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1. Mapping large-scale-structure evolution over cosmic times

Author: Kirit Karkare, Ely D. Kovetz, Jacques Delabrouille, Matthieu Béthermin, Garrett K. Keating, M. B. Silva, Azadeh Moradinezhad Dizgah, Patrick C. Breysse, José Luis Bernal, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), 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, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), 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), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and Ministerio de Ciencia, Innovación y Universidades (España)
Subjects: Submillimeter: general, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmological parameters, Dark matter, Large-scale structure of universe, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, general [Submillimeter], 7. Clean energy, 01 natural sciences, Cosmology, high-redshift [Galaxies], Cosmic infrared background, 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, Reionization, Astrophysics::Galaxy Astrophysics, Physics, (cosmology:) Cosmological parameters, 010308 nuclear & particles physics, Galaxies: high-redshift, Galaxies: evolution, Astronomy and Astrophysics, Cosmic variance, (cosmology:) Large-scale structure of universe, evolution [Galaxies], Redshift, 13. Climate action, Space and Planetary Science, Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: This paper outlines the science case for line-intensity mapping with a space-borne instrument targeting the sub-millimeter (microwaves) to the far-infrared (FIR) wavelength range. Our goal is to observe and characterize the large-scale structure in the Universe from present times to the high redshift Epoch of Reionization. This is essential to constrain the cosmology of our Universe and form a better understanding of various mechanisms that drive galaxy formation and evolution. We argue that the proposed frequency range would make it possible to probe important metal cooling lines such as [CII] up to very high redshift as well as a large number of rotational lines of the CO molecule. These can be used to trace molecular gas and dust evolution and constrain the buildup in both the cosmic star formation rate density and the cosmic infrared background (CIB). Moreover, surveys at the highest frequencies will detect FIR lines which are used as diagnostics of galaxies and AGN. Tomography of these lines over a wide redshift range will enable invaluable measurements of the cosmic expansion history at epochs inaccessible to other methods, competitive constraints on the parameters of the standard model of cosmology, and numerous tests of dark matter, dark energy, modified gravity and inflation. To reach these goals, large-scale structure must be mapped over a wide range in frequency to trace its time evolution over a reasonable fraction of the volume of the observable Universe. In addition, the surveyed area needs to be very large to beat cosmic variance and to probe the largest scales where its easier to separate the astrophysical and cosmological contributions to the observed signal. Only, a space-borne mission can properly meet these requirements., 25 pages, 6 figures, ESA Voyage-2050 White Paper
Published: 2021

2. The Simons Observatory: Band-Pass calibration using a Frequency-tunable Laser Source (FLS)

Author: Shreya Sutariya, Kathleen Harrington, Thomas Alford, Carlos E. Sierra, Grace Chesmore, Jeffrey J. McMahon, The Simons Observatory Collaboration, Kirit Karkare, and Ryan McGeehan
Published: 2022

3. 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

4. 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

5. Microwave spectro-polarimetry of matter and radiation across space and time

Author: Mattia Negrello, Guilaine Lagache, Selim C. Hotinli, F. Piacentini, Marta B. Silva, Dale J. Fixsen, Helmut Dannerbauer, Íñigo Zubeldia, J. Colin Hill, Jose Alberto Rubino Martin, Naonori Sugiyama, Kazunori Kohri, Simone Ferraro, Tarun Souradeep, Kirit Karkare, Maximilian H. Abitbol, N. Mandolesi, Andrea Tartari, L. Rodriguez, Alan J. Kogut, K. Karatsu, José Luis Bernal, Suvodip Mukherjee, Nabila Aghanim, I. Khabibullin, Zhen-Yi Cai, Subodh P. Patil, Matteo Bonato, Carlo Burigana, Tiziana Trombetti, Jean-Baptiste Melin, Marcelo A. Alvarez, David Alonso, Emanuela Dimastrogiovanni, François R. Bouchet, John C. Mather, Daniela Paoletti, R. A. Sunyaev, Gianfranco De Zotti, Luke Hart, Boris Bolliet, Patrick C. Breysse, Eugene Churazov, Ely D. Kovetz, Paolo de Bernardis, Silvia Masi, Eric R. Switzer, Matthieu Béthermin, Aditya Rotti, Douglas Scott, Jochem J. A. Baselmans, Julien Lesgourgues, V. Reveret, Jose Ramon Bermejo Climent, Carlos Martins, Jens Chluba, Garrett K. Keating, Nathalie Palanque-Delabrouille, Bruno Maffei, Yacine Ali-Haïmoud, Jens Erler, Eleonora Di Valentino, Srinivasan Raghunathan, Nicholas Battaglia, Azadeh Moradinezhad Dizgah, Jack Sayers, Mathew S. Madhavacheril, A. J. Banday, Shaul Hanany, Joseph Silk, Tony Mroczkowski, Daisuke Nagai, Akira Endo, Mathieu Remazeilles, Jacques Delabrouille, Fabio Finelli, James G. Bartlett, Kaustuv Basu, Andrea Ravenni, Carlos Hernández-Monteagudo, 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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)-Centre National d’Études Spatiales [Paris] (CNES), Institut de recherche en astrophysique et planétologie (IRAP), 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), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), 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), European Commission, Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), 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), and Physics of Nanodevices
Subjects: cosmological model, dimension: 3, Cosmic microwave background, Galaxy clusters, cosmic background radiation, CMB, 7. Clean energy, 01 natural sciences, Early Universe, General Relativity and Quantum Cosmology, flow: velocity, law.invention, mass spectrum, neutrino, law, Observatory, DISTORTIONS, ENERGY-RELEASE, 010303 astronomy & astrophysics, Physics, COSMIC BACKGROUND-RADIATION, formation, Astrophysics::Instrumentation and Methods for Astrophysics, imaging, HYDROGEN, Cosmology, observatory, black body, Sunyaev-Zel'dovich effect, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - Instrumentation and Methods for Astrophysics, Astronomical and Space Sciences, radiation: background, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), polarization: anisotropy, lens, Cosmic background radiation, Polarimetry, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Sunyaev–Zel'dovich effect, energy: injection, MAGNETIC-FIELDS, Telescope, 0103 physical sciences, Angular resolution, structure, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], inflation, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Spectrometer, beam: width, HOT-MODEL, deformation, gravitational radiation, Astronomy, Astronomy and Astrophysics, CLUSTER, Galaxies, Astrophysics - Astrophysics of Galaxies, THERMALIZATION, cosmic background radiation: temperature, angular resolution, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), microwaves: emission, ddc:520, spectral, spectrometer, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Delabrouille, J., et al., This paper discusses the science case for a sensitive spectro-polarimetric survey of the microwave sky. Such a survey would provide a tomographic and dynamic census of the three-dimensional distribution of hot gas, velocity flows, early metals, dust, and mass distribution in the entire Hubble volume, exploit CMB temperature and polarisation anisotropies down to fundamental limits, and track energy injection and absorption into the radiation background across cosmic times by measuring spectral distortions of the CMB blackbody emission. In addition to its exceptional capability for cosmology and fundamental physics, such a survey would provide an unprecedented view of microwave emissions at sub-arcminute to few-arcminute angular resolution in hundreds of frequency channels, a data set that would be of immense legacy value for many branches of astrophysics. We propose that this survey be carried out with a large space mission featuring a broad-band polarised imager and a moderate resolution spectro-imager at the focus of a 3.5 m aperture telescope actively cooled to about 8K, complemented with absolutely-calibrated Fourier Transform Spectrometer modules observing at degree-scale angular resolution in the 10–2000 GHz frequency range. We propose two observing modes: a survey mode to map the entire sky as well as a few selected wide fields, and an observatory mode for deeper observations of regions of specific interest., This work has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No 725456, CMBSPEC) as well as the Royal Society (grants UF130435 and RG140523). JARM acknowledges financial support from the Spanish Ministry of Science and Innovation (MICINN) under the project AYA2017-84185-P, and from the European Union’s Horizon 2020 research and innovation programme under Grant Agreement 687312 (RADIOFOREGROUNDS). C.H.-M. acknowledges the support of the Spanish Ministry of Science through project PGC2018-097585-B-C21. Financial support from the ASI/Physics Department of the University of Roma–Tor Vergata agreement n. 2016-24-H.0 for study activities of the Italian cosmology community is acknowledged. JLB is supported by the Allan C. and Dorothy H. Davis Fellowship, and has been supported by the Spanish MINECO under grant BES-2015-071307, co-funded by the ESF during part of the development of this work.
Published: 2021

