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42 results on '"D. V. Wiebe"'

1. A Detection of Cosmological 21 cm Emission from CHIME in Cross-correlation with eBOSS Measurements of the Lyα Forest

Author

Mandana Amiri, Kevin Bandura, Arnab Chakraborty, Matt Dobbs, Mateus Fandino, Simon Foreman, Hyoyin Gan, Mark Halpern, Alex S. Hill, Gary Hinshaw, Carolin Höfer, T. L. Landecker, Zack Li, Joshua MacEachern, Kiyoshi Masui, Juan Mena-Parra, Nikola Milutinovic, Arash Mirhosseini, Laura Newburgh, Anna Ordog, Sourabh Paul, Ue-Li Pen, Tristan Pinsonneault-Marotte, Alex Reda, J. Richard Shaw, Seth R. Siegel, Keith Vanderlinde, Haochen Wang, D. V. Wiebe, Dallas Wulf, and The CHIME Collaboration

Subjects
Cosmology, H I line emission, Lyα forest, Astrophysics, QB460-466
Abstract

We report the detection of 21 cm emission at an average redshift $\bar{z}=2.3$ in the cross-correlation of data from the Canadian Hydrogen Intensity Mapping Experiment (CHIME) with measurements of the Ly α forest from eBOSS. Data collected by CHIME over 88 days in the 400–500 MHz frequency band (1.8 < z < 2.5) are formed into maps of the sky and high-pass delay filtered to suppress the foreground power, corresponding to removing cosmological scales with k _∥ ≲ 0.13 Mpc ^−1 at the average redshift. Line-of-sight spectra to the eBOSS background quasar locations are extracted from the CHIME maps and combined with the Ly α forest flux transmission spectra to estimate the 21 cm–Ly α cross-correlation function. Fitting a simulation-derived template function to this measurement results in a 9 σ detection significance. The coherent accumulation of the signal through cross-correlation is sufficient to enable a detection despite excess variance from foreground residuals ∼6–10 times brighter than the expected thermal noise level in the correlation function. These results are the highest-redshift measurement of 21 cm emission to date, and they set the stage for future 21 cm intensity mapping analyses at z > 1.8.

Published
2024
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2. 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
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3. 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
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4. 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
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5. 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
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6. A Constraint on Primordial B-modes from the First Flight of the Spider Balloon-borne Telescope

Author

P. A. R. Ade, M. Amiri, S. J. Benton, A. S. Bergman, R. Bihary, J. J. Bock, J. R. Bond, J. A. Bonetti, S. A. Bryan, H. C. Chiang, C. R. Contaldi, O. Doré, A. J. Duivenvoorden, H. K. Eriksen, M. Farhang, J. P. Filippini, A. A. Fraisse, K. Freese, M. Galloway, A. E. Gambrel, N. N. Gandilo, K. Ganga, R. Gualtieri, J. E. Gudmundsson, M. Halpern, J. Hartley, M. Hasselfield, G. Hilton, W. Holmes, V. V. Hristov, Z. Huang, K. D. Irwin, W. C. Jones, A. Karakci, C. L. Kuo, Z. D. Kermish, J. S.-Y. Leung, S. Li, D. S. Y. Mak, P. V. Mason, K. Megerian, L. Moncelsi, T. A. Morford, J. M. Nagy, C. B. Netterfield, M. Nolta, R. O’Brient, B. Osherson, I. L. Padilla, B. Racine, A. S. Rahlin, C. Reintsema, J. E. Ruhl, M. C. Runyan, T. M. Ruud, J. A. Shariff, E. C. Shaw, C. Shiu, J. D. Soler, X. Song, A. Trangsrud, C. Tucker, R. S. Tucker, A. D. Turner, J. F. van der List, A. C. Weber, I. K. Wehus, S. Wen, D. V. Wiebe, and E. Y. Young

Published
2022
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7. In-Flight Gain Monitoring of SPIDER’s Transition-Edge Sensor Arrays

Author

J. P. Filippini, A. E. Gambrel, A. S. Rahlin, E. Y. Young, P. A. R. Ade, M. Amiri, S. J. Benton, A. S. Bergman, R. Bihary, J. J. Bock, J. R. Bond, J. A. Bonetti, S. A. Bryan, H. C. Chiang, C. R. Contaldi, O. Doré, A. J. Duivenvoorden, H. K. Eriksen, M. Farhang, A. A. Fraisse, K. Freese, M. Galloway, N. N. Gandilo, K. Ganga, R. Gualtieri, J. E. Gudmundsson, M. Halpern, J. Hartley, M. Hasselfield, G. Hilton, W. Holmes, V. V. Hristov, Z. Huang, K. D. Irwin, W. C. Jones, A. Karakci, C. L. Kuo, Z. D. Kermish, J. S.- Y. Leung, S. Li, D. S. Y. Mak, P. V. Mason, K. Megerian, L. Moncelsi, T. A. Morford, J. M. Nagy, C. B. Netterfield, M. Nolta, R. O’Brient, B. Osherson, I. L. Padilla, B. Racine, C. Reintsema, J. E. Ruhl, M. C. Runyan, T. M. Ruud, J. A. Shariff, E. C. Shaw, C. Shiu, J. D. Soler, X. Song, A. Trangsrud, C. Tucker, R. S. Tucker, A. D. Turner, J. F. van der List, A. C. Weber, I. K. Wehus, S. Wen, D. V. Wiebe, AstroParticule et Cosmologie (APC (UMR_7164)), 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 de Paris (UP), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, General Materials Science, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, Condensed Matter Physics, Transition edge sensor, Instrumentation and Methods for Astrophysics (astro-ph.IM), Atomic and Molecular Physics, and Optics, Cosmic microwave background
Abstract

Experiments deploying large arrays of transition-edge sensors (TESs) often require a robust method to monitor gain variations with minimal loss of observing time. We propose a sensitive and non-intrusive method for monitoring variations in TES responsivity using small square waves applied to the TES bias. We construct an estimator for a TES's small-signal power response from its electrical response that is exact in the limit of strong electrothermal feedback. We discuss the application and validation of this method using flight data from SPIDER, a balloon-borne telescope that observes the polarization of the cosmic microwave background with more than 2000 TESs. This method may prove useful for future balloon- and space-based instruments, where observing time and ground control bandwidth are limited., Comment: 7 pages, 3 figures; Proceedings of the 19th International Workshop on Low Temperature Detectors (LTD19); Minor updates to match published version

Published
2022

8. 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
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9. 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

10. 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
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11. 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

12. 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
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13. Sub-second periodicity in a fast radio burst

Author

Bridget C. Andersen, Kevin Bandura, Mohit Bhardwaj, P. J. Boyle, Charanjot Brar, Daniela Breitman, Tomas Cassanelli, Shami Chatterjee, Pragya Chawla, Jean-Franc¸ois Cliche, Davor Cubranic, Alice P. Curtin, Meiling Deng, Matt Dobbs, Fengqiu Adam Dong, Emanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Deborah C. Good, Alex S. Hill, Alexander Josephy, J. F. Kaczmarek, Zarif Kader, Joseph Kania, Victoria M. Kaspi, Calvin Leung, D. Z. Li, Hsiu-Hsien Lin, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Marcus Merryfield, B. W. Meyers, D. Michilli, Arun Naidu, Laura Newburgh, C. Ng, Anna Ordog, Chitrang Patel, Aaron B. Pearlman, Ue-Li Pen, Emily Petroff, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Andre Renard, Pranav Sanghavi, Paul Scholz, J. Richard Shaw, Kaitlyn Shin, Seth R. Siegel, Saurabh Singh, Kendrick Smith, Ingrid Stairs, Chia Min Tan, Shriharsh P. Tendulkar, Keith Vanderlinde, D. V. Wiebe, Dallas Wulf, Andrew Zwaniga, Daniele Michilli, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Multidisciplinary, 13. Climate action, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

