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Casas FJ, Pascual-Cisneros G. Mach-Zehnder Modulators for Microwave Polarization Measurement in Astronomy Applications. SENSORS (BASEL, SWITZERLAND) 2023; 23:6300. [PMID: 37514594 PMCID: PMC10385403 DOI: 10.3390/s23146300] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/12/2023] [Revised: 06/29/2023] [Accepted: 06/30/2023] [Indexed: 07/30/2023]
Abstract
This paper presents a study of the performances of different Mach-Zehnder modulation technologies with applications in microwave polarimeters based on a near-infrared (NIR) frequency up-conversion stage, allowing for optical correlation and signal detection at a wavelength of 1550 nm. Commercial Mach-Zehnder modulators (MZMs) are traditionally implemented using LiNbO3 technology, which does not enable integration for the fabrication of MZMs. In this work, we propose the use of an alternative technology based on InP, which allows for integration in the fabrication process. In this way, it is possible to obtain advantages in terms of bandwidth, cost, and size reductions, which yield results that are very interesting for wide-band applications such as microwave instrumentation for the study of the cosmic microwave background (CMB). Here, we describe and compare the modulation performances of different MZMs, with one commercial unit presenting a higher bandwidth than those in previous works, and another three InP integrated units provided by the Fraunhofer Institute for Telecommunications, Heinrich-Hertz-Institute (HHI). Then, these modulators were coupled to a microwave polarimeter demonstrator, which has also been presented previously, to compare the polarization measurement performances of each of the MZMs.
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Affiliation(s)
- Francisco J Casas
- Instituto de Física de Cantabria (IFCA), Avda. Los Castros s/n, 39005 Santander, Spain
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Casas FJ, Vielva P, Barreiro RB, Martínez-González E, Pascual-Cisneros G. Polarization Calibration of a Microwave Polarimeter with Near-Infrared Up-Conversion for Optical Correlation and Detection. SENSORS (BASEL, SWITZERLAND) 2022; 22:8080. [PMID: 36298431 PMCID: PMC9609977 DOI: 10.3390/s22208080] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 10/06/2022] [Revised: 10/19/2022] [Accepted: 10/19/2022] [Indexed: 06/16/2023]
Abstract
This paper presents a polarization calibration method applied to a microwave polarimeter demonstrator based on a near-infrared (NIR) frequency up-conversion stage that allows both optical correlation and signal detection at a wavelength of 1550 nm. The instrument was designed to measure the polarization of cosmic microwave background (CMB) radiation from the sky, obtaining the Stokes parameters of the incoming signal simultaneously, in a frequency range from 10 to 20 GHz. A linearly polarized input signal with a variable polarization angle is used as excitation in the polarimeter calibration setup mounted in the laboratory. The polarimeter systematic errors can be corrected with the proposed calibration procedure, achieving high levels of polarization efficiency (low polarization percentage errors) and low polarization angle errors. The calibration method is based on the fitting of polarization errors by means of sinusoidal functions composed of additive or multiplicative terms. The accuracy of the fitting increases with the number of terms in such a way that the typical error levels required in low-frequency CMB experiments can be achieved with only a few terms in the fitting functions. On the other hand, assuming that the calibration signal is known with the required accuracy, additional terms can be calculated to reach the error levels needed in ultrasensitive B-mode polarization CMB experiments.
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Baleato Lizancos A, Ferraro S. Impact of extragalactic foregrounds on internal delensing of the CMB
B
-mode polarization. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.063534] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Guan Y, Kosowsky A. Distinguishing primordial magnetic fields from inflationary tensor perturbations in the cosmic microwave background. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.063505] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Abstract
This review aims at proposing to the field an overview of the Cusp-core problem, including a discussion of its advocated solutions, assessing how each can satisfactorily provide a description of central densities. Whether the Cusp-core problem reflects our insufficient grasp on the nature of dark matter, of gravity, on the impact of baryonic interactions with dark matter at those scales, as included in semi-analytical models or fully numerical codes, the solutions to it can point either to the need for a paradigm change in cosmology, or to to our lack of success in ironing out the finer details of the ΛCDM paradigm.
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Cai YF, Jiang J, Sasaki M, Vardanyan V, Zhou Z. Beating the Lyth Bound by Parametric Resonance during Inflation. PHYSICAL REVIEW LETTERS 2021; 127:251301. [PMID: 35029452 DOI: 10.1103/physrevlett.127.251301] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/04/2021] [Revised: 10/26/2021] [Accepted: 11/24/2021] [Indexed: 06/14/2023]
Abstract
We propose a novel mechanism for enhancing primordial gravitational waves without significantly affecting the curvature perturbations produced during inflation. This is achieved due to nonlinear sourcing of resonantly amplified scalar field fluctuations. Our result is an explicit scale-dependent counterexample of the famous Lyth bound, which opens up a promising perspective of producing detectable inflationary tensor modes with low-scale inflation and a sub-Planckian field excursion. We explicitly demonstrate the testability of our mechanism with upcoming cosmic microwave background B-mode observations.