6. 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

7. 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

8. 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

9. 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

10. Microwave multiplexing on the Keck Array

Author: Howard Hui, J. Willmert, Gene C. Hilton, John E. Dusatko, S. Fatigoni, K. G. Megerian, Joel N. Ullom, L. Duband, Carole Tucker, D. V. Wiebe, Ari Cukierman, Gunther Haller, Shawn W. Henderson, Tyler St. Germaine, Stephen E. Kuenstner, Jeffrey P. Filippini, S. R. Hildebrandt, S. A. Kernasovskiy, David Brown, M. Crumrine, K. W. Yoon, Leila R. Vale, Jake Connors, G. Hall, Bradley Dober, Saptarshi Chaudhuri, Toshiya Namikawa, H. Yang, Chao-Lin Kuo, Josef Frisch, A. D. Turner, E. Karpel, J. Cornelison, C. Umilta, Ahmed Soliman, Zeeshan Ahmed, K. L. Thompson, Johannes Hubmayr, Mark Halpern, E. Y. Young, Bryan Steinbach, J. Cheshire, E. Bullock, John A. B. Mates, C. Pryke, Sarah M. Harrison, Attila Kovács, Roger O'Brient, M. Amiri, J. Kang, Jesus Vasquez, Lingzhen Zeng, R. Basu Thakur, Victor Buza, B. Racine, John M. D'Ewart, Denis Barkats, H. T. Nguyen, S. Palladino, A. C. Weber, C. D. Reintsema, Marion Dierickx, Stefan Richter, Chao Zhang, A. Schillaci, J. J. Bock, R. Schwarz, Stephen J. Smith, H. Boenish, S. Kefeli, Dale Li, John M Kovac, Kirit Karkare, Kent D. Irwin, A. Wandui, Colin A. Bischoff, Daniel D. Van Winkle, R. V. Sudiwala, W. L. K. Wu, C. D. Sheehy, C. Yu, Peter A. R. Ade, Lorenzo Moncelsi, Abigail G. Vieregg, Kei May Lau, Service des Basses Températures (SBT ), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)
Subjects: SMuRF, Coaxial cable, Cosmic microwave background, Polarimetry, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, CMB, 01 natural sciences, Multiplexing, 010305 fluids & plasmas, law.invention, Optics, law, Tone tracking, 0103 physical sciences, General Materials Science, Electronics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Condensed Matter Physics, BICEP, Atomic and Molecular Physics, and Optics, Cardinal point, Microwave multiplexing, Keck Array, Radio frequency, business, Astrophysics - Instrumentation and Methods for Astrophysics, Microwave
Abstract: We describe an on-sky demonstration of a microwave-multiplexing readout system in one of the receivers of the Keck Array, a polarimetry experiment observing the cosmic microwave background at the South Pole. During the austral summer of 2018-2019, we replaced the time-division multiplexing readout system with microwave-multiplexing components including superconducting microwave resonators coupled to radio-frequency superconducting quantum interference devices at the sub-Kelvin focal plane, coaxial-cable plumbing and amplification between room temperature and the cold stages, and a SLAC Microresonator Radio Frequency system for the warm electronics. In the range 5-6 GHz, a single coaxial cable reads out 528 channels. The readout system is coupled to transition-edge sensors, which are in turn coupled to 150-GHz slot-dipole phased-array antennas. Observations began in April 2019, and we report here on an initial characterization of the system performance., 9 pages, 11 figures, Accepted by the Journal of Low Temperature Physics (Proceedings of the 18th International Workshop on Low Temperature Detectors)
Published: 2020