Fast radio bursts (FRBs) are millisecond-duration flashes of radio waves that are visible at distances of billions of light-years. The nature of their progenitors and their emission mechanism remain open astrophysical questions. Here we report the detection of the multi-component FRB 20191221A and the identification of a periodic separation of 216.8(1) ms between its components with a significance of 6.5 sigmas. The long (~3 s) duration and nine or more components forming the pulse profile make this source an outlier in the FRB population. Such short periodicity provides strong evidence for a neutron-star origin of the event. Moreover, our detection favours emission arising from the neutron-star magnetosphere, as opposed to emission regions located further away from the star, as predicted by some models., Comment: Updated to conform to the accepted version

Published
2021

14. 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

15. 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

16. A Simulation-Based Method for Correcting Mode Coupling in CMB Angular Power Spectra

Author

J. S.-Y. Leung, J. Hartley, J. M. Nagy, C. B. Netterfield, J. A. Shariff, P. A. R. Ade, M. Amiri, S. J. Benton, A. S. Bergman, R. Bihary, J. J. Bock, J. R. Bond, J. A. Bonetti, S. A. Bryan, H. C. Chiang, C. R. Contaldi, O. Doré, A. J. Duivenvoorden, H. K. Eriksen, M. Farhang, J. P. Filippini, A. A. Fraisse, K. Freese, M. Galloway, A. E. Gambrel, N. N. Gandilo, K. Ganga, R. Gualtieri, J. E. Gudmundsson, M. Halpern, M. Hasselfield, G. Hilton, W. Holmes, V. V. Hristov, Z. Huang, K. D. Irwin, W. C. Jones, A. Karakci, C. L. Kuo, Z. D. Kermish, S. Li, D. S. Y. Mak, P. V. Mason, K. Megerian, L. Moncelsi, T. A. Morford, M. Nolta, R. O’Brient, B. Osherson, I. L. Padilla, B. Racine, A. S. Rahlin, C. Reintsema, J. E. Ruhl, M. C. Runyan, T. M. Ruud, E. C. Shaw, C. Shiu, J. D. Soler, X. Song, A. Trangsrud, C. Tucker, R. S. Tucker, A. D. Turner, J. F. van der List, A. C. Weber, I. K. Wehus, S. Wen, D. V. Wiebe, E. Y. Young, AstroParticule et Cosmologie (APC (UMR_7164)), 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 de Paris (UP), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Modern CMB analysis pipelines regularly employ complex time-domain filters, beam models, masking, and other techniques during the production of sky maps and their corresponding angular power spectra. However, these processes can generate couplings between multipoles from the same spectrum and from different spectra, in addition to the typical power attenuation. Within the context of pseudo-$C_\ell$ based, MASTER-style analyses, the net effect of the time-domain filtering is commonly approximated by a multiplicative transfer function, $F_{\ell}$, that can fail to capture mode mixing and is dependent on the spectrum of the signal. To address these shortcomings, we have developed a simulation-based spectral correction approach that constructs a two-dimensional transfer matrix, $J_{\ell\ell'}$, which contains information about mode mixing in addition to mode attenuation. We demonstrate the application of this approach on data from the first flight of the SPIDER balloon-borne CMB experiment., Comment: 14 pages, 7 figures; updated to match published version

Published
2021
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17. Receiver development for BICEP Array, a next-generation CMB polarimeter at the South Pole

Author

Zeeshan Ahmed, G. Hall, B. Racine, Lingzhen Zeng, P. A. R. Ade, Colin A. Bischoff, K. G. Megerian, L. Minutolo, E. M. Leitch, S. Palladino, Denis Barkats, K. L. Thompson, B. L. Schmitt, M. Crumrine, Rashmikant V. Sudiwala, Kent D. Irwin, E. V. Denison, Alessandro Schillaci, J. Kang, T. Namikawa, S. Fatigoni, L. Duband, P. Grimes, Edward D. Young, Howard Hui, Neil Goeckner-Wald, M. Amiri, S. Henderson, N. Precup, A. C. Weber, C. Umiltà, D. C. Goldfinger, Victor Buza, J. Cornelison, T. Prouvé, Jeffrey P. Filippini, A. Wandui, Ahmed Soliman, Shou-Cheng Zhang, K. W. Yoon, Sarah M. Harrison, W. L. K. Wu, Anthony D. Turner, J. A. Grayson, Y. Nakato, Chao-Lin Kuo, H. T. Nguyen, John M Kovac, Kirit Karkare, James J. Bock, Carole Tucker, Jake Connors, Sergi R. Hildebrandt, S. Kefeli, J. Willmert, C. Yu, A. J. Cukierman, Johannes Hubmayr, Mark Halpern, D. V. Wiebe, Chao Zhang, R. Basu Thakur, M. Eiben, Gene C. Hilton, C. Pryke, T. St. Germaine, Lorenzo Moncelsi, Marion Dierickx, Abigail G. Vieregg, Kam Y. Lau, Carl D. Reintsema, Eui-Hyeok Yang, Bryan Steinbach, J. Cheshire, Roger O'Brient, 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, and Gao, Jian-Rong

Subjects
Physics - Instrumentation and Detectors, Cosmology and Nongalactic Astrophysics (astro-ph.CO), detector: performance, detector: cryogenics, Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, cosmic background radiation: polarization, cosmic background radiation, 01 natural sciences, 7. Clean energy, Cosmology, gravitation: lens, 0103 physical sciences, Cosmic Microwave Background, synchrotron, detector: calibration, [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, Physics, polarization, beam: polarization, 010308 nuclear & particles physics, Detector, Astronomy, Polarimeter, Instrumentation and Detectors (physics.ins-det), lensing, Polarization (waves), BICEP, Inflation, Galaxy, optics, detector: sensitivity, Gravitational lens, B-mode, B-Modes, readout, galaxy, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

A detection of curl-type ($B$-mode) polarization of the primary CMB would be direct evidence for the inflationary paradigm of the origin of the Universe. The BICEP/Keck Array (BK) program targets the degree angular scales, where the power from primordial $B$-mode polarization is expected to peak, with ever-increasing sensitivity and has published the most stringent constraints on inflation to date. BICEP Array (BA) is the Stage-3 instrument of the BK program and will comprise four BICEP3-class receivers observing at 30/40, 95, 150 and 220/270 GHz with a combined 32,000+ detectors; such wide frequency coverage is necessary for control of the Galactic foregrounds, which also produce degree-scale $B$-mode signal. The 30/40 GHz receiver is designed to constrain the synchrotron foreground and has begun observing at the South Pole in early 2020. By the end of a 3-year observing campaign, the full BICEP Array instrument is projected to reach $\sigma_r$ between 0.002 and 0.004, depending on foreground complexity and degree of removal of $B$-modes due to gravitational lensing (delensing). This paper presents an overview of the design, measured on-sky performance and calibration of the first BA receiver. We also give a preview of the added complexity in the time-domain multiplexed readout of the 7,776-detector 150 GHz receiver., Comment: Proceedings of SPIE 2020 (AS111). This article supersedes arXiv:1808.00568 and arXiv:2002.05228

Published
2020

18. 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

19. 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

20. Design and pre-flight performance of SPIDER 280 GHz receivers

Author

Jeffrey P. Filippini, Ingunn Kathrine Wehus, P. A. R. Ade, Peter Mason, Zigmund Kermish, Carlo R. Contaldi, X. Song, M. Galloway, Aurelien A. Fraisse, K. Ganga, I. L. Padilla, J. F. van der List, J. R. Bond, A. E. Gambrel, D. V. Wiebe, Michael R. Vissers, L. M. Fissel, Joel N. Ullom, Adriaan J. Duivenvoorden, Dan Becker, A. D. Turner, S. Akers, Steven J. Benton, Matthew Hasselfield, R. Gualtieri, Marzieh Farhang, J. J. Bock, S. Li, A. Trangsrud, M. R. Nolta, E. Y. Young, A. S. Bergman, O. Doré, Shyang Wen, M. C. Runyan, J. E. Ruhl, Warren Holmes, J. A. Beall, Calvin B. Netterfield, C. Tucker, H. C. Chiang, Carl D. Reintsema, A. C. Weber, C. Shiu, R. S. Tucker, Mandana Amiri, R. S. Domagalski, Susan Redmond, Lorenzo Moncelsi, Kent D. Irwin, K. G. Megerian, J. Austermann, Antoine Kahn, Johannes Hubmayr, J. M. Nagy, Sean Bryan, J. Hartley, Arpi Grigorian, W. C. Jones, Jon E. Gudmundsson, Shannon M. Duff, Natalie N. Gandilo, L. J. Romualdez, Viktor Hristov, Mark Halpern, R. Nie, Katherine Freese, A. Lennox, Gene C. Hilton, H. Thommesen, B. Osherson, E. C. Shaw, J. S.-Y. Leung, Jamil A. Shariff, H. K. Eriksen, Zhi-Feng Huang, T. A. Morford, Juan D. Soler, L. M. Mocanu, C. L. Kuo, Alexandra S. Rahlin, J. Van Lanen, Science and Technology Facilities Council (STFC), Science and Technology Facilities Council, AstroParticule et Cosmologie (APC (UMR_7164)), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Zmuidzinas, Jonas, and Gao, Jian-Rong