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Affiliation(s)
- Yi-Fu Cai
- Department of Astronomy, School of Physical Sciences, University of Science and Technology of China, Hefei, Anhui 230026, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei, Anhui 230026, China
- CAS Key Laboratory for Researches in Galaxies and Cosmology, University of Science and Technology of China, Hefei, Anhui 230026, China
| | - Jie Jiang
- Department of Astronomy, School of Physical Sciences, University of Science and Technology of China, Hefei, Anhui 230026, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei, Anhui 230026, China
- CAS Key Laboratory for Researches in Galaxies and Cosmology, University of Science and Technology of China, Hefei, Anhui 230026, China
| | - Misao Sasaki
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), UTIAS, The University of Tokyo, Chiba 277-8583, Japan
- Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan
- Leung Center for Cosmology and Particle Astrophysics, National Taiwan University, Taipei 10617, Taiwan
| | - Valeri Vardanyan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), UTIAS, The University of Tokyo, Chiba 277-8583, Japan
| | - Zihan Zhou
- Department of Astronomy, School of Physical Sciences, University of Science and Technology of China, Hefei, Anhui 230026, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei, Anhui 230026, China
- CAS Key Laboratory for Researches in Galaxies and Cosmology, University of Science and Technology of China, Hefei, Anhui 230026, China
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Abstract
A hundred years ago, two British expeditions measured the deflection of starlight by the Sun’s gravitational field, confirming the prediction made by Einstein’s General Theory of Relativity. One hundred years later many physicists around the world are involved in studying the consequences and use as a research tool, of the deflection of light by gravitational fields, a discipline that today receives the generic name of Gravitational Lensing. The present review aims to commemorate the centenary of Einstein’s Eclipse expeditions by presenting a historical perspective of the development and milestones on gravitational light bending, covering from early XIX century speculations, to its current use as an important research tool in astronomy and cosmology.
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Riedel B, Bryant L, Carlstrom J, Crawford T, Gardner RW, Harrington N, Huang N, Rahlin A, Stephen J, Whitehorn N. SPT-3G Computing. EPJ WEB OF CONFERENCES 2019. [DOI: 10.1051/epjconf/201921403051] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/15/2022] Open
Abstract
SPT-3G, the third generation camera on the South Pole Telescope (SPT), was deployed in the 2016-2017 Austral summer season. The SPT is a 10-meter telescope located at the geographic South Pole and designed for observations in the millimeter-wave and submillimeter-wave regions of the electromagnetic spectrum. The SPT is primarily used to study the cosmic microwave background (CMB). The upgraded camera produces an order of magnitude more data than the previous generations of SPT cameras. The telescope is expected to collect a petabyte (PB) of data over course of five years, which is a significantly larger data volume than any other CMB telescope in operation. The increase in data rate required radical changes to the SPT computing model both at the South Pole and University of Chicago. This paper will describe the overall integration of distributed storage and compute resources into a common interface, deployment of on-site data reduction and storage infrastructure, and the usage of the Open Science Grid (OSG) by the SPT collaboration.
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Christensen N. Stochastic gravitational wave backgrounds. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2019; 82:016903. [PMID: 30462612 DOI: 10.1088/1361-6633/aae6b5] [Citation(s) in RCA: 10] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
A stochastic background of gravitational waves could be created by the superposition of a large number of independent sources. The physical processes occurring at the earliest moments of the universe certainly created a stochastic background that exists, at some level, today. This is analogous to the cosmic microwave background, which is an electromagnetic record of the early universe. The recent observations of gravitational waves by the Advanced LIGO and Advanced Virgo detectors imply that there is also a stochastic background that has been created by binary black hole and binary neutron star mergers over the history of the universe. Whether the stochastic background is observed directly, or upper limits placed on it in specific frequency bands, important astrophysical and cosmological statements about it can be made. This review will summarize the current state of research of the stochastic background, from the sources of these gravitational waves to the current methods used to observe them.