11. Design and Performance of the First BICEP Array Receiver

Author: Jake Connors, E. Karpel, A. Cukierman, B. Racine, Howard Hui, Rashmikant V. Sudiwala, Gene C. Hilton, John M Kovac, Kirit Karkare, Sarah M. Harrison, Eui-Hyeok Yang, Chao Zhang, Mandana Amiri, G. Hall, Che-Hang Yu, S. Fatigoni, K. G. Megerian, Kent D. Irwin, King Tong Lau, Toshiya Namikawa, S. Henderson, J. Cornelison, C. D. Sheehy, Chao-Lin Kuo, Bryan Steinbach, James J. Bock, C. Umiltà, Jeffrey P. Filippini, J. Willmert, J. Cheshire, Zeeshan Ahmed, Donald V. Wiebe, C. Pryke, W. L. K. Wu, Peter A. R. Ade, T. Prouvé, A. Wandui, Lorenzo Moncelsi, Marion Dierickx, Mark Halpern, Victor Buza, Abigail G. Vieregg, A. C. Weber, Ki Won Yoon, S. Richter, Edward D. Young, Ahmed Soliman, H. T. Nguyen, Carole Tucker, T. St. Germaine, N. Precup, Anthony D. Turner, Benjamin L. Schmitt, Roger O'Brient, Alessandro Schillaci, R. Basu Thakur, Keith L. Thompson, Lionel Duband, Sergi R. Hildebrandt, Colin A. Bischoff, M. Crumrine, Denis Barkats, S. Palladino, Carl D. Reintsema, J. Kang, R. Schwarz, H. Boenish, S. Kefeli, and E. Bullock
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 010305 fluids & plasmas, 0103 physical sciences, General Materials Science, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, media_common, Physics, Inflation (cosmology), COSMIC cancer database, Gravitational wave, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Condensed Matter Physics, Atomic and Molecular Physics, and Optics, Amplitude, Sky, Astrophysics - Instrumentation and Methods for Astrophysics, Microwave, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Branches of cosmic inflationary models, such as slow-roll inflation, predict a background of primordial gravitational waves that imprints a unique odd-parity B-mode pattern in the Cosmic Microwave Background (CMB) at amplitudes that are within experimental reach. The BICEP/Keck (BK) experiment targets this primordial signature, the amplitude of which is parameterized by the tensor-to-scalar ratio r, by observing the polarized microwave sky through the exceptionally clean and stable atmosphere at the South Pole. B-mode measurements require an instrument with exquisite sensitivity, tight control of systematics, and wide frequency coverage to disentangle the primordial signal from the Galactic foregrounds. BICEP Array represents the most recent stage of the BK program, and comprises four BICEP3-class receivers observing at 30/40, 95, 150 and 220/270 GHz. The 30/40 GHz receiver will be deployed at the South Pole during the 2019/2020 austral summer. After 3 full years of observations with 30,000+ detectors, BICEP Array will measure primordial gravitational waves to a precision $\sigma(r)$ between 0.002 and 0.004, depending on foreground complexity and the degree of lensing removal. In this paper we give an overview of the instrument, highlighting the design features in terms of cryogenics, magnetic shielding, detectors and readout architecture as well as reporting on the integration and tests that are ongoing with the first receiver at 30/40 GHz., Comment: 9 pages, 5 figures, presented at LTD18 in Milan (July 2019), accepted on JLTP (February 2020)
Published: 2020

12. 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

13. Full-Array Noise Performance of Deployment-Grade SuperSpec mm-wave On-Chip Spectrometers

Author: Reinier M. J. Janssen, Charles M. Bradford, Henry G. LeDuc, S. Gordon, Kirit Karkare, Jordan Wheeler, Peter S. Barry, Carole Tucker, Jason Glenn, Attila Kovács, Simon Doyle, Scott Chapman, Erik Shirokoff, J. Redford, Ryan McGeehan, Jonas Zmuidzinas, S. Hailey-Dunsheath, and P. Mauskopf
Subjects: Physics, Photon, Spectrometer, business.industry, Large Millimeter Telescope, Detector, Intensity mapping, FOS: Physical sciences, Condensed Matter Physics, 7. Clean energy, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Atomic and Molecular Physics, and Optics, 010305 fluids & plasmas, Optics, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, General Materials Science, Millimeter, Wideband, 010306 general physics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Noise (radio)
Abstract: SuperSpec is an on-chip filter-bank spectrometer designed for wideband moderate-resolution spectroscopy at millimeter wavelengths, employing TiN kinetic inductance detectors. SuperSpec technology will enable large-format spectroscopic integral field units suitable for high-redshift line intensity mapping and multi-object spectrographs. In previous results we have demonstrated noise performance in individual detectors suitable for photon noise limited ground-based observations at excellent mm-wave sites. In these proceedings we present the noise performance of a full $R\sim 275$ spectrometer measured using deployment-ready RF hardware and software. We report typical noise equivalent powers through the full device of $\sim 3 \times 10^{-16} \ \mathrm{W}/\sqrt{\mathrm{Hz}}$ at expected sky loadings, which are photon noise dominated. Based on these results, we plan to deploy a six-spectrometer demonstration instrument to the Large Millimeter Telescope in early 2020., 8 pages, 5 figures. Accepted by the Journal of Low Temperature Physics (Proceedings of the 18th International Workshop on Low Temperature Detectors)
Published: 2020

