensor-to-scalar ratio of $\sigma(r) = 0.020$. In this work we characterize the beams and constrain potential systematic contamination from main beam shape mismatch at the three BK15 frequencies (95, 150, and 220 GHz). Far-field maps of 7,360 distinct beam patterns taken from 2010-2015 are used to measure differential beam parameters and predict the contribution of temperature-to-polarization leakage to the BK15 B-mode maps. In the multifrequency, multicomponent likelihood analysis that uses BK15, Planck, and WMAP maps to separate sky components, we find that adding this predicted leakage to simulations induces a bias of $\Delta r = 0.0027 \pm 0.0019$. Future results using higher-quality beam maps and improved techniques to detect such leakage in CMB data will substantially reduce this uncertainty, enabling the levels of systematics control needed for BICEP Array and other experiments that plan to definitively probe large-field inflation., Comment: 18 pages, 9 figures, 4 tables. Minor correction to Figure 2 and caption

Published
2019

22. BICEP3 performance overview and planned Keck Array upgrade

Author

Z. Ahmed, S. A. Kernasovskiy, Mark Halpern, J. E. Tolan, Roger O'Brient, A. D. Turner, Howard Hui, R. Bowens-Rubin, K. W. Yoon, E. Karpel, K. L. Thompson, Victor Buza, Jake Connors, C. L. Kuo, J. Kang, Sarah M. Harrison, A. C. Weber, Kate D. Alexander, V. Monticue, I. Buder, C. Pryke, R. Schwarz, R. W. Ogburn, Bryan Steinbach, M. Amiri, D. V. Wiebe, Calvin B. Netterfield, C. D. Reintsema, James J. Bock, Stefan Richter, M. Lueker, John M Kovac, Kirit Karkare, J. Willmert, Gene C. Hilton, E. Bullock, V. V. Hristov, H. T. Nguyen, Kent D. Irwin, H. Boenish, E. M. Leitch, Denis Barkats, J. A. Grayson, Grant Teply, K. G. Megerian, S. J. Benton, Jeffrey P. Filippini, S. Kefeli, S. Fliescher, Carole Tucker, Z. Staniszewski, W. L. K. Wu, T. Namikawa, C. Sorensen, A. Wandui, Colin A. Bischoff, C. D. Sheehy, Peter A. R. Ade, Abigail G. Vieregg, Holland, Wayne S., and Zmuidzinas, Jonas

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Computer science, business.industry, Detector, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), 7. Clean energy, 01 natural sciences, Cardinal point, Upgrade, Optics, Frequency coverage, Refracting telescope, 0103 physical sciences, 010306 general physics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Transition edge, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

BICEP3 is a 520 mm aperture, compact two-lens refractor designed to observe the polarization of the cosmic microwave background (CMB) at 95 GHz. Its focal plane consists of modularized tiles of antenna-coupled transition edge sensors (TESs), similar to those used in BICEP2 and the Keck Array. The increased per-receiver optical throughput compared to BICEP2/Keck Array, due to both its faster f/1.7 optics and the larger aperture, more than doubles the combined mapping speed of the BICEP/Keck program. The BICEP3 receiver was recently upgraded to a full complement of 20 tiles of detectors (2560 TESs) and is now beginning its second year of observation (and first science season) at the South Pole. We report on its current performance and observing plans. Given its high per-receiver throughput while maintaining the advantages of a compact design, BICEP3-class receivers are ideally suited as building blocks for a 3rd-generation CMB experiment, consisting of multiple receivers spanning 35 GHz to 270 GHz with total detector count in the tens of thousands. We present plans for such an array, the new "BICEP Array" that will replace the Keck Array at the South Pole, including design optimization, frequency coverage, and deployment/observing strategies., 17 pages, 6 figures. To be published in Proc. SPIE. Presented at SPIE Astronomical Telescopes and Instrumentation Conference 9914: Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII, June 2016

Published
2016

23. Optical Characterization of the BICEP3 CMB Polarimeter at the South Pole

Author

M. Lueker, John M Kovac, Kirit Karkare, Kent D. Irwin, Roger O'Brient, H. Boenish, J. Kang, S. Fliescher, K. G. Megerian, J. A. Grayson, Toshiya Namikawa, S. Kefeli, Ki Won Yoon, S. A. Harrison, Colin A. Bischoff, Chao-Lin Kuo, Carole Tucker, I. Buder, James J. Bock, C. L. Wong, Bryan Steinbach, J. Willmert, Gene C. Hilton, Viktor Hristov, Denis Barkats, V. Monticue, Howard Hui, W. L. K. Wu, Zeeshan Ahmed, A. D. Turner, E. Karpel, Jeffrey P. Filippini, Carl D. Reintsema, K. L. Thompson, Mandana Amiri, Peter A. R. Ade, Abigail G. Vieregg, Z. K. Staniszewski, M. T. St. Germaine, C. D. Sheehy, A. C. Weber, Calvin B. Netterfield, Victor Buza, S. A. Kernasovskiy, R. Bowens-Rubin, Kate D. Alexander, C. Pryke, A. Wandui, H. T. Nguyen, E. M. Leitch, S. J. Benton, S. Richter, Mark Halpern, R. Schwarz, E. Bullock, J. E. Tolan, Jake Connors, R. W. Ogburn, Grant Teply, Holland, Wayne S., and Zmuidzinas, Jonas

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Gravitational wave, business.industry, Cosmic microwave background, Cosmic background radiation, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Near and far field, Polarimeter, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), 01 natural sciences, law.invention, Telescope, Beamwidth, Optics, law, 0103 physical sciences, 010306 general physics, business, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

BICEP3 is a small-aperture refracting cosmic microwave background (CMB) telescope designed to make sensitive polarization maps in pursuit of a potential B-mode signal from inflationary gravitational waves. It is the latest in the BICEP/Keck Array series of CMB experiments at the South Pole, which has provided the most stringent constraints on inflation to date. For the 2016 observing season, BICEP3 was outfitted with a full suite of 2400 optically coupled detectors operating at 95 GHz. In these proceedings we report on the far field beam performance using calibration data taken during the 2015-2016 summer deployment season in situ with a thermal chopped source. We generate high-fidelity per-detector beam maps, show the array-averaged beam profile, and characterize the differential beam response between co-located, orthogonally polarized detectors which contributes to the leading instrumental systematic in pair differencing experiments. We find that the levels of differential pointing, beamwidth, and ellipticity are similar to or lower than those measured for BICEP2 and Keck Array. The magnitude and distribution of BICEP3's differential beam mismatch - and the level to which temperature-to-polarization leakage may be marginalized over or subtracted in analysis - will inform the design of next-generation CMB experiments with many thousands of detectors., Comment: 17 pages, 9 figures. Presented at SPIE Astronomical Telescopes and Instrumentation Conference 9914: Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII, June 2016

Published
2016
Full Text
View/download PDF

24. Initial Performance of BICEP3: A Degree Angular Scale 95 GHz Band Polarimeter

Author

S. Kefeli, H. T. Nguyen, E. Bullock, Sarah M. Harrison, S. J. Benton, J. E. Tolan, M. Amiri, Roger O'Brient, S. Fliescher, Jake Connors, Peter A. R. Ade, I. Buder, John M Kovac, Gene C. Hilton, Kirit Karkare, Abigail G. Vieregg, Keith L. Thompson, R. W. Ogburn, Howard Hui, Carl D. Reintsema, K. G. Megerian, Kent D. Irwin, J. A. Grayson, A. C. Weber, Victor Buza, S. A. Kernasovskiy, Chao-Lin Kuo, Carole Tucker, Z. K. Staniszewski, A. D. Turner, James J. Bock, Mark Halpern, Grant Teply, Colin A. Bischoff, Bryan Steinbach, Ki Won Yoon, W. L. K. Wu, Zeeshan Ahmed, Denis Barkats, C. Sorensen, J. Willmert, Donald V. Wiebe, S. Richter, R. Bowens-Rubin, Kate D. Alexander, Jeffrey P. Filippini, J. Kang, Viktor Hristov, Rashmikant V. Sudiwala, C. Pryke, E. Karpel, and Calvin B. Netterfield

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, law.invention, Telescope, symbols.namesake, Materials Science(all), law, 0103 physical sciences, General Materials Science, Planck, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), QC, Astrophysics::Galaxy Astrophysics, Physics, Pixel, 010308 nuclear & particles physics, Gravitational wave, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Polarimeter, Condensed Matter Physics, Polarization (waves), Atomic and Molecular Physics, and Optics, symbols, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

BICEP3 is a $550~mm$ aperture telescope with cold, on-axis, refractive optics designed to observe at the $95~GHz$ band from the South Pole. It is the newest member of the BICEP/Keck family of inflationary probes specifically designed to measure the polarization of the cosmic microwave background (CMB) at degree-angular scales. BICEP3 is designed to house 1280 dual-polarization pixels, which, when fully-populated, totals to $\sim$9$\times$ the number of pixels in a single Keck $95~GHz$ receiver, thus further advancing the BICEP/Keck program's $95~GHz$ mapping speed. BICEP3 was deployed during the austral summer of 2014-2015 with 9 detector tiles, to be increased to its full capacity of 20 in the second season. After instrument characterization measurements were taken, CMB observation commenced in April 2015. Together with multi-frequency observation data from Planck, BICEP2, and the Keck Array, BICEP3 is projected to set upper limits on the tensor-to-scalar ratio to $r$ $\lesssim 0.03$ at $95\%$ C.L.., 7 pages, LTD-16 proceedings