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Affiliation(s)
- Nelson Christensen
- ARTEMIS, Université Côte d'Azur, Observatoire Côte d'Azur, CNRS, 06304 Nice, France
- Physics and Astronomy, Carleton College, Northfield, MN 55057, United States of America
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Ishak M. Testing general relativity in cosmology. LIVING REVIEWS IN RELATIVITY 2018; 22:1. [PMID: 30613193 PMCID: PMC6299071 DOI: 10.1007/s41114-018-0017-4] [Citation(s) in RCA: 19] [Impact Index Per Article: 3.2] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 05/28/2018] [Accepted: 11/06/2018] [Indexed: 06/09/2023]
Abstract
We review recent developments and results in testing general relativity (GR) at cosmological scales. The subject has witnessed rapid growth during the last two decades with the aim of addressing the question of cosmic acceleration and the dark energy associated with it. However, with the advent of precision cosmology, it has also become a well-motivated endeavor by itself to test gravitational physics at cosmic scales. We overview cosmological probes of gravity, formalisms and parameterizations for testing deviations from GR at cosmological scales, selected modified gravity (MG) theories, gravitational screening mechanisms, and computer codes developed for these tests. We then provide summaries of recent cosmological constraints on MG parameters and selected MG models. We supplement these cosmological constraints with a summary of implications from the recent binary neutron star merger event. Next, we summarize some results on MG parameter forecasts with and without astrophysical systematics that will dominate the uncertainties. The review aims at providing an overall picture of the subject and an entry point to students and researchers interested in joining the field. It can also serve as a quick reference to recent results and constraints on testing gravity at cosmological scales.
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Affiliation(s)
- Mustapha Ishak
- Department of Physics, The University of Texas at Dallas, Richardson, TX 75080 USA
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Zhan H, Anthony Tyson J. Cosmology with the Large Synoptic Survey Telescope: an overview. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2018; 81:066901. [PMID: 29473548 DOI: 10.1088/1361-6633/aab1bd] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/08/2023]
Abstract
The Large Synoptic Survey Telescope (LSST) is a high étendue imaging facility that is being constructed atop Cerro Pachón in northern Chile. It is scheduled to begin science operations in 2022. With an [Formula: see text] ([Formula: see text] effective) aperture, a novel three-mirror design achieving a seeing-limited [Formula: see text] field of view, and a 3.2 gigapixel camera, the LSST has the deep-wide-fast imaging capability necessary to carry out an [Formula: see text] survey in six passbands (ugrizy) to a coadded depth of [Formula: see text] over 10 years using [Formula: see text] of its observational time. The remaining [Formula: see text] of the time will be devoted to considerably deeper and faster time-domain observations and smaller surveys. In total, each patch of the sky in the main survey will receive 800 visits allocated across the six passbands with [Formula: see text] exposure visits. The huge volume of high-quality LSST data will provide a wide range of science opportunities and, in particular, open a new era of precision cosmology with unprecedented statistical power and tight control of systematic errors. In this review, we give a brief account of the LSST cosmology program with an emphasis on dark energy investigations. The LSST will address dark energy physics and cosmology in general by exploiting diverse precision probes including large-scale structure, weak lensing, type Ia supernovae, galaxy clusters, and strong lensing. Combined with the cosmic microwave background data, these probes form interlocking tests on the cosmological model and the nature of dark energy in the presence of various systematics. The LSST data products will be made available to the US and Chilean scientific communities and to international partners with no proprietary period. Close collaborations with contemporaneous imaging and spectroscopy surveys observing at a variety of wavelengths, resolutions, depths, and timescales will be a vital part of the LSST science program, which will not only enhance specific studies but, more importantly, also allow a more complete understanding of the Universe through different windows.
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Affiliation(s)
- Hu Zhan
- CAS Key Laboratory of Space Astronomy and Technology, National Astronomical Observatories, A20 Datun Road, Chaoyang District, Beijing 100012, People's Republic of China
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Staggs S, Dunkley J, Page L. Recent discoveries from the cosmic microwave background: a review of recent progress. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2018; 81:044901. [PMID: 29051392 DOI: 10.1088/1361-6633/aa94d5] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/07/2023]
Abstract
Measurements of the anisotropies in the cosmic microwave background (CMB) radiation have provided a wealth of information about the cosmological model that describes the contents and evolution of the universe. These data have led to a standard model described by just six parameters. In this review we focus on discoveries made in the past decade from satellite and ground-based experiments, and look ahead to those anticipated in the coming decade. We provide an introduction to the key CMB observables including temperature and polarization anisotropies, and describe recent progress towards understanding the initial conditions of structure formation, and establishing the properties of the contents of the universe including neutrinos. Results are now being derived both from the primordial CMB signal that traces the behavior of the universe at 400 000 years of cosmic time, as well as from the signals imprinted at later times due to scattering from galaxy clusters, from the motion of electrons in the ionized universe, and from the gravitational lensing of the CMB photons. We describe current experimental methods to measure the CMB, particularly focusing on details relevant for ground and balloon-based instruments, and give an overview of the broad data analysis methods required to convert measurements of the microwave sky into cosmological parameters.