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

Author: Roger O'Brient, John M Kovac, Kirit Karkare, T. Natoli, Kent D. Irwin, A. E. Lowitz, N. Huang, Y. Omori, Victor Buza, Robert I. Citron, S. A. Kernasovskiy, W. L. Holzapfel, Ahmed Soliman, Jeff McMahon, C. Corbett Moran, P. A. R. Ade, Lingzhen Zeng, S. Henderson, W. B. Everett, J. D. Hrubes, Jessica Avva, C. Yu, Calvin B. Netterfield, Lorenzo Moncelsi, J. R. Cheshire, Jason W. Henning, J. A. Grayson, S. Patil, K. K. Schaffer, Elizabeth George, Abigail G. Vieregg, Denis Barkats, V. G. Yefremenko, Jason E. Austermann, N. W. Halverson, A. Cukierman, H. Boenish, B. L. Schmitt, Marion Dierickx, M. Crumrine, K. W. Yoon, Joaquin Vieira, E. Young, G. Hall, Stefan Richter, C. Sievers, Toshiya Namikawa, Graeme Smecher, C. Umilta, D. V. Wiebe, S. Fliescher, T.-L. Chou, H. C. Chiang, Johannes Hubmayr, H. Yang, C. D. Sheehy, Chao-Lin Kuo, Mark Halpern, Christian L. Reichardt, Marius Millea, Joshua Montgomery, S. Kefeli, J. Cornelison, J. J. Bock, Bryan Steinbach, Howard Hui, Gensheng Wang, Andreas Bender, Neil Goeckner-Wald, J. E. Ruhl, Dale Li, C. Tucker, K. G. Megerian, T. M. Crawford, M. A. Dobbs, Mandana Amiri, V. Novosad, R. Schwarz, S. Fatigoni, S. R. Hildebrandt, S. Padin, John E. Carlstrom, E. Bullock, Chao Zhang, T. de Haan, D. C. Goldfinger, John P. Nibarger, Andrew Nadolski, J. Willmert, Carl D. Reintsema, Gene C. Hilton, N. Whitehorn, B. Racine, H. T. Nguyen, A. A. Stark, E. M. Leitch, Alessandro Schillaci, A. D. Turner, E. Karpel, T. Veach, R. Basu Thakur, K. L. Thompson, T. Prouve, A. T. Crites, C. Pryke, C. L. Wong, C. L. Chang, J. Kang, Adam Anderson, Grant Teply, Benjamin Saliwanchik, A. Wandui, Gilbert Holder, A. Manzotti, A. C. Weber, G. I. Noble, Federico Bianchini, Nikhel Gupta, Jeffrey P. Filippini, R. V. Sudiwala, Adrian T. Lee, Bradford Benson, Lloyd Knox, W. L. K. Wu, Colin A. Bischoff, S. S. Meyer, Jason Gallicchio, T. St. Germaine, S. Palladino, L. Duband, J. E. Tolan, Zeeshan Ahmed, L. M. Mocanu, Jake Connors, Kei May Lau, Sarah M. Harrison, Lindsey Bleem, R. W. Ogburn, J. A. Beall, Département des Systèmes Basses Températures (DSBT ), Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), SPTpol, BICEP/Keck, BICEP, and Keck
Subjects: data analysis method, satellite: Planck, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, Cosmic background radiation, cosmic background radiation: polarization, FOS: Physical sciences, cosmic background radiation, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, cosmic rays, gravitation: lens, statistical analysis, Cosmic infrared background, 0103 physical sciences, Experiments in gravity, Sample variance, Planck, numerical calculations, 010306 general physics, Astrophysics::Galaxy Astrophysics, Physics, polarization, background, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: primordial, BICEP, South Pole Telescope, Gravitational lens, B-mode, infrared, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a constraint on the tensor-to-scalar ratio, $r$, derived from measurements of cosmic microwave background (CMB) polarization $B$-modes with "delensing," whereby the uncertainty on $r$ contributed by the sample variance of the gravitational lensing $B$-modes is reduced by cross-correlating against a lensing $B$-mode template. This template is constructed by combining an estimate of the polarized CMB with a tracer of the projected large-scale structure. The large-scale-structure tracer used is a map of the cosmic infrared background derived from Planck satellite data, while the polarized CMB map comes from a combination of South Pole Telescope, BICEP/Keck, and Planck data. We expand the BICEP/Keck likelihood analysis framework to accept a lensing template and apply it to the BICEP/Keck data set collected through 2014 using the same parametric foreground modelling as in the previous analysis. From simulations, we find that the uncertainty on $r$ is reduced by $\sim10\%$, from $��(r)$= 0.024 to 0.022, which can be compared with a $\sim26\%$ reduction obtained when using a perfect lensing template. Applying the technique to the real data, the constraint on $r$ is improved from $r_{0.05} < 0.090$ to $r_{0.05} < 0.082$ (95\% C.L.). This is the first demonstration of improvement in an $r$ constraint through delensing., 23 pages, 11 figures; match published version
Published: 2020
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16. CMB-S4 Decadal Survey APC White Paper

