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BICEP2 VISUALS
BICEP2 Focal Plane. The BICEP2 telescope's focal plane consisting of an array of 512 superconducting bolometers, designed to operate at 0.25 K (0.25 degrees Celsius above absolute zero) in order to reduce thermal noise in the detectors. The focal plane was developed andproduced at
FIGURES FROM BK-X: CONSTRAINTS ON PRIMORDIAL GRAVITATIONAL Figures Download Bundle; BK15 E-mode maps: Figure 1: Maps of degree angular scale E-modes (50 < ℓ < 120) at three frequencies made using Keck Array data from the 2015 season only. The similarity of the pattern indicates that ΛCDM E-modes dominate at all three frequencies (and that the signal-to-noise is high).The color scale is in μK, and the range is allowed to vary slightly to (partially FIGURES FROM BK-III: INSTRUMENTAL SYSTEMATICS Figures from BK-III: Instrumental Systematics. Figure 1: Map coverage of a single BICEP2 detector pair located (top panel) near the edge of the focal plane and (bottom panel) near the center of the focal plane. The coverage at different deck angles overlaps significantly for KECK ARRAY/BICEP2 OCTOBER 2015 DATA PRODUCTS History. 2017-05-24: Added BK14 apodization mask. 2016-09-13: Updated CosmoMC tarball for backwards compatibility with BKPlanck version. 2015-10-30: Added bandpowers, CosmoMC tarball, r likelihood text file, and component separated spectra. KECK ARRAY/BICEP2 OCTOBER 2018 DATA PRODUCTS BK-X: Constraints on Primordial Gravitational Waves Using Planck, WMAP, and New BICEP2/Keck Observations through the 2015 Season TheKeck Array and
BICEP2 2014 RELEASE FREQUENTLY ASKED QUESTIONS BICEP2 is the second stage of a coordinated program, the BICEP and Keck Array series of experiments, developed for the South Pole. This coordinated program has a co-PI structure. The four PIs of this series are John Kovac ( Harvard ), Clem Pryke ( UMN ), Jamie Bock ( Caltech/JPL ), and Chao-Lin Kuo ( Stanford/SLAC ). MICROWAVE MULTIPLEXING ON THE KECK ARRAY Microwave multiplexing on the Keck Array 3 the TES current changes, the magnetic flux and, therefore, the resonant frequency change, i.e., the TES signal is transduced to a shift in resonant frequency. DESIGN AND CHARACTERIZATION OF ANTENNA-COUPLED 30/40 GHZ Journal of Low Temperature Physics manuscript No. (will be inserted by the editor) Design and Characterization of Antenna-Coupled 30/40 GHz Detectors and Modules for the BICEP Array Experiment BICEP2 MARCH 2014 RESULTS AND DATA PRODUCTS BICEP2 March 2014 Results and Data Products. 1. BICEP2 2014 Release Papers. 2. BICEP2 2014 Release Data Products. Text file containing the tabulated likelihood for the tensor-to-scalar ratio, r, computed using the “direct likelihood calculation” described in Section THE BICEP AND KECK ARRAY CMB EXPERIMENTSFIGURES FROM BK-VIIFIGURES FROM BK-IIIFIGURES FROM BK-VIFIGURES FROM BK-IVLINKS The Keck Array and BICEP2 Collaborations, Phys. Rev. Lett. 121, 221301, 2018. PDF / figures / arXiv / ADS / Data Products. BK-IX: New Bounds on Anisotropies of CMB Polarization Rotation and Implications for Axion-Like Particles and Primordial Magnetic Fields. The Keck Array and BICEP2 Collaborations, Phys. Rev. D 96, 102003, 2017.BICEP2 VISUALS
BICEP2 Focal Plane. The BICEP2 telescope's focal plane consisting of an array of 512 superconducting bolometers, designed to operate at 0.25 K (0.25 degrees Celsius above absolute zero) in order to reduce thermal noise in the detectors. The focal plane was developed andproduced at
FIGURES FROM BK-X: CONSTRAINTS ON PRIMORDIAL GRAVITATIONAL Figures Download Bundle; BK15 E-mode maps: Figure 1: Maps of degree angular scale E-modes (50 < ℓ < 120) at three frequencies made using Keck Array data from the 2015 season only. The similarity of the pattern indicates that ΛCDM E-modes dominate at all three frequencies (and that the signal-to-noise is high).The color scale is in μK, and the range is allowed to vary slightly to (partially FIGURES FROM BK-III: INSTRUMENTAL SYSTEMATICS Figures from BK-III: Instrumental Systematics. Figure 1: Map coverage of a single BICEP2 detector pair located (top panel) near the edge of the focal plane and (bottom panel) near the center of the focal plane. The coverage at different deck angles overlaps significantly for KECK ARRAY/BICEP2 OCTOBER 2015 DATA PRODUCTS History. 2017-05-24: Added BK14 apodization mask. 2016-09-13: Updated CosmoMC tarball for backwards compatibility with BKPlanck version. 2015-10-30: Added bandpowers, CosmoMC tarball, r likelihood text file, and component separated spectra. KECK ARRAY/BICEP2 OCTOBER 2018 DATA PRODUCTS BK-X: Constraints on Primordial Gravitational Waves Using Planck, WMAP, and New BICEP2/Keck Observations through the 2015 Season TheKeck Array and