Subjects
scientific ballooning, cosmic microwave background, cosmological model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Computer science, media_common.quotation_subject, Cosmic microwave background, scientific instrumentation, FOS: Physical sciences, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, B-mode: primordial, law.invention, Telescope, law, optical, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Remote sensing, media_common, Spider, polarization, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, millimeter wave instrumentation, Polarization (waves), transition-edge sensor, SPIDER, experimental equipment, Wide area, B-mode, Sky, astro-ph.CO, galaxy, Astrophysics - Instrumentation and Methods for Astrophysics, cosmology, performance, Dust emission, Astrophysics - Cosmology and Nongalactic Astrophysics, experimental results, astro-ph.IM
Abstract

In this work we describe upgrades to the Spider balloon-borne telescope in preparation for its second flight, currently planned for December 2021. The Spider instrument is optimized to search for a primordial B-mode polarization signature in the cosmic microwave background at degree angular scales. During its first flight in 2015, Spider mapped ~10% of the sky at 95 and 150 GHz. The payload for the second Antarctic flight will incorporate three new 280 GHz receivers alongside three refurbished 95- and 150 GHz receivers from Spider's first flight. In this work we discuss the design and characterization of these new receivers, which employ over 1500 feedhorn-coupled transition-edge sensors. We describe pre-flight laboratory measurements of detector properties, and the optical performance of completed receivers. These receivers will map a wide area of the sky at 280 GHz, providing new information on polarized Galactic dust emission that will help to separate it from the cosmological signal., 13 pages, 8 figures; as published in the conference proceedings for SPIE Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X (2020)

Published
2020

21. Microwave multiplexing on the Keck Array

Author

Howard Hui, J. Willmert, Gene C. Hilton, John E. Dusatko, S. Fatigoni, K. G. Megerian, Joel N. Ullom, L. Duband, Carole Tucker, D. V. Wiebe, Ari Cukierman, Gunther Haller, Shawn W. Henderson, Tyler St. Germaine, Stephen E. Kuenstner, Jeffrey P. Filippini, S. R. Hildebrandt, S. A. Kernasovskiy, David Brown, M. Crumrine, K. W. Yoon, Leila R. Vale, Jake Connors, G. Hall, Bradley Dober, Saptarshi Chaudhuri, Toshiya Namikawa, H. Yang, Chao-Lin Kuo, Josef Frisch, A. D. Turner, E. Karpel, J. Cornelison, C. Umilta, Ahmed Soliman, Zeeshan Ahmed, K. L. Thompson, Johannes Hubmayr, Mark Halpern, E. Y. Young, Bryan Steinbach, J. Cheshire, E. Bullock, John A. B. Mates, C. Pryke, Sarah M. Harrison, Attila Kovács, Roger O'Brient, M. Amiri, J. Kang, Jesus Vasquez, Lingzhen Zeng, R. Basu Thakur, Victor Buza, B. Racine, John M. D'Ewart, Denis Barkats, H. T. Nguyen, S. Palladino, A. C. Weber, C. D. Reintsema, Marion Dierickx, Stefan Richter, Chao Zhang, A. Schillaci, J. J. Bock, R. Schwarz, Stephen J. Smith, H. Boenish, S. Kefeli, Dale Li, John M Kovac, Kirit Karkare, Kent D. Irwin, A. Wandui, Colin A. Bischoff, Daniel D. Van Winkle, R. V. Sudiwala, W. L. K. Wu, C. D. Sheehy, C. Yu, Peter A. R. Ade, Lorenzo Moncelsi, Abigail G. Vieregg, Kei May Lau, 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)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)

Subjects
SMuRF, Coaxial cable, Cosmic microwave background, Polarimetry, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, CMB, 01 natural sciences, Multiplexing, 010305 fluids & plasmas, law.invention, Optics, law, Tone tracking, 0103 physical sciences, General Materials Science, Electronics, [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), Physics, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Condensed Matter Physics, BICEP, Atomic and Molecular Physics, and Optics, Cardinal point, Microwave multiplexing, Keck Array, Radio frequency, business, Astrophysics - Instrumentation and Methods for Astrophysics, Microwave
Abstract

We describe an on-sky demonstration of a microwave-multiplexing readout system in one of the receivers of the Keck Array, a polarimetry experiment observing the cosmic microwave background at the South Pole. During the austral summer of 2018-2019, we replaced the time-division multiplexing readout system with microwave-multiplexing components including superconducting microwave resonators coupled to radio-frequency superconducting quantum interference devices at the sub-Kelvin focal plane, coaxial-cable plumbing and amplification between room temperature and the cold stages, and a SLAC Microresonator Radio Frequency system for the warm electronics. In the range 5-6 GHz, a single coaxial cable reads out 528 channels. The readout system is coupled to transition-edge sensors, which are in turn coupled to 150-GHz slot-dipole phased-array antennas. Observations began in April 2019, and we report here on an initial characterization of the system performance., 9 pages, 11 figures, Accepted by the Journal of Low Temperature Physics (Proceedings of the 18th International Workshop on Low Temperature Detectors)

Published
2020

22. Optical Design and Characterization of 40-GHz Detector and Module for the BICEP Array

Author

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

Subjects
BICEP array, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, CMB, 01 natural sciences, 010305 fluids & plasmas, Optics, Frequency coverage, Polarization, 0103 physical sciences, General Materials Science, 010306 general physics, Anisotropy, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, business.industry, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Detectors, Condensed Matter Physics, Polarization (waves), Inflation, Atomic and Molecular Physics, and Optics, Cosmology, Amplitude, Cardinal point, Antennas, Transition edge sensor, Astrophysics - Instrumentation and Methods for Astrophysics, business
Abstract

Families of cosmic inflation models predict a primordial gravitational-wave background that imprints B-mode polarization pattern in the Cosmic Microwave Background (CMB). High sensitivity instruments with wide frequency coverage and well-controlled systematic errors are needed to constrain the faint B-mode amplitude. We have developed antenna-coupled Transition Edge Sensor (TES) arrays for high-sensitivity polarized CMB observations over a wide range of millimeter-wave bands. BICEP Array, the latest phase of the BICEP/Keck experiment series, is a multi-receiver experiment designed to search for inflationary B-mode polarization to a precision $\sigma$(r) between 0.002 and 0.004 after 3 full years of observations, depending on foreground complexity and the degree of lensing removal. We describe the electromagnetic design and measured performance of BICEP Array low-frequency 40-GHz detector, their packaging in focal plane modules, and optical characterization including efficiency and beam matching between polarization pairs. We summarize the design and simulated optical performance, including an approach to improve the optical efficiency due to mismatch losses. We report the measured beam maps for a new broad-band corrugation design to minimize beam differential ellipticity between polarization pairs caused by interactions with the module housing frame, which helps minimize polarized beam mismatch that converts CMB temperature to polarization ($T \rightarrow P$) anisotropy in CMB maps., Comment: 8 pages, 7 figures, Accepted by the Journal of Low Temperature Physics (Proceedings of the 18th International Workshop on Low Temperature Detectors)

Published
2020
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23. 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
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24. Particle response of antenna-coupled TES arrays: results from SPIDER and the lab