Author: Shaul Hanany, Georges Obied, J. Colin Hill, Thomas Cecil, Keith L. Thompson, Adam Anderson, Michael L. Brown, Doug Johnstone, Lorenzo Moncelsi, Erminia Calabrese, Howard Hui, Haruki Nishino, Sara M. Simon, James Kerby, Theodore Kisner, K. T. Story, Moritz Münchmeyer, Aritoki Suzuki, Joseph J. Mohr, Adrian T. Lee, Bradley R. Johnson, Sanah Bhimani, W. C. Jones, A. E. Lowitz, Nathan Whitehorn, Valentine Novosad, Marcelo A. Alvarez, Anze Slosar, Kam Arnold, Kevork N. Abazajian, Mustafa A. Amin, Evan Grohs, Abigail G. Vieregg, Siavash Yasini, Mathew S. Madhavacheril, Julien Carron, Ritoban Basu Thakur, Jean-Baptiste Melin, Shawn W. Henderson, Asantha Cooray, Chris Stoughton, Peter Timbie, Matteo Bonato, Ki Won Yoon, Blakesley Burkhart, Salman Habib, T. Natoli, Jacques Delabrouille, Carlo Baccigalupi, Victor Guarino, Steven W. Allen, Kathy Bailey, Aurelien A. Fraisse, Osamu Tajima, Silvia Galli, Denis Barkats, Antony Lewis, Ari Cukierman, Johannes Hubmayr, Marilena LoVerde, Erik Shirokoff, G. P. Holder, James G. Bartlett, James Yeck, Dale Li, N. W. Halverson, Graeme E. Addison, Adam Mantz, Matthieu Tristram, Laura Newburgh, Sarah Shandera, Alessandro Schillaci, Lindsey Bleem, Raphael Flauger, Marcel Schmittfull, S. Pandey, Kent D. Irwin, N. Kurita, Gregory S. Tucker, Matthew Hasselfield, Reijo Keskitalo, Levon Pogosian, Rachel S. Somerville, C. D. Sheehy, Srini Rajagopalan, Jesse Treu, Giuseppe Puglisi, Eric J. Baxter, John M Kovac, Emmanuel Schaan, Marcel Demarteau, Akito Kusaka, Suzanne T. Staggs, Kirit Karkare, Josquin Errard, Thomas Essinger-Hileman, Anne Lähteenmäki, Mattia Negrello, Toshiya Namikawa, Zhilei Xu, Mark Halpern, Simone Ferraro, Edo Berger, François R. Bouchet, Zeeshan Ahmed, Frederick Matsuda, Joseph Eimer, Alexandra S. Rahlin, W. L. Kimmy Wu, Giulio Fabbian, Chao-Lin Kuo, Christian L. Reichardt, Marius Millea, Stephen Padin, A. T. Crites, Joel Meyers, William Edwards, R. Gualtieri, Jason W. Henning, Arthur Kosowsky, Edward J. Wollack, W. L. Holzapfel, Michael D. Niemack, John E. Carlstrom, Rachel Bean, Cora Dvorkin, Ely D. Kovetz, David Alonso, Nicholas Battaglia, Sean Bryan, Gianfranco De Zotti, Anthony Challinor, Graca Rocha, Federico Nati, Jeffrey P. Filippini, Katrin Heitmann, Eric V. Linder, Antony A. Stark, Martin Nordby, Grant Teply, Benjamin Saliwanchik, Peter Adshead, P. Daniel Meerburg, Victoria Calafut, Francis-Yan Cyr-Racine, M.E. Huffer, Chris Bebek, Lloyd Knox, Masashi Hazumi, Eleonora Di Valentino, Natalie A. Roe, Nicholas Galitzki, Masaya Hasegawa, Sarah Kernovsky, Victor Buza, Darcy Barron, C. Pryke, Tijmen de Haan, Tony Mroczkowski, Vera Gluscevic, Andrea Zonca, Daniel Green, Kimberly K. Boddy, Srinivasan Raghunathan, Jeff McMahon, J. E. Ruhl, Steve Kuhlmann, Blake D. Sherwin, Joaquin Vieira, Peter S. Barry, Daisuke Nagai, Karen Byrum, Neelima Sehgal, Murdock Gilchriese, Marco Raveri, M. Tomasi, Douglas Scott, James J. Bock, Martin White, Chang Feng, Ken Ganga, Martina Gerbino, Suvodip Mukherjee, Radek Stompor, Gensheng Wang, B. Racine, Mark Reichanadter, Paul O'Connor, Alexander van Engelen, Kevin M. Huffenberger, Maria Salatino, Kathleen Harrington, Nobuhiko Katayama, Bradford Benson, Daniel Grin, Colin A. Bischoff, Charles R. Lawrence, Mark Vogelsberger, Shannon M. Duff, Scott Watson, Sebastian Bocquet, C. Umiltà, Andrei V. Frolov, C. L. Chang, Johanna Nagy, J. Richard Bond, Philip Daniel Mauskopf, B. Flaugher, Robert R. Caldwell, Mark J. Devlin, Renée Hlozek, Anirban Roy, Elena Pierpaoli, Amy N. Bender, Bruce Partridge, E. Y. Young, Matt Dobbs, Julian Borrill, Adriaan J. Duivenvoorden, Yuji Chinone, Mathieu Remazeilles, T. M. Crawford, Jon E. Gudmundsson, Hsiao-Mei Sherry Cho, and Gunther Haller
Subjects: White paper, 010308 nuclear & particles physics, 0103 physical sciences, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Environmental science, Astrophysics::Cosmology and Extragalactic Astrophysics, Project plan, 010306 general physics, 01 natural sciences
Abstract: We provide an overview of the science case, instrument configuration and project plan for the next-generation ground-based cosmic microwave background experiment CMB-S4, for consideration by the 2020 Decadal Survey.
Published: 2019

