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46 results on '"Jeffrey P. Filippini"'

1. 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

2. 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

3. 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

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

Author

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

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

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

Published
2020

5. 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

6. 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

7. 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

8. 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

9. Characterizing the Sensitivity of 40 GHz TES Bolometers for BICEP Array

Author

A. C. Weber, John M Kovac, Kirit Karkare, Lorenzo Moncelsi, Abigail G. Vieregg, Denis Barkats, Kent D. Irwin, J. Kang, J. Cornelison, Marion Dierickx, Mark Halpern, Colin A. Bischoff, S. Fatigoni, B. Racine, Ki Won Yoon, R. Schwarz, K. G. Megerian, N. Precup, Howard Hui, T. Prouvé, A. Wandui, H. Boenish, Lionel Duband, Rashmikant V. Sudiwala, P. A. R. Ade, Zeeshan Ahmed, E. Young, Bryan Steinbach, H. T. Nguyen, Jeffrey P. Filippini, W. L. K. Wu, S. Kefeli, Chao Zhang, Mandana Amiri, J. Cheshire, Carole Tucker, S. Palladino, Carl D. Reintsema, King Tong Lau, Toshiya Namikawa, Roger O'Brient, C. D. Sheehy, Chao-Lin Kuo, Anthony D. Turner, Keith L. Thompson, James J. Bock, Benjamin L. Schmitt, Jake Connors, Sergi R. Hildebrandt, C. Pryke, E. Bullock, M. Crumrine, A. Cukierman, Eui-Hyeok Yang, J. Willmert, Donald V. Wiebe, S. Richter, Victor Buza, T. St. Germaine, R. Basu Thakur, Sarah M. Harrison, Che-Hang Yu, G. Hall, S. Henderson, Ahmed Soliman, C. Umiltà, Gene C. Hilton, E. Karpel, and Alessandro Schillaci

Subjects
Physics - Instrumentation and Detectors, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, Spectral line, 010305 fluids & plasmas, law.invention, law, 0103 physical sciences, General Materials Science, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Physics, Gravitational wave, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Instrumentation and Detectors (physics.ins-det), Spectral bands, Condensed Matter Physics, Polarization (waves), Atomic and Molecular Physics, and Optics, Gravitational lens, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The BICEP/Keck (BK) experiment aims to detect the imprint of primordial gravitational waves in the Cosmic Microwave Background polarization, which would be direct evidence of the inflation theory. While the tensor-to-scalar ratio has been constrained to be r_0.05 < 0.06 at 95% c.l., further improvements on this upper limit are hindered by polarized Galactic foreground emissions and removal of gravitational lensing polarization. The 30/40 GHz receiver of the BICEP Array (BA) will deploy at the end of 2019 and will constrain the synchrotron foreground with unprecedented accuracy within the BK sky patch. We will show the design of the 30/40 GHz detectors and test results summarizing its performance. The low optical and atmospheric loading at these frequencies requires our TES detectors to have low saturation power in order to be photon-noise dominated. To realize the low thermal conductivity required from a 250 mK base temperature, we developed new bolometer leg designs. We will present the relevant measured detector parameters: G, Tc, Rn, Psat , and spectral bands, and noise spectra. We achieved a per bolometer NEP including all noise components of 2.07E-17 W/sqrt(Hz), including an anticipated photon noise level 1.54E-17 W/sqrt(Hz)., Accepted for publication in Journal of Low Temperature Physics

Published
2020

10. 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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11. 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

12. 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

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

Author

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

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

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

Published
2018

14. A new limit on CMB circular polarization from SPIDER

Author

Marzieh Farhang, Michael R. Nolta, H. K. Eriksen, T. A. Morford, Juan D. Soler, M. Galloway, Carole Tucker, K. Ganga, Alexandra S. Rahlin, Kent D. Irwin, Carlo R. Contaldi, Peter A. R. Ade, Lorenzo Moncelsi, W. Holmes, Marcus Runyan, Jon E. Gudmundsson, S. Li, Calvin B. Netterfield, Katherine Freese, H. C. Chiang, A. E. Gambrel, E. Y. Young, J. R. Bond, A. A. Fraisse, Olivier Doré, Viktor Hristov, B. Racine, Ivan L. Padilla, P. V. Mason, Gene C. Hilton, Carl D. Reintsema, Zigmund Kermish, K. G. Megerian, Laura M. Fissel, Adri Duivenvoorden, Matthew Hasselfield, Zhiqi Huang, Ingunn Kathrine Wehus, X. Song, Jamil A. Shariff, Mark Halpern, Jeffrey P. Filippini, Amy Trangsrud, R. Bihary, Donald V. Wiebe, J. E. Ruhl, A. C. Weber, R. S. Tucker, Mandana Amiri, W. C. Jones, T. M. Ruud, Chao-Lin Kuo, A. S. Bergman, James J. Bock, Johanna Nagy, J. F. van der List, A. D. Turner, Sean Bryan, J. Hartley, Natalie N. Gandilo, Steven J. Benton, AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, SPIDER, 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), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Science and Technology Facilities Council (STFC), 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
0306 Physical Chemistry (Incl. Structural), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, cosmic background radiation: polarization, cosmic background radiation, 0305 Organic Chemistry, 01 natural sciences, Waveplate, law.invention, law, 010303 astronomy & astrophysics, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], QC, QB, Physics, Linear polarization, Astrophysics::Instrumentation and Methods for Astrophysics, Polarization (waves), SPIDER, Physical Sciences, astro-ph.CO, spectrum: thermal, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), SUBMILLIMETER INSTRUMENTS, Cosmic background radiation, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Electromagnetic radiation, Telescope, cosmic background radiation: B-mode, HALF-WAVE PLATE, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], cosmic background radiation: power spectrum, inflation, Instrumentation and Methods for Astrophysics (astro-ph.IM), Circular polarization, polarization: linear, Science & Technology, 010308 nuclear & particles physics, Astronomy and Astrophysics, Computational physics, 0201 Astronomical And Space Sciences, Space and Planetary Science, MICROWAVE BACKGROUND ASTRONOMY, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], astro-ph.IM
Abstract

We present a new upper limit on CMB circular polarization from the 2015 flight of SPIDER, a balloon-borne telescope designed to search for $B$-mode linear polarization from cosmic inflation. Although the level of circular polarization in the CMB is predicted to be very small, experimental limits provide a valuable test of the underlying models. By exploiting the non-zero circular-to-linear polarization coupling of the HWP polarization modulators, data from SPIDER's 2015 Antarctic flight provide a constraint on Stokes $V$ at 95 and 150 GHz from $33, Comment: 9 pages, 4 figures, 5 tables - Updated to version accepted for publication in ApJ, modified acknowledgements