Published
2016

25. BICEP3 focal plane design and detector performance

Author

Peter A. R. Ade, Ki Won Yoon, Abigail G. Vieregg, Bryan Steinbach, J. Kang, S. Fliescher, M. Lueker, Gene C. Hilton, John M Kovac, Kirit Karkare, Viktor Hristov, W. L. K. Wu, Zeeshan Ahmed, I. Buder, Kent D. Irwin, Victor Buza, Roger O'Brient, V. Monticue, C. D. Sheehy, E. Bullock, S. A. Kernasovskiy, Sarah M. Harrison, Keith L. Thompson, E. Karpel, Carl D. Reintsema, Z. K. Staniszewski, Calvin B. Netterfield, R. Schwarz, J. A. Grayson, H. Boenish, K. G. Megerian, Carole Tucker, Jeffrey P. Filippini, E. M. Leitch, Denis Barkats, S. Kefeli, C. Sorensen, A. C. Weber, Colin A. Bischoff, S. Richter, G. P. Teply, J. Willmert, J. E. Tolan, Donald V. Wiebe, Jake Connors, Steven J. Benton, R. W. Ogburn, Anthony D. Turner, R. Bowens-Rubin, Toshiya Namikawa, Chao-Lin Kuo, James J. Bock, Howard Hui, Mandana Amiri, A. Wandui, H. T. Nguyen, Mark Halpern, Kate D. Alexander, C. Pryke, Holland, Wayne S., and Zmuidzinas, Jonas

Subjects
Cosmic microwave background, Spectral response, FOS: Physical sciences, 02 engineering and technology, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, law.invention, Telescope, Optics, law, 0103 physical sciences, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Optical efficiency, Physics, business.industry, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, 021001 nanoscience & nanotechnology, Polarization (waves), Cardinal point, Refracting telescope, Astrophysics - Instrumentation and Methods for Astrophysics, 0210 nano-technology, business
Abstract

BICEP3, the latest telescope in the BICEP/Keck program, started science observations in March 2016. It is a 550mm aperture refractive telescope observing the polarization of the cosmic microwave background at 95 GHz. We show the focal plane design and detector performance, including spectral response, optical efficiency and preliminary sensitivity of the upgraded BICEP3. We demonstrate 9.72$\mu$K$\sqrt{\textrm{s}}$ noise performance of the BICEP3 receiver., Comment: 11 pages, 10 figures. To be published in Proc. SPIE. Presented at SPIE Astronomical Telescopes and Instrumentation Conference 9914: Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII, June 2016

Published
2016
Full Text
View/download PDF

26. BICEP2/Keck Array V: Measurements of B-mode Polarization at Degree Angular Scales and 150 GHz by the Keck Array

Author

L. Duband, Roger O'Brient, Brian Keating, Grant Teply, J. Willmert, Victor Buza, Gene C. Hilton, S. A. Kernasovskiy, John M Kovac, Kirit Karkare, A. C. Weber, Bicep, Zeeshan Ahmed, S. R. Hildebrandt, Kent D. Irwin, E. M. Leitch, C. D. Sheehy, M. Lueker, Colin A. Bischoff, Jeffrey P. Filippini, Denis Barkats, J. E. Tolan, J. P. Kaufman, Jake Connors, A. Orlando, I. Buder, S. Fliescher, Cora Dvorkin, Ki Won Yoon, Z. K. Staniszewski, Justus A. Brevik, K. G. Megerian, B. P. Crill, R. W. Ogburn, R. Schwarz, A. D. Turner, C. L. Wong, R. Sudiwala, Howard Hui, Matthew Hasselfield, K. L. Thompson, Sunil Golwala, Peter A. R. Ade, E. Bullock, Abigail G. Vieregg, Randol W. Aikin, Viktor Hristov, Peter Mason, Kate D. Alexander, C. Pryke, Keck Array Collaborations, S. Kefeli, Calvin B. Netterfield, H. T. Nguyen, C. D. Dowell, S. J. Benton, S. Richter, Carl D. Reintsema, Chao-Lin Kuo, James J. Bock, and Mark Halpern

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Frequency band, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Polarization (waves), 01 natural sciences, Power over, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Keck Array is a system of cosmic microwave background (CMB) polarimeters, each similar to the BICEP2 experiment. In this paper we report results from the 2012 and 2013 observing seasons, during which the Keck Array consisted of five receivers all operating in the same (150 GHz) frequency band and observing field as BICEP2. We again find an excess of B-mode power over the lensed-$\Lambda$CDM expectation of $> 5 \sigma$ in the range $30 < \ell < 150$ and confirm that this is not due to systematics using jackknife tests and simulations based on detailed calibration measurements. In map difference and spectral difference tests these new data are shown to be consistent with BICEP2. Finally, we combine the maps from the two experiments to produce final Q and U maps which have a depth of 57 nK deg (3.4 $\mu$K arcmin) over an effective area of 400 deg$^2$ for an equivalent survey weight of 250,000 $\mu$K$^{-2}$. The final BB band powers have noise uncertainty a factor of 2.3 times better than the previous results, and a significance of detection of excess power of $> 6\sigma$., Comment: 13 pages, 9 figures