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Affiliation(s)
- Suzanne Staggs
- Department of Physics, Princeton University, Princeton NJ, United States of America
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15
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Lopez-Eiguren A, Urrestilla J, Achúcarro A, Avgoustidis A, Martins C. Evolution of semilocal string networks. II. Velocity estimators. Int J Clin Exp Med 2017. [DOI: 10.1103/physrevd.96.023526] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Romano JD, Cornish NJ. Detection methods for stochastic gravitational-wave backgrounds: a unified treatment. LIVING REVIEWS IN RELATIVITY 2017; 20:2. [PMID: 28690422 PMCID: PMC5478100 DOI: 10.1007/s41114-017-0004-1] [Citation(s) in RCA: 25] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 08/23/2016] [Accepted: 01/17/2017] [Indexed: 06/07/2023]
Abstract
We review detection methods that are currently in use or have been proposed to search for a stochastic background of gravitational radiation. We consider both Bayesian and frequentist searches using ground-based and space-based laser interferometers, spacecraft Doppler tracking, and pulsar timing arrays; and we allow for anisotropy, non-Gaussianity, and non-standard polarization states. Our focus is on relevant data analysis issues, and not on the particular astrophysical or early Universe sources that might give rise to such backgrounds. We provide a unified treatment of these searches at the level of detector response functions, detection sensitivity curves, and, more generally, at the level of the likelihood function, since the choice of signal and noise models and prior probability distributions are actually what define the search. Pedagogical examples are given whenever possible to compare and contrast different approaches. We have tried to make the article as self-contained and comprehensive as possible, targeting graduate students and new researchers looking to enter this field.
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Affiliation(s)
- Joseph D. Romano
- Department of Physics and Astronomy, University of Texas Rio Grande Valley, Brownsville, TX 78520 USA
| | - Neil. J. Cornish
- Department of Physics, Montana State University, Bozeman, MT 59717 USA
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Bicep2/KECK ARRAYVIII: MEASUREMENT OF GRAVITATIONAL LENSING FROM LARGE-SCALEB-MODE POLARIZATION. ACTA ACUST UNITED AC 2016. [DOI: 10.3847/1538-4357/833/2/228] [Citation(s) in RCA: 67] [Impact Index Per Article: 8.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Koh S, Lee BH, Tumurtushaa G. Primordial gravitational waves from the space-condensate inflation model. Int J Clin Exp Med 2016. [DOI: 10.1103/physrevd.93.083518] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Cooray A. Extragalactic background light measurements and applications. ROYAL SOCIETY OPEN SCIENCE 2016; 3:150555. [PMID: 27069645 PMCID: PMC4821256 DOI: 10.1098/rsos.150555] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 10/14/2015] [Accepted: 02/08/2016] [Indexed: 06/05/2023]
Abstract
This review covers the measurements related to the extragalactic background light intensity from γ-rays to radio in the electromagnetic spectrum over 20 decades in wavelength. The cosmic microwave background (CMB) remains the best measured spectrum with an accuracy better than 1%. The measurements related to the cosmic optical background (COB), centred at 1 μm, are impacted by the large zodiacal light associated with interplanetary dust in the inner Solar System. The best measurements of COB come from an indirect technique involving γ-ray spectra of bright blazars with an absorption feature resulting from pair-production off of COB photons. The cosmic infrared background (CIB) peaking at around 100 μm established an energetically important background with an intensity comparable to the optical background. This discovery paved the way for large aperture far-infrared and sub-millimetre observations resulting in the discovery of dusty, starbursting galaxies. Their role in galaxy formation and evolution remains an active area of research in modern-day astrophysics. The extreme UV (EUV) background remains mostly unexplored and will be a challenge to measure due to the high Galactic background and absorption of extragalactic photons by the intergalactic medium at these EUV/soft X-ray energies. We also summarize our understanding of the spatial anisotropies and angular power spectra of intensity fluctuations. We motivate a precise direct measurement of the COB between 0.1 and 5 μm using a small aperture telescope observing either from the outer Solar System, at distances of 5 AU or more, or out of the ecliptic plane. Other future applications include improving our understanding of the background at TeV energies and spectral distortions of CMB and CIB.