BICEP2 2014 RELEASE FREQUENTLY ASKED QUESTIONS BICEP2 is the second stage of a coordinated program, the BICEP and Keck Array series of experiments, developed for the South Pole. This coordinated program has a co-PI structure. The four PIs of this series are John Kovac ( Harvard ), Clem Pryke ( UMN ), Jamie Bock ( Caltech/JPL ), and Chao-Lin Kuo ( Stanford/SLAC ). MICROWAVE MULTIPLEXING ON THE KECK ARRAY Microwave multiplexing on the Keck Array 3 the TES current changes, the magnetic flux and, therefore, the resonant frequency change, i.e., the TES signal is transduced to a shift in resonant frequency. DESIGN AND CHARACTERIZATION OF ANTENNA-COUPLED 30/40 GHZ Journal of Low Temperature Physics manuscript No. (will be inserted by the editor) Design and Characterization of Antenna-Coupled 30/40 GHz Detectors and Modules for the BICEP Array Experiment BICEP2 MARCH 2014 RESULTS AND DATA PRODUCTS BICEP2 March 2014 Results and Data Products. 1. BICEP2 2014 Release Papers. 2. BICEP2 2014 Release Data Products. Text file containing the tabulated likelihood for the tensor-to-scalar ratio, r, computed using the “direct likelihood calculation” described in Section FIGURES FROM BK-III: INSTRUMENTAL SYSTEMATICS Figures from BK-III: Instrumental Systematics. Figure 1: Map coverage of a single BICEP2 detector pair located (top panel) near the edge of the focal plane and (bottom panel) near the center of the focal plane. The coverage at different deck angles overlaps significantly for FIGURES FROM BK-IV: OPTICAL CHARACTERIZATION AND Figures Download Bundle; A schematic of the BICEP2 optical chain: Figure 1: A schematic of the BICEP2 optical chain with each optical element labeled. The relative position of the lenses and focal plane is to scale. The Keck Array optical chain is identical except that the IR-blocking filters in front of the objective lens are all on the 50 K stage in the Keck Array and the positions of the FIGURES FROM BK-V: MEASUREMENTS OF B-MODE POLARIZATION AT Figures Download Bundle; Individual receiver of the Keck Array: Figure 1: Individual receiver of the Keck Array. Each receiver is cryogenic, with a pulse tube refrigerator cooling the optics to 4 K and a three-stage sorption refrigerator cooling the focal plane to 270 mK. FIGURES FROM BK-VI: IMPROVED CONSTRAINTS ON COSMOLOGY AND Figures Download Bundle; BK14 Q/U maps: Figure 1: Deep Q maps at 95 & 150 GHz using all BICEP2/Keck data through the end of the 2014 observing season—we refer to these maps as BK14. Noise levels are 127 nK deg (left) and 50 nK deg (right). Both maps show a high signal-to-noise pattern dominated by E-mode polarization; the 95 GHz map appears smoother because of the larger beam size. FIGURES FROM BK-XI: BEAM CHARACTERIZATION AND TEMPERATURE Figures Download Bundle; Setup for far-field beam mapping: Figure 1: Several weeks of each South Pole deployment season are spent generating far-field beam maps using the pictured setup.Left: Keck Array and BICEP3 taking far-field beam maps simultaneously at South Pole. Both choppers and far-field flat mirrors are visible. Middle: Carbon fiber chopper blade coated in Eccosorb HR-10, mounted in FIGURES FROM BK-XII: CONSTRAINTS ON AXION-LIKE Figures Download Bundle; Pipeline diagram: Figure 1: Flow diagram of the axion-oscillation analysis pipeline. The three main components areindicated on the
FIGURES FROM BK-VII: MATRIX BASED E/B SEPARATION APPLIED History. 2016-07-01: Minor updates to figures and captions in order to match ApJ published version. 2016-03-22: Posted BK-VII: Matrix Based E/B Separation Applied to BICEP2 and the Keck Array figures. KECK ARRAY VI: IMPROVED CONSTRAINTS ON COSMOLOGY AND 2 for how these conditions occurred. The theory of in ation is an extension to the standard model, which postulates a phase of exponential expansion at a still earlier epoch THE BICEP AND KECK ARRAY CMB EXPERIMENTS The BICEP and Keck Array CMB Experiments1 PEAK 60 /L 0
Title: paper_plots/welter_cdf_plot.eps Created Date: 4/11/2018 2:11:50PM
THE BICEP AND KECK ARRAY CMB EXPERIMENTSFIGURES FROM BK-VIIFIGURES FROM BK-IIIFIGURES FROM BK-VIFIGURES FROM BK-IVLINKS The Keck Array and BICEP2 Collaborations, Phys. Rev. Lett. 121, 221301, 2018. PDF / figures / arXiv / ADS / Data Products. BK-IX: New Bounds on Anisotropies of CMB Polarization Rotation and Implications for Axion-Like Particles and Primordial Magnetic Fields. The Keck Array and BICEP2 Collaborations, Phys. Rev. D 96, 102003, 2017.BICEP2 VISUALS
BICEP2 Focal Plane. The BICEP2 telescope's focal plane consisting of an array of 512 superconducting bolometers, designed to operate at 0.25 K (0.25 degrees Celsius above absolute zero) in order to reduce thermal noise in the detectors. The focal plane was developed andproduced at
BICEP AND KECK ARRAY EXPERIMENTS PUBLIC WEB PAGES BICEP and Keck Array Experiments Public Web Pages. Harvard University; California Institute of Technology; Stanford University FIGURES FROM BK-X: CONSTRAINTS ON PRIMORDIAL GRAVITATIONAL Figures Download Bundle; BK15 E-mode maps: Figure 1: Maps of degree angular scale E-modes (50 < ℓ < 120) at three frequencies made using Keck Array data from the 2015 season only. The similarity of the pattern indicates that ΛCDM E-modes dominate at all three frequencies (and that the signal-to-noise is high).The color scale is in μK, and the range is allowed to vary slightly to (partially FIGURES FROM BK-III: INSTRUMENTAL SYSTEMATICS Figures from BK-III: Instrumental Systematics. Figure 1: Map coverage of a single BICEP2 detector pair located (top panel) near the edge of the focal plane and (bottom panel) near the center of the focal plane. The coverage at different deck angles overlaps significantly for KECK ARRAY/BICEP2 OCTOBER 2015 DATA PRODUCTS History. 2017-05-24: Added BK14 apodization mask. 2016-09-13: Updated CosmoMC tarball for backwards compatibility with BKPlanck version. 2015-10-30: Added bandpowers, CosmoMC tarball, r likelihood text file, and component separated spectra. DESIGN AND PERFORMANCE OF THE FIRST BICEP ARRAY RECEIVER Journal of Low Temperature Physics manuscript No. (will be inserted by the editor) Design and performance of the first BICEP Array receiver A. Schillaci1 2P. A. KECK ARRAY VI: IMPROVED CONSTRAINTS ON COSMOLOGY AND 2 for how these conditions occurred. The theory of in ation is an extension to the standard model, which postulates a phase of exponential expansion at a still earlier epoch MICROWAVE MULTIPLEXING ON THE KECK ARRAY Microwave multiplexing on the Keck Array 3 the TES current changes, the magnetic flux and, therefore, the resonant frequency change, i.e., the TES signal is transduced to a shift in resonant frequency. BICEP2 MARCH 2014 RESULTS AND DATA PRODUCTS BICEP2 March 2014 Results and Data Products. 1. BICEP2 2014 Release Papers. 2. BICEP2 2014 Release Data Products. Text file containing the tabulated likelihood for the tensor-to-scalar ratio, r, computed using the “direct likelihood calculation” described in Section THE BICEP AND KECK ARRAY CMB EXPERIMENTSFIGURES FROM BK-VIIFIGURES FROM BK-IIIFIGURES FROM BK-VIFIGURES FROM BK-IVLINKS The Keck Array and BICEP2 Collaborations, Phys. Rev. Lett. 121, 221301, 2018. PDF / figures / arXiv / ADS / Data Products. BK-IX: New Bounds on Anisotropies of CMB Polarization Rotation and Implications for Axion-Like Particles and Primordial Magnetic Fields. The Keck Array and BICEP2 Collaborations, Phys. Rev. D 96, 102003, 2017.BICEP2 VISUALS
BICEP2 Focal Plane. The BICEP2 telescope's focal plane consisting of an array of 512 superconducting bolometers, designed to operate at 0.25 K (0.25 degrees Celsius above absolute zero) in order to reduce thermal noise in the detectors. The focal plane was developed andproduced at
BICEP AND KECK ARRAY EXPERIMENTS PUBLIC WEB PAGES BICEP and Keck Array Experiments Public Web Pages. Harvard University; California Institute of Technology; Stanford University FIGURES FROM BK-X: CONSTRAINTS ON PRIMORDIAL GRAVITATIONAL Figures Download Bundle; BK15 E-mode maps: Figure 1: Maps of degree angular scale E-modes (50 < ℓ < 120) at three frequencies made using Keck Array data from the 2015 season only. The similarity of the pattern indicates that ΛCDM E-modes dominate at all three frequencies (and that the signal-to-noise is high).The color scale is in μK, and the range is allowed to vary slightly to (partially FIGURES FROM BK-III: INSTRUMENTAL SYSTEMATICS Figures from BK-III: Instrumental Systematics. Figure 1: Map coverage of a single BICEP2 detector pair located (top panel) near the edge of the focal plane and (bottom panel) near the center of the focal plane. The coverage at different deck angles overlaps significantly for KECK ARRAY/BICEP2 OCTOBER 2015 DATA PRODUCTS History. 2017-05-24: Added BK14 apodization mask. 2016-09-13: Updated CosmoMC tarball for backwards compatibility with BKPlanck version. 2015-10-30: Added bandpowers, CosmoMC tarball, r likelihood text file, and component separated spectra. DESIGN AND PERFORMANCE OF THE FIRST BICEP ARRAY RECEIVER Journal of Low Temperature Physics manuscript No. (will be inserted by the editor) Design and performance of the first BICEP Array receiver A. Schillaci1 2P. A. KECK ARRAY VI: IMPROVED CONSTRAINTS ON COSMOLOGY AND 2 for how these conditions occurred. The theory of in ation is an extension to the standard model, which postulates a phase of exponential expansion at a still earlier epoch MICROWAVE MULTIPLEXING ON THE KECK ARRAY Microwave multiplexing on the Keck Array 3 the TES current changes, the magnetic flux and, therefore, the resonant frequency change, i.e., the TES signal is transduced to a shift in resonant frequency. BICEP2 MARCH 2014 RESULTS AND DATA PRODUCTS BICEP2 March 2014 Results and Data Products. 1. BICEP2 2014 Release Papers. 2. BICEP2 2014 Release Data Products. Text file containing the tabulated likelihood for the tensor-to-scalar ratio, r, computed using the “direct likelihood calculation” described in Section FIGURES FROM BK-X: CONSTRAINTS ON PRIMORDIAL GRAVITATIONAL Figures Download Bundle; BK15 E-mode maps: Figure 1: Maps of degree angular scale E-modes (50 < ℓ < 120) at three frequencies made using Keck Array data from the 2015 season only. The similarity of the pattern indicates that ΛCDM E-modes dominate at all three frequencies (and that the signal-to-noise is high).The color scale is in μK, and the range is allowed to vary slightly to (partially FIGURES FROM BK-VI: IMPROVED CONSTRAINTS ON COSMOLOGY AND Figures Download Bundle; BK14 Q/U maps: Figure 1: Deep Q maps at 95 & 150 GHz using all BICEP2/Keck data through the end of the 2014 observing season—we refer to these maps as BK14. Noise levels are 127 nK deg (left) and 50 nK deg (right). Both maps show a high signal-to-noise pattern dominated by E-mode polarization; the 95 GHz map appears smoother because of the larger beam size. FIGURES FROM BK-XI: BEAM CHARACTERIZATION AND TEMPERATURE Figures Download Bundle; Setup for far-field beam mapping: Figure 1: Several weeks of each South Pole deployment season are spent generating far-field beam maps using the pictured setup.Left: Keck Array and BICEP3 taking far-field beam maps simultaneously at South Pole. Both choppers and far-field flat mirrors are visible. Middle: Carbon fiber chopper blade coated in Eccosorb HR-10, mounted in FIGURES FROM BK-V: MEASUREMENTS OF B-MODE POLARIZATION AT Figures Download Bundle; Individual receiver of the Keck Array: Figure 1: Individual receiver of the Keck Array. Each receiver is cryogenic, with a pulse tube refrigerator cooling the optics to 4 K and a three-stage sorption refrigerator cooling the focal plane to 270 mK. FIGURES FROM A JOINT ANALYSIS OF BICEP2/KECK ARRAY AND Figures Download Bundle; T, Q, and U maps Figure 1: Planck 353 GHz T, Q, and U maps before (left) and after (right) the application of BICEP2/Keck filtering. In both cases the maps have been multiplied by the BICEP2/Keck apodization mask. The Planck maps are presmoothed to the BICEP2/Keck beam profile and have the mean value subtracted. BICEP2 2014 RELEASE FREQUENTLY ASKED QUESTIONS BICEP2 is the second stage of a coordinated program, the BICEP and Keck Array series of experiments, developed for the South Pole. This coordinated program has a co-PI structure. The four PIs of this series are John Kovac ( Harvard ), Clem Pryke ( UMN ), Jamie Bock ( Caltech/JPL ), and Chao-Lin Kuo ( Stanford/SLAC ). 