Author

Johanna Nagy, Steven J. Benton, W. A. Holmes, Carlo R. Contaldi, Gene C. Hilton, Jeffrey P. Filippini, D. V. Wiebe, Amy Trangsrud, A. S. Rahlin, J. E. Ruhl, Marcus Runyan, Calvin B. Netterfield, J. J. Bock, E. Young, E. C. Shaw, A. D. Turner, Carole Tucker, J. Fu, Sean Bryan, J. Hartley, O. Doré, H. C. Chiang, R. S. Tucker, Mandana Amiri, Kent D. Irwin, Natalie N. Gandilo, T. A. Morford, Carl D. Reintsema, Peter Mason, A. C. Weber, Jon E. Gudmundsson, A. E. Gambrel, Aurelien A. Fraisse, B. Osherson, R. Gualtieri, K. G. Megerian, W. C. Jones, Matthew Hasselfield, Jamil A. Shariff, Mark Halpern, Viktor Hristov, R. V. Gramillano, I. L. Padilla, Juan D. Soler, Peter A. R. Ade, Lorenzo Moncelsi, Zigmund Kermish, J. R. Bond, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112))

Subjects
General Physics, Physics - Instrumentation and Detectors, Bolometer, Transition-edge sensor, Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, 0204 Condensed Matter Physics, FOS: Physical sciences, Cosmic ray, 7. Clean energy, 01 natural sciences, Space exploration, Physics, Applied, 0203 Classical Physics, 010305 fluids & plasmas, law.invention, symbols.namesake, Optics, law, 0103 physical sciences, General Materials Science, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Planck, 010306 general physics, physics.ins-det, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Spider, Science & Technology, 0105 Mathematical Physics, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Instrumentation and Detectors (physics.ins-det), Condensed Matter Physics, Atomic and Molecular Physics, and Optics, Glitch, Physics, Condensed Matter, Physical Sciences, symbols, Antenna (radio), Astrophysics - Instrumentation and Methods for Astrophysics, business, astro-ph.IM
Abstract

Future mm-wave and sub-mm space missions will employ large arrays of multiplexed Transition Edge Sensor (TES) bolometers. Such instruments must contend with the high flux of cosmic rays beyond our atmosphere that induce "glitches" in bolometer data, which posed a challenge to data analysis from the Planck bolometers. Future instruments will face the additional challenges of shared substrate wafers and multiplexed readout wiring. In this work we explore the susceptibility of modern TES arrays to the cosmic ray environment of space using two data sets: the 2015 long-duration balloon flight of the SPIDER cosmic microwave background polarimeter, and a laboratory exposure of SPIDER flight hardware to radioactive sources. We find manageable glitch rates and short glitch durations, leading to minimal effect on SPIDER analysis. We constrain energy propagation within the substrate through a study of multi-detector coincidences, and give a preliminary look at pulse shapes in laboratory data., Comment: 9 pages, 6 figures, Proceedings of the 18th International Workshop on Low Temperature Detectors

Published
2019

25. 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

26. 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

27. The CHIME Fast Radio Burst Project: System Overview

Author

A. Josephy, Bryan Gaensler, T. L. Landecker, Scott M. Ransom, M. Fandino, E. Fonseca, Laura Newburgh, A. Naidu, M. M. Boyce, K. Vanderlinde, S. R. Siegel, P. J. Boyle, S. P. Tendulkar, Cherry Ng, D. V. Wiebe, Charanjot Brar, Ziggy Pleunis, H. Liao, Kendrick M. Smith, A. Renard, M. Dobbs, Kris Sigurdson, Victoria M. Kaspi, Ingrid H. Stairs, C. Höfer, M. Rafiei Ravandi, M. Amiri, Ue-Li Pen, Philippe Berger, M. Burhanpurkar, Gary Hinshaw, J. Mena-Parra, S. Guliani, T. Pinsonneault-Marotte, Mohit Bhardwaj, J. F. Cliche, A. J. Gilbert, J. Chowdhury, M. Deng, Kevin Bandura, Mark Halpern, D. Cubranic, D. Lang, Miles Cranmer, P. Scholz, Kiyoshi Masui, N. Denman, P. Chawla, C. Patel, Utkarsh Giri, and Deborah C. Good

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Fast radio burst, Canadian Hydrogen Intensity Mapping Experiment, Real-time computing, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, Methods observational, Space and Planetary Science, 0103 physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

The Canadian Hydrogen Intensity Mapping Experiment (CHIME) is a novel transit radio telescope operating across the 400-800-MHz band. CHIME is comprised of four 20-m x 100-m semi-cylindrical paraboloid reflectors, each of which has 256 dual-polarization feeds suspended along its axis, giving it a >200 square degree field-of-view. This, combined with wide bandwidth, high sensitivity, and a powerful correlator makes CHIME an excellent instrument for the detection of Fast Radio Bursts (FRBs). The CHIME Fast Radio Burst Project (CHIME/FRB) will search beam-formed, high time-and frequency-resolution data in real time for FRBs in the CHIME field-of-view. Here we describe the CHIME/FRB backend, including the real-time FRB search and detection software pipeline as well as the planned offline analyses. We estimate a CHIME/FRB detection rate of 2-42 FRBs/sky/day normalizing to the rate estimated at 1.4-GHz by Vander Wiel et al. (2016). Likely science outcomes of CHIME/FRB are also discussed. CHIME/FRB is currently operational in a commissioning phase, with science operations expected to commence in the latter half of 2018., 27 pages, submitted to ApJ

Published
2018
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28. Limits on the Ultra-bright Fast Radio Burst Population from the CHIME Pathfinder

Author

Peter Klages, Emilie Storer, Liam Connor, Meiling Deng, R. S. Domagalski, Keith Vanderlinde, S. R. Siegel, T. L. Landecker, M. A. Dobbs, Mandana Amiri, A. Renard, Laura Newburgh, Kris Sigurdson, Philippe Berger, Kiyoshi Masui, A. J. Gilbert, C. Höfer, D. S. Hanna, Deborah C. Good, Mark Halpern, Jeffrey B. Peterson, T. Pinsonneault-Marotte, J. Mena-Parra, Kendrick M. Smith, J. R. Bond, J. F. Cliche, J. R. Shaw, Niels Oppermann, I. Tretyakov, Kevin Bandura, M. Fandino, G. Hsyu, Adam D. Hincks, Ue-Li Pen, Nolan Denman, Gary Hinshaw, D. V. Wiebe, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Fast radio burst, media_common.quotation_subject, Canadian Hydrogen Intensity Mapping Experiment, Population, FOS: Physical sciences, Astronomy and Astrophysics, Field of view, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Power law, Pathfinder, Space and Planetary Science, Sky, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010306 general physics, education, 010303 astronomy & astrophysics, media_common
Abstract

We present results from a new incoherent-beam Fast Radio Burst (FRB) search on the Canadian Hydrogen Intensity Mapping Experiment (CHIME) Pathfinder. Its large instantaneous field of view (FoV) and relative thermal insensitivity allow us to probe the ultra-bright tail of the FRB distribution, and to test a recent claim that this distribution's slope, $\alpha\equiv-\frac{\partial \log N}{\partial \log S}$, is quite small. A 256-input incoherent beamformer was deployed on the CHIME Pathfinder for this purpose. If the FRB distribution were described by a single power-law with $\alpha=0.7$, we would expect an FRB detection every few days, making this the fastest survey on sky at present. We collected 1268 hours of data, amounting to one of the largest exposures of any FRB survey, with over 2.4\,$\times$\,10$^5$\,deg$^2$\,hrs. Having seen no bursts, we have constrained the rate of extremely bright events to $