Published
2017

15. CMB-S4 Technology Book, First Edition

Author

Shaul Hanany, Thomas Essinger-Hileman, Philip Daniel Mauskopf, Tijmen de Haan, Joaquin Vieira, Shawn W. Henderson, Charles A. Hill, Ki Won Yoon, Suzanne T. Staggs, Stephen C. Parshley, Lorenzo Moncelsi, Karl Young, C. Pryke, Abigail G. Vieregg, Gregory S. Tucker, Salatino Maria, John M Kovac, Adrian T. Lee, Michael D. Niemack, David T. Chuss, Aritoki Suzuki, Amy N. Bender, Peter T. Timbie, Kent D. Irwin, Eric R. Switzer, Jeffrey P. Filippini, N. W. Halverson, Ken Ganga, Ritoban Basu Thakur, Sean Bryan, Akito Kusaka, Zeeshan Ahmed, Edward J. Wollack, Stephen Padin, S. P. Ho, E. Y. Young, Andrew Nadolski, Karwan Rostem, Jon E. Gudmundsson, Natalie A. Roe, S. A. Kernasovskiy, Johannes Hubmayr, Maximilian H. Abitbol, Darcy Barron, Roger O'Brient, Jeff McMahon, Keith L. Thompson, Ari Cukierman, Benjamin Westbrook, Oliver Jeong, John E. Carlstrom, J. E. Ruhl, Sara M. Simon, Bradley R. Johnson, Matt Dobbs, Bradford Benson, Colin A. Bischoff, C. L. Chang, and Johanna Nagy

Subjects
Physics, media_common.quotation_subject, Cosmic microwave background, Dark matter, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, 02 engineering and technology, Astrophysics, Cosmic variance, 021001 nanoscience & nanotechnology, Polarization (waves), 01 natural sciences, Optical coupling, Universe, 0103 physical sciences, Dark energy, Neutrino, 0210 nano-technology, 010303 astronomy & astrophysics, media_common
Abstract

CMB-S4 is a proposed experiment to map the polarization of the Cosmic Microwave Background (CMB) to nearly the cosmic variance limit for the angular scales that are accessible from the ground. The science goals and capabilities of CMB-S4 in illuminating cosmic inflation, measuring the sum of neutrino masses, searching for relativistic relics in the early universe, characterizing dark energy and dark matter, and mapping the matter distribution in the universe have been described in the CMB-S4 Science Book. This Technology Book is a companion volume to the Science Book. The ambitious science goals of the proposed "Stage-IV" CMB-S4 will require a step forward in experimental capability from the current Stage-III experiments. To guide this process, the community summarized the current state of the technology and identify RD Receiver Optics; Focal-Plane Optical Coupling; and Focal-Plane Sensor and Readout.

Published
2017

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

Author

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

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

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

Published
2016

17. 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

18. CMB-S4 Science Book, First Edition

Author

Nicholas Battaglia, Daniel Green, Kam Arnold, Blake D. Sherwin, Joaquin Vieira, Tijmen de Haan, Marilena LoVerde, M. Lilley, Marco Peloso, Raphael Flauger, John M Kovac, Josquin Errard, Scott Watson, Cora Dvorkin, Tristan L. Smith, Stephen M. Feeney, P. D. Meerburg, Sperello di Serego Alighieri, Akito Kusaka, J. Colin Hill, Glenn D. Starkman, Zeeshan Ahmed, W. L. Holzapfel, George M. Fuller, Julian B. Muñoz, Maude Le Jeune, Chao-Lin Kuo, Nathan Whitehorn, Adam Mantz, Reijo Keskitalo, Marcel Schmittfull, Christian L. Reichardt, Julian Borrill, Victor Buza, Michael D. Niemack, Emmanuel Schaan, Giulio Fabbian, Simone Ferraro, T. M. Crawford, Lorenzo Sorbo, Mathew S. Madhavacheril, Jeff McMahon, Ely D. Kovetz, Kevork N. Abazajian, James G. Bartlett, Jason W. Henning, Lloyd Knox, Evan Grohs, J. Peloton, K. T. Story, Robert R. Caldwell, Erminia Calabrese, Francesco De Bernardis, Wayne Hu, Steven W. Allen, Levon Pogosian, Sarah Shandera, David J. E. Marsh, Amber Miller, Joel Meyers, Arthur Kosowsky, John E. Carlstrom, Carlo Baccigalupi, Joanna Dunkley, Kevin M. Huffenberger, C. Pryke, Jeffrey P. Filippini, Alexander van Engelen, Francis-Yan Cyr-Racine, Bradford Benson, Marco Raveri, Daniel Grin, Colin A. Bischoff, Ho Nam Nguyen, Neelima Sehgal, Aditya Rotti, C. L. Chang, Vera Gluscevic, Douglas Scott, W. L. Kimmy Wu, David Alonso, Adrian T. Lee, Renée Hlozek, Graca Rocha, Peter Adshead, and Gilbert Holder

Subjects
Physics, Gravitational wave, General relativity, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, Northern Hemisphere, Cosmic background radiation, Dark energy, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Neutrino, Polarization (waves)
Abstract

This book lays out the scientific goals to be addressed by the next-generation ground-based cosmic microwave background experiment, CMB-S4, envisioned to consist of dedicated telescopes at the South Pole, the high Chilean Atacama plateau and possibly a northern hemisphere site, all equipped with new superconducting cameras. CMB-S4 will dramatically advance cosmological studies by crossing critical thresholds in the search for the B-mode polarization signature of primordial gravitational waves, in the determination of the number and masses of the neutrinos, in the search for evidence of new light relics, in constraining the nature of dark energy, and in testing general relativity on large scales.

Published
2016

19. 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

20. 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

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

Author

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

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

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

Published
2016
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22. Initial Performance of BICEP3: A Degree Angular Scale 95 GHz Band Polarimeter

Author

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

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

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

Published
2016

23. BICEP3 focal plane design and detector performance

Author

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

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

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

Published
2016
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24. 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

25. Characterization and Fabrication of the TES Arrays for the Spider, Keck and BICEP2 CMB Polarimeters

Author

M. Lueker, A. D. Turner, W. C. Jones, Peter Day, John M Kovac, Angiola Orlando, M. Kenyon, W. A. Holmes, H. T. Nguyen, Chao-Lin Kuo, James J. Bock, Z. K. Staniszewski, R. V. Sudiwala, Marcus Runyan, Amy Trangsrud, Roger O'Brient, Sunil Golwala, J. A. Bonetti, Jeffrey P. Filippini, Justus A. Brevik, and Henry G. LeDuc

Subjects
Physics, Spider, Fabrication, business.industry, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Large format, Normal state, Condensed Matter Physics, Polarization (waves), Atomic and Molecular Physics, and Optics, Optics, General Materials Science, business, Transition edge, Device parameters, Remote sensing
Abstract

Spider, the Keck Array, and BICEP2 are projects to study the polarization of the cosmic microwave background (CMB). All three use large format arrays of antenna-coupled, membrane-isolated, transition edge sensors (TES’s). Although similar, each project requires its own set of device parameters, such as thermal conductance, time constants, and normal state resistances. We have perfected a fabrication process that achieves two primary objectives: (1) high device yields of 95% or greater, and (2) very low spreads in devices parameters. Currently our arrays are taking science data at the South Pole in both the BICEP2 and Keck array telescopes. The focal planes for Spider, a high altitude balloon mission, are on schedule for a 2012 deployment. An overview of fabrication and development is given as well as a snapshot of scientific data.

Published
2012

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

Author

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

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

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

Published
2015

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

Author

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

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

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

Published
2015

28. BICEP3: a 95GHz refracting telescope for degree-scale CMB polarization

Author

R. Bowens-Rubin, M. Amiri, C. Pryke, A. D. Turner, E. Karpel, K. L. Thompson, Howard Hui, Jake Connors, K. W. Yoon, R. W. Ogburn, J. J. Bock, John M Kovac, Kirit Karkare, Chao-Lin Kuo, Kent D. Irwin, H. Nguyen, J. A. Grayson, V. V. Hristov, I. Buder, Gene C. Hilton, Roger O'Brient, C. D. Reintsema, Stefan Richter, E. Bullock, Calvin B. Netterfield, Mark Halpern, W. L. K. Wu, Abigail G. Vieregg, Z. Ahmed, Jeffrey P. Filippini, J. Kang, S. J. Benton, Holland, Wayne S., and Zmuidzinas, Jonas

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), COSMIC cancer database, Pixel, business.industry, Cosmic microwave background, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Polarimetry, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), 7. Clean energy, law.invention, Cardinal point, Optics, law, Refracting telescope, Astrophysics - Instrumentation and Methods for Astrophysics, business, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

BICEP3 is a 550 mm-aperture refracting telescope for polarimetry of radiation in the cosmic microwave background at 95 GHz. It adopts the methodology of BICEP1, BICEP2 and the Keck Array experiments - it possesses sufficient resolution to search for signatures of the inflation-induced cosmic gravitational-wave background while utilizing a compact design for ease of construction and to facilitate the characterization and mitigation of systematics. However, BICEP3 represents a significant breakthrough in per-receiver sensitivity, with a focal plane area 5$\times$ larger than a BICEP2/Keck Array receiver and faster optics ($f/1.6$ vs. $f/2.4$). Large-aperture infrared-reflective metal-mesh filters and infrared-absorptive cold alumina filters and lenses were developed and implemented for its optics. The camera consists of 1280 dual-polarization pixels; each is a pair of orthogonal antenna arrays coupled to transition-edge sensor bolometers and read out by multiplexed SQUIDs. Upon deployment at the South Pole during the 2014-15 season, BICEP3 will have survey speed comparable to Keck Array 150 GHz (2013), and will significantly enhance spectral separation of primordial B-mode power from that of possible galactic dust contamination in the BICEP2 observation patch., 12 pages, 5 figures. Presented at SPIE Astronomical Telescopes and Instrumentation 2014: Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VII. To be published in Proceedings of SPIE Volume 9153

Published
2014

29. 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

30. Keck array and BICEP3: spectral characterization of 5000+ detectors

Author

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

Subjects
Physics, Spectrometer, business.industry, Gravitational wave, Cosmic microwave background, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), Spectral line, law.invention, Optics, law, Transition edge sensor, business
Abstract

The inflationary paradigm of the early universe predicts a stochastic background of gravitational waves which would generate a B-mode polarization pattern in the cosmic microwave background (CMB) at degree angular scales. Precise measurement of B-modes is one of the most compelling observational goals in modern cosmology. Since 2011, the Keck Array has deployed over 2500 transition edge sensor (TES) bolometer detectors at 100 and 150 GHz to the South Pole in pursuit of degree-scale B-modes, and Bicep3 will follow in 2015 with 2500 more at 100 GHz. Characterizing the spectral response of these detectors is important for controlling systematic effects that could lead to leakage from the temperature to polarization signal, and for understanding potential coupling to atmospheric and astrophysical emission lines. We present complete spectral characterization of the Keck Array detectors, made with a Martin-Puplett Fourier Transform Spectrometer at the South Pole, and preliminary spectra of Bicep3 detectors taken in lab. We show band centers and effective bandwidths for both Keck Array bands, and use models of the atmosphere at the South Pole to cross check our absolute calibration. Our procedure for obtaining interferograms in the field with automated 4-axis coupling to the focal plane represents an important step towards efficient and complete spectral characterization of next-generation instruments more than 10000 detectors.

Published
2014

31. Detection of B-mode polarization at degree angular scales by BICEP2

Author

Ki Won Yoon, Peter A. R. Ade, Abigail G. Vieregg, M. Lueker, Sunil Golwala, Carl D. Reintsema, Randol W. Aikin, Roger O'Brient, J. E. Tolan, E. Bullock, Jeffrey P. Filippini, C. L. Wong, John M Kovac, Kirit Karkare, C. D. Sheehy, Kent D. Irwin, S. Richter, A. Orlando, I. Buder, R. W. Ogburn, Viktor Hristov, Denis Barkats, Rashmikant V. Sudiwala, R. Schwarz, Z. K. Staniszewski, S. R. Hildebrandt, A. D. Turner, Justus A. Brevik, Grant Teply, Chao-Lin Kuo, H. T. Nguyen, James J. Bock, S. J. Benton, Gene C. Hilton, M. Hasselfield, E. M. Leitch, J. P. Kaufman, Mark Halpern, Calvin B. Netterfield, Brian Keating, C. D. Dowell, C. Pryke, Peter Mason, Colin A. Bischoff, S. Fliescher, L. Duband, and S. A. Kernasovskiy

Subjects
Physics, Spectral index, Cosmic microwave background, Antenna aperture, Cosmic background radiation, Astrophysics::Instrumentation and Methods for Astrophysics, General Physics and Astronomy, Spectral density, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), CMB cold spot, 13. Climate action, Observational cosmology, Astrophysics::Galaxy Astrophysics, QC, QB
Abstract

We report results from the BICEP2 experiment, a cosmic microwave background (CMB) polarimeter specifically designed to search for the signal of inflationary gravitational waves in the B-mode power spectrum around ℓ∼80. The telescope comprised a 26 cm aperture all-cold refracting optical system equipped with a focal plane of 512 antenna coupled transition edge sensor 150 GHz bolometers each with temperature sensitivity of ≈300 μK_(CMB)√s. BICEP2 observed from the South Pole for three seasons from 2010 to 2012. A low-foreground region of sky with an effective area of 380 square deg was observed to a depth of 87 nK deg in Stokes Q and U. In this paper we describe the observations, data reduction, maps, simulations, and results. We find an excess of B-mode power over the base lensed-ΛCDM expectation in the range 305σ. Through jackknife tests and simulations based on detailed calibration measurements we show that systematic contamination is much smaller than the observed excess. Cross correlating against WMAP 23 GHz maps we find that Galactic synchrotron makes a negligible contribution to the observed signal. We also examine a number of available models of polarized dust emission and find that at their default parameter values they predict power ∼(5–10)× smaller than the observed excess signal (with no significant cross-correlation with our maps). However, these models are not sufficiently constrained by external public data to exclude the possibility of dust emission bright enough to explain the entire excess signal. Cross correlating BICEP2 against 100 GHz maps from the BICEP1 experiment, the excess signal is confirmed with 3σ significance and its spectral index is found to be consistent with that of the CMB, disfavoring dust at 1.7σ. The observed B-mode power spectrum is well fit by a lensed-ΛCDM+tensor theoretical model with tensor-to-scalar ratio r=0.20^(+0.07)_(−0.05), with r=0 disfavored at 7.0σ. Accounting for the contribution of foreground, dust will shift this value downward by an amount which will be better constrained with upcoming data sets.

Published
2014

32. Degree-scale Cosmic Microwave Background Polarization Measurements from Three Years of BICEP1 Data

Author

E. M. Leitch, J. P. Kaufman, Colin A. Bischoff, W. C. Jones, Chao-Lin Kuo, James J. Bock, N. Ponthieu, P. V. Mason, C. D. Sheehy, Ki Won Yoon, Sarah S. Kernasovskiy, Peter A. R. Ade, Brian Keating, Randol W. Aikin, I. Buder, John M Kovac, Y. D. Takahashi, J. Battle, L. Duband, H. C. Chiang, W. L. Holzapfel, C. Pryke, E. M. Bierman, V. V. Hristov, Meng Su, H. T. Nguyen, S. Richter, Denis Barkats, G. Rocha, J. E. Tolan, E. Hivon, Tomotake Matsumura, C. D. Dowell, and Jeffrey P. Filippini

Subjects
Physics, Cold dark matter, 010308 nuclear & particles physics, Cosmic microwave background, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Lambda, Polarization (waves), 01 natural sciences, Measure (mathematics), Cosmology, Spectral line, Space and Planetary Science, Consistency (statistics), 0103 physical sciences, 010303 astronomy & astrophysics
Abstract

BICEP1 is a millimeter-wavelength telescope designed specifically to measure the inflationary B-mode polarization of the Cosmic Microwave Background (CMB) at degree angular scales. We present results from an analysis of the data acquired during three seasons of observations at the South Pole (2006 to 2008). This work extends the two-year result published in Chiang et al. (2010), with additional data from the third season and relaxed detector-selection criteria. This analysis also introduces a more comprehensive estimation of band-power window functions, improved likelihood estimation methods and a new technique for deprojecting monopole temperature-to-polarization leakage which reduces this class of systematic uncertainty to a negligible level. We present maps of temperature, E- and B-mode polarization, and their associated angular power spectra. The improvement in the map noise level and polarization spectra error bars are consistent with the 52% increase in integration time relative to Chiang et al. (2010). We confirm both self-consistency of the polarization data and consistency with the two-year results. We measure the angular power spectra at 21

Published
2014

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

Author

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

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

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

Published
2016

34. Antenna-coupled TES bolometers for the Keck Array, Spider, and Polar-1

Author

J. A. Bonetti, Donald V. Wiebe, P. Wilson, G. Davis, Gene C. Hilton, Zeeshan Ahmed, Carl D. Reintsema, Chao-Lin Kuo, M. Lueker, R. Sudiwala, James J. Bock, V. V. Hristov, John M Kovac, W. L. K. Wu, R. W. Aikin, J. E. Tolan, Roger O'Brient, Jeffrey P. Filippini, E. M. Leitch, C. L. Wong, B. Burger, Kent D. Irwin, Howard Hui, Z. K. Staniszewski, Colin A. Bischoff, R. W. Ogburn, J. E. Ruhl, R. S. Tucker, A. D. Turner, Mandana Amiri, C. D. Dowell, S. Fliescher, Grant Teply, C. D. Sheehy, Ki Won Yoon, M. Hasselfield, J. A. Grayson, Justus A. Brevik, K. G. Megerian, Marcus Runyan, Calvin B. Netterfield, H. T. Nguyen, S. J. Benton, R. Schwarz, S. A. Kernasovskiy, C. Pryke, Sunil Golwala, L. Duband, Mark Halpern, Peter A. R. Ade, Lorenzo Moncelsi, Abigail G. Vieregg, Peter K. Day, Holland, Wayne S., and Zmuidzinas, Jonas

Subjects
Physics, business.industry, Cosmic microwave background, Bolometer, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), Microstrip, law.invention, Optics, Planar, law, Side lobe, business, Penetration depth, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

Between the BICEP2 and Keck Array experiments, we have deployed over 1500 dual polarized antenna coupled bolometers to map the Cosmic Microwave Background's polarization. We have been able to rapidly deploy these detectors because they are completely planar with an integrated phased-array antenna. Through our experience in these experiments, we have learned of several challenges with this technology- specifically the beam synthesis in the antenna- and in this paper we report on how we have modified our designs to mitigate these challenges. In particular, we discus differential steering errors between the polarization pairs' beam centroids due to microstrip cross talk and gradients of penetration depth in the niobium thin films of our millimeter wave circuits. We also discuss how we have suppressed side lobe response with a Gaussian taper of our antenna illumination pattern. These improvements will be used in Spider, Polar-1, and this season's retrofit of Keck Array., Comment: Presented at SPIE Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI, July 6, 2012. To be published in Proceedings of SPIE Volume 8452

Published
2012

35. 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

36. BICEP2 and Keck array operational overview and status of observations

Author

John M Kovac, Kent D. Irwin, M. C. Runyan, Brian Keating, M. Lueker, C. Pryke, J. E. Tolan, Roger O'Brient, H. T. Nguyen, A. Orlando, C. D. Dowell, Justus A. Brevik, J. A. Bonetti, Keith L. Thompson, S. J. Benton, L. Duband, S. A. Kernasovskiy, Colin A. Bischoff, R. Schwarz, R. W. Ogburn, V. V. Hristov, Anthony D. Turner, C. D. Sheehy, Sunil Golwala, E. Bullock, C. L. Wong, M. Hasselfield, J. P. Kaufman, B. Burger, E. M. Leitch, S. Fliescher, Rashmikant V. Sudiwala, Gene C. Hilton, P. Wilson, Peter A. R. Ade, Jeffrey P. Filippini, Calvin B. Netterfield, Abigail G. Vieregg, Z. K. Staniszewski, J. E. Ruhl, Michael S. Gordon, Mark Halpern, R. W. Aikin, S. Richter, T. E. Montroy, G. P. Teply, Carl D. Reintsema, Donald V. Wiebe, G. Davis, Chao-Lin Kuo, James J. Bock, Howard Hui, Mandana Amiri, Holland, Wayne S., and Zmuidzinas, Jonas

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Cosmic microwave background, Detector, FOS: Physical sciences, Astronomy, Polarization (waves), 01 natural sciences, 0103 physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The BICEP2 and Keck Array experiments are designed to measure the polarization of the cosmic microwave background (CMB) on angular scales of 2-4 degrees (l=50-100). This is the region in which the B-mode signal, a signature prediction of cosmic inflation, is expected to peak. BICEP2 was deployed to the South Pole at the end of 2009 and is in the middle of its third year of observing with 500 polarization-sensitive detectors at 150 GHz. The Keck Array was deployed to the South Pole at the end of 2010, initially with three receivers--each similar to BICEP2. An additional two receivers have been added during the 2011-12 summer. We give an overview of the two experiments, report on substantial gains in the sensitivity of the two experiments after post-deployment optimization, and show preliminary maps of CMB polarization from BICEP2., Presented at SPIE Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VI, July 6, 2012. To be published in Proceedings of SPIE Volume 8452

Published
2012

37. Optical Characterization of the Keck Array Polarimeter at the South Pole

Author

Roger O'Brient, Chao-Lin Kuo, M. Lueker, T. E. Montroy, John M Kovac, James J. Bock, H. T. Nguyen, Z. K. Staniszewski, G. P. Teply, C. Pryke, Colin A. Bischoff, Anthony D. Turner, R. Schwarz, Calvin B. Netterfield, L. Duband, J. E. Tolan, C. L. Wong, K. J. Bradford, Mark Halpern, V. V. Hristov, Michael S. Gordon, R. W. Ogburn, R. W. Aikin, M. C. Runyan, Kent D. Irwin, Rashmikant V. Sudiwala, C. D. Dowell, E. M. Leitch, S. Fliescher, P. Wilson, Sarah S. Kernasovskiy, Peter A. R. Ade, Abigail G. Vieregg, Gene C. Hilton, J. A. Bonetti, Sunil Golwala, Jeffrey P. Filippini, C. D. Sheehy, J. E. Ruhl, Justus A. Brevik, Holland, Wayne S., and Zmuidzinas, J.

Subjects
Physics, Large field of view, business.industry, Detector, Cosmic microwave background, Polarimetry, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Polarimeter, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), 01 natural sciences, Summer season, Optics, 0103 physical sciences, 14. Life underwater, 010306 general physics, business, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Microwave
Abstract

The Keck Array (SPUD) is a set of microwave polarimeters that observes from the South Pole at degree angular scales in search of a signature of Inflation imprinted as B-mode polarization in the Cosmic Microwave Background (CMB). The first three Keck Array receivers were deployed during the 2010-2011 Austral summer, followed by two new receivers in the 2011-2012 summer season, completing the full five-receiver array. All five receivers are currently observing at 150 GHz. The Keck Array employs the field-proven BICEP/BICEP2 strategy of using small, cold, on-axis refractive optics, providing excellent control of systematics while maintaining a large field of view. This design allows for full characterization of far-field optical performance using microwave sources on the ground. We describe our efforts to characterize the main beam shape and beam shape mismatch between co-located orthogonally-polarized detector pairs, and discuss the implications of measured differential beam parameters on temperature to polarization leakage in CMB analysis., Comment: 13 pages, 11 figures, Proceedings of the SPIE, Vol 8452: Millimeter, Submillimeter and Far-Infrared Detectors and Instrumentation for Astronomy VI, July 2012

Published
2012
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38. Design and performance of the Spider instrument

Author

Amy Trangsrud, Kent D. Irwin, S. J. Benton, Marzieh Farhang, Alexandra S. Rahlin, Carlo R. Contaldi, Jeffrey P. Filippini, M. Hasselfield, Peter A. R. Ade, Mark Halpern, Jamil A. Shariff, Olivier Doré, R. Bihary, Anthony D. Turner, Marcus Runyan, John Bond, T. A. Morford, Calvin B. Netterfield, Sunil Golwala, Carole Tucker, H. C. Chiang, Jon E. Gudmundsson, Sean Bryan, Peter Mason, Carl D. Reintsema, Natalie N. Gandilo, Viktor Hristov, W. C. Jones, Laura M. Fissel, J. E. Ruhl, Juan D. Soler, T. E. Montroy, J. A. Bonetti, D. O'Dea, Warren Holmes, Matthew A. Schenker, R. S. Tucker, Mandana Amiri, Chao-Lin Kuo, James J. Bock, B. P. Crill, C. J. MacTavish, Gene C. Hilton, Holland, Wayne S., and Zmuidzinas, Jonas

Subjects
Spider, 010308 nuclear & particles physics, Computer science, business.industry, media_common.quotation_subject, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Design elements and principles, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), 01 natural sciences, Multiplexer, Optics, Cardinal point, Sky, 0103 physical sciences, Electromagnetic shielding, 010306 general physics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), media_common
Abstract

Here we describe the design and performance of the Spider instrument. Spider is a balloon-borne cosmic microwave background polarization imager that will map part of the sky at 90, 145, and 280 GHz with sub-degree resolution and high sensitivity. This paper discusses the general design principles of the instrument inserts, mechanical structures, optics, focal plane architecture, thermal architecture, and magnetic shielding of the TES sensors and SQUID multiplexer. We also describe the optical, noise, and magnetic shielding performance of the 145 GHz prototype instrument insert., 12 pages, 5 figures, Proceedings of SPIE, Astronomical Telescopes and Instrumentation 2010, San Diego, CA

Published
2011

39. Optical performance of the BICEP2 Telescope at the South Pole

Author

Brian Keating, J. A. Bonetti, John M Kovac, V. V. Hristov, Lionel Duband, C. D. Sheehy, Andrew E. Lange, S. Stokes, Kent D. Irwin, Jeffrey P. Filippini, M. C. Runyan, J. E. Tolan, S. J. Benton, Justus A. Brevik, R. W. Ogburn, C. L. Wong, Anthony D. Turner, Rashmikant V. Sudiwala, J. P. Kaufman, J. E. Ruhl, Sunil Golwala, Peter A. R. Ade, Angiola Orlando, R. W. Aikin, P. Wilson, C. Pryke, C. D. Dowell, Calvin B. Netterfield, H. T. Nguyen, G. P. Teply, S. Richter, Chao-Lin Kuo, James J. Bock, Mark Halpern, Holland, Wayne S., and Zmuidzinas, Jonas

Subjects
Physics, business.industry, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmic background radiation, Near and far field, Astrophysics::Cosmology and Extragalactic Astrophysics, Ghost imaging, Polarization (waves), Cosmology, law.invention, Telescope, Optics, law, business, Microwave
Abstract

Bicep2 deployed to the South Pole during the 2009-2010 austral summer, and is now mapping the polarization of the cosmic microwave background (CMB), searching for evidence of inflationary cosmology. Bicep2 belongs to a new class of telescopes including Keck (ground-based) and Spider (balloon-borne) that follow on Bicep's strategy of employing small, cold, on-axis refracting optics. This common design provides key advantages ideal for targeting the polarization signature from inflation, including: (i) A large field of view, allowing substantial light collecting power despite the small aperture, while still resolving the degree-scale polarization of the CMB; (ii) liquid helium-cooled optics and cold stop, allowing for low, stable instrument loading; (iii) the ability to rotate the entire telescope about the boresight; (iv) a baffled primary aperture, reducing sidelobe pickup; and (v) the ability to characterize the far field optical performance of the telescope using ground-based sources. We describe the last of these advantages in detail, including our efforts to measure the main beam shape, beammatch between orthogonally-polarized pairs, polarization efficiency and response angle, sidelobe pickup, and ghost imaging. We do so with ground-based polarized microwave sources mounted in the far field as well as with astronomical calibrators. Ultimately, Bicep2's sensitivity to CMB polarization from inflation will rely on precise calibration of these beam features.

Published
2010

40. Modeling and characterization of the SPIDER half-wave plate

Author

B. P. Crill, J. A. Bonetti, Matthew Hasselfield, Warren Holmes, Jamil A. Shariff, Jeffrey P. Filippini, Kent D. Irwin, D. O'Dea, Viktor Hristov, R. Bihary, Laura M. Fissel, C. Barth Netterfield, Carl D. Reintsema, Carlo R. Contaldi, T. A. Morford, Peter A. R. Ade, Peter Mason, Alexandra S. Rahlin, S. J. Benton, Juan D. Soler, Mark Halpern, H. Cynthia Chiang, Kyle Helson, Daniel Riley, Olivier Doré, Sunil Golwala, Jon E. Gudmundsson, Matthew A. Schenker, Anthony D. Turner, Marcus Runyan, T. E. Montroy, Amy Transrud, Sean Bryan, Natalie N. Gandilo, J. Richard Bond, C. J. MacTavish, J. E. Ruhl, Gene C. Hilton, Carole Tucker, W. C. Jones, Marzieh Farhang, Chao-Lin Kuo, James J. Bock, R. S. Tucker, Mandana Amiri, Holland, Wayne S., and Zmuidzinas, Jonas

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics::Instrumentation and Detectors, business.industry, Bolometer, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Physical optics, Polarization (waves), Waveplate, Particle detector, law.invention, Telescope, Optics, law, Astrophysics - Instrumentation and Methods for Astrophysics, business, Instrumentation and Methods for Astrophysics (astro-ph.IM), Microwave, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Spider is a balloon-borne array of six telescopes that will observe the Cosmic Microwave Background. The 2624 antenna-coupled bolometers in the instrument will make a polarization map of the CMB with approximately one-half degree resolution at 145 GHz. Polarization modulation is achieved via a cryogenic sapphire half-wave plate (HWP) skyward of the primary optic. We have measured millimeter-wave transmission spectra of the sapphire at room and cryogenic temperatures. The spectra are consistent with our physical optics model, and the data gives excellent measurements of the indices of A-cut sapphire. We have also taken preliminary spectra of the integrated HWP, optical system, and detectors in the prototype Spider receiver. We calculate the variation in response of the HWP between observing the CMB and foreground spectra, and estimate that it should not limit the Spider constraints on inflation.

Published
2010

41. Initial performance of the BICEP2 antenna-coupled superconducting bolometers at the South Pole

Author

J. E. Tolan, R. Sudiwala, R. W. Ogburn, John M Kovac, Charles D. Dowell, Kent D. Irwin, C. D. Sheehy, S. Richter, L. Duband, P. Wilson, Jeffrey P. Filippini, Carl D. Reintsema, J. E. Ruhl, Randol W. Aikin, S. J. Benton, M. Hasselfield, Marcus Runyan, Calvin B. Netterfield, Brian Keating, Mark Halpern, Mandana Amiri, Sunil Golwala, B. Burger, Justus A. Brevik, Andrew E. Lange, C. L. Wong, Viktor Hristov, C. Pryke, J. A. Bonetti, H. T. Nguyen, Chao-Lin Kuo, E. M. Leitch, James J. Bock, J. P. Kaufman, Gene C. Hilton, Angiola Orlando, Z. K. Staniszewski, A. D. Turner, Holland, Wayne S., and Zmuidzinas, Jonas

Subjects
Physics, Pixel, Physics::Instrumentation and Detectors, business.industry, Bolometer, Detector, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, Polarization (waves), Multiplexer, Microstrip, Particle detector, law.invention, Optics, law, business
Abstract

We report on the preliminary detector performance of the B icep 2 mm-wave p olarimeter, deployed in 2009 tothe South Pole. B icep 2 is currently imaging the polarization of the cosmic micro wave bac kground at 150 GHzusing an array of 512 antenna-coupled superconducting bolometers. The antennas, band-de“ning “lters andtransition edge sensor (TES) bolometers are photolithographically fabricated on 4 silicon tiles. Each tile consistsof an 8 × 8 grid of 7 mm spatial pixels, for a total of 256 detector pairs. A spatial pixel contains 2 sets oforthogonal antenna slots summed in-phase, with each set coupled to a TES by a “ltered microstrip. The detectorsare read out using time-domain multiplexed SQUIDs. The detector pair of each spatial pixel is dierenced tomeasure polarization. We report on the performance of the B icep 2 detectors in the “eld, including the focalplane yield, detector and multiplexer optimization, detector noise and stability, and a preliminary estimate ofthe improvement in mapping speed compared to B icep 1.Keywords: Cosmic micr owave bac kground, polarization, TES, noise, in”ation, gravitational waves, cosmology

Published
2010

42. Antenna-coupled TES Bolometer Arrays for BICEP2/Keck and SPIDER

Author

B. Burger, P. R. Wilson, R. Sudiwala, J. A. Bonetti, Sunil Golwala, Amy Trangsrud, John M Kovac, Nuria Llombart, M. Kenyon, Kent D. Irwin, Andrew E. Lange, Henry G. LeDuc, Mandana Amiri, M. Hasselfield, H. T. Nguyen, Anthony D. Turner, Chao-Lin Kuo, Jeffrey P. Filippini, James J. Bock, G. Chattopadthyay, Justus A. Brevik, Abigail Claire Orlando, Gene C. Hilton, R. W. Ogburn, Z. K. Staniszewski, R. W. Aikin, Carl D. Reintsema, Marcus Runyan, Peter K. Day, Mark Halpern, G. P. Teply, Holland, Wayne S., and Zmuidzinas, Jonas

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), business.industry, Cosmic microwave background, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), Multiplexer, law.invention, Planar, Cardinal point, Optics, law, NIST, business, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

BICEP2/Keck and SPIDER are cosmic microwave background (CMB) polarimeters targeting the B-mode polarization induced by primordial gravitational waves from inflation. They will be using planar arrays of polarization sensitive antenna-coupled TES bolometers, operating at frequencies between 90 GHz and 220 GHz. At 150 GHz each array consists of 64 polarimeters and four of these arrays are assembled together to make a focal plane, for a total of 256 dual-polarization elements (512 TES sensors). The detector arrays are integrated with a time-domain SQUID multiplexer developed at NIST and read out using the multi-channels electronics (MCE) developed at the University of British Columbia. Following our progress in improving detector parameters uniformity across the arrays and fabrication yield, our main effort has focused on improving detector arrays optical and noise performances, in order to produce science grade focal planes achieving target sensitivities. We report on changes in detector design implemented to optimize such performances and following focal plane arrays characterization. BICEP2 has deployed a first 150 GHz science grade focal plane to the South Pole in December 2009., Comment: 10 pages, 7 figures; SPIE proceedings for Millimeter, Submillimeter and Far-Infrared Detectors and Instrumentation for Astronomy V (Conference 7741, June 2010, San Diego, CA, USA)

Published
2010
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43. BICEP2. II. EXPERIMENT AND THREE-YEAR DATA SET

Author

J. E. Tolan, R. W. Ogburn, Ki Won Yoon, Gene C. Hilton, M. Lueker, S. R. Hildebrandt, C. D. Sheehy, P. Wilson, Denis Barkats, Matthew Hasselfield, S. Fliescher, J. P. Kaufman, Chao-Lin Kuo, Grant Teply, Nuria Llombart, John M Kovac, Kirit Karkare, James J. Bock, Peter A. R. Ade, L. Duband, G. Davis, A. D. Turner, Kent D. Irwin, K. T. Story, I. Buder, M. Amiri, Abigail G. Vieregg, C. Pryke, R. Sudiwala, Randol W. Aikin, S. A. Kernasovskiy, C. D. Reintsema, Brian Keating, C. L. Wong, Roger O'Brient, S. Richter, Viktor Hristov, Colin A. Bischoff, E. M. Leitch, H. T. Nguyen, Z. K. Staniszewski, S. J. Benton, Mark Halpern, Calvin B. Netterfield, C. D. Dowell, R. Schwarz, Sunil Golwala, E. Bullock, Justus A. Brevik, Jeffrey P. Filippini, and A. Orlando

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, law.invention, Telescope, Optics, law, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, business.industry, Gravitational wave, Detector, Antenna aperture, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, Astronomy and Astrophysics, Polarization (waves), Square degree, Space and Planetary Science, Astrophysics - Instrumentation and Methods for Astrophysics, business, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report on the design and performance of the BICEP2 instrument and on its three-year data set. BICEP2 was designed to measure the polarization of the cosmic microwave background (CMB) on angular scales of 1 to 5 degrees ($\ell$=40-200), near the expected peak of the B-mode polarization signature of primordial gravitational waves from cosmic inflation. Measuring B-modes requires dramatic improvements in sensitivity combined with exquisite control of systematics. The BICEP2 telescope observed from the South Pole with a 26~cm aperture and cold, on-axis, refractive optics. BICEP2 also adopted a new detector design in which beam-defining slot antenna arrays couple to transition-edge sensor (TES) bolometers, all fabricated on a common substrate. The antenna-coupled TES detectors supported scalable fabrication and multiplexed readout that allowed BICEP2 to achieve a high detector count of 500 bolometers at 150 GHz, giving unprecedented sensitivity to B-modes at degree angular scales. After optimization of detector and readout parameters, BICEP2 achieved an instrument noise-equivalent temperature of 15.8 $\mu$K sqrt(s). The full data set reached Stokes Q and U map depths of 87.2 nK in square-degree pixels (5.2 $\mu$K arcmin) over an effective area of 384 square degrees within a 1000 square degree field. These are the deepest CMB polarization maps at degree angular scales to date. The power spectrum analysis presented in a companion paper has resulted in a significant detection of B-mode polarization at degree scales., Comment: 30 pages, 24 figures

Published
2014

44. SPIDER: probing the early Universe with a suborbital polarimeter

Author

C. N. Clark, Carole Tucker, J. A. Bonetti, H. C. Chiang, Marzieh Farhang, Warren Holmes, B. P. Crill, R. S. Tucker, Amy Trangsrud, Mandana Amiri, W. C. Jones, Marcus Runyan, Jamil A. Shariff, Calvin B. Netterfield, Peter A. R. Ade, Juan D. Soler, Sunil Golwala, Viktor Hristov, A. A. Fraisse, Laura M. Fissel, Carl D. Reintsema, T. E. Montroy, C. J. MacTavish, Sean Bryan, Kent D. Irwin, Carlo R. Contaldi, G. Davis, Gene C. Hilton, Natalie N. Gandilo, Matthew A. Schenker, Chao-Lin Kuo, J. R. Bond, Jeffrey P. Filippini, T. A. Morford, B. Burger, Jon E. Gudmundsson, James J. Bock, Alexandra S. Rahlin, J. E. Ruhl, S. J. Benton, M. Hasselfield, O. Doré, Anthony D. Turner, D. O'Dea, Peter Mason, and Donald V. Wiebe

Subjects
Physics, Systematic error, Spider, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Polarimeter, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Polarization (waves), 01 natural sciences, symbols.namesake, Amplitude, 0103 physical sciences, symbols, Stokes parameters, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmic dust
Abstract

We evaluate the ability of SPIDER, a balloon-borne polarimeter, to detect a divergence-free polarization pattern ("B-modes") in the Cosmic Microwave Background (CMB). In the inflationary scenario, the amplitude of this signal is proportional to that of the primordial scalar perturbations through the tensor-to-scalar ratio r. We show that the expected level of systematic error in the SPIDER instrument is significantly below the amplitude of an interesting cosmological signal with r=0.03. We present a scanning strategy that enables us to minimize uncertainty in the reconstruction of the Stokes parameters used to characterize the CMB, while accessing a relatively wide range of angular scales. Evaluating the amplitude of the polarized Galactic emission in the SPIDER field, we conclude that the polarized emission from interstellar dust is as bright or brighter than the cosmological signal at all SPIDER frequencies (90 GHz, 150 GHz, and 280 GHz), a situation similar to that found in the "Southern Hole." We show that two ~20-day flights of the SPIDER instrument can constrain the amplitude of the B-mode signal to r, 29 pages, 8 figures, 4 tables; v2: matches published version, flight schedule updated, two typos fixed in Table 2, references and minor clarifications added, results unchanged

Published
2013

45. SPIDER OPTIMIZATION. II. OPTICAL, MAGNETIC, AND FOREGROUND EFFECTS

Author

C. N. Clark, T. E. Montroy, John Bond, B. P. Crill, H. C. Chiang, Amy Trangsrud, Olivier Doré, Peter A. R. Ade, Sean Bryan, Natalie N. Gandilo, Sunil Golwala, J. A. Bonetti, Donald V. Wiebe, Matthew A. Schenker, Carl D. Reintsema, Jamil A. Shariff, Kent D. Irwin, Warren Holmes, Peter Mason, Carlo R. Contaldi, G. Davis, Jeffrey P. Filippini, Alexandra S. Rahlin, Viktor Hristov, D. O'Dea, Anthony D. Turner, M. Hasselfield, C. J. MacTavish, Gene C. Hilton, Laura M. Fissel, Marcus Runyan, Marzieh Farhang, Calvin B. Netterfield, T. A. Morford, Jon E. Gudmundsson, Chao-Lin Kuo, Juan D. Soler, S. J. Benton, J. E. Ruhl, James J. Bock, W. C. Jones, A. A. Fraisse, R. S. Tucker, Mandana Amiri, B. Burger, and Carole Tucker

Subjects
Physics, Spider, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Gravitational wave, media_common.quotation_subject, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmic background radiation, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Polarization (waves), Cosmology, Amplitude, Space and Planetary Science, Sky, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, media_common
Abstract

Spider is a balloon-borne instrument designed to map the polarization of the cosmic microwave background (CMB) with degree-scale resolution over a large fraction of the sky. Spider's main goal is to measure the amplitude of primordial gravitational waves through their imprint on the polarization of the CMB if the tensor-to-scalar ratio, r, is greater than 0.03. To achieve this goal, instrumental systematic errors must be controlled with unprecedented accuracy. Here, we build on previous work to use simulations of Spider observations to examine the impact of several systematic effects that have been characterized through testing and modeling of various instrument components. In particular, we investigate the impact of the non-ideal spectral response of the half-wave plates, coupling between focal plane components and the Earth's magnetic field, and beam mismatches and asymmetries. We also present a model of diffuse polarized foreground emission based on a three-dimensional model of the Galactic magnetic field and dust, and study the interaction of this foreground emission with our observation strategy and instrumental effects. We find that the expected level of foreground and systematic contamination is sufficiently low for Spider to achieve its science goals., submitted to APJ, 15 pages, 12 figures

Published
2011

46. SPIDER: CMB polarimetry from the edge of space

Author

Carlo R. Contaldi, A. C. Weber, A. E. Gambrel, S. Li, W. Holmes, Carl D. Reintsema, Katherine Freese, W. C. Jones, T. M. Ruud, Alexandra S. Rahlin, Juan D. Soler, Steven J. Benton, Johanna Nagy, John Bond, Mark Halpern, J. F. van der List, Jon E. Gudmundsson, A. S. Bergman, X. Song, Chao-Lin Kuo, James J. Bock, P. V. Mason, Ingunn Kathrine Wehus, Zhiqi Huang, H. C. Chiang, O. Doré, Ivan L. Padilla, B. Osherson, Adri Duivenvoorden, Matthew Hasselfield, Marcus Runyan, M. Galloway, Calvin B. Netterfield, J. E. Ruhl, Carole Tucker, Gene C. Hilton, R. V. Gramillano, Sean Bryan, Jamil A. Shariff, Peter A. R. Ade, R. S. Tucker, Mandana Amiri, Lorenzo Moncelsi, J. Hartley, Kent D. Irwin, Natalie N. Gandilo, R. Gualtieri, Ken Ganga, Viktor Hristov, Amy Trangsrud, Michael R. Nolta, Laura M. Fissel, E. Y. Young, Jeffrey P. Filippini, Zigmund Kermish, Anthony D. Turner, Marzieh Farhang, B. Racine, K. G. Megerian, R. Bihary, Donald V. Wiebe, A. A. Fraisse, H. K. Eriksen, T. A. Morford, 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), 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), SPIDER, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Science and Technology Facilities Council (STFC), and Science and Technology Facilities Council

Subjects
Cosmic microwave background, cosmic background radiation, 01 natural sciences, General Materials Science, 010303 astronomy & astrophysics, media_common, Physics, 0105 Mathematical Physics, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, BICEP, Condensed Matter Physics, Polarization (waves), Bolometers, SPIDER, detector: upgrade, Atomic and Molecular Physics, and Optics, Physics, Condensed Matter, B-mode, Physical Sciences, astro-ph.CO, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, General Physics, Transition-edge sensors, Cosmology and Nongalactic Astrophysics (astro-ph.CO), detector: performance, media_common.quotation_subject, 0204 Condensed Matter Physics, Cosmic background radiation, Polarimetry, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Physics, Applied, 0203 Classical Physics, 0103 physical sciences, transition edge sensors, [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, Spider, Science & Technology, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: primordial, Inflation, polarization: monitoring, Sky, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], astro-ph.IM
Abstract

SPIDER is a balloon-borne instrument designed to map the polarization of the millimeter-wave sky at large angular scales. SPIDER targets the B-mode signature of primordial gravitational waves in the cosmic microwave background (CMB), with a focus on mapping a large sky area with high fidelity at multiple frequencies. SPIDER's first longduration balloon (LDB) flight in January 2015 deployed a total of 2400 antenna-coupled Transition Edge Sensors (TESs) at 90 GHz and 150 GHz. In this work we review the design and in-flight performance of the SPIDER instrument, with a particular focus on the measured performance of the detectors and instrument in a space-like loading and radiation environment. SPIDER's second flight in December 2018 will incorporate payload upgrades and new receivers to map the sky at 285 GHz, providing valuable information for cleaning polarized dust emission from CMB maps., Comment: 10 pages, 7 figures, LTD17 Conference

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