3 BK15 XBK15 EE BK15 XBK15 EE BK15 XBK15 EE BK15 XP EE 95 −0.01 0 0.01 0.02 BK15 95 xBK15 95 BB −0.01 0 0.01 0.02 BK15 150 xBK15 150 BB 0 0.2 0.4 BK15 220 xBK15 220 BB 0 100 200 −10 0 10 P 353 xP 353 BB Multipole −0.01 BICEP2/KECK ARRAY JANUARY 2015 DATA PRODUCTS Data Products; BK_bandpowers_20150130.txt: Text file containing bandpowers and statistical uncertainties of combined BICEP2 and Keck Array maps, corresponding to Figure 9 of Keck Array DESIGN AND CHARACTERIZATION OF ANTENNA-COUPLED 30/40 GHZ 4 A. Soliman1 et al. Fig. 2 Top/Left: The simulated real and imaginary impedance at the optimized feed point on the slot vs. frequency. Top/Right:The contour matching of the input microstrip impedance/capacitor to the antenna THE BICEP AND KECK ARRAY CMB EXPERIMENTS The BICEP and Keck Array CMB Experiments THE BICEP AND KECK ARRAY CMB EXPERIMENTSFIGURES FROM BK-VIIFIGURES FROM BK-IIIFIGURES FROM BK-VIFIGURES FROM BK-IVLINKS The Keck Array and BICEP2 Collaborations, Phys. Rev. Lett. 121, 221301, 2018. PDF / figures / arXiv / ADS / Data Products. BK-IX: New Bounds on Anisotropies of CMB Polarization Rotation and Implications for Axion-Like Particles and Primordial Magnetic Fields. The Keck Array and BICEP2 Collaborations, Phys. Rev. D 96, 102003, 2017. BICEP AND KECK ARRAY EXPERIMENTS PUBLIC WEB PAGES BICEP and Keck Array Experiments Public Web Pages. Harvard University; California Institute of Technology; Stanford University FIGURES FROM BK-X: CONSTRAINTS ON PRIMORDIAL GRAVITATIONAL Figures Download Bundle; BK15 E-mode maps: Figure 1: Maps of degree angular scale E-modes (50 < ℓ < 120) at three frequencies made using Keck Array data from the 2015 season only. The similarity of the pattern indicates that ΛCDM E-modes dominate at all three frequencies (and that the signal-to-noise is high).The color scale is in μK, and the range is allowed to vary slightly to (partially FIGURES FROM BK-III: INSTRUMENTAL SYSTEMATICS Figures from BK-III: Instrumental Systematics. Figure 1: Map coverage of a single BICEP2 detector pair located (top panel) near the edge of the focal plane and (bottom panel) near the center of the focal plane. The coverage at different deck angles overlaps significantly for KECK ARRAY/BICEP2 OCTOBER 2015 DATA PRODUCTS History. 2017-05-24: Added BK14 apodization mask. 2016-09-13: Updated CosmoMC tarball for backwards compatibility with BKPlanck version. 2015-10-30: Added bandpowers, CosmoMC tarball, r likelihood text file, and component separated spectra. KECK ARRAY/BICEP2 OCTOBER 2018 DATA PRODUCTS BK-X: Constraints on Primordial Gravitational Waves Using Planck, WMAP, and New BICEP2/Keck Observations through the 2015 Season TheKeck Array and
3 BK15 XBK15 EE BK15 XBK15 EE BK15 XBK15 EE BK15 XP EE 95 −0.01 0 0.01 0.02 BK15 95 xBK15 95 BB −0.01 0 0.01 0.02 BK15 150 xBK15 150 BB 0 0.2 0.4 BK15 220 xBK15 220 BB 0 100 200 −10 0 10 P 353 xP 353 BB Multipole −0.01 MICROWAVE MULTIPLEXING ON THE KECK ARRAY Microwave multiplexing on the Keck Array 3 the TES current changes, the magnetic flux and, therefore, the resonant frequency change, i.e., the TES signal is transduced to a shift in resonant frequency. BICEP2 MARCH 2014 RESULTS AND DATA PRODUCTS BICEP2 March 2014 Results and Data Products. 1. BICEP2 2014 Release Papers. 2. BICEP2 2014 Release Data Products. Text file containing the tabulated likelihood for the tensor-to-scalar ratio, r, computed using the “direct likelihood calculation” described in Section THE BICEP AND KECK ARRAY CMB EXPERIMENTS The BICEP and Keck Array CMB Experiments THE BICEP AND KECK ARRAY CMB EXPERIMENTSFIGURES FROM BK-VIIFIGURES FROM BK-IIIFIGURES FROM BK-VIFIGURES FROM BK-IVLINKS The Keck Array and BICEP2 Collaborations, Phys. Rev. Lett. 121, 221301, 2018. PDF / figures / arXiv / ADS / Data Products. BK-IX: New Bounds on Anisotropies of CMB Polarization Rotation and Implications for Axion-Like Particles and Primordial Magnetic Fields. The Keck Array and BICEP2 Collaborations, Phys. Rev. D 96, 102003, 2017. BICEP AND KECK ARRAY EXPERIMENTS PUBLIC WEB PAGES BICEP and Keck Array Experiments Public Web Pages. Harvard University; California Institute of Technology; Stanford University FIGURES FROM BK-X: CONSTRAINTS ON PRIMORDIAL GRAVITATIONAL Figures Download Bundle; BK15 E-mode maps: Figure 1: Maps of degree angular scale E-modes (50 < ℓ < 120) at three frequencies made using Keck Array data from the 2015 season only. The similarity of the pattern indicates that ΛCDM E-modes dominate at all three frequencies (and that the signal-to-noise is high).The color scale is in μK, and the range is allowed to vary slightly to (partially FIGURES FROM BK-III: INSTRUMENTAL SYSTEMATICS Figures from BK-III: Instrumental Systematics. Figure 1: Map coverage of a single BICEP2 detector pair located (top panel) near the edge of the focal plane and (bottom panel) near the center of the focal plane. The coverage at different deck angles overlaps significantly for KECK ARRAY/BICEP2 OCTOBER 2015 DATA PRODUCTS History. 2017-05-24: Added BK14 apodization mask. 2016-09-13: Updated CosmoMC tarball for backwards compatibility with BKPlanck version. 2015-10-30: Added bandpowers, CosmoMC tarball, r likelihood text file, and component separated spectra. KECK ARRAY/BICEP2 OCTOBER 2018 DATA PRODUCTS BK-X: Constraints on Primordial Gravitational Waves Using Planck, WMAP, and New BICEP2/Keck Observations through the 2015 Season TheKeck Array and
3 BK15 XBK15 EE BK15 XBK15 EE BK15 XBK15 EE BK15 XP EE 95 −0.01 0 0.01 0.02 BK15 95 xBK15 95 BB −0.01 0 0.01 0.02 BK15 150 xBK15 150 BB 0 0.2 0.4 BK15 220 xBK15 220 BB 0 100 200 −10 0 10 P 353 xP 353 BB Multipole −0.01 MICROWAVE MULTIPLEXING ON THE KECK ARRAY Microwave multiplexing on the Keck Array 3 the TES current changes, the magnetic flux and, therefore, the resonant frequency change, i.e., the TES signal is transduced to a shift in resonant frequency. BICEP2 MARCH 2014 RESULTS AND DATA PRODUCTS BICEP2 March 2014 Results and Data Products. 1. BICEP2 2014 Release Papers. 2. BICEP2 2014 Release Data Products. Text file containing the tabulated likelihood for the tensor-to-scalar ratio, r, computed using the “direct likelihood calculation” described in Section THE BICEP AND KECK ARRAY CMB EXPERIMENTS The BICEP and Keck Array CMB ExperimentsBICEP2 VISUALS
BICEP2 Focal Plane. The BICEP2 telescope's focal plane consisting of an array of 512 superconducting bolometers, designed to operate at 0.25 K (0.25 degrees Celsius above absolute zero) in order to reduce thermal noise in the detectors. The focal plane was developed andproduced at
FIGURES FROM BK-XI: BEAM CHARACTERIZATION AND TEMPERATURE Figures Download Bundle; Setup for far-field beam mapping: Figure 1: Several weeks of each South Pole deployment season are spent generating far-field beam maps using the pictured setup.Left: Keck Array and BICEP3 taking far-field beam maps simultaneously at South Pole. Both choppers and far-field flat mirrors are visible. Middle: Carbon fiber chopper blade coated in Eccosorb HR-10, mounted in FIGURES FROM BK-VI: IMPROVED CONSTRAINTS ON COSMOLOGY AND Figures Download Bundle; BK14 Q/U maps: Figure 1: Deep Q maps at 95 & 150 GHz using all BICEP2/Keck data through the end of the 2014 observing season—we refer to these maps as BK14. Noise levels are 127 nK deg (left) and 50 nK deg (right). Both maps show a high signal-to-noise pattern dominated by E-mode polarization; the 95 GHz map appears smoother because of the larger beam size. FIGURES FROM BK-V: MEASUREMENTS OF B-MODE POLARIZATION AT Figures Download Bundle; Individual receiver of the Keck Array: Figure 1: Individual receiver of the Keck Array. Each receiver is cryogenic, with a pulse tube refrigerator cooling the optics to 4 K and a three-stage sorption refrigerator cooling the focal plane to 270 mK. FIGURES FROM BK-VII: MATRIX BASED E/B SEPARATION APPLIED History. 2016-07-01: Minor updates to figures and captions in order to match ApJ published version. 2016-03-22: Posted BK-VII: Matrix Based E/B Separation Applied to BICEP2 and the Keck Array figures. 3 BK15 XBK15 EE BK15 XBK15 EE BK15 XBK15 EE BK15 XP EE 95 −0.01 0 0.01 0.02 BK15 95 xBK15 95 BB −0.01 0 0.01 0.02 BK15 150 xBK15 150 BB 0 0.2 0.4 BK15 220 xBK15 220 BB 0 100 200 −10 0 10 P 353 xP 353 BB Multipole −0.01 OPTICAL CHARACTERIZATION OF THE KECK ARRAY AND BICEP3 CMB Optical characterization of the Keck Array and BICEP3 CMB Polarimeters from 2016 to 2019 3 for sensitivity to CMB polarization at degree angular scales (‘ ˘100). BICEP2/KECK ARRAY JANUARY 2015 DATA PRODUCTS Data Products; BK_bandpowers_20150130.txt: Text file containing bandpowers and statistical uncertainties of combined BICEP2 and Keck Array maps, corresponding to Figure 9 of Keck Array DESIGN AND CHARACTERIZATION OF ANTENNA-COUPLED 30/40 GHZ 4 A. Soliman1 et al. Fig. 2 Top/Left: The simulated real and imaginary impedance at the optimized feed point on the slot vs. frequency. Top/Right:The contour matching of the input microstrip impedance/capacitor to the antenna KECK ARRAY VI: IMPROVED CONSTRAINTS ON COSMOLOGY AND 2 for how these conditions occurred. The theory of in ation is an extension to the standard model, which postulates a phase of exponential expansion at a still earlier epoch THE BICEP AND KECK ARRAY CMB EXPERIMENTSFIGURES FROM BK-VIIFIGURES FROM BK-IIIFIGURES FROM BK-VIFIGURES FROM BK-IVLINKS The Keck Array and BICEP2 Collaborations, Phys. Rev. Lett. 121, 221301, 2018. PDF / figures / arXiv / ADS / Data Products. BK-IX: New Bounds on Anisotropies of CMB Polarization Rotation and Implications for Axion-Like Particles and Primordial Magnetic Fields. The Keck Array and BICEP2 Collaborations, Phys. Rev. D 96, 102003, 2017. BICEP AND KECK ARRAY EXPERIMENTS PUBLIC WEB PAGES BICEP and Keck Array Experiments Public Web Pages. Harvard University; California Institute of Technology; Stanford University FIGURES FROM BK-X: CONSTRAINTS ON PRIMORDIAL GRAVITATIONAL Figures Download Bundle; BK15 E-mode maps: Figure 1: Maps of degree angular scale E-modes (50 < ℓ < 120) at three frequencies made using Keck Array data from the 2015 season only. The similarity of the pattern indicates that ΛCDM E-modes dominate at all three frequencies (and that the signal-to-noise is high).The color scale is in μK, and the range is allowed to vary slightly to (partially FIGURES FROM BK-III: INSTRUMENTAL SYSTEMATICS Figures from BK-III: Instrumental Systematics. Figure 1: Map coverage of a single BICEP2 detector pair located (top panel) near the edge of the focal plane and (bottom panel) near the center of the focal plane. The coverage at different deck angles overlaps significantly for KECK ARRAY/BICEP2 OCTOBER 2015 DATA PRODUCTS History. 2017-05-24: Added BK14 apodization mask. 2016-09-13: Updated CosmoMC tarball for backwards compatibility with BKPlanck version. 2015-10-30: Added bandpowers, CosmoMC tarball, r likelihood text file, and component separated spectra. KECK ARRAY/BICEP2 OCTOBER 2018 DATA PRODUCTS BK-X: Constraints on Primordial Gravitational Waves Using Planck, WMAP, and New BICEP2/Keck Observations through the 2015 Season TheKeck Array and
3 BK15 XBK15 EE BK15 XBK15 EE BK15 XBK15 EE BK15 XP EE 95 −0.01 0 0.01 0.02 BK15 95 xBK15 95 BB −0.01 0 0.01 0.02 BK15 150 xBK15 150 BB 0 0.2 0.4 BK15 220 xBK15 220 BB 0 100 200 −10 0 10 P 353 xP 353 BB Multipole −0.01 MICROWAVE MULTIPLEXING ON THE KECK ARRAY Microwave multiplexing on the Keck Array 3 the TES current changes, the magnetic flux and, therefore, the resonant frequency change, i.e., the TES signal is transduced to a shift in resonant frequency. BICEP2 MARCH 2014 RESULTS AND DATA PRODUCTS BICEP2 March 2014 Results and Data Products. 1. BICEP2 2014 Release Papers. 2. BICEP2 2014 Release Data Products. Text file containing the tabulated likelihood for the tensor-to-scalar ratio, r, computed using the “direct likelihood calculation” described in Section THE BICEP AND KECK ARRAY CMB EXPERIMENTS The BICEP and Keck Array CMB Experiments THE BICEP AND KECK ARRAY CMB EXPERIMENTSFIGURES FROM BK-VIIFIGURES FROM BK-IIIFIGURES FROM BK-VIFIGURES FROM BK-IVLINKS The Keck Array and BICEP2 Collaborations, Phys. Rev. Lett. 121, 221301, 2018. PDF / figures / arXiv / ADS / Data Products. BK-IX: New Bounds on Anisotropies of CMB Polarization Rotation and Implications for Axion-Like Particles and Primordial Magnetic Fields. The Keck Array and BICEP2 Collaborations, Phys. Rev. D 96, 102003, 2017. BICEP AND KECK ARRAY EXPERIMENTS PUBLIC WEB PAGES BICEP and Keck Array Experiments Public Web Pages. Harvard University; California Institute of Technology; Stanford University FIGURES FROM BK-X: CONSTRAINTS ON PRIMORDIAL GRAVITATIONAL Figures Download Bundle; BK15 E-mode maps: Figure 1: Maps of degree angular scale E-modes (50 < ℓ < 120) at three frequencies made using Keck Array data from the 2015 season only. The similarity of the pattern indicates that ΛCDM E-modes dominate at all three frequencies (and that the signal-to-noise is high).The color scale is in μK, and the range is allowed to vary slightly to (partially FIGURES FROM BK-III: INSTRUMENTAL SYSTEMATICS Figures from BK-III: Instrumental Systematics. Figure 1: Map coverage of a single BICEP2 detector pair located (top panel) near the edge of the focal plane and (bottom panel) near the center of the focal plane. The coverage at different deck angles overlaps significantly for KECK ARRAY/BICEP2 OCTOBER 2015 DATA PRODUCTS History. 2017-05-24: Added BK14 apodization mask. 2016-09-13: Updated CosmoMC tarball for backwards compatibility with BKPlanck version. 2015-10-30: Added bandpowers, CosmoMC tarball, r likelihood text file, and component separated spectra. KECK ARRAY/BICEP2 OCTOBER 2018 DATA PRODUCTS BK-X: Constraints on Primordial Gravitational Waves Using Planck, WMAP, and New BICEP2/Keck Observations through the 2015 Season TheKeck Array and
3 BK15 XBK15 EE BK15 XBK15 EE BK15 XBK15 EE BK15 XP EE 95 −0.01 0 0.01 0.02 BK15 95 xBK15 95 BB −0.01 0 0.01 0.02 BK15 150 xBK15 150 BB 0 0.2 0.4 BK15 220 xBK15 220 BB 0 100 200 −10 0 10 P 353 xP 353 BB Multipole −0.01 MICROWAVE MULTIPLEXING ON THE KECK ARRAY Microwave multiplexing on the Keck Array 3 the TES current changes, the magnetic flux and, therefore, the resonant frequency change, i.e., the TES signal is transduced to a shift in resonant frequency. BICEP2 MARCH 2014 RESULTS AND DATA PRODUCTS BICEP2 March 2014 Results and Data Products. 1. BICEP2 2014 Release Papers. 2. BICEP2 2014 Release Data Products. Text file containing the tabulated likelihood for the tensor-to-scalar ratio, r, computed using the “direct likelihood calculation” described in Section THE BICEP AND KECK ARRAY CMB EXPERIMENTS The BICEP and Keck Array CMB ExperimentsBICEP2 VISUALS
BICEP2 Focal Plane. The BICEP2 telescope's focal plane consisting of an array of 512 superconducting bolometers, designed to operate at 0.25 K (0.25 degrees Celsius above absolute zero) in order to reduce thermal noise in the detectors. The focal plane was developed andproduced at
FIGURES FROM BK-XI: BEAM CHARACTERIZATION AND TEMPERATURE Figures Download Bundle; Setup for far-field beam mapping: Figure 1: Several weeks of each South Pole deployment season are spent generating far-field beam maps using the pictured setup.Left: Keck Array and BICEP3 taking far-field beam maps simultaneously at South Pole. Both choppers and far-field flat mirrors are visible. Middle: Carbon fiber chopper blade coated in Eccosorb HR-10, mounted in FIGURES FROM BK-VI: IMPROVED CONSTRAINTS ON COSMOLOGY AND Figures Download Bundle; BK14 Q/U maps: Figure 1: Deep Q maps at 95 & 150 GHz using all BICEP2/Keck data through the end of the 2014 observing season—we refer to these maps as BK14. Noise levels are 127 nK deg (left) and 50 nK deg (right). Both maps show a high signal-to-noise pattern dominated by E-mode polarization; the 95 GHz map appears smoother because of the larger beam size. FIGURES FROM BK-V: MEASUREMENTS OF B-MODE POLARIZATION AT Figures Download Bundle; Individual receiver of the Keck Array: Figure 1: Individual receiver of the Keck Array. Each receiver is cryogenic, with a pulse tube refrigerator cooling the optics to 4 K and a three-stage sorption refrigerator cooling the focal plane to 270 mK. FIGURES FROM BK-VII: MATRIX BASED E/B SEPARATION APPLIED History. 2016-07-01: Minor updates to figures and captions in order to match ApJ published version. 2016-03-22: Posted BK-VII: Matrix Based E/B Separation Applied to BICEP2 and the Keck Array figures. 3 BK15 XBK15 EE BK15 XBK15 EE BK15 XBK15 EE BK15 XP EE 95 −0.01 0 0.01 0.02 BK15 95 xBK15 95 BB −0.01 0 0.01 0.02 BK15 150 xBK15 150 BB 0 0.2 0.4 BK15 220 xBK15 220 BB 0 100 200 −10 0 10 P 353 xP 353 BB Multipole −0.01 OPTICAL CHARACTERIZATION OF THE KECK ARRAY AND BICEP3 CMB Optical characterization of the Keck Array and BICEP3 CMB Polarimeters from 2016 to 2019 3 for sensitivity to CMB polarization at degree angular scales (‘ ˘100). BICEP2/KECK ARRAY JANUARY 2015 DATA PRODUCTS Data Products; BK_bandpowers_20150130.txt: Text file containing bandpowers and statistical uncertainties of combined BICEP2 and Keck Array maps, corresponding to Figure 9 of Keck Array DESIGN AND CHARACTERIZATION OF ANTENNA-COUPLED 30/40 GHZ 4 A. Soliman1 et al. Fig. 2 Top/Left: The simulated real and imaginary impedance at the optimized feed point on the slot vs. frequency. Top/Right:The contour matching of the input microstrip impedance/capacitor to the antenna KECK ARRAY VI: IMPROVED CONSTRAINTS ON COSMOLOGY AND 2 for how these conditions occurred. The theory of in ation is an extension to the standard model, which postulates a phase of exponential expansion at a still earlier epoch THE BICEP AND KECK ARRAY CMB EXPERIMENTS OFFICIAL WEBSITE FOR RESULTS FROM THE BICEP AND KECK ARRAY SERIES OF CMB POLARIZATION EXPERIMENTS BICEP and Keck Array experiments public web pages ------------------------- RESULTS AND DATA PRODUCTS * BICEP2/Keck Array October 2018 Data Products * BICEP2/Keck Array October 2015 Data Products * BICEP2/Keck Array and Planck Joint Analysis January 2015 DataProducts
* BICEP2/Keck Array January 2015 Data Products * BICEP2 March 2014 Results and Data Products BICEP/KECK PUBLICATIONS BICEP/KECK ARRAY RESULTS PAPERS Series of results papers from the BICEP and Keck Array experiments, starting with initial BICEP2 results in March 2014. * BK-XII: Constraints on axion-like polarization oscillations in the cosmic microwave background BICEP / Keck Array Collaboration, 2020PDF / figures
/ arXiv /
ADS
* BK-XI: Beam Characterization and Temperature-to-Polarization Leakage in the BK15 Dataset The Keck Array and BICEP2 Collaborations, ApJ 844, 114, 2019PDF / figures
/ arXiv / ADS
* BK-X: Constraints on Primordial Gravitational Waves Using Planck, WMAP, and New BICEP2/Keck Observations through the 2015 Season The Keck Array and BICEP2 Collaborations, Phys. Rev. Lett. 121,221301, 2018
PDF / figures
/ arXiv / ADS
/
Data Products
* BK-IX: New Bounds on Anisotropies of CMB Polarization Rotation and Implications for Axion-Like Particles and Primordial Magnetic Fields The Keck Array and BICEP2 Collaborations, Phys. Rev. D 96, 102003,2017
PDF / figures
/ arXiv / ADS
/
Data Products
* BK-VIII: Measurement of Gravitational Lensing from Large-scaleB-mode Polarization
The Keck Array and BICEP2 Collaborations, ApJ 833, 228, 2016PDF / figures
/ arXiv /
ADS
* BK-VII: Matrix Based E/B Separation Applied to BICEP2 and the KeckArray
The Keck Array and BICEP2 Collaborations, ApJ 825, 66, 2016PDF / figures
/ arXiv / ADS
* BK-VI: Improved Constraints On Cosmology and Foregrounds When Adding 95 GHz Data From Keck Array The Keck Array and BICEP2 Collaborations, Phys. Rev. Lett. 116,031302, 2016
PDF / figures
/ arXiv / ADS
/
Data Products
* BK-V: Measurements of B-mode Polarization at Degree Angular Scales and 150 GHz by Keck Array The Keck Array and BICEP2 Collaborations, ApJ 811, 126, 2015PDF / figures /
arXiv / ADS
/
Data Products
* BK-IV: Optical Characterization and Performance of the BICEP2 and Keck Array Experiments The BICEP2 and Keck Array Collaborations, ApJ 806, 206, 2015PDF / figures
/ arXiv / ADS
* BK-III: Instrumental Systematics The BICEP2 Collaboration, ApJ 814, 110, 2015PDF / figures
/ arXiv / ADS
* BK-II: Experiment and Three-year Data Set The BICEP2 Collaboration, ApJ 792, 62, 2014PDF / figures
/ arXiv
/ ADS
/
Data Products
* BK-I: Detection of B-mode Polarization at Degree Angular Scales byBICEP2
The BICEP2 Collaboration, Phys. Rev. Lett. 112, 241101, 2014PDF /
figures / arXiv
/ ADS
/
Data Products
JOINT PAPERS: BICEP / KECK PLUS OTHER COLLABORATIONS Papers produced as joint efforts of the BICEP / Keck Array teams and other collaborations * A Demonstration of Improved Constraints on Primordial Gravitational Waves with Delensing The BICEP/Keck and SPTpol Collaborations, 2020PDF / figures
/ arXiv
/ ADS
* A Joint Analysis of BICEP2/Keck Array and Planck Data The BICEP2/Keck and Planck Collaborations, Phys. Rev. Lett. 114,101301, 2015
PDF / figures
/ arXiv
/ ADS
/
Data Products
* Antenna-coupled TES Bolometers used in BICEP2, Keck Array, andSPIDER
The BICEP2, Keck Array, and SPIDER Collaborations, ApJ 812, 176, 2015PDF / figures
/ arXiv
/ ADS
OTHER PUBLICATIONS
PROCEEDINGS PAPERS
from BICEP Array, BICEP3, Keck Array, BICEP2, and related experiments * Design and performance of the first BICEP Array receiver Schillaci, A.; et. al. / JLTP / 2019 / PDF/ ADS
* Characterizing the Sensitivity of 40 GHz TES Bolometers for BICEPArray
Zhang, C.; et. al. / JLTP / 2019 / PDF/ ADS
* Optical characterization of the Keck Array and BICEP3 CMB Polarimeters from 2016 to 2019 St. Germaine, T.; et. al. / JLTP / 2019 / PDF/ ADS
* Microwave multiplexing on the Keck Array Cukierman, A.; et. al. / JLTP / 2019 / PDF/ ADS
* Design and Characterization of Antenna-Coupled 30/40 GHz Detectors and Modules for the BICEP Array Experiment Soliman, A.; et. al. / JLTP / 2019 / PDF/ ADS
* 2017 upgrade and performance of BICEP3: a 95GHz refracting telescope for degree-scale CMB polarization Kang, J. H.; et. al. / SPIE / 2018 / ADS * BICEP Array cryostat and mount design Crumrine, M.; et. al. / SPIE / 2018 / ADS * BICEP Array: a multi-frequency degree-scale CMB polarimeter Hui, H.; et. al. / SPIE / 2018 / ADS * Ultra-Thin Large-Aperture Vacuum Windows for Millimeter Wavelengths Receivers Barkats, D.; Dierickx, M.; et. al. / SPIE / 2018 / ADS * Design and performance of wide-band corrugated walls for the BICEP Array detector modules at 30/40 GHz Soliman, A.; et. al. / SPIE / 2018 / ADS * Measurements of Degree-Scale B-mode Polarization with the BICEP/Keck Experiments at South Pole Racine, B.; et. al. / Moriond / 2018 / ADS * BICEP3 performance overview and planned Keck Array upgrade Grayson, J.; et. al. / SPIE / 2016 / ADS * Optical Characterization of the BICEP3 CMB Polarimeter at theSouth Pole
Karkare, K.; et. al. / SPIE / 2016 / ADS * BICEP3 focal plane design and detector performance Hui, H.; et. al. / SPIE / 2016 / ADS * Initial Performance of BICEP3: A Degree Angular Scale 95 GHz BandPolarimeter
Wu, W. L. K.; et al. / JLTP / 2016 / ADS * BICEP3: a 95GHz refracting telescope for degree-scale CMBpolarization
Ahmed, Z.; et. al. / SPIE / 2014 / ADS * BICEP2 and Keck array: upgrades and improved beam characterization Buder, I.; et. al. / SPIE / 2014 / ADS * Keck array and BICEP3: spectral characterization of 5000+detectors
Karkare, K. S.; et. al. / SPIE / 2014 / ADS * Antenna-coupled TES bolometers for the Keck array, Spider, andPolar-1
O'Brient, R.; et. al. / SPIE / 2012 / ADS * BICEP2 and Keck array operational overview and status ofobservations
Ogburn, R. W.; et. al. / SPIE / 2012 / ADS * Characterization and Fabrication of the TES Arrays for the Spider, Keck and BICEP2 CMB Polarimeters Bonetti, J. A.; et. al. / JLTP / 2012 / ADS * Optical characterization of the Keck array polarimeter at theSouth Pole
Vieregg, A. G.; et. al. / SPIE / 2012 / ADS * The Keck Array: A Multi Camera CMB Polarimeter at the South Pole Staniszewski, Z.; et. al. / JLTP / 2012 / ADS * Optimization and sensitivity of the Keck array Kernasovskiy, S.; et. al. / SPIE / 2012 / ADS * Antenna-coupled TES bolometer arrays for BICEP2/Keck and SPIDER Orlando, A.; et. al. / SPIE / 2010 / ADS * The BICEP2 CMB polarization experiment Ogburn, R. W.; et. al. / SPIE / 2010 / ADS * Initial performance of the BICEP2 antenna-coupled superconducting bolometers at the South Pole Brevik, J. A.; et. al. / SPIE / 2010 / ADS * The Keck Array: a pulse tube cooled CMB polarimeter Sheehy, C. D.; et. al. / SPIE / 2010 / ADS * Optical performance of the BICEP2 Telescope at the South Pole Aikin, R. W.; et. al. / SPIE / 2010 / ADS * Microfabrication and Device Parameter Testing of the Focal Plane Arrays for the Spider and BICEP2/Keck CMB Polarimeter Bonetti, J. A.; et. al. / AIP / 2009 / ADS * Antenna-coupled TES bolometer arrays for CMB polarimetry Kuo, C. L.; et. al. / SPIE / 2008 / ADS * BICEP2/SPUD: searching for inflation with degree scale polarimetryfrom the South Pole
Nguyen, H. T.; et. al. / SPIE / 2008 / ADSBICEP1 PAPERS
* Degree-scale Cosmic Microwave Background Polarization Measurements from Three Years of BICEP1 Data Barkats, D.; et. al. / ApJ / 2014 / ADS/
Data Products
* Self-Calibration of BICEP1 Three-Year Data and Constraints on Astrophysical Polarization Rotation Kaufman, J. P.; et. al. / PRD / 2014 / ADS * Scientific Verification of Faraday Rotation Modulators: Detection of Diffuse Polarized Galactic Emission Moyerman, S.; et. al. / ApJ / 2013 / ADS * A Millimeter-wave Galactic Plane Survey with the BICEP Polarimeter Bierman, E. M.; et. al. / ApJ / 2011 / ADS * Absolute polarization angle calibration using polarized diffuse Galactic emission observed by BICEP Matsumura, T.; et. al. / SPIE / 2010 / ADS * Characterization of the BICEP Telescope for High-precision Cosmic Microwave Background Polarimetry Takahashi, Y. D.; et. al. / ApJ / 2010 / ADS * Measurement of Cosmic Microwave Background Polarization Power Spectra from Two Years of BICEP Data Chiang, H. C.; et. al. / ApJ / 2010 / ADS/
Data Products
* CMB polarimetry with BICEP: instrument characterization, calibration, and performance Takahashi, Y. D.; et. al. / SPIE / 2008 / ADS * The Robinson Gravitational Wave Background Telescope (BICEP): a bolometric large angular scale CMB polarimeter Yoon, K. W.; et. al. / SPIE / 2006 / ADS * BICEP: a large angular scale CMB polarimeter Keating, B. G.; et. al. / SPIE / 2003 / ADS⇧ Top ⇧
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