Published
2017

29. 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

30. Design of 280 GHz feedhorn-coupled TES arrays for the balloon-borne polarimeter SPIDER

Author

James A. Beall, B. Racine, Jeffrey P. Filippini, J. Richard Bond, Aurelien A. Fraisse, K. Ganga, M. Galloway, Lorenzo Moncelsi, Juan D. Soler, R. Gualtieri, Joel N. Ullom, X. Song, A. Stevie Bergman, Gene C. Hilton, Jason E. Austermann, Ingunn Kathrine Wehus, Johannes Hubmayr, Mark Halpern, H. K. Eriksen, Shannon M. Duff, Steven J. Benton, Daniel T. Becker, Sean Bryan, J. Hartley, Johanna Nagy, D. V. Wiebe, Ivan L. Padilla, T. M. Rudd, Adri Duivenvoorden, B. Osherson, Calvin B. Netterfield, E. Y. Young, Jamil A. Shariff, Jon E. Gudmundsson, Arpi Grigorian, W. C. Jones, J. E. Ruhl, A. E. Gambrel, Michael R. Vissers, Shyang Wen, Jeff McMahon, Alexandra S. Rahlin, Jeff Van Lanen, Holland, Wayne S., and Zmuidzinas, Jonas

Subjects
Physics, Physics::Instrumentation and Detectors, business.industry, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Polarimetry, FOS: Physical sciences, Polarimeter, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), 01 natural sciences, law.invention, Optics, law, 0103 physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, 010306 general physics, business, Phonon noise, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Waveguide, Astrophysics::Galaxy Astrophysics, Microwave
Abstract

We describe 280 GHz bolometric detector arrays that instrument the balloon-borne polarimeter SPIDER. A primary science goal of SPIDER is to measure the large-scale B-mode polarization of the cosmic microwave background in search of the cosmic-inflation, gravitational-wave signature. 280 GHz channels aid this science goal by constraining the level of B-mode contamination from galactic dust emission. We present the focal plane unit design, which consists of a 16$\times$16 array of conical, corrugated feedhorns coupled to a monolithic detector array fabricated on a 150 mm diameter silicon wafer. Detector arrays are capable of polarimetric sensing via waveguide probe-coupling to a multiplexed array of transition-edge-sensor (TES) bolometers. The SPIDER receiver has three focal plane units at 280 GHz, which in total contains 765 spatial pixels and 1,530 polarization sensitive bolometers. By fabrication and measurement of single feedhorns, we demonstrate 14.7$^{\circ}$ FHWM Gaussian-shaped beams with $, Comment: Proceedings of SPIE Astronomical Telescopes + Instrumentation 2016

Published
2016

31. 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

32. The Keck Array: A Multi Camera CMB Polarimeter at the South Pole

Author

J. E. Tolan, M. Lueker, D. V. Wiebe, R. W. Ogburn, C. D. Sheehy, Mark Halpern, J. E. Ruhl, Roger O'Brient, Viktor Hristov, S. J. Benton, Colin A. Bischoff, P. Wilson, John M Kovac, Mandana Amiri, Carl D. Reintsema, J. A. Bonetti, S. Stokes, Kent D. Irwin, C. Pryke, Grant Teply, Jeffrey P. Filippini, Abigail G. Vieregg, Chao-Lin Kuo, Randol W. Aikin, Justus A. Brevik, H. T. Nguyen, M. Hasselfield, B. Burger, Gene C. Hilton, A. D. Turner, K. L. Thompson, C. D. Dowell, Z. K. Staniszewski, Angiola Orlando, T. Montroy, Sunil Golwala, J. J. Bock, R. Schwarz, L. Duband, and Chin Lin Wong

Subjects
Physics, Gravitational wave, business.industry, Cosmic microwave background, Bolometer, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Polarimeter, Astrophysics::Cosmology and Extragalactic Astrophysics, Condensed Matter Physics, Polarization (waves), Atomic and Molecular Physics, and Optics, law.invention, Telescope, Optics, law, General Materials Science, Transition edge sensor, business
Abstract

The Keck array is a new multi-camera Cosmic Microwave Background (CMB) polarimeter. Each camera contains 256 polarization pairs of antenna-coupled transition edge sensor (TES) bolometers. We recently deployed three of five cameras at the geographic South Pole, and plan to deploy the final two cameras in early 2012. This new telescope is an ideal instrument to search for the primordial B-mode polarization signal imprinted in the CMB by inflationary gravitational waves. We will discuss the design of the detectors and receivers, the status of current observations, and report on progress toward upgrading the instrument with the full compliment of polarized receivers.

Published
2012

33. BICEP2 and Keck array: upgrades and improved beam characterization

Author

J. P. Kaufman, Grant Teply, D. Barkats, H. T. Nguyen, D. V. Wiebe, E. M. Leitch, A. D. Turner, Calvin B. Netterfield, K. L. Thompson, Peter A. R. Ade, Jeffrey P. Filippini, J. E. Tolan, Abigail G. Vieregg, Kate D. Alexander, C. Pryke, Randol W. Aikin, Peter Mason, R. W. Ogburn, M. Hasselfield, Gene C. Hilton, Howard Hui, M. Lueker, Carl D. Reintsema, S. Fliescher, K. G. Megerian, A. Orlando, Ki Won Yoon, Viktor Hristov, S. Richter, Mark Halpern, Zeeshan Ahmed, Mandana Amiri, B. P. Crill, B. Burger, C. D. Dowell, G. Davis, S. A. Kernasovskiy, Chao-Lin Kuo, R. V. Sudiwala, John M Kovac, C. D. Sheehy, James J. Bock, Brian Keating, Kirit Karkare, Z. K. Staniszewski, S. Kefeli, Kent D. Irwin, P. Wilson, J. A. Bonetti, L. Duband, Sunil Golwala, E. Bullock, C. L. Wong, S. R. Hildebrandt, A. C. Weber, R. Schwarz, Colin A. Bischoff, Justus A. Brevik, Roger O'Brient, I. Buder, Michael S. Gordon, S. J. Benton, Holland, Wayne S., and Zmuidzinas, Jonas

Subjects
Physics, Gravitational wave, business.industry, Cosmic microwave background, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Noise-equivalent temperature, Polarization (waves), law.invention, Telescope, Optics, Side lobe, law, business, Beam (structure)
Abstract

Searching for evidence of inflation by measuring B-modes in the cosmic microwave background (CMB) polarization at degree angular scales remains one of the most compelling experimental challenges in cosmology. BICEP2 and the Keck Array are part of a program of experiments at the South Pole whose main goal is to achieve the sensitivity and systematic control necessary for measurements of the tensor-to-scalar ratio at σ(r) ~0:01. Beam imperfections that are not sufficiently accounted for are a potential source of spurious polarization that could interfere with that goal. The strategy of BICEP2 and the Keck Array is to completely characterize their telescopes' polarized beam response with a combination of in-lab, pre-deployment, and on-site calibrations. We Sereport the status of these experiments, focusing on continued improved understanding of their beams. Far-field measurements of the BICEP2 beam with a chopped thermal source, combined with analysis improvements, show that the level of residual beam-induced systematic errors is acceptable for the goal of σ(r) ~ 0:01 measurements. Beam measurements of the Keck Array side lobes helped identify a way to reduce optical loading with interior cold baffles, which we installed in late 2013. These baffles reduced total optical loading, leading to a ~ 10% increase in mapping speed for the 2014 observing season. The sensitivity of the Keck Array continues to improve: for the 2013 season it was 9:5 μK _/s noise equivalent temperature (NET). In 2014 we converted two of the 150-GHz cameras to 100 GHz for foreground separation capability. We have shown that the BICEP2 and the Keck Array telescope technology is sufficient for the goal of σ(r) ~ 0:01 measurements. Furthermore, the program is continuing with BICEP3, a 100-GHz telescope with 2560 detectors. © (2014) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.