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Affiliation(s)
- Asantha Cooray
- Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA
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Niemack MD. Designs for a large-aperture telescope to map the CMB 10× faster. APPLIED OPTICS 2016; 55:1688-1696. [PMID: 26974631 DOI: 10.1364/ao.55.001688] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/05/2023]
Abstract
Current large-aperture cosmic microwave background (CMB) telescopes have nearly maximized the number of detectors that can be illuminated while maintaining diffraction-limited image quality. The polarization-sensitive detector arrays being deployed in these telescopes in the next few years will have roughly 10⁴ detectors. Increasing the mapping speed of future instruments by at least an order of magnitude is important to enable precise probes of the inflationary paradigm in the first fraction of a second after the big bang and provide strong constraints on cosmological parameters. The CMB community has begun planning a next generation "Stage IV" CMB project that will be comprised of multiple telescopes with between 10⁵-10⁶ detectors to pursue these goals. This paper introduces the new crossed Dragone telescope and receiver optics designs that increase the usable diffraction-limited field-of-view, and therefore the mapping speed, by an order of magnitude compared to the upcoming generation of large-aperture instruments. Polarization systematics and engineering considerations are presented, including a preliminary receiver model to demonstrate that these designs will enable high efficiency illumination of >10⁵ detectors in a next generation CMB telescope.
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Ferté A, Peloton J, Grain J, Stompor R. Detecting the tensor-to-scalar ratio with the pure pseudospectrum reconstruction ofB-mode. Int J Clin Exp Med 2015. [DOI: 10.1103/physrevd.92.083510] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Ade PAR, Ahmed Z, Aikin RW, Alexander KD, Barkats D, Benton SJ, Bischoff CA, Bock JJ, Brevik JA, Buder I, Bullock E, Buza V, Connors J, Crill BP, Dowell CD, Dvorkin C, Duband L, Filippini JP, Fliescher S, Golwala SR, Halpern M, Harrison S, Hasselfield M, Hildebrandt SR, Hilton GC, Hristov VV, Hui H, Irwin KD, Karkare KS, Kaufman JP, Keating BG, Kefeli S, Kernasovskiy SA, Kovac JM, Kuo CL, Leitch EM, Lueker M, Mason P, Megerian KG, Netterfield CB, Nguyen HT, O’Brient R, Ogburn IV RW, Orlando A, Pryke C, Reintsema CD, Richter S, Schwarz R, Sheehy CD, Staniszewski ZK, Sudiwala RV, Teply GP, Thompson KL, Tolan JE, Turner AD, Vieregg AG, Weber AC, Willmert J, Wong CL, Yoon KW. BICEP2/KECK ARRAY V: MEASUREMENTS OFB-MODE POLARIZATION AT DEGREE ANGULAR SCALES AND 150 GHz BY THE KECK ARRAY. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/811/2/126] [Citation(s) in RCA: 71] [Impact Index Per Article: 7.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/11/2022]
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Story KT, Hanson D, Ade PAR, Aird KA, Austermann JE, J. A. Beall, Bender AN, Benson BA, Bleem LE, Carlstrom JE, Chang CL, Chiang HC, Cho HM, Citron R, Crawford TM, Crites AT, Haan TD, Dobbs MA, Everett W, Gallicchio J, Gao J, George EM, Gilbert A, Halverson NW, Harrington N, Henning JW, Hilton GC, Holder GP, Holzapfel WL, Hoover S, Hou Z, Hrubes JD, Huang N, Hubmayr J, Irwin KD, Keisler R, Knox L, Lee AT, Leitch EM, Li D, Liang C, Luong-Van D, McMahon JJ, Mehl J, Meyer SS, Mocanu L, Montroy TE, Natoli T, Nibarger JP, Novosad V, Padin S, Pryke C, Reichardt CL, Ruhl JE, Saliwanchik BR, Sayre JT, Schaffer KK, Smecher G, Stark AA, Tucker C, Vanderlinde K, Vieira JD, Wang G, Whitehorn N, Yefremenko V, Zahn O. A MEASUREMENT OF THE COSMIC MICROWAVE BACKGROUND GRAVITATIONAL LENSING POTENTIAL FROM 100 SQUARE DEGREES OF SPTPOL DATA. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/810/1/50] [Citation(s) in RCA: 82] [Impact Index Per Article: 9.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/11/2022]