17. Astro 2020 Science White Paper: Fundamental Cosmology in the Dark Ages with 21-cm Line Fluctuations

Author: Furlanetto, Steven, Bowman, Judd D., Mirocha, Jordan, Pober, Jonathan C., Burns, Jack, Carilli, Chris L., Munoz, Julian, Aguirre, James, Ali-Haimoud, Yacine, Alvarez, Marcelo, Beardsley, Adam, Becker, George, Breysse, Patrick, Bromm, Volker, Bull, Philip, Chang, Tzu-Ching, Chen, Xuelei, Chiang, Hsin, Cohn, Joanne, Davies, Frederick, Deboer, David, Dillon, Joshua, Doré, Olivier, Dvorkin, Cora, Fialkov, Anastasia, Hazelton, Bryna, Jacobs, Daniel, Kirit Karkare, Kohn, Saul, Koopmans, Leon, Kovetz, Ely, La Plante, Paul, Lidz, Adam, Liu, Adrian, Ma, Yin-Zhe, Mao, Yi, Masui, Kiyoshi, Mesinger, Andrew, Murray, Steven, Parsons, Aaron, Saliwanchik, Benjamin, Sievers, Jonathan, Thyagarajan, Nithyanandan, Trac, Hy, Visbal, Eli, and Zaldarriaga, Matias
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Dark Ages are the period between the last scattering of the cosmic microwave background and the appearance of the first luminous sources, spanning approximately 1100 < z < 30. The only known way to measure fluctuations in this era is through the 21-cm line of neutral hydrogen. Such observations have enormous potential for cosmology, because they span a large volume while the fluctuations remain linear even on small scales. Observations of 21-cm fluctuations during this era can therefore constrain fundamental aspects of our Universe, including inflation and any exotic physics of dark matter. While the observational challenges to these low-frequency 21-cm observations are enormous, especially from the terrestrial environment, they represent an important goal for cosmology., 10 pages, 4 figures
Published: 2019
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18. Primordial Non-Gaussianity

Author: Meerburg, P. Daniel, Green, Daniel, Abidi, Muntazir, Amin, Mustafa A., Adshead, Peter, Ahmed, Zeeshan, Alonso, David, Ansarinejad, Behzad, Armstrong, Robert, Avila, Santiago, Baccigalupi, Carlo, Baldauf, Tobias, Ballardini, Mario, Bandura, Kevin, Bartolo, Nicola, Battaglia, Nicholas, Baumann, Daniel, Bavdhankar, Chetan, Bernal, José Luis, Beutler, Florian, Biagetti, Matteo, Bischoff, Colin, Blazek, Jonathan, Bond, J. Richard, Borrill, Julian, Bouchet, François R., Bull, Philip, Burgess, Cliff, Byrnes, Christian, Calabrese, Erminia, Carlstrom, John E., Castorina, Emanuele, Challinor, Anthony, Chang, Tzu-Ching, Chaves-Montero, Jonás, Chen, Xingang, Yèche, Christophe, Cooray, Asantha, Coulton, William, Crawford, Thomas, Chisari, Elisa, Cyr-Racine, Francis-Yan, D Amico, Guido, Bernardis, Paolo, La Macorra, Axel, Doré, Olivier, Duivenvoorden, Adri, Dunkley, Joanna, Dvorkin, Cora, Eggemeier, Alexander, Escoffier, Stephanie, Essinger-Hileman, Tom, Fasiello, Matteo, Ferraro, Simone, Flauger, Raphael, Font-Ribera, Andreu, Foreman, Simon, Friedrich, Oliver, García-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Goon, Garrett, Górski, Krzysztof M., Gudmundsson, Jon E., Gupta, Nikhel, Hanany, Shaul, Handley, Will, Hawken, Adam J., Hill, J. Colin, Hirata, Christopher M., Hložek, Renée, Holder, Gilbert, Huterer, Dragan, Kamionkowski, Marc, Kirit Karkare, Keeley, Ryan E., Kinney, William, Kisner, Theodore, Kneib, Jean-Paul, Knox, Lloyd, Koushiappas, Savvas M., Kovetz, Ely D., Koyama, Kazuya, L Huillier, Benjamin, Lahav, Ofer, Lattanzi, Massimiliano, Lee, Hayden, Liguori, Michele, Loverde, Marilena, Madhavacheril, Mathew, Maldacena, Juan, Marsh, M. C. David, Masui, Kiyoshi, Matarrese, Sabino, Mcallister, Liam, Mcmahon, Jeff, Mcquinn, Matthew, Meyers, Joel, Mirbabayi, Mehrdad, Moradinezhad Dizgah, Azadeh, Motloch, Pavel, Mukherjee, Suvodip, Muñoz, Julian B., Myers, Adam D., Nagy, Johanna, Naselsky, Pavel, Nati, Federico, Newburgh, Nicolis, Alberto, Niemack, Michael D., Niz, Gustavo, Nomerotski, Andrei, Page, Lyman, Pajer, Enrico, Padmanabhan, Hamsa, Palma, Gonzalo A., Peiris, Hiranya V., Percival, Will J., Piacentni, Francesco, Pimentel, Guilherme L., Pogosian, Levon, Prescod-Weinstein, Chanda, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Stompor, Radek, Raveri, Marco, Remazeilles, Mathieu, Rocha, Graça, Ross, Ashley J., Rossi, Graziano, Ruhl, John, Sasaki, Misao, Schaan, Emmanuel, Schillaci, Alessandro, Schmittfull, Marcel, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shan, Huanyuan, Shandera, Sarah, Sherwin, Blake D., Silverstein, Eva, Simon, Sara, Slosar, Anze, Staggs, Suzanne, Starkman, Glenn, Stebbins, Albert, Suzuki, Aritoki, Switzer, Eric R., Timbie, Peter, Tolley, Andrew J., Tomasi, Maurizio, Tristram, Matthieu, Trodden, Mark, Tsai, Yu-Dai, Uhlemann, Cora, Umiltà, Caterina, Engelen, Alexander, Vargas-Magaña, M., Vieregg, Abigail, Wallisch, Benjamin, Wands, David, Wandelt, Benjamin, Wang, Yi, Watson, Scott, Wise, Mark, Wu, W. L. K., Xianyu, Zhong-Zhi, Xu, Weishuang, Yasini, Siavash, Young, Sam, Yutong, Duan, Zaldarriaga, Matias, Zemcov, Michael, Zhao, Gong-Bo, Zheng, Yi, and Zhu, Ningfeng
Subjects: High Energy Physics - Theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), High Energy Physics - Theory (hep-th), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Our current understanding of the Universe is established through the pristine measurements of structure in the cosmic microwave background (CMB) and the distribution and shapes of galaxies tracing the large scale structure (LSS) of the Universe. One key ingredient that underlies cosmological observables is that the field that sources the observed structure is assumed to be initially Gaussian with high precision. Nevertheless, a minimal deviation from Gaussianityis perhaps the most robust theoretical prediction of models that explain the observed Universe; itis necessarily present even in the simplest scenarios. In addition, most inflationary models produce far higher levels of non-Gaussianity. Since non-Gaussianity directly probes the dynamics in the early Universe, a detection would present a monumental discovery in cosmology, providing clues about physics at energy scales as high as the GUT scale., Comment: 5 pages + references; Submitted to the Astro2020 call for science white papers. This version: fixed author list
Published: 2019
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19. Delensing Degree-Scale $B$-Mode Polarization with High-Redshift Line Intensity Mapping