Published
2014

34. Calibrating CHIME, A New Radio Interferometer to Probe Dark Energy

Author

Ue-Li Pen, Gary Hinshaw, Adam D. Hincks, G. Davis, Rick Smegal, Kenneth Gibbs, Jeffrey B. Peterson, Kiyoshi Masui, C. Höfer, J. F. Cliche, J. Richard Bond, David Hanna, Laura Newburgh, A. Gilbert, Graeme Smecher, Kris Sigurdson, Keith Vanderlinde, T. L. Landecker, J. Richard Shaw, Mandana Amiri, Heather Fong, Peter Klages, Nolan Denman, Juan Mena Parra, Kevin Bandura, Andre Recnik, Graeme E. Addison, Matt Dobbs, Elizabeth Griffin, M. Fandino, D. V. Wiebe, Liam Connor, Meiling Deng, Mark Halpern, and Michael Sitwell

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Radio interferometers, media_common.quotation_subject, FOS: Physical sciences, Intensity mapping, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 7. Clean energy, 01 natural sciences, Acoustic oscillation, Astrophysical observatory, Observatory, Dark energy, 0103 physical sciences, Astronomical interferometer, 21cm, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, media_common, Physics, Interferometers, 010308 nuclear & particles physics, Canadian Hydrogen Intensity Mapping Experiment, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Spectral density, Cosmology, Interferometry, Sky, Calibration schemes, Calibration, Probes, Airborne telescopes, Baryon acoustic oscillations, Astrophysics - Instrumentation and Methods for Astrophysics, Frequency ranges, Hydrogen, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Canadian Hydrogen Intensity Mapping Experiment (CHIME) is a transit interferometer currently being built at the Dominion Radio Astrophysical Observatory (DRAO) in Penticton, BC, Canada. We will use CHIME to map neutral hydrogen in the frequency range 400 - 800MHz over half of the sky, producing a measurement of baryon acoustic oscillations (BAO) at redshifts between 0.8 - 2.5 to probe dark energy. We have deployed a pathfinder version of CHIME that will yield constraints on the BAO power spectrum and provide a test-bed for our calibration scheme. I will discuss the CHIME calibration requirements and describe instrumentation we are developing to meet these requirements., Ground-Based and Airborne Telescopes V, June 22-27, 2014, Series: Proceedings of SPIE; no. 9145

Published
2014

35. The Second-generation z (Redshift) and Early Universe Spectrometer. I. First-light Observation of a Highly Lensed Local-ulirg Analog at High-z

Author

James L. Higdon, Justin Schoenwald, Drew Brisbin, D. V. Wiebe, Peter A. R. Ade, H. M. Cho, Kent D. Irwin, Thomas Nikola, S. Hailey-Dunsheath, Karl M. Menten, Sarah J.U. Higdon, Aprajita Verma, Rolf Güsten, Dominik Riechers, C. Tucker, Michael D. Niemack, Matthew Hasselfield, Mark Halpern, Stephen C. Parshley, Axel Weiß, Mandana Amiri, Gordon J. Stacey, and Carl Ferkinhoff

Subjects
Physics, 010504 meteorology & atmospheric sciences, Spectrometer, media_common.quotation_subject, Astronomy and Astrophysics, First light, Astrophysics, 01 natural sciences, Redshift, Galaxy, Universe, Luminosity, Space and Planetary Science, 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Line (formation), media_common
Abstract

We report first science results from our new spectrometer, the 2nd generation z(Redshift) and Early Universe Spectrometer (ZEUS-2), recently commissioned on the Atacama Pathfinder Experiment telescope (APEX). ZEUS-2 is a submillimeter grating spectrometer optimized for detecting the faint and broad lines from distant galaxies that are redshifted into the telluric windows from 200 to 850 microns. It utilizes a focal plane array of transition-edge sensed bolometers, the first use of these arrays for astrophysical spectroscopy. ZEUS-2 promises to be an important tool for studying galaxies in the years to come due to its synergy with ALMA and its capabilities in the short submillimeter windows that are unique in the post Herschel era. Here we report on our first detection of the [CII] 158 $\mu m$ line with ZEUS-2. We detect the line at z ~ 1.8 from H-ATLAS J091043.1-000322 with a line flux of $(6.44 \pm 0.42) \times 10^{-18} W m^{-2}$. Combined with its far-infrared luminosity and a new Herschel-PACS detection of the [OI] 63 $\mu m $ line we model the line emission as coming from a photo-dissociation region with far-ultraviolet radiation field, $G \approx 2 \times 10^{4} G_{0}$, gas density, $n \approx 1 \times 10^{3} cm^{-3}$ and size between ~ 0.4 and 1 kpc. Based on this model, we conclude that H-ATLAS J091043.1-000322 is a high redshift analogue of a local ultra-luminous infrared galaxy, i.e. it is likely the site of a compact starburst due to a major merger. Further identification of these merging systems is important for constraining galaxy formation and evolution models.

Published
2014

36. Design and construction of a carbon fiber gondola for the SPIDER balloon-borne telescope

Author

Marzieh Farhang, Juan D. Soler, Johanna Nagy, C. J. MacTavish, J. E. Ruhl, Gene C. Hilton, Peter A. R. Ade, Lorenzo Moncelsi, A. E. Gambrel, J. R. Bond, Aurelien A. Fraisse, W. A. Holmes, Alexandra S. Rahlin, S. J. Benton, C. C. Contaldi, B. P. Crill, T. A. Morford, R. S. Tucker, Carole Tucker, A. C. Weber, Mandana Amiri, Sean Bryan, Mark Halpern, A. D. Turner, Natalie N. Gandilo, Peter Mason, Z. K. Kermish, Matthew Hasselfield, C. Chiang, Carl D. Reintsema, W. C. Jones, Marcus Runyan, Amy Trangsrud, Calvin B. Netterfield, Chao-Lin Kuo, K. G. Megerian, J. J. Bock, O. Doré, Jeffrey P. Filippini, Sunil Golwala, Jon E. Gudmundsson, Jamil A. Shariff, E. Y. Young, Kent D. Irwin, Viktor Hristov, Laura M. Fissel, D. V. Wiebe, Stepp, Larry M., Gilmozzi, Roberto, and Hall, Helen J.

Subjects
Carbon fiber reinforced polymer, Spider, Physics - Instrumentation and Detectors, business.industry, Cosmic microwave background, Carbon fibers, Astrophysics::Instrumentation and Methods for Astrophysics, Structural integrity, FOS: Physical sciences, Instrumentation and Detectors (physics.ins-det), 7. Clean energy, Finite element method, law.invention, Telescope, law, visual_art, visual_art.visual_art_medium, Environmental science, Balloon-borne telescope, Aerospace engineering, business, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

We introduce the light-weight carbon fiber and aluminum gondola designed for the SPIDER balloon-borne telescope. SPIDER is designed to measure the polarization of the Cosmic Microwave Background radiation with unprecedented sensitivity and control of systematics in search of the imprint of inflation: a period of exponential expansion in the early Universe. The requirements of this balloon-borne instrument put tight constrains on the mass budget of the payload. The SPIDER gondola is designed to house the experiment and guarantee its operational and structural integrity during its balloon-borne flight, while using less than 10% of the total mass of the payload. We present a construction method for the gondola based on carbon fiber reinforced polymer tubes with aluminum inserts and aluminum multi-tube joints. We describe the validation of the model through Finite Element Analysis and mechanical tests., Comment: 16 pages, 11 figures. Presented at SPIE Ground-based and Airborne Telescopes V, June 23, 2014. To be published in Proceedings of SPIE Volume 9145

Published
2014
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37. Canadian Hydrogen Intensity Mapping Experiment (CHIME) Pathfinder

Author

Graeme E. Addison, Duncan Campbell-Wilson, Kris Sigurdson, Laura Newburgh, Meiling Deng, Liam Connor, Nolan Denman, J. Richard Bond, Kiyoshi Masui, C. Höfer, T. L. Landecker, Kevin Bandura, Gary Hinshaw, Mark Halpern, Graeme Smecher, Kenneth Gibbs, J. Richard Shaw, Matt Dobbs, David Hanna, Keith Vanderlinde, A. Gilbert, J. F. Cliche, Jeffrey B. Peterson, Ue-Li Pen, Adam D. Hincks, Mike Sitwell, Rick Smegal, M. Fandino, Mandana Amiri, G. Davis, Juan Mena Parra, Andre Recnik, Peter Klages, and D. V. Wiebe

Subjects
Frequency band, Acoustics, FOS: Physical sciences, Field of view, Intensity mapping, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 7. Clean energy, Acoustic oscillation, Power spectrum, Astrophysical observatory, Polarization, Astronomical interferometer, Frequency bands, Radio astronomy, Correlation matrix, Instrumentation and Methods for Astrophysics (astro-ph.IM), Wide-field surveys, Physics, BAO, Canadian Hydrogen Intensity Mapping Experiment, Low noise amplifiers, Astrophysics::Instrumentation and Methods for Astrophysics, Program processors, Cosmology, Pathfinder, Mapping, CHIME, Baryon acoustic oscillations, Airborne telescopes, Astrophysics - Instrumentation and Methods for Astrophysics, Hydrogen
Abstract

A pathfinder version of CHIME (the Canadian Hydrogen Intensity Mapping Experiment) is currently being commissioned at the Dominion Radio Astrophysical Observatory (DRAO) in Penticton, BC. The instrument is a hybrid cylindrical interferometer designed to measure the large scale neutral hydrogen power spectrum across the redshift range 0.8 to 2.5. The power spectrum will be used to measure the baryon acoustic oscillation (BAO) scale across this poorly probed redshift range where dark energy becomes a significant contributor to the evolution of the Universe. The instrument revives the cylinder design in radio astronomy with a wide field survey as a primary goal. Modern low-noise amplifiers and digital processing remove the necessity for the analog beam forming that characterized previous designs. The Pathfinder consists of two cylinders 37m long by 20m wide oriented north-south for a total collecting area of 1,500 square meters. The cylinders are stationary with no moving parts, and form a transit instrument with an instantaneous field of view of ∼100 degrees by 1-2 degrees. Each CHIME Pathfinder cylinder has a feedline with 64 dual polarization feeds placed every ∼30 cm which Nyquist sample the north-south sky over much of the frequency band. The signals from each dual-polarization feed are independently amplified, filtered to 400-800 MHz, and directly sampled at 800 MSps using 8 bits. The correlator is an FX design, where the Fourier transform channelization is performed in FPGAs, which are interfaced to a set of GPUs that compute the correlation matrix. The CHIME Pathfinder is a 1/10th scale prototype version of CHIME and is designed to detect the BAO feature and constrain the distance-redshift relation. The lessons learned from its implementation will be used to inform and improve the final CHIME design., Ground-Based and Airborne Telescopes V, June 22-27, 2014, Series: Proceedings of SPIE; no. 9145

Published
2014
Full Text
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38. BLASTbus electronics: General-purpose readout and control for balloon-borne experiments

Author

J. R. Bond, O. Doré, T. A. Morford, B. Dober, Aurelien A. Fraisse, B. P. Crill, Nicholas Galitzki, N. N. Gandilo, Tony Mroczkowski, N. E. Thomas, M. Hasselfield, D. V. Wiebe, Mark Halpern, Jacob Klein, Marzieh Farhang, Kent D. Irwin, S. R. Golwala, Calvin B. Netterfield, C. J. MacTavish, A. Trangsrud, M. Amiri, Yasuo Fukui, K. G. Megerian, Juan D. Soler, Sean Bryan, Francisco E. Angile, Gene C. Hilton, Carlo R. Contaldi, Gregory S. Tucker, W. A. Holmes, Jeffrey P. Filippini, F. Poidevin, Jamil A. Shariff, C. L. Kuo, A. D. Turner, Tristan G. Matthews, Douglas Scott, Matthew D. P. Truch, Carole Tucker, H. C. Chiang, R. W. Ogburn, Peter Mason, A. L. Korotkov, David John Nutter, M. J. Devlin, Derek Ward-Thompson, C. D. Reintsema, C. D. Dowell, A. C. Weber, Enzo Pascale, Jon E. Gudmundsson, Zigmund Kermish, Alexandra S. Rahlin, S. J. Benton, E. Y. Young, Johanna Nagy, L. M. Fissel, Giorgio Savini, Peter A. R. Ade, Lorenzo Moncelsi, Giles Novak, James J. Bock, W. C. Jones, M. C. Runyan, J. E. Ruhl, R. S. Tucker, A. E. Gambrel, V. V. Hristov, Roger O'Brient, Stepp, Larry M., Gilmozzi, Roberto, and Hall, Helen J.

Subjects
Digital signal processor, Motherboard, Computer science, FOS: Physical sciences, balloon-borne telescope, 7. Clean energy, 01 natural sciences, BLASTbus, 010309 optics, Gate array, 0103 physical sciences, Electronic, bolometer readout, attitude control, BLASTPol, cryogenics, Spider, Electronic, Optical and Magnetic Materials, Condensed Matter Physics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Applied Mathematics, Electrical and Electronic Engineering, Electronics, Optical and Magnetic Materials, Field-programmable gate array, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Digital signal processing, business.industry, Electrical engineering, Analog signal, Astrophysics - Instrumentation and Methods for Astrophysics, business
Abstract

We present the second generation BLASTbus electronics. The primary purposes of this system are detector readout, attitude control, and cryogenic housekeeping, for balloon-borne telescopes. Readout of neutron transmutation doped germanium (NTD-Ge) bolometers requires low noise and parallel acquisition of hundreds of analog signals. Controlling a telescope's attitude requires the capability to interface to a wide variety of sensors and motors, and to use them together in a fast, closed loop. To achieve these different goals, the BLASTbus system employs a flexible motherboard-daughterboard architecture. The programmable motherboard features a digital signal processor (DSP) and field-programmable gate array (FPGA), as well as slots for three daughterboards. The daughterboards provide the interface to the outside world, with versions for analog to digital conversion, and optoisolated digital input/output. With the versatility afforded by this design, the BLASTbus also finds uses in cryogenic, thermometry, and power systems. For accurate timing control to tie everything together, the system operates in a fully synchronous manner. BLASTbus electronics have been successfully deployed to the South Pole, and flown on stratospheric balloons., Presented at SPIE Ground-based and Airborne Telescopes V, June 23, 2014. To be published in Proceedings of SPIE Volume 9145

Published
2014

39. Optimization and sensitivity of the Keck Array

Author

D. V. Wiebe, Peter A. R. Ade, C. L. Wongg, Abigail G. Vieregg, James J. Bock, C. L. Kuo, M. Lueker, Z. K. Staniszewski, A. D. Turner, John M Kovac, C. D. Dowell, C. D. Sheehy, R. V. Sudiwala, Justus A. Brevik, Kent D. Irwin, M. Amiri, L. Duband, G. P. Teply, R. W. Aikin, J. E. Tolan, Sunil Golwala, S. Fliescher, S. A. Kernasovskiy, M. Hasselfield, J. E. Ruhl, G. Hiltion, R. W. Ogburn, C. D. Reintsema, Roger O'Brient, G. Davis, Colin A. Bischoff, Calvin B. Netterfield, Jeffrey P. Filippini, P. R. Wilson, R. Schwarz, H. T. Nguyen, E. M. Leitch, J. A. Bonetti, Mark Halpern, B. Burger, C. Pryke, M. C. Runyan, S. J. Benton, V. V. Hristov, Holland, Wayne S., and Zmuidzinas, J.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Optics, law, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Physics, Time domain multiplexing, business.industry, Bolometer, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Polarization (waves), Refracting telescope, Imaging array, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, business, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Keck Array (SPUD) began observing the cosmic microwave background's polarization in the winter of 2011 at the South Pole. The Keck Array follows the success of the predecessor experiments Bicep and Bicep2, using five on-axis refracting telescopes. These have a combined imaging array of 2500 antenna-coupled TES bolometers read with a SQUID-based time domain multiplexing system. We will discuss the detector noise and the optimization of the readout. The achieved sensitivity of the Keck Array is 11.5 {\mu}K_(CMB)*sqrt{s} in the 2012 configuration., Comment: Presented at SPIE 2012 Astronomical Telescopes and Instrumentation Conference. Will be published in the proceedings