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Engelen AV, Sherwin BD, Sehgal N, Addison GE, Allison R, Battaglia N, Bernardis FD, Bond JR, Calabrese E, Coughlin K, Crichton D, Datta R, Devlin MJ, Dunkley J, Dünner R, Gallardo P, Grace E, Gralla M, Hajian A, Hasselfield M, Henderson S, Hill JC, Hilton M, Hincks AD, Hlozek R, Huffenberger KM, Hughes JP, Koopman B, Kosowsky A, Louis T, Lungu M, Madhavacheril M, Maurin L, McMahon J, Moodley K, Munson C, Naess S, Nati F, Newburgh L, Niemack MD, Nolta MR, Page LA, Pappas C, Partridge B, Schmitt BL, Sievers JL, Simon S, Spergel DN, Staggs ST, Switzer ER, Ward JT, Wollack EJ. THE ATACAMA COSMOLOGY TELESCOPE: LENSING OF CMB TEMPERATURE AND POLARIZATION DERIVED FROM COSMIC INFRARED BACKGROUND CROSS-CORRELATION. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/808/1/7] [Citation(s) in RCA: 61] [Impact Index Per Article: 6.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/11/2022]
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Keisler R, Hoover S, Harrington N, Henning JW, Ade PAR, Aird KA, Austermann JE, Beall JA, Bender AN, Benson BA, Bleem LE, Carlstrom JE, Chang CL, Chiang HC, Cho HM, Citron R, Crawford TM, Crites AT, de Haan T, Dobbs MA, Everett W, Gallicchio J, Gao J, George EM, Gilbert A, Halverson NW, Hanson D, Hilton GC, Holder GP, Holzapfel WL, Hou Z, Hrubes JD, Huang N, Hubmayr J, Irwin KD, Knox L, Lee AT, Leitch EM, Li D, Luong-Van D, Marrone DP, McMahon JJ, Mehl J, Meyer SS, Mocanu L, Natoli T, Nibarger JP, Novosad V, Padin S, Pryke C, Reichardt CL, Ruhl JE, Saliwanchik BR, Sayre JT, Schaffer KK, Shirokoff E, Smecher G, Stark AA, Story KT, Tucker C, Vanderlinde K, Vieira JD, Wang G, Whitehorn N, Yefremenko V, Zahn O. MEASUREMENTS OF SUB-DEGREEB-MODE POLARIZATION IN THE COSMIC MICROWAVE BACKGROUND FROM 100 SQUARE DEGREES OF SPTPOL DATA. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/807/2/151] [Citation(s) in RCA: 111] [Impact Index Per Article: 12.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
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Bielefeld J, Caldwell RR. Cosmological consequences of classical flavor-space locked gauge field radiation. Int J Clin Exp Med 2015. [DOI: 10.1103/physrevd.91.124004] [Citation(s) in RCA: 10] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Crites AT, Henning JW, Ade PAR, Aird KA, Austermann JE, Beall JA, Bender AN, Benson BA, Bleem LE, Carlstrom JE, Chang CL, Chiang HC, Cho HM, Citron R, Crawford TM, Haan TD, Dobbs MA, Everett W, Gallicchio J, Gao J, George EM, Gilbert A, Halverson NW, Hanson D, Harrington N, Hilton GC, Holder GP, Holzapfel WL, Hoover S, Hou Z, Hrubes JD, Huang N, Hubmayr J, Irwin KD, Keisler R, Knox L, Lee AT, Leitch EM, Li D, Liang C, Luong-Van D, McMahon JJ, Mehl J, Meyer SS, Mocanu L, Montroy TE, Natoli T, Nibarger JP, Novosad V, Padin S, Pryke C, Reichardt CL, Ruhl JE, Saliwanchik BR, Sayre JT, Schaffer KK, Smecher G, Stark AA, Story KT, Tucker C, Vanderlinde K, Vieira JD, Wang G, Whitehorn N, Yefremenko V, Zahn O. MEASUREMENTS OF E-MODE POLARIZATION AND TEMPERATURE-E-MODE CORRELATION IN THE COSMIC MICROWAVE BACKGROUND FROM 100 SQUARE DEGREES OF SPTPOL DATA. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/805/1/36] [Citation(s) in RCA: 46] [Impact Index Per Article: 5.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/11/2022]
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Madhavacheril M, Sehgal N, Allison R, Battaglia N, Bond JR, Calabrese E, Caligiuri J, Coughlin K, Crichton D, Datta R, Devlin MJ, Dunkley J, Dünner R, Fogarty K, Grace E, Hajian A, Hasselfield M, Hill JC, Hilton M, Hincks AD, Hlozek R, Hughes JP, Kosowsky A, Louis T, Lungu M, McMahon J, Moodley K, Munson C, Naess S, Nati F, Newburgh L, Niemack MD, Page LA, Partridge B, Schmitt B, Sherwin BD, Sievers J, Spergel DN, Staggs ST, Thornton R, Van Engelen A, Ward JT, Wollack EJ. Evidence of lensing of the cosmic microwave background by dark matter halos. PHYSICAL REVIEW LETTERS 2015; 114:151302. [PMID: 25933304 DOI: 10.1103/physrevlett.114.151302] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/30/2014] [Indexed: 06/04/2023]
Abstract
We present evidence of the gravitational lensing of the cosmic microwave background by 10(13) solar mass dark matter halos. Lensing convergence maps from the Atacama Cosmology Telescope Polarimeter (ACTPol) are stacked at the positions of around 12 000 optically selected CMASS galaxies from the SDSS-III/BOSS survey. The mean lensing signal is consistent with simulated dark matter halo profiles and is favored over a null signal at 3.2σ significance. This result demonstrates the potential of microwave background lensing to probe the dark matter distribution in galaxy group and galaxy cluster halos.