Published
2015

27. Joint analysis of BICEP2/Keck array and planck data

Author

K. Ganga, N. Krachmalnicoff, Olivier Doré, W. A. Holmes, M. Lueker, Jose M. Diego, A. Mennella, Nabila Aghanim, Ben Rusholme, F. Elsner, Reijo Keskitalo, C. L. Wong, L. Toffolatti, H. T. Nguyen, J. Jewell, Federico Nati, Valeria Pettorino, Davide Maino, S. J. Benton, Anthony Lasenby, Jacques Delabrouille, Luca Terenzi, C. Combet, F. Piacentini, Simon D. M. White, J. A. Murphy, J. E. Tolan, W. Hovest, Cora Dvorkin, Fabio Finelli, R. Schwarz, M. Frailis, P. B. Lilje, Carlo Baccigalupi, James G. Bartlett, A. Mangilli, Jussi-Pekka Väliviita, F. Pasian, Alessandro Gruppuso, Sunil Golwala, E. Bullock, Guilaine Lagache, François Levrier, E. Hivon, E. Keihänen, M. Rowan-Robinson, G. Patanchon, F. Couchot, L. P. L. Colombo, Dmitry Novikov, Jake Connors, Antony Lewis, M. Tomasi, M. López-Caniego, George Helou, François R. Bouchet, L. A. Wade, Daniela Paoletti, Dipak Munshi, George Efstathiou, Jean-François Cardoso, Ingunn Kathrine Wehus, Marco Bersanelli, J.-F. Sygnet, E. Martínez-González, Etienne Pointecouteau, Charles R. Lawrence, A. D. Turner, J. Aumont, D. Herranz, R. W. Ogburn, J.-M. Lamarre, M. Tucci, Rafael Rebolo, A. C. Weber, Kevin M. Huffenberger, D. Yvon, Roger O'Brient, M. Piat, O. Perdereau, Alain Benoit, Planck Collaborations, Luca Valenziano, Massimiliano Lattanzi, Mark Halpern, Zeeshan Ahmed, S. R. Hildebrandt, E. M. Leitch, A. de Rosa, R. Sudiwala, Mika Juvela, C. Renault, Kate D. Alexander, N. Ponthieu, Alessandro Melchiorri, D. Santos, Hannu Kurki-Suonio, A. Ducout, Stéphane Plaszczynski, Marian Douspis, Daniel J. Mortlock, Fabrizio Villa, Luigi Danese, C. D. Sheehy, Carlo Burigana, G. Hurier, C. Pryke, M. Rossetti, Olivier Forni, L. Montier, M. Tristram, K. L. Thompson, Davide Pietrobon, Lloyd Knox, M.-A. Miville-Deschênes, R. Kneissl, Jörg P. Rachen, Pavel Naselsky, Colin A. Bischoff, R. J. Davis, Locke D. Spencer, Silvia Masi, Andrea Zacchei, W. C. Jones, Bicep, Michael Seiffert, G. Polenta, M. Linden-Vørnle, Duncan Hanson, R. C. Butler, Theodore Kisner, L. Perotto, F. K. Hansen, Bruce Partridge, F. Boulanger, J.-P. Bernard, William T. Reach, F. Noviello, D. L. Harrison, S. Donzelli, A. Renzi, J.-M. Delouis, J.-L. Puget, G. Roudier, Michele Liguori, A. Curto, S. Fliescher, J. F. Macías-Pérez, M. Maris, V. Stolyarov, H. K. Eriksen, Bruno Maffei, E. Franceschi, Benjamin D. Wandelt, Julian Borrill, Jeffrey P. Filippini, R. B. Barreiro, Calvin B. Netterfield, Graca Rocha, Roberta Paladini, T. J. Pearson, P. Vielva, S. Richter, Viktor Hristov, Grant Teply, L. Duband, Giorgio Savini, Michael P. Hobson, F. Pajot, Martin Kunz, A. Catalano, Laura Bonavera, R. A. Sunyaev, A. A. Fraisse, Justus A. Brevik, Mathieu Remazeilles, D. Sutton, Erminia Calabrese, Howard Hui, C. D. Dowell, Anne Lähteenmäki, Ranga-Ram Chary, J. Willmert, Anthony Challinor, M. Sandri, Jon E. Gudmundsson, L. Pagano, Robert A. Watson, L. Mendes, Sabino Matarrese, Victor Buza, A. Karakci, N. Mandolesi, K. G. Megerian, S. Galeotta, J. Knoche, Andrew H. Jaffe, A. Moneti, Simon Prunet, Gene C. Hilton, I. D. Novikov, I. Buder, Philip Lubin, S. A. Kernasovskiy, Peter G. Martin, P. Bielewicz, Jo Dunkley, H. Dole, Subhabrata Mitra, J. A. Tauber, M. Savelainen, L. Vibert, X. Dupac, Brian Keating, Adam Moss, P. de Bernardis, R. D. Davies, Denis Barkats, M. Reinecke, Peter Mason, K. Benabed, Nicola Bartolo, A.-S. Suur-Uski, Martin White, M. Bucher, Douglas Scott, Z. K. Staniszewski, J. R. Bond, E. Gjerløw, Andrea Zonca, Clive Dickinson, Krzysztof M. Gorski, A. Gregorio, H. C. Chiang, P. R. Christensen, E. Battaner, Chao-Lin Kuo, F. Cuttaia, Torsten A. Enßlin, James J. Bock, I. Ristorcelli, Anna Bonaldi, E. Falgarone, Monique Arnaud, Peter Meinhold, Serge Gratton, S. Kefeli, F.-X. Désert, J. González-Nuevo, J. P. Kaufman, Tuhin Ghosh, B. Van Tent, Hans Ulrik Nørgaard-Nielsen, A. J. Banday, Sophie Henrot-Versille, Paolo Natoli, John M Kovac, Kirit Karkare, A. Coulais, Kent D. Irwin, Jose Alberto Rubino-Martin, G. de Zotti, Ki Won Yoon, A. Benoit-Lévy, M. Giard, B. P. Crill, A. Frejsel, Matthew Hasselfield, T. R. Jaffe, M. Migliaccio, Peter A. R. Ade, Abigail G. Vieregg, Randol W. Aikin, R. Leonardi, A. Orlando, S. Galli, G. W. Pratt, Gianluca Morgante, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies (SISSA / ISAS), Joint ALMA Observatory (JAO), National Radio Astronomy Observatory (NRAO)-European Southern Observatory (ESO), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), INO-CNR BEC Center and Dipartimento di Fisica, Università degli Studi di Trento (UNITN), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut für Planetologie [Münster], Westfälische Wilhelms-Universität Münster (WWU), ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), SCANCO Medical AG, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Institute for Climate and Atmospheric Science [Leeds] (ICAS), School of Earth and Environment [Leeds] (SEE), University of Leeds-University of Leeds, Dipartimento di Ingegneria Meccanica-Settore Materiali, Universita degli Studi di Padova, Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Dipartimento di Fisica, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], AUTRES, Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Service des Basses Températures (SBT ), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Laboratoire de Génie Electrique de Grenoble (G2ELab), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Agence nationale de sécurité sanitaire de l'alimentation, de l'environnement et du travail (ANSES), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Istituto Nazionale di Astrofisica (INAF), Department of Physics and Astronomy [Vancouver], University of British Columbia (UBC), National Center for Atmospheric Research [Boulder] (NCAR), Queens Med Res Inst, Div Pathol, Univ Edinburgh, Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH), Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies (UMR 6174) (FEMTO-ST), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, International Center for Relativistic Astrophysics (ICRA), Università degli Studi di Roma, School of Physics and Astronomy, University of Manchester [Manchester], Laboratory for Experimental Medicine and Endocrinology, Catholic University of Leuven (LEGENDO), Université Catholique de Louvain = Catholic University of Louvain (UCL), Dipartimento di Fisica, Universita` di Roma Tor Vergata, Università degli Studi di Roma Tor Vergata [Roma], Istituto Nazionale di Fisica Nucleare, Sezione di Padova (INFN, Sezione di Padova), Istituto Nazionale di Fisica Nucleare (INFN), Astrophysics Group, Blackett Laboratory, Imperial College London-Imperial College London, School of Social and Community Medicine [Bristol], University of Bristol [Bristol], Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), National High Magnetic Field Laboratory (NHMFL), Florida State University [Tallahassee] (FSU), Département de Physique des Particules (ex SPP) (DPP), BICEPS2/Keck Array, Planck, Anne Lähteenmäki Group, Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, R, P, Aghanim, N, Ahmed, Z, Aikin, R, Alexander, K, Arnaud, M, Aumont, J, Baccigalupi, C, Banday, A, Barkats, D, Barreiro, R, Bartlett, J, Bartolo, N, Battaner, E, Benabed, K, Benoit, A, Benoit Levy, A, Benton, S, Bernard, J, Bersanelli, M, Bielewicz, P, Bischoff, C, Bock, J, Bonaldi, A, Bonavera, L, Bond, J, Borrill, J, Bouchet, F, Boulanger, F, Brevik, J, Bucher, M, Buder, I, Bullock, E, Burigana, C, Butler, R, Buza, V, Calabrese, E, Cardoso, J, Catalano, A, Challinor, A, Chary, R, Chiang, H, Christensen, P, L, ., Combet, C, Connors, J, Couchot, F, Coulais, A, Crill, B, Curto, A, Cuttaia, F, Danese, L, Davies, R, Davis, R, DE BERNARDIS, P, Rosa, A, Zotti, G, Delabrouille, J, Delouis, J, Desert, F, Dickinson, C, Diego, J, Dole, H, Donzelli, S, Dore, O, Douspis, M, Dowell, C, Duband, L, Ducout, A, Dunkley, J, Dupac, X, Dvorkin, C, Efstathiou, G, Elsner, F, Ensslin, T, Eriksen, H, Falgarone, E, Filippini, J, Finelli, F, Fliescher, S, Forni, O, Frailis, M, Fraisse, A, Franceschi, E, Frejsel, A, Galeotta, S, Galli, S, Ganga, K, Ghosh, T, Giard, M, Gjerlow, E, Golwala, S, Gonzalez Nuevo, J, Gorski, K, Gratton, S, Gregorio, A, Gruppuso, A, Gudmundsson, J, Halpern, M, Hansen, F, Hanson, D, Harrison, D, Hasselfield, M, Helou, G, Henrot Versillee, S, Herranz, D, Hildebrandt, S, Hilton, G, Hivon, E, Hobson, M, Holmes, W, Hovest, W, Hristov, V, Huffenberger, K, Hui, H, Hurier, G, Irwin, K, Jaffe, A, Jaffe, T, Jewell, J, Jones, W, Juvela, M, Karakci, A, Karkare, K, Kaufman, J, Keating, B, Kefeli, S, Keihanen, E, Kernasovskiy, S, Keskitalo, R, Kisner, T, Kneissl, R, Knoche, J, Knox, L, Kovac, J, Krachmalnicoff, N, Kunz, M, Kuo, C, Kurki Suonio, H, Lagache, G, Lahteenmaki, A, Lamarre, J, Lasenby, A, Lattanzi, M, Lawrence, C, Leitch, E, Leonardi, R, Levrier, F, Lewis, A, Liguori, M, Lilje, P, Linden Vornle, M, Lopez Caniego, M, Lubin, P, Lueker, M, Macias Perez, J, Maffei, B, Maino, D, Mandolesi, N, Mangilli, A, Maris, M, Martin, P, Martinez Gonzalez, E, Masi, S, Mason, P, Matarrese, S, Megerian, K, Meinhold, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Mitra, S, Miville Deschenes, M, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Moss, A, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Netterfield, C, Nguyen, H, Norgaard Nielsen, H, Noviello, F, Novikov, D, Novikov, I, O'Brient, R, Ogburn, R, Orlando, A, Pagano, L, Pajot, F, Paladini, R, Paoletti, D, Partridge, B, Pasian, F, Patanchon, G, Pearson, T, Perdereau, O, Perotto, L, Pettorino, V, Piacentini, F, Piat, M, Pietrobon, D, Plaszczynski, S, Pointecouteau, E, Polenta, G, Ponthieu, N, Pratt, G, Prunet, S, Pryke, C, Puget, J, Rachen, J, Reach, W, Rebolo, R, Reinecke, M, Remazeilles, M, Renault, C, Renzi, A, Richter, S, Ristorcelli, I, Rocha, G, Rossetti, M, Roudier, G, Rowan Robinson, M, Rubino Martin, J, Rusholme, B, Sandri, M, Santos, D, Savelainen, M, Savini, G, Schwarz, R, Scott, D, Seiffert, M, Sheehy, C, Spencer, L, Staniszewski, Z, Stolyarov, V, Sudiwala, R, Sunyaev, R, Sutton, D, Suur Uski, A, Sygnet, J, Tauber, J, Teply, G, Terenzi, L, Thompson, K, Toffolatti, L, Tolan, J, Tomasi, M, Tristram, M, Tucci, M, Turner, A, Valenziano, L, Valiviita, J, Tent, B, Vibert, L, Vielva, P, Vieregg, A, Villa, F, Wade, L, Wandelt, B, Watson, R, Weber, A, Wehus, I, White, M, M, S, Willmert, J, Wong, C, Yoon, K, Yvon, D, Zacchei, A, Zonca, A, Bicep, K, Planck, C, Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Département d'Astrophysique (ex SAP) ( DAP ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies ( SISSA / ISAS ), Joint ALMA Observatory, Physique Corpusculaire et Cosmologie - Collège de France ( PCC ), Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Università di Trento, Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), HELFA - Hélium : du fondamental aux applications, Institut Néel ( NEEL ), Université Grenoble Alpes [Saint Martin d'Hères]-Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes [Saint Martin d'Hères]-Centre National de la Recherche Scientifique ( CNRS ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Westfälische Wilhelms-Universität Münster ( WWU ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), ONERA - The French Aerospace Lab ( Chatillon ), ONERA, Laboratoire de Physique Subatomique et de Cosmologie ( LPSC ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut polytechnique de Grenoble - Grenoble Institute of Technology ( Grenoble INP ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ), Institute for Climate and Atmospheric Science [Leeds] ( ICAS ), University of Leeds, Universita degli Studi di Padova = University of Padua = Université de Padoue, Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique ( LERMA ), École normale supérieure - Paris ( ENS Paris ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Cergy Pontoise ( UCP ), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique ( CNRS ), Università degli Studi di Roma 'La Sapienza' [Rome], APC - Gravitation ( APC-Gravitation ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale ( LCCS ), Service des Basses Températures ( SBT - UMR 9004 ), Institut Nanosciences et Cryogénie ( INAC ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Grenoble Alpes ( UGA ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Grenoble Alpes ( UGA ) -Institut Nanosciences et Cryogénie ( INAC ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Grenoble Alpes ( UGA ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Grenoble Alpes ( UGA ), Centre d'étude spatiale des rayonnements ( CESR ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Génie Electrique de Grenoble ( G2ELab ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut polytechnique de Grenoble - Grenoble Institute of Technology ( Grenoble INP ) -Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ), Agence Nationale de Sécurité Sanitaire de l’Alimentation, de l’Environnement et du Travail ( ANSES Maisons-Alfort ), APC - Cosmologie, Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire de Paris-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna ( IASF-Bo ), Istituto Nazionale di Astrofisica ( INAF ), Department of Physics and Astronomy, University of British Columbia ( UBC ), National Center for Atmospheric Research [Boulder] ( NCAR ), Infrared Processing and Analysis Center ( IPAC ), California Institute of Technology ( CALTECH ), Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies ( FEMTO-ST ), Université de Technologie de Belfort-Montbeliard ( UTBM ) -Ecole Nationale Supérieure de Mécanique et des Microtechniques ( ENSMM ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Franche-Comté ( UFC ), Max-Planck-Institut für Astronomie ( MPIA ), International Center for Relativistic Astrophysics ( ICRA ), Laboratory for Experimental Medicine and Endocrinology, Catholic University of Leuven ( LEGENDO ), Université Catholique de Louvain ( UCL ), Università degli studi di Roma II, Istituto Nazionale di Fisica Nucleare, Sezione di Padova ( INFN, Sezione di Padova ), National Institute for Nuclear Physics ( INFN ), Antarctic Research a European Network for Astrophysics ( ARENA ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Laboratoire de Physique Théorique d'Orsay [Orsay] ( LPT ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), National High Magnetic Field Laboratory ( NHMFL ), Florida State University, Département de Physique des Particules (ex SPP) ( DPP ), National Science Foundation (US), European Research Council, Ministerio de Economía y Competitividad (España), Junta de Andalucía, Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), European Southern Observatory (ESO)-National Radio Astronomy Observatory (NRAO), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Westfälische Wilhelms-Universität Münster = University of Münster (WWU), DAAA, ONERA, Université Paris-Saclay [Châtillon], ONERA-Université Paris-Saclay, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), LERMA Cergy (LERMA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), School of Physics and Astronomy [Manchester], Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Technologie de Belfort-Montbeliard (UTBM), Université Catholique de Louvain (UCL), National Institute for Nuclear Physics (INFN), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Ade, P. A. R., Aghanim, N., Ahmed, Z., Aikin, R. W., Alexander, K. D., Arnaud, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barkats, D., Barreiro, R. B., Bartlett, J. G., Bartolo, N., Battaner, E., Benabed, K., Benoît, A., Benoit Lévy, A., Benton, S. J., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bischoff, C. A., Bock, J. J., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Brevik, J. A., Bucher, M., Buder, I., Bullock, E., Burigana, C., Butler, R. C., Buza, V., Calabrese, E., Cardoso, J. F., Catalano, A., Challinor, A., Chary, R. R., Chiang, H. C., Christensen, P. R., Colombo, L. P. L., Combet, C., Connors, J., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Delouis, J. M., Désert, F. X., Dickinson, C., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Dowell, C. D., Duband, L., Ducout, A., Dunkley, J., Dupac, X., Dvorkin, C., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Filippini, J. P., Finelli, F., Fliescher, S., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Ghosh, T., Giard, M., Gjerløw, E., Golwala, S. R., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Gudmundsson, J. E., Halpern, M., Hansen, F. K., Hanson, D., Harrison, D. L., Hasselfield, M., Helou, G., Henrot Versillé, S., Herranz, D., Hildebrandt, S. R., Hilton, G. C., Hivon, E., Hobson, M., Holmes, W. A., Hovest, W., Hristov, V. V., Huffenberger, K. M., Hui, H., Hurier, G., Irwin, K. D., Jaffe, A. H., Jaffe, T. R., Jewell, J., Jones, W. C., Juvela, M., Karakci, A., Karkare, K. S., Kaufman, J. P., Keating, B. G., Kefeli, S., Keihänen, E., Kernasovskiy, S. A., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Knox, L., Kovac, J. M., Krachmalnicoff, N., Kunz, M., Kuo, C. L., Kurki Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leitch, E. M., Leonardi, R., Levrier, F., Lewis, A., Liguori, M., Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., Lueker, M., Macías Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez González, E., Masi, S., Mason, P., Matarrese, S., Megerian, K. G., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nguyen, H. T., Nørgaard Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., O'Brient, R., Ogburn, R. W., Orlando, A., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, T. J., Perdereau, O., Perotto, L., Pettorino, V., Piacentini, F., Piat, M., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Pratt, G. W., Prunet, S., Pryke, C., Puget, J. L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Richter, S., Ristorcelli, I., Rocha, G., Rossetti, M., Roudier, G., Rowan Robinson, M., Rubiño Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Savini, G., Schwarz, R., Scott, D., Seiffert, M. D., Sheehy, C. D., Spencer, L. D., Staniszewski, Z. K., Stolyarov, V., Sudiwala, R., Sunyaev, R., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Teply, G. P., Terenzi, L., Thompson, K. L., Toffolatti, L., Tolan, J. E., Tomasi, M., Tristram, M., Tucci, M., Turner, A. D., Valenziano, L., Valiviita, J., Van Tent, B., Vibert, L., Vielva, P., Vieregg, A. G., Villa, F., Wade, L. A., Wandelt, B. D., Watson, R., Weber, A. C., Wehus, I. K., White, M., White, S. D. M., Willmert, J., Wong, C. L., Yoon, K. W., Yvon, D., Zacchei, A., and Zonca, A.