Author: Kirit Karkare
Subjects: Physics, Line-of-sight, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Cosmic microwave background, Intensity mapping, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), 01 natural sciences, Redshift, Gravitational lens, Cosmic infrared background, 0103 physical sciences, 010306 general physics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Cosmic microwave background (CMB) experiments that constrain the tensor-to-scalar ratio $r$ are now approaching the sensitivity at which delensing---removing the $B$ modes induced by the gravitational lensing of large-scale structure---is necessary. We consider the improvement in delensing that maps of large-scale structure from tomographic line intensity mapping (IM) experiments targeting $2 < z < 10$ could provide. Compared to a nominal baseline of cosmic infrared background and internal delensing at CMB-S4 sensitivity, we find that the addition of high-redshift IM data could improve delensing performance by ~11%. Achieving the requisite sensitivity in the IM data is feasible with next-generation experiments that are now being planned. However, these results are contingent on the ability to measure low-$k$ modes along the line of sight. Without these modes, IM datasets are unable to to correlate with the lensing kernel and do not aid in delensing., 9 pages, 4 figures, 1 table. Matches version published in Phys. Rev. D
Published: 2019
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20. 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

21. Constraining the expansion history and early dark energy with line intensity mapping

Author: Simeon Bird and Kirit Karkare
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Intensity mapping, FOS: Physical sciences, Rotational transition, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Measure (mathematics), Redshift, Amplitude, 0103 physical sciences, Dark energy, Baryon acoustic oscillations, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Line (formation)
Abstract: We consider the potential for line intensity mapping (IM) experiments to measure the baryon acoustic oscillations (BAO) from 3 < z < 6. This would constrain the expansion history in a redshift range that is currently unexplored. We calculate the map depths that future IM experiments targeting the CO(1-0) rotational transition line and [CII] ionized carbon fine-structure line would need to achieve in order to measure the BAO. We find that near-future IM experiments could constrain the BAO scale to 5% or better depending on CO/[CII] model amplitude. This measurement is at a precision that could make competitive constraints on models of early dark energy., 9 pages, 3 figures. Updated to reflect published version
Published: 2018

22. On-sky demonstration of the SuperSpec millimeter-wave spectrometer (Conference Presentation)

Author: Christopher M. McKenney, Ryan McGeehan, George Che, Jordan A. Turner, Samantha Walker, Theodore Reck, Erik Shirokoff, Carole Tucker, Peter S. Barry, J. Redford, Henry G. LeDuc, Matthew I. Hollister, Jason Glenn, Charles M. Bradford, Samuel Gordon, Jonas Zmuidzinas, Attila Kovács, Scott Chapman, Jordan Wheeler, S. Hailey-Dunsheath, Kirit Karkare, and Philip Daniel Mauskopf
Subjects: Physics, Spectrometer, Physics::Instrumentation and Detectors, business.industry, Large Millimeter Telescope, Astrophysics::Instrumentation and Methods for Astrophysics, Intensity mapping, Astrophysics::Cosmology and Extragalactic Astrophysics, law.invention, Telescope, Optics, law, Extremely high frequency, Millimeter, business, Reionization, Astrophysics::Galaxy Astrophysics, Noise (radio)
Abstract: SuperSpec is an on-chip filter-bank spectrometer designed for wideband moderate-resolution spectroscopy at millimeter and submillimeter wavelengths. Employing TiN kinetic inductance detectors, the device has demonstrated noise performance suitable for photon noise limited ground-based observations at excellent millimeter-wave observing sites. In these proceedings we present a demonstration instrument featuring six independent single-polarization SuperSpec chips, covering 190-310 GHz with 300 channels. We summarize spectrometer performance, describe the cryostat and optical coupling, and present the readout and telescope control system. In an initial deployment to the Large Millimeter Telescope, we plan to observe submillimeter galaxies in [CII] emission at redshifts 5 < z < 9 and CO emission from lower-redshift galaxies. Real on-sky performance will inform the design of the next generation of instruments using large numbers of SuperSpec devices, which could include multi-object spectrometers or line intensity mapping experiments that target [CII] during the Epoch of Reionization.
Published: 2018

23. The design and characterization of a 300 channel, optimized full-band millimeter filterbank for science with SuperSpec

Author: Henry G. LeDuc, R. McGeehan, George Che, Jordan Wheeler, Charles M. Bradford, Peter S. Barry, Philip Daniel Mauskopf, Erik Shirokoff, Jason Glenn, Steve Hailey-Dunsheath, T. Reck, Kirit Karkare, Jonas Zmuidzinas, J. Redford, Zmuidzinas, Jonas, and Gao, Jian-Rong
Subjects: Materials science, Spectrometer, Frequency band, business.industry, Large Millimeter Telescope, 01 natural sciences, Microstrip, law.invention, Lens (optics), Resonator, Optics, law, 0103 physical sciences, Extremely high frequency, Millimeter, 010306 general physics, business, 010303 astronomy & astrophysics
Abstract: SuperSpec is an integrated, on-chip spectrometer for millimeter and sub-millimeter astronomy. We report the approach, design optimization, and partial characterization of a 300 channel filterbank covering the 185 to 315 GHz frequency band that targets a resolving power R ~ 310, and fits on a 3.5×5.5 cm chip. SuperSpec uses a lens and broadband antenna to couple radiation into a niobium microstrip that feeds a bank of niobium microstrip half-wave resonators for frequency selectivity. Each half-wave resonator is coupled to the inductor of a titanium nitride lumped-element kinetic inductance detector (LEKID) that detects the incident radiation. The device was designed for use in a demonstration instrument at the Large Millimeter Telescope (LMT).
Published: 2018

24. 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

25. 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

26. 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

27. 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

28. 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

29. 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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30. 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

31. 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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32. 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

33. 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

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

Author: M. Lueker, Grant Teply, Sunil Golwala, E. Bullock, R. Schwarz, Howard Hui, H. T. Nguyen, Nuria Llombart, J. A. Bonetti, Roger O'Brient, Ki Won Yoon, C. L. Wong, S. J. Benton, I. Buder, Gene C. Hilton, R. S. Tucker, Mandana Amiri, Justus A. Brevik, A. C. Weber, Matthew Hasselfield, Colin A. Bischoff, W. C. Jones, Peter K. Day, Donald V. Wiebe, John M Kovac, A. D. Turner, Kirit Karkare, P. Wilson, Henry G. LeDuc, Kent D. Irwin, K. G. Megerian, E. M. Leitch, Goutam Chattopadhyay, Alexandra S. Rahlin, J. E. Tolan, Carl D. Reintsema, G. Davis, L. Duband, S. Richter, Jeffrey P. Filippini, Amy Trangsrud, R. W. Ogburn, S. A. Kernasovskiy, Chao-Lin Kuo, James J. Bock, R. Sudiwala, P. V. Mason, Z. K. Staniszewski, Marcus Runyan, Calvin B. Netterfield, Denis Barkats, C. D. Dowell, C. Pryke, J. P. Kaufman, Mark Halpern, S. Fliescher, Brian Keating, Jonas Zmuidzinas, S. Kefeli, Viktor Hristov, A. Orlando, S. R. Hildebrandt, C. D. Sheehy, Peter A. R. Ade, Lorenzo Moncelsi, Abigail G. Vieregg, and Randol W. Aikin
Subjects: Physics, Spider, business.industry, Detector, Cosmic microwave background, Bandwidth (signal processing), Bolometer, Polarimetry, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Spectral bands, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Multiplexing, law.invention, Optics, Space and Planetary Science, law, 0103 physical sciences, 010306 general physics, business, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: We have developed antenna-coupled transition-edge sensor (TES) bolometers for a wide range of cosmic microwave background (CMB) polarimetry experiments, including BICEP2, Keck Array, and the balloon borne SPIDER. These detectors have reached maturity and this paper reports on their design principles, overall performance, and key challenges associated with design and production. Our detector arrays repeatedly produce spectral bands with 20%-30% bandwidth at 95, 150, or 220~GHz. The integrated antenna arrays synthesize symmetric co-aligned beams with controlled side-lobe levels. Cross-polarized response on boresight is typically ~0.5%, consistent with cross-talk in our multiplexed readout system. End-to-end optical efficiencies in our cameras are routinely 35% or higher, with per detector sensitivities of NET~300 uKrts. Thanks to the scalability of this design, we have deployed 2560 detectors as 1280 matched pairs in Keck Array with a combined instantaneous sensitivity of ~9 uKrts, as measured directly from CMB maps in the 2013 season. Similar arrays have recently flown in the SPIDER instrument, and development of this technology is ongoing., Comment: 16 pgs, 20 figs
Published: 2015
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35. 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

36. 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

37. 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

38. 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

39. 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

40. 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

41. Mapping Cosmic Dawn and Reionization: Challenges and Synergies

Author: Alvarez, Marcelo A., Fialkov, Anastasia, La Plante, Paul, Aguirre, James, Ali-Haïmoud, Yacine, Becker, George, Bowman, Judd, Breysse, Patrick, Bromm, Volker, Bull, Philip, Burns, Jack, Cappelluti, Nico, Carucci, Isabella, Chang, Tzu-Ching, Cleary, Kieran, Cooray, Asantha, Chen, Xuelei, Chiang, Hsin, Cohn, Joanne, Deboer, David, Dillon, Joshua, Doré, Olivier, Dvorkin, Cora, Ferraro, Simone, Furlanetto, Steven, Hazelton, Bryna, Hill, J. Colin, Jacobs, Daniel, Kirit Karkare, Keating, Garrett K., Koopmans, Léon, Kovetz, Ely, Lidz, Adam, Liu, Adrian, Ma, Yin-Zhe, Mao, Yi, Masui, Kiyoshi, Mcquinn, Matthew, Mirocha, Jordan, Muñoz, Julian, Murray, Steven, Parsons, Aaron, Pober, Jonathan, Saliwanchik, Benjamin, Sievers, Jonathan, Thyagarajan, Nithyanandan, Trac, Hy, Vikhlinin, Alexey, Visbal, Eli, and Zaldarriaga, Matias
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Cosmic dawn and the Epoch of Reionization (EoR) are among the least explored observational eras in cosmology: a time at which the first galaxies and supermassive black holes formed and reionized the cold, neutral Universe of the post-recombination era. With current instruments, only a handful of the brightest galaxies and quasars from that time are detectable as individual objects, due to their extreme distances. Fortunately, a multitude of multi-wavelength intensity mapping measurements, ranging from the redshifted 21 cm background in the radio to the unresolved X-ray background, contain a plethora of synergistic information about this elusive era. The coming decade will likely see direct detections of inhomogenous reionization with CMB and 21 cm observations, and a slew of other probes covering overlapping areas and complementary physical processes will provide crucial additional information and cross-validation. To maximize scientific discovery and return on investment, coordinated survey planning and joint data analysis should be a high priority, closely coupled to computational models and theoretical predictions., 5 pages, 1 figure, submitted to the Astro2020 Decadal Survey Science White Paper call

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