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Affiliation(s)
- Mathew Madhavacheril
- Physics and Astronomy Department, Stony Brook University, Stony Brook, New York 11794, USA
| | - Neelima Sehgal
- Physics and Astronomy Department, Stony Brook University, Stony Brook, New York 11794, USA
| | - Rupert Allison
- Sub-Department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, United Kingdom
| | - Nick Battaglia
- McWilliams Center for Cosmology, Carnegie Mellon University, Department of Physics, 5000 Forbes Ave., Pittsburgh, Pennsylvania 15213, USA
| | - J Richard Bond
- Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario, Canada M5S 3H8
| | - Erminia Calabrese
- Sub-Department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, United Kingdom
| | | | - Kevin Coughlin
- Department of Physics, University of Michigan, Ann Arbor, Michigan 48103, USA
| | - Devin Crichton
- Department of Physics and Astronomy, The Johns Hopkins University, 3400 N. Charles St., Baltimore, Maryland 21218-2686, USA
| | - Rahul Datta
- Department of Physics, University of Michigan, Ann Arbor, Michigan 48103, USA
| | - Mark J Devlin
- Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, Pennsylvania 19104, USA
| | - Joanna Dunkley
- Sub-Department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, United Kingdom
| | - Rolando Dünner
- Departamento de Astronomía y Astrofísica, Pontificía Universidad Católica, Casilla 306, Santiago 22, Chile
| | - Kevin Fogarty
- Department of Physics and Astronomy, The Johns Hopkins University, 3400 N. Charles St., Baltimore, Maryland 21218-2686, USA
| | - Emily Grace
- Joseph Henry Laboratories of Physics, Jadwin Hall, Princeton University, Princeton, New Jersey 08544, USA
| | - Amir Hajian
- Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario, Canada M5S 3H8
| | - Matthew Hasselfield
- Department of Astrophysical Sciences, Peyton Hall, Princeton University, Princeton, New Jersey 08544, USA
| | - J Colin Hill
- Department of Astronomy, Pupin Hall, Columbia University, New York, New York 10027, USA
| | - Matt Hilton
- Astrophysics and Cosmology Research Unit, School of Mathematics, Statistics and Computer Science, University of KwaZulu-Natal, Durban 4041, South Africa
| | - Adam D Hincks
- Department of Physics and Astronomy, University of British Columbia, Vancouver, British Columbia, Canada V6T 1Z4
| | - Renée Hlozek
- Department of Astrophysical Sciences, Peyton Hall, Princeton University, Princeton, New Jersey 08544, USA
| | - John P Hughes
- Department of Physics and Astronomy, Rutgers, The State University of New Jersey, Piscataway, New Jersey 08854-8019, USA
| | - Arthur Kosowsky
- Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, Pennsylvania 15260, USA
| | - Thibaut Louis
- Sub-Department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, United Kingdom
| | - Marius Lungu
- Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, Pennsylvania 19104, USA
| | - Jeff McMahon
- Department of Physics, University of Michigan, Ann Arbor, Michigan 48103, USA
| | - Kavilan Moodley
- Astrophysics and Cosmology Research Unit, School of Mathematics, Statistics and Computer Science, University of KwaZulu-Natal, Durban 4041, South Africa
| | - Charles Munson
- Department of Physics, University of Michigan, Ann Arbor, Michigan 48103, USA
| | - Sigurd Naess
- Sub-Department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, United Kingdom
| | - Federico Nati
- Dipartimento di Fisica, Università La Sapienza, P. le A. Moro 2, 00185 Roma, Italy
| | - Laura Newburgh
- Dunlap Institute, University of Toronto, 50 St. George St., Toronto, Ontario, Canada M5S 3H4
| | - Michael D Niemack
- Department of Physics, Cornell University, Ithaca, New York 14853, USA
| | - Lyman A Page
- Joseph Henry Laboratories of Physics, Jadwin Hall, Princeton University, Princeton, New Jersey 08544, USA
| | - Bruce Partridge
- Department of Physics and Astronomy, Haverford College, Haverford, Pennsylvania 19041, USA