Subjects
Observational cosmology, High Energy Physics - Theory, Background radiations, Gravitational wave detectors and experiments, Astronomy, General Physics and Astronomy, ComputingMilieux_LEGALASPECTSOFCOMPUTING, Astrophysics, 01 natural sciences, Spectral line, General Relativity and Quantum Cosmology, law.invention, High Energy Physics - Phenomenology (hep-ph), law, Spectral behaviors, probe wmap observations gravity-waves polarization anisotropy emission submillimeter spectrum scaledust Physics, 010303 astronomy & astrophysics, QC, ComputingMilieux_MISCELLANEOUS, media_common, QB, Physics, Power-spectra, Lower frequencies, ta213, CDM modeling, Cross correlations, Dust emission, Joint analysis, Model variation, Polarization (waves), Synchrotron, High Energy Physics - Phenomenology, symbols, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, ta221, Cosmic background radiation, ta1171, Radio microwave, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, [ PHYS.ASTR.CO ] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], NO, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Physics and Astronomy (all), Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Planck, ta216, Astrophysics::Galaxy Astrophysics, ta115, ta114, 010308 nuclear & particles physics, Gravitational wave, High Energy Physics - Theory (hep-th), Sky, [SDU]Sciences of the Universe [physics], Data_GENERAL
Abstract

We report the results of a joint analysis of data from BICEP2/Keck Array and Planck. BICEP2 and Keck Array have observed the same approximately 400 deg2 patch of sky centered on RA 0 h, Dec. −57.5°. The combined maps reach a depth of 57 nK deg in Stokes Q and U in a band centered at 150 GHz. Planck has observed the full sky in polarization at seven frequencies from 30 to 353 GHz, but much less deeply in any given region (1.2 μK deg in Q and U at 143 GHz). We detect 150×353 cross-correlation in B modes at high significance. We fit the single- and cross-frequency power spectra at frequencies ≥150 GHz to a lensed-ΛCDM model that includes dust and a possible contribution from inflationary gravitational waves (as parametrized by the tensor-to-scalar ratio r), using a prior on the frequency spectral behavior of polarized dust emission from previous Planck analysis of other regions of the sky. We find strong evidence for dust and no statistically significant evidence for tensor modes. We probe various model variations and extensions, including adding a synchrotron component in combination with lower frequency data, and find that these make little difference to the r constraint. Finally, we present an alternative analysis which is similar to a map-based cleaning of the dust contribution, and show that this gives similar constraints. The final result is expressed as a likelihood curve for r, and yields an upper limit r0.05, National Science Foundation (NSF) ANT-0742818 ANT-1044978 ANT-0742592 ANT-1110087, JPL Research and Technology Development Fund from the NASA 06-ARPA206-0040 10-SAT10-0017, National Science Foundation (NSF) ANT-1145172 ANT-1145143 ANT-1145248, Keck Foundation (Caltech), European Space Agency, Centre National D'etudes Spatiales, CNRS/INSU-IN2P3-INP (France), Italian Space Agency (ASI), Italian National Research Council, Istituto Nazionale Astrofisica (INAF), National Aeronautics & Space Administration (NASA), United States Department of Energy (DOE), Science & Technology Facilities Council (STFC), UKSA (UK), Consejo Superior de Investigaciones Cientificas (CSIC), MINECO (Spain), JA (Spain), RES (Spain), Finnish Funding Agency for Technology & Innovation (TEKES), AoF (Finland), CSC (Finland), Helmholtz Association, German Aerospace Centre (DLR), Max Planck Society, CSA (Canada), DTU Space (Denmark), SER/SSO (Switzerland), RCN (Norway), Science Foundation Ireland, Portuguese Foundation for Science and Technology, ERC (EU), European Union (EU), Science & Technology Facilities Council (STFC) ST/K00106X/1 ST/K001051/1 ST/K002805/1 ST/L000768/1 ST/K004131/1 ST/N001206/1 ST/K000985/1 ST/L000636/1 ST/K003674/1 ST/M007685/1 ST/L000393/1 ST/L000652/1, Villum Fonden 10056

Published
2015

28. Antenna-coupled TES bolometers used in BICEP2, Keck array, and SPIDER

Author

M. Lueker, Grant Teply, Sunil Golwala, E. Bullock, R. Schwarz, Howard Hui, H. T. Nguyen, Nuria Llombart, J. A. Bonetti, Roger O'Brient, Ki Won Yoon, C. L. Wong, S. J. Benton, I. Buder, Gene C. Hilton, R. S. Tucker, Mandana Amiri, Justus A. Brevik, A. C. Weber, Matthew Hasselfield, Colin A. Bischoff, W. C. Jones, Peter K. Day, Donald V. Wiebe, John M Kovac, A. D. Turner, Kirit Karkare, P. Wilson, Henry G. LeDuc, Kent D. Irwin, K. G. Megerian, E. M. Leitch, Goutam Chattopadhyay, Alexandra S. Rahlin, J. E. Tolan, Carl D. Reintsema, G. Davis, L. Duband, S. Richter, Jeffrey P. Filippini, Amy Trangsrud, R. W. Ogburn, S. A. Kernasovskiy, Chao-Lin Kuo, James J. Bock, R. Sudiwala, P. V. Mason, Z. K. Staniszewski, Marcus Runyan, Calvin B. Netterfield, Denis Barkats, C. D. Dowell, C. Pryke, J. P. Kaufman, Mark Halpern, S. Fliescher, Brian Keating, Jonas Zmuidzinas, S. Kefeli, Viktor Hristov, A. Orlando, S. R. Hildebrandt, C. D. Sheehy, Peter A. R. Ade, Lorenzo Moncelsi, Abigail G. Vieregg, and Randol W. Aikin

Subjects
Physics, Spider, business.industry, Detector, Cosmic microwave background, Bandwidth (signal processing), Bolometer, Polarimetry, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Spectral bands, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Multiplexing, law.invention, Optics, Space and Planetary Science, law, 0103 physical sciences, 010306 general physics, business, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

We have developed antenna-coupled transition-edge sensor (TES) bolometers for a wide range of cosmic microwave background (CMB) polarimetry experiments, including BICEP2, Keck Array, and the balloon borne SPIDER. These detectors have reached maturity and this paper reports on their design principles, overall performance, and key challenges associated with design and production. Our detector arrays repeatedly produce spectral bands with 20%-30% bandwidth at 95, 150, or 220~GHz. The integrated antenna arrays synthesize symmetric co-aligned beams with controlled side-lobe levels. Cross-polarized response on boresight is typically ~0.5%, consistent with cross-talk in our multiplexed readout system. End-to-end optical efficiencies in our cameras are routinely 35% or higher, with per detector sensitivities of NET~300 uKrts. Thanks to the scalability of this design, we have deployed 2560 detectors as 1280 matched pairs in Keck Array with a combined instantaneous sensitivity of ~9 uKrts, as measured directly from CMB maps in the 2013 season. Similar arrays have recently flown in the SPIDER instrument, and development of this technology is ongoing., Comment: 16 pgs, 20 figs

Published
2015
Full Text
View/download PDF

29. BICEP2/KECK ARRAY. VII. MATRIX BASEDE/BSEPARATION APPLIED TO BICEP2 AND THE KECK ARRAY

Author

Ki Won Yoon, Grant Teply, S. Fliescher, Z. K. Staniszewski, Roger O'Brient, Angiola Orlando, B. P. Crill, Howard Hui, R. V. Sudiwala, Calvin B. Netterfield, Donald V. Wiebe, J. E. Tolan, Brian Keating, W. L. K. Wu, Jake Connors, Steven J. Benton, S. R. Hildebrandt, R. W. Ogburn, C. L. Wong, John M Kovac, Kirit Karkare, J. Kang, H. T. Nguyen, J. Willmert, Kent D. Irwin, A. D. Turner, E. M. Leitch, S. A. Kernasovskiy, J. P. Kaufman, Lionel Duband, Gene C. Hilton, I. Buder, A. C. Weber, Victor Buza, Bryan Steinbach, R. Bowens-Rubin, Toshiya Namikawa, Colin A. Bischoff, J. A. Grayson, Kate D. Alexander, Jeffrey P. Filippini, Justus A. Brevik, C. Pryke, Chao-Lin Kuo, Carole Tucker, S. Richter, E. Karpel, James J. Bock, K. L. Thompson, Mark Halpern, C. D. Sheehy, Sarah M. Harrison, Denis Barkats, Zeeshan Ahmed, Cora Dvorkin, R. Schwarz, E. Bullock, S. Kefeli, Peter A. R. Ade, Abigail G. Vieregg, K. G. Megerian, Randol W. Aikin, and M. Lueker

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Pixel, Spatial filter, Linear polarization, media_common.quotation_subject, FOS: Physical sciences, Spherical harmonics, Astronomy and Astrophysics, Covariance, Polarization (waves), 01 natural sciences, Computational physics, Space and Planetary Science, Sky, 0103 physical sciences, Tensor, Astrophysics - Instrumentation and Methods for Astrophysics, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, media_common
Abstract

A linear polarization field on the sphere can be uniquely decomposed into an E-mode and a B-mode component. These two components are analytically defined in terms of spin-2 spherical harmonics. Maps that contain filtered modes on a partial sky can also be decomposed into E-mode and B-mode components. However, the lack of full sky information prevents orthogonally separating these components using spherical harmonics. In this paper, we present a technique for decomposing an incomplete map into E and B-mode components using E and B eigenmodes of the pixel covariance in the observed map. This method is found to orthogonally define E and B in the presence of both partial sky coverage and spatial filtering. This method has been applied to the BICEP2 and the Keck Array maps and results in reducing E to B leakage from LCDM E-modes to a level corresponding to a tensor-to-scalar ratio of $r, 21 pages, 23 figures, minor updates to reflect accepted version

Published
2016

30. High-sensitivity transition-edge-sensed bolometers: Improved speed and characterization with AC and DC bias.

Author

Foote, Logan, Audley, Michael D., Bradford, Charles, de Lange, Gert, Echternach, Pierre, Fixsen, Dale J., Hui, Howard, Kenyon, Matthew, Nguyen, Hien, O'Brient, Roger, Sharp, Elmer H., Staguhn, Johannes G., van der Kuur, Jan, and Zmuidzinas, Jonas

Subjects
BOLOMETERS, WHITE noise, PLASMA etching, HEAT capacity, SPEED
Abstract

We report on efforts to improve the speed of low-G far-infrared transition-edged-sensed bolometers. We use a fabrication process that does not require any dry etch steps to reduce heat capacity on the suspended device and measure a reduction in the detector time constant. However, we also measure an increase in the temperature-normalized thermal conductance (G) and a corresponding increase in the noise-equivalent power (NEP). We employ a new near-IR photon-noise technique using a near-IR laser to calibrate the frequency-domain multiplexed AC system and compare the results to a well-understood DC circuit. We measure an NEP white noise level of 0.8 aW/rtHz with a 1/f knee below 0.1 Hz and a time constant of 3.2 ms. [ABSTRACT FROM AUTHOR]

Published
2023
Full Text
View/download PDF

31. A novel method for the measurement of superconducting transmission lines at terahertz frequencies.

Author

Peng, Zhaohang, Fan, Bowen, Miao, Wei, Wang, Zheng, Ren, Yuan, Li, Jing, and Shi, Shengcai

Subjects
ELECTRIC lines, ASTRONOMICAL instruments, BANDPASS filters, PERMITTIVITY, ANTENNAS (Electronics), QUANTUM cascade lasers
Abstract

Characterizing the properties (e.g., effective dielectric constant εeff, attenuation constant α, and characteristic impedance Z0) of terahertz (THz) superconducting transmission lines is of particular interest in designing on-chip integrated THz bandpass filters, which are a critical component for THz astronomical instruments, such as multi-color camera and broadband imaging spectrometers. Here, we propose a novel method for the characterization of three parameters (εeff, α, and Z0) of THz superconducting transmission lines. This method measures the ratio of the THz signal powers through two different-length branches of the superconducting transmission line to be measured. In addition, only one measurement is required for an all-in-one device chip, including an antenna, a half-power divider, the superconducting transmission line to be measured, and two detectors. The key point is that the superconducting transmission line to be measured is impedance-mismatched with the two integrated detectors. The method is validated through simulation and measurement for superconducting coplanar waveguide transmission lines around 400 GHz. [ABSTRACT FROM AUTHOR]

Published
2023
Full Text
View/download PDF

32. Thermal kinetic inductance detectors for millimeter-wave detection.

Author

Wandui, Albert, Bock, James J., Frez, Clifford, Hollister, M., Minutolo, Lorenzo, Nguyen, Hien, Steinbach, Bryan, Turner, Anthony, Zmuidzinas, Jonas, and O'Brient, Roger

Subjects
THERMISTORS, QUALITY factor, DETECTORS, ELECTRIC inductance, RADIO frequency, HEAT capacity
Abstract

Thermal Kinetic-Inductance Detectors (TKIDs) combine the excellent noise performance of traditional bolometers with a radio frequency multiplexing architecture that enables the large detector counts needed for the next generation of millimeter-wave instruments. In this paper, we first discuss the expected noise sources in TKIDs and derive the limits where the phonon noise contribution dominates over the other detector noise terms: generation–recombination, amplifier, and two-level system noise. Second, we characterize aluminum TKIDs in a dark environment. We present measurements of TKID resonators with quality factors of about 10 5 at 80 mK. We also discuss the bolometer thermal conductance, heat capacity, and time constants. These were measured by the use of a resistor on the thermal island to excite the bolometers. These dark aluminum TKIDs demonstrate a noise equivalent power, NEP = 2 × 10 − 17 W / Hz , with a 1 / f knee at 0.1 Hz, which provides background noise limited performance for ground-based telescopes observing at 150 GHz. [ABSTRACT FROM AUTHOR]

Published
2020
Full Text
View/download PDF

33. SLAC microresonator RF (SMuRF) electronics: A tone-tracking readout system for superconducting microwave resonator arrays.

Author

Yu, Cyndia, Ahmed, Zeeshan, Frisch, Josef C., Henderson, Shawn W., Silva-Feaver, Max, Arnold, Kam, Brown, David, Connors, Jake, Cukierman, Ari J., D'Ewart, J. Mitch, Dober, Bradley J., Dusatko, John E., Haller, Gunther, Herbst, Ryan, Hilton, Gene C., Hubmayr, Johannes, Irwin, Kent D., Kuo, Chao-Lin, Mates, John A. B., and Ruckman, Larry

Subjects
SUPERCONDUCTING resonators, SUPERCONDUCTING quantum interference devices, COMPUTER firmware, DIGITAL control systems, PARTICLE physics, SENSOR arrays
Abstract

We describe the newest generation of the SLAC Microresonator RF (SMuRF) electronics, a warm digital control and readout system for microwave-frequency resonator-based cryogenic detector and multiplexer systems, such as microwave superconducting quantum interference device multiplexers (μmux) or microwave kinetic inductance detectors. Ultra-sensitive measurements in particle physics and astronomy increasingly rely on large arrays of cryogenic sensors, which in turn necessitate highly multiplexed readout and accompanying room-temperature electronics. Microwave-frequency resonators are a popular tool for cryogenic multiplexing, with the potential to multiplex thousands of detector channels on one readout line. The SMuRF system provides the capability for reading out up to 3328 channels across a 4–8 GHz bandwidth. Notably, the SMuRF system is unique in its implementation of a closed-loop tone-tracking algorithm that minimizes RF power transmitted to the cold amplifier, substantially relaxing system linearity requirements and effective noise from intermodulation products. Here, we present a description of the hardware, firmware, and software systems of the SMuRF electronics, comparing achieved performance with science-driven design requirements. In particular, we focus on the case of large-channel-count, low-bandwidth applications, but the system has been easily reconfigured for high-bandwidth applications. The system described here has been successfully deployed in lab settings and field sites around the world and is baselined for use on upcoming large-scale observatories. [ABSTRACT FROM AUTHOR]

Published
2023
Full Text
View/download PDF

34. Anti-reflection coated vacuum window for the Primordial Inflation Polarization ExploreR (PIPER) balloon-borne instrument.

Author

Datta, Rahul, Chuss, David T., Eimer, Joseph, Essinger-Hileman, Thomas, Gandilo, Natalie N., Helson, Kyle, Kogut, Alan J., Lowe, Luke, Mirel, Paul, Rostem, Karwan, Sagliocca, Marco, Sponseller, Danielle, Switzer, Eric R., Taraschi, Peter A., and Wollack, Edward J.

Subjects
OPTICAL instruments, OPTICAL measurements, COSMIC background radiation, ANTIREFLECTIVE coatings, OPTICAL elements, POLARIMETRY, TELESCOPES, OPTICAL polarization
Abstract

Measuring the faint polarization signal of the cosmic microwave background (CMB) not only requires high optical throughput and instrument sensitivity but also control over systematic effects. Polarimetric cameras or receivers used in this setting often employ dielectric vacuum windows, filters, or lenses to appropriately prepare light for detection by cooled sensor arrays. These elements in the optical chain are typically designed to minimize reflective losses and hence improve sensitivity while minimizing potential imaging artifacts such as glint and ghosting. The Primordial Inflation Polarization ExploreR (PIPER) is a balloon-borne instrument designed to measure the polarization of the CMB radiation at the largest angular scales and characterize astrophysical dust foregrounds. PIPER's twin telescopes and detector systems are submerged in an open-aperture liquid helium bucket dewar. A fused-silica window anti-reflection (AR) coated with polytetrafluoroethylene is installed on the vacuum cryostat that houses the cryogenic detector arrays. Light passes from the skyward portions of the telescope to the detector arrays through this window, which utilizes an indium seal to prevent superfluid helium leaks into the vacuum cryostat volume. The AR coating implemented reduces reflections from each interface to <1% compared to ∼10% from an uncoated window surface. The AR coating procedure and room temperature optical measurements of the window are presented. The indium vacuum sealing process is also described in detail, and test results characterizing its integrity to superfluid helium leaks are provided. [ABSTRACT FROM AUTHOR]

Published
2021
Full Text
View/download PDF

35. Superconducting On-chip Fourier Transform Spectrometer.

Author

Basu Thakur, R., Klimovich, N., Day, P. K., Shirokoff, E., Mauskopf, P. D., Faramarzi, F., and Barry, P. S.

Subjects
FOURIER transform spectrometers, ELECTRIC lines, SPECTROMETERS, THIN films, ELECTRIC inductance
Abstract

The kinetic inductance effect is strongly nonlinear with applied current in NbTiN, TiN and NbN thin films. This can be utilized to realize novel devices. We present results from transmission lines made with these materials, where DC (current) control is used to modulate the phase velocity thereby enabling on-chip spectrometers. Utility of such compact spectrometers is discussed, along with their natural connection with parametric amplifiers. [ABSTRACT FROM AUTHOR]

Published
2020
Full Text
View/download PDF

36. Suppression of radiation loss in high kinetic inductance superconducting co-planar waveguides.

Author

Hähnle, S., Marrewijk, N. v., Endo, A., Karatsu, K., Thoen, D. J., Murugesan, V., and Baselmans, J. J. A.

Subjects
ELECTRIC inductance, RADIATION, RADIATION sources, ELECTRIC lines, COPLANAR waveguides, RESONATORS, PLANAR waveguides
Abstract

We present a lab-on-chip technique to measure the very low losses in superconducting transmission lines at (sub-) mm wavelengths. The chips consist of a 100 nm-thick NbTiN Co-planar Waveguide (CPW) Fabry–Pérot (FP) resonator, coupled, on one side, to an antenna and, on the other side, to a Microwave Kinetic Inductance detector. Using a single frequency radiation source allows us to measure the frequency response of the FP around 350 GHz and deduce its losses. We show that the loss is dominated by radiation loss inside the CPW line that forms the FP and that it decreases with the decreasing linewidth and increasing kinetic inductance as expected. The results can be quantitatively understood using SONNET simulations. The lowest loss is observed for a CPW with a total width of 6 μ m and corresponds to a Q-factor of ≈ 15 000. [ABSTRACT FROM AUTHOR]

Published
2020
Full Text
View/download PDF

37. Optical Characterization of the Keck Array and BICEP3 CMB Polarimeters from 2016 to 2019.

Author

St Germaine, T., Ade, P. A. R., Ahmed, Z., Amiri, M., Barkats, D., Basu Thakur, R., Bischoff, C. A., Bock, J. J., Boenish, H., Bullock, E., Buza, V., Cheshire, J., Connors, J., Cornelison, J., Crumrine, M., Cukierman, A., Dierickx, M., Duband, L., Fatigoni, S., and Filippini, J. P.

Subjects
COSMIC background radiation, OPTICAL receivers, FOURIER transform spectrometers, SPECTRAL sensitivity, GRAVITATIONAL waves, POLARISCOPE
Abstract

The BICEP/Keck experiment (BK) is a series of small-aperture refracting telescopes observing degree-scale cosmic microwave background (CMB) polarization from the South Pole in search of a primordial B-mode signature. This B-mode signal arises from primordial gravitational waves interacting with the CMB and has amplitude parametrized by the tensor-to-scalar ratio r. Since 2016, BICEP3 and the Keck Array have been observing with 4800 total antenna-coupled transition-edge sensor detectors, with frequency bands spanning 95, 150, 220, and 270 GHz. Here we present the optical performance of these receivers from 2016 to 2019, including far-field beams measured in situ with an improved chopped thermal source and instrument spectral response measured with a field-deployable Fourier transform spectrometer. As a pair differencing experiment, an important systematic that must be controlled is the differential beam response between the co-located, orthogonally polarized detectors. We generate per-detector far-field beam maps and the corresponding differential beam mismatch that is used to estimate the temperature-to-polarization leakage in our CMB maps and to give feedback on detector and optics fabrication. The differential beam parameters presented here were estimated using improved low-level beam map analysis techniques, including efficient removal of non-Gaussian noise as well as improved spatial masking. These techniques help minimize systematic uncertainty in the beam analysis, with the goal of constraining the bias on r induced by temperature-to-polarization leakage to be subdominant to the statistical uncertainty. This is essential as we progress to higher detector counts in the next generation of CMB experiments. [ABSTRACT FROM AUTHOR]

Published
2020
Full Text
View/download PDF

38. A simple method to measure the temperature and levitation height of devices rotating at cryogenic temperatures.

Author

de Bernardis, Paolo, Columbro, Fabio, Masi, Silvia, Paiella, Alessandro, and Romeo, Giovanni

Subjects
LEVITATION, COSMIC background radiation, MAGNETIC suspension, SENSOR networks, POLARISCOPE, THERMISTORS, MAGNETIC bearings, TEMPERATURE
Abstract

We describe a simple system to measure the temperature and levitation height of levitating cryogenic devices in rotation. Devices of this kind are the half-wave-plates rotating on superconducting magnetic bearings used in several cryogenic polarimeters for the cosmic microwave background. The temperature measurement is important to monitor the radiative background and potential systematic effects in the polarimeter. In our implementation, the temperature sensor is a thermistor, physically mounted on the rotating device. The sensor is biased with an AC current, which is transferred from the stationary electronics to the rotating device via capacitive coupling. The levitation height sensor is a network of capacitors, similar to the one used for the capacitive coupling of the thermistor. We describe the optimization of the readout system and its performance, which has been tested on a room-temperature prototype. We show that this system reaches an accuracy better than 3% for the measurement of the thermistor resistance and an accuracy of ∼10 μm for the measurement of its levitation height. [ABSTRACT FROM AUTHOR]

Published
2020
Full Text
View/download PDF

39. BoloCalc: a sensitivity calculator for the design of Simons Observatory.

Author

Hill, Charles A., Bruno, Sarah Marie M., Simon, Sara M., Ali, Aamir, Arnold, Kam S., Ashton, Peter C., Barron, Darcy, Bryan, Sean, Yuji Chinone, Coppi, Gabriele, Crowley, Kevin T., Cukierman, Ari, Dicker, Simon, Dunkley, Jo, Fabbian, Giulio, Galitzki, Nicholas, Gallardo, Patricio A., Gudmundsson, Jon E., Hubmayr, Johannes, and Keating, Brian

Published
2018
Full Text
View/download PDF

41. SAGE: A proposal for a space atomic gravity explorer.

Author

Tino, Guglielmo M., Bassi, Angelo, Bianco, Giuseppe, Bongs, Kai, Bouyer, Philippe, Cacciapuoti, Luigi, Capozziello, Salvatore, Chen, Xuzong, Chiofalo, Maria L., Derevianko, Andrei, Ertmer, Wolfgang, Gaaloul, Naceur, Gill, Patrick, Graham, Peter W., Hogan, Jason M., Iess, Luciano, Kasevich, Mark A., Katori, Hidetoshi, Klempt, Carsten, and Lu, Xuanhui

Subjects
QUANTUM theory, GRAVITY, ATOMIC clocks, GRAVITATIONAL waves, SAGE, MICHELSON interferometer
Abstract

The proposed mission "Space Atomic Gravity Explorer" (SAGE) has the scientific objective to investigate gravitational waves, dark matter, and other fundamental aspects of gravity as well as the connection between gravitational physics and quantum physics using new quantum sensors, namely, optical atomic clocks and atom interferometers based on ultracold strontium atoms. [ABSTRACT FROM AUTHOR]

Published
2019
Full Text
View/download PDF

42. The POLARBEAR Fourier transform spectrometer calibrator and spectroscopic characterization of the POLARBEAR instrument.

Author

Matsuda, F., Lowry, L., Suzuki, A., Aguilar Fáundez, M., Arnold, K., Barron, D., Bianchini, F., Cheung, K., Chinone, Y., Elleflot, T., Fabbian, G., Goeckner-Wald, N., Hasegawa, M., Kaneko, D., Katayama, N., Keating, B., Lee, A. T., Navaroli, M., Nishino, H., and Paar, H.

Subjects
FOURIER transform spectrometers, PARABOLIC reflectors, COSMIC background radiation, FOCAL planes, SPECTRAL sensitivity, POLARIZERS (Light), OPTICAL reflectors
Abstract

We describe the Fourier Transform Spectrometer (FTS) used for in-field testing of the POLARBEAR receiver, an experiment located in the Atacama Desert of Chile which measures the cosmic microwave background (CMB) polarization. The POLARBEAR-FTS (PB-FTS) is a Martin-Puplett interferometer designed to couple to the Huan Tran Telescope (HTT) on which the POLARBEAR receiver is installed. The PB-FTS measured the spectral response of the POLARBEAR receiver with signal-to-noise ratio >20 for ∼69% of the focal plane detectors due to three features: a high throughput of 15.1 sr cm2, optimized optical coupling to the POLARBEAR optics using a custom designed output parabolic mirror, and a continuously modulated output polarizer. The PB-FTS parabolic mirror is designed to mimic the shape of the 2.5 m-diameter HTT primary reflector, which allows for optimum optical coupling to the POLARBEAR receiver, reducing aberrations and systematics. One polarizing grid is placed at the output of the PB-FTS and modulated via continuous rotation. This modulation allows for decomposition of the signal into different harmonics that can be used to probe potentially pernicious sources of systematic error in a polarization-sensitive instrument. The high throughput and continuous output polarizer modulation features are unique compared to other FTS calibrators used in the CMB field. In-field characterization of the POLARBEAR receiver was accomplished using the PB-FTS in April 2014. We discuss the design, construction, and operation of the PB-FTS and present the spectral characterization of the POLARBEAR receiver. We introduce future applications for the PB-FTS in the next-generation CMB experiment, the Simons Array. [ABSTRACT FROM AUTHOR]

Published
2019
Full Text
View/download PDF

43. Tile-and-trim micro-resonator array fabrication optimized for high multiplexing factors.

Author

McKenney, Christopher M., Austermann, Jason E., Beall, James A., Dober, Bradley J., Duff, Shannon M., Gao, Jiansong, Hilton, Gene C., Hubmayr, Johannes, Li, Dale, Ullom, Joel N., Van Lanen, Jeff L., and Vissers, Michael R.

Subjects
MULTIPLEXING, MICRORESONATORS (Optoelectronics), SUPERCONDUCTING arrays, PHOTOLITHOGRAPHY, TITANIUM nitride films, GAUSSIAN distribution
Abstract

We present a superconducting micro-resonator array fabrication method that is scalable and reconfigurable and has been optimized for high multiplexing factors. The method uses uniformly sized tiles patterned on stepper photolithography reticles as the building blocks of an array. We demonstrate this technique on a 101-element microwave kinetic inductance detector (MKID) array made from a titanium-nitride superconducting film. Characterization reveals 1.5% maximum fractional frequency spacing deviations caused primarily by material parameters that vary smoothly across the wafer. However, local deviations exhibit a Gaussian distribution in fractional frequency spacing with a standard deviation of 2.7 × 10−3. We exploit this finding to increase the yield of the BLAST-TNG 250 μm production wafer by placing resonators in the array close in both physical and frequency space. This array consists of 1836 polarization-sensitive MKIDs wired in three multiplexing groups. We present the array design and show that the achieved yield is consistent with our model of frequency collisions and is comparable to what has been achieved in other low temperature detector technologies. [ABSTRACT FROM AUTHOR]

Published
2019
Full Text
View/download PDF

44. Session 5: Microwave Background.

Subjects
COSMIC background radiation, PARTICLE physics, NEUTRINO astrophysics, EXPANDING universe, ASTRONOMICAL observations
Published
2016

45. Electro-optic correlator for large-format microwave interferometry: Up-conversion and correlation stages performance analysis.

Author

Ortiz, D., Casas, Francisco J., Ruiz-Lombera, R., and Mirapeix, J.

Subjects
OPTICAL correlators, ELECTROOPTICS, INTERFEROMETRY, LITHIUM niobate, WAVELENGTHS
Abstract

In this paper, a microwave interferometer prototype with a near-infra-red optical correlator is proposed as a solution to get a large-format interferometer with hundreds of receivers for radio astronomy applications. A 10 Gbits/s Lithium Niobate modulator has been tested as part of an electro-optic correlator up-conversion stage that will be integrated in the interferometer prototype. Its internal circuitry consists of a single-drive modulator biased by a SubMiniature version A (SMA) connector allowing to up-convert microwave signals with bandwidths up to 12.5 GHz to the near infrared band. In order to characterize it, a 12 GHz tone and a bias voltage were applied to the SMA input using a polarization tee. Two different experimental techniques to stabilize the modulator operation point in its minimum optical carrier output power are described. The best achieved results showed a rather stable spectrum in amplitude and wavelength at the output of the modulator with an optical carrier level 23 dB lower than the signal of interest. On the other hand, preliminary measurements were made to analyze the correlation stage, using 4f and 6f optical configurations to characterize both the antenna/fiber array configuration and the corresponding point spread function. [ABSTRACT FROM AUTHOR]

Published
2017
Full Text
View/download PDF

46. Using the Crab Nebula as a high precision calibrator for cosmic microwave background polarimeters.

Author

Kaufman, Jonathan, Leon, David, and Keating, Brian

Subjects
CRAB Nebula, COSMIC background radiation, POLARISCOPE, GRAVITATIONAL waves, INFLATIONARY universe
Abstract

The polarization of the cosmic microwave background (CMB) provides a plethora of information about the early universe. Most notably, gravitational waves from the Inflationary epoch (the leading explanation of the origin of the universe) create a unique CMB polarization -mode signal. An unambiguous detection of the Inflationary -mode signal would be a window into the physics of the universe as it was s after the Big Bang, at energy scales many orders of magnitude larger than what the LHC can produce. However, there are several instrumental and astrophysical sources that can obfuscate the Inflationary -mode signal. One of the most difficult parameters to calibrate for CMB telescopes is the absolute orientation of the antenna's polarization sensitive axis. A miscalibration of the polarization orientation rotates the much brighter -mode signal, producing a false -mode signal. The current best uncertainty on polarization orientation in the CMB community is , set from extrapolating IRAM measurements of the Crab Nebula supernova remnant at 90 GHz to 150 GHz, where the CMB signals peak. This accuracy is not sufficient to convincingly detect -modes predicted by currently allowable models of Inflation. We suggest to precisely measure the Crab Nebula's polarization, which can be calibrated absolutely to from measurements of the polarized emission of Mars, and use these data to calibrate current and upcoming CMB experiments. In addition to Inflationary -modes, more precise calibration will allow us to better constrain the sum of the neutrino masses and set limits on exotic physics such as parity violation through cosmic polarization rotation. [ABSTRACT FROM AUTHOR]

Published
2016
Full Text
View/download PDF

47. A Quasi-Analytical Tool for the Characterization of Transmission Lines at High Frequencies [EM Programmer's Notebook].

Author

van Berkel, Sven L., Garufo, Alessandro, Llombart, Nuria, and Neto, Andrea

Subjects
ELECTRIC lines, ELECTRIC impedance, RADIATION, WAVELENGTHS, COMPUTER simulation
Abstract

In this article, we present a freely accessible software tool that allows for fast characterization of dynamic phenomena in a wide variety of transmission lines that include characteristic impedance, effective dielectric constant, and losses, such as radiation into space and surface waves. For printed transmission lines, the radiation effects are of particular importance when the transverse dimensions of the transmission lines become significant in terms of wavelength. Generally, dispersion and losses of the line due to these dynamic phenomena are predicted by full-wave simulations as quasi-static formula do not suffice. The presented software tool, freely downloaded from http://terahertz.tudelft.nl, is capable of accurately analyzing the most widely used transmission lines at high frequencies. [ABSTRACT FROM PUBLISHER]

Published
2016
Full Text
View/download PDF

48. Gravitational Thermodynamics for Interstellar Gas and Weakly Degenerate Quantum Gas.

Author

Ding Yu Zhu and Jian Qi Shen

Abstract

The temperature distribution of an ideal gas in gravitational fields has been identified as a longstanding problem in thermodynamics and statistical physics. According to the principle of entropy increase (i.e., the principle of maximum entropy), we apply a variational principle to the thermodynamical entropy functional of an ideal gas and establish a relationship between temperature gradient and gravitational field strength. As an illustrative example, the temperature and density distributions of an ideal gas in two simple but typical gravitational fields (i.e., a uniform gravitational field and an inverse-square gravitational field) are considered on the basis of entropic and hydrostatic equilibrium conditions. The effect of temperature inhomogeneity in gravitational fields is also addressed for a weakly degenerate quantum gas (e.g., Fermi and Bose gas). The present gravitational thermodynamics of a gas would have potential applications in quantum fluids, e.g., Bose-Einstein condensates in Earth's gravitational field and the temperature fluctuation spectrum in cosmic microwave background radiation. [ABSTRACT FROM AUTHOR]

Published
2016
Full Text
View/download PDF

49. A cryogenic rotation stage with a large clear aperture for the half-wave plates in the Spider instrument.

Author

Bryan, Sean, Ade, Peter, Amiri, Mandana, Benton, Steven, Bihary, Richard, Bock, James, Richard Bond, J., Chiang, H. Cynthia, Contaldi, Carlo, Crill, Brendan, Dore, Olivier, Elder, Benjamin, Filippini, Jeffrey, Fraisse, Aurelien, Gambrel, Anne, Gandilo, Natalie, Gudmundsson, Jon, Hasselfield, Matthew, Halpern, Mark, and Hilton, Gene

Subjects
OPTICAL retarders, ROTATIONAL motion (Rigid dynamics), COSMIC background radiation, OPTICAL shaft encoders, OPTOELECTRONIC devices
Abstract

We describe the cryogenic half-wave plate rotation mechanisms built for and used in SPIDER, a polarization-sensitive balloon-borne telescope array that observed the cosmic microwave background at 95 GHz and 150 GHz during a stratospheric balloon flight from Antarctica in January 2015. The mechanisms operate at liquid helium temperature in flight. A three-point contact design keeps the mechanical bearings relatively small but allows for a large (305 mm) diameter clear aperture. A worm gear driven by a cryogenic stepper motor allows for precise positioning and prevents undesired rotation when the motors are depowered. A custom-built optical encoder system monitors the bearing angle to an absolute accuracy of ±0.1°. The system performed well in SPIDER during its successful 16 day flight. [ABSTRACT FROM AUTHOR]

Published
2016
Full Text
View/download PDF

50. The substance of gravity.

Author

Annila, Arto

Subjects
GRAVITY, ATOMIC mass, SPEED of light, TORSION, ENERGY density
Abstract

Copyright of Physics Essays is the property of Physics Essays Publication and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)

Published
2015
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results