Published
2012

40. HerMES: The SPIRE confusion limit

Author

Mark Halpern, Bruno Maffei, Robyn L. Ward, Jennifer L. Marshall, M. Fox, Dimitra Rigopoulou, Stephen Anthony Eales, G. Mainetti, Luca Conversi, N. Castro-Rodriguez, Hien Nguyen, H. Aussel, A. Conley, David L. Clements, Chris Pearson, Asantha Cooray, Alexandre Amblard, D. V. Wiebe, Mat Page, P. Chanial, Michael Pohlen, Edo Ibar, G. Marsden, Ivan Valtchanov, Gillian S. Wright, Douglas Scott, L. R. Levenson, L. Vigroux, B. O'Halloran, Benjamin L. Schulz, P. Panuzzo, James J. Bock, E. L. Chapin, Jamie Stevens, Walter Kieran Gear, K. E. Tugwell, Tom Babbedge, Michael Zemcov, Rob Ivison, A. Boselli, Lingyu Wang, S. C. Madden, V. Buat, Matthew Joseph Griffin, Andrew Blain, C. K. Xu, Antonio Cava, Evanthia Hatziminaoglou, Nanyao Y. Lu, M. Symeonidis, K. G. Isaak, Jason Glenn, Seb Oliver, Lucia Marchetti, Michael Rowan-Robinson, V. Arumugam, N. Rangwala, C. D. Dowell, D. Elbaz, Nick Seymour, Alberto Franceschini, Markos Trichas, Mattia Vaccari, D. L. Shupe, Isaac Roseboom, A. Omont, A. J. Smith, Andreas Papageorgiou, I. Perez-Fournon, E. Dwek, D. Rizzo, Guilaine Lagache, Centre de recherches Paul Pascal (CRPP), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de photonique et de nanostructures (LPN), Centre National de la Recherche Scientifique (CNRS), AUTRES, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Department of Astronomy and Astrophysics [Universty of Toronto], University of Toronto, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Colloïdes et Matériaux Divisés (LCMD), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Cardiff], Cardiff University, Royal Observatory Edinburgh (ROE), University of Edinburgh, Division of Engineering, Colorado School of Mines, Science et Ingénierie des Matériaux et Procédés (SIMaP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National Polytechnique de Grenoble (INPG)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Service de Chimie Physique (SCP), Département de Physico-Chimie (DPC), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), Department of Chemistry and Biochemistry, University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), National Institute of Water and Atmospheric Research [Wellington] (NIWA), British Antarctic Survey (BAS), Natural Environment Research Council (NERC), Laboratoire de Mathématiques Raphaël Salem (LMRS), Université de Rouen Normandie (UNIROUEN), Normandie Université (NU)-Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut de Chimie du CNRS (INC)-Institut National Polytechnique de Grenoble (INPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), University of California-University of California, ESPCI ParisTech-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), CEA-Direction de l'Energie Nucléaire (CEA-DEN), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-CEA-Direction de l'Energie Nucléaire (CEA-DEN)

Subjects
Time delay and integration, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Measure (physics), FOS: Physical sciences, Astrophysics, 01 natural sciences, law.invention, law, 0103 physical sciences, medicine, Limit (mathematics), 010303 astronomy & astrophysics, QB, Confusion, media_common, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Photometer, Spire, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Sky, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], medicine.symptom, Noise (radio), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report on the sensitivity of SPIRE photometers on the Herschel Space Observatory. Specifically, we measure the confusion noise from observations taken during the Science Demonstration Phase of the Herschel Multi-tiered Extragalactic Survey. Confusion noise is defined to be the spatial variation of the sky intensity in the limit of infinite integration time, and is found to be consistent among the different fields in our survey at the level of 5.8, 6.3 and 6.8 mJy/beam at 250, 350 and 500 microns, respectively. These results, together with the measured instrument noise, may be used to estimate the integration time required for confusion-limited maps, and provide a noise estimate for maps obtained by SPIRE., Astronomy and Astrophysics, Herschel Special Issue, in press as a Letter; 5 pages

Published
2010

41. SANEPIC: a mapmaking method for time stream data from large arrays

Author

Marco Viero, Christopher Semisch, D. V. Wiebe, Jacob Klein, Peter Charles Hargrave, Calvin B. Netterfield, Marie Rex, David H. Hughes, J. J. Bock, Luca Olmi, G. S. Tucker, J. O. Gundersen, Matthew D. P. Truch, Douglas Scott, Simon Dicker, Carole Tucker, P. A. R. Ade, M. J. Devlin, Enzo Pascale, P. D. Mauskopf, E. L. Chapin, Gaelen Marsden, Mark Halpern, Peter G. Martin, G. Patanchon, Matthew Joseph Griffin, APC - Cosmologie, 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)-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), 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-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)), 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)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
Nuclear and High Energy Physics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], media_common.quotation_subject, FOS: Physical sciences, Inverse, Astrophysics, 01 natural sciences, Signal, law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Telescope, Methods: Data Analysis, Techniques: Image Processing, Sampling (signal processing), law, 0103 physical sciences, Submillimeter, 010303 astronomy & astrophysics, Computer memory, media_common, Physics, Balloons, 010308 nuclear & particles physics, Covariance matrix, Astrophysics (astro-ph), Detector, Astronomy and Astrophysics, Space and Planetary Science, Sky, Methods: data analysis, Techniques: image processing, Algorithm
Abstract

We describe a map-making method which we have developed for the Balloon-borne Large Aperture Submillimeter Telescope (BLAST) experiment, but which should have general application to data from other submillimeter arrays. Our method uses a Maximum Likelihood based approach, with several approximations, which allows images to be constructed using large amounts of data with fairly modest computer memory and processing requirements. This new approach, Signal And Noise Estimation Procedure Including Correlations (SANEPIC), builds upon several previous methods, but focuses specifically on the regime where there is a large number of detectors sampling the same map of the sky, and explicitly allowing for the the possibility of strong correlations between the detector timestreams. We provide real and simulated examples of how well this method performs compared with more simplistic map-makers based on filtering. We discuss two separate implementations of SANEPIC: a brute-force approach, in which the inverse pixel-pixel covariance matrix is computed; and an iterative approach, which is much more efficient for large maps. SANEPIC has been successfully used to produce maps using data from the 2005 BLAST flight., Comment: 27 Pages, 15 figures; Submitted to the Astrophysical Journal; related results available at http://blastexperiment.info/ [the BLAST Webpage]

Published
2008

42. The balloon-borne large aperture submillimeter telescope (blast) 2005: A 4 deg2 galactic plane survey in vulpecula (ℓ=59°)

Author

M. Rex, D. V. Wiebe, M. J. Devlin, E. L. Chapin, Simon Dicker, Jacob Klein, Douglas Scott, P. D. Mauskopf, David H. Hughes, Peter Charles Hargrave, Matthew Joseph Griffin, P. A. R. Ade, Christopher M. Brunt, Pierrick Martin, J. O. Gundersen, Mark Halpern, G. S. Tucker, Matthew D. P. Truch, Carole Tucker, Enzo Pascale, Calvin B. Netterfield, Marco Viero, Christopher Semisch, G. Patanchon, Luca Olmi, G. Marsden, and J. J. Bock

Subjects
Physics, 010504 meteorology & atmospheric sciences, Molecular cloud, Balloons, ISM: clouds, Stars: formation, Submillimeter, Nuclear and High Energy Physics, Space and Planetary Science, Perseus Arm, Astronomy and Astrophysics, Astrophysics, Galactic plane, 01 natural sciences, Galaxy, law.invention, Telescope, Stars, law, 0103 physical sciences, Protostar, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Open cluster
Abstract

We present the first results from a new 250, 350, and 500 micron Galactic Plane survey taken with the Balloon-borne Large-Aperture Submillimeter Telescope (BLAST) in 2005. This survey's primary goal is to identify and characterize high-mass proto-stellar objects (HMPOs). The region studied here covers 4 sq. deg near the open cluster NGC 6823 in the constellation Vulpecula (l=59). We find 60 compact sources ( 0) velocities combined with a variety of other velocity and morphological data in the literature. In total, 49 sources are associated with a molecular cloud complex encompassing NGC 6823 (distance ~2.3kpc), 10 objects with the Perseus Arm (~8.5kpc) and one object is probably in the outer Galaxy (~14kpc). Near NGC 6823, the inferred luminosities and masses of BLAST sources span ~40-10^4 L_\odot, and ~15-700 M_\odot, respectively. The mass spectrum is compatible with molecular gas masses in other high-mass star forming regions. Several luminous sources appear to be Ultra Compact HII regions powered by early B stars. However, many of the objects are cool, massive gravitationally-bound clumps with no obvious internal radiation from a protostar, and hence excellent HMPO candidates.

Published
2008

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