| | - Benjamin Schmitt
- Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, Pennsylvania 19104, USA
| | - Blake D Sherwin
- Berkeley Center for Cosmological Physics, LBL and Department of Physics, University of California, Berkeley, California 94720, USA
| | - Jon Sievers
- Astrophysics and Cosmology Research Unit, School of Chemistry and Physics, University of KwaZulu-Natal, Durban 4041, South Africa
- National Institute for Theoretical Physics (NITheP), University of KwaZulu-Natal, Private Bag X54001, Durban 4000, South Africa
| | - David N Spergel
- Department of Astrophysical Sciences, Peyton Hall, Princeton University, Princeton, New Jersey 08544, USA
| | - Suzanne T Staggs
- Joseph Henry Laboratories of Physics, Jadwin Hall, Princeton University, Princeton, New Jersey 08544, USA
| | - Robert Thornton
- Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, Pennsylvania 19104, USA
- Department of Physics, West Chester University of Pennsylvania, West Chester, Pennsylvania 19383, USA
| | - Alexander Van Engelen
- Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario, Canada M5S 3H8
| | - Jonathan T Ward
- Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, Pennsylvania 19104, USA
| | - Edward J Wollack
- NASA/Goddard Space Flight Center, Greenbelt, Maryland 20771, USA
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Bianchini F, Bielewicz P, Lapi A, Gonzalez-Nuevo J, Baccigalupi C, de Zotti G, Danese L, Bourne N, Cooray A, Dunne L, Dye S, Eales S, Ivison R, Maddox S, Negrello M, Scott D, Smith MWL, Valiante E. CROSS-CORRELATION BETWEEN THE CMB LENSING POTENTIAL MEASURED BYPLANCKAND HIGH-zSUBMILLIMETER GALAXIES DETECTED BY THEHERSCHEL-ATLAS SURVEY. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/802/1/64] [Citation(s) in RCA: 52] [Impact Index Per Article: 5.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/11/2022]
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Ade PAR, Aghanim N, Ahmed Z, Aikin RW, Alexander KD, Arnaud M, Aumont J, Baccigalupi C, Banday AJ, Barkats D, Barreiro RB, Bartlett JG, Bartolo N, Battaner E, Benabed K, Benoît A, Benoit-Lévy A, Benton SJ, Bernard JP, Bersanelli M, Bielewicz P, Bischoff CA, Bock JJ, Bonaldi A, Bonavera L, Bond JR, Borrill J, Bouchet FR, Boulanger F, Brevik JA, Bucher M, Buder I, Bullock E, Burigana C, Butler RC, Buza V, Calabrese E, Cardoso JF, Catalano A, Challinor A, Chary RR, Chiang HC, Christensen PR, Colombo LPL, Combet C, Connors J, Couchot F, Coulais A, Crill BP, Curto A, Cuttaia F, Danese L, Davies RD, Davis RJ, de Bernardis P, de Rosa A, de Zotti G, Delabrouille J, Delouis JM, Désert FX, Dickinson C, Diego JM, Dole H, Donzelli S, Doré O, Douspis M, Dowell CD, Duband L, Ducout A, Dunkley J, Dupac X, Dvorkin C, Efstathiou G, Elsner F, Enßlin TA, Eriksen HK, Falgarone E, Filippini JP, Finelli F, Fliescher S, Forni O, Frailis M, Fraisse AA, Franceschi E, Frejsel A, Galeotta S, Galli S, Ganga K, Ghosh T, Giard M, Gjerløw E, Golwala SR, González-Nuevo J, Górski KM, Gratton S, Gregorio A, Gruppuso A, Gudmundsson JE, Halpern M, Hansen FK, Hanson D, Harrison DL, Hasselfield M, Helou G, Henrot-Versillé S, Herranz D, Hildebrandt SR, Hilton GC, Hivon E, Hobson M, Holmes WA, Hovest W, Hristov VV, Huffenberger KM, Hui H, Hurier G, Irwin KD, Jaffe AH, Jaffe TR, Jewell J, Jones WC, Juvela M, Karakci A, Karkare KS, Kaufman JP, Keating BG, Kefeli S, Keihänen E, Kernasovskiy SA, Keskitalo R, Kisner TS, Kneissl R, Knoche J, Knox L, Kovac JM, Krachmalnicoff N, Kunz M, Kuo CL, Kurki-Suonio H, Lagache G, Lähteenmäki A, Lamarre JM, Lasenby A, Lattanzi M, Lawrence CR, Leitch EM, Leonardi R, Levrier F, Lewis A, Liguori M, Lilje PB, Linden-Vørnle M, López-Caniego M, Lubin PM, Lueker M, Macías-Pérez JF, Maffei B, Maino D, Mandolesi N, Mangilli A, Maris M, Martin PG, Martínez-González E, Masi S, Mason P, Matarrese S, Megerian KG, Meinhold PR, Melchiorri A, Mendes L, Mennella A, Migliaccio M, Mitra S, Miville-Deschênes MA, Moneti A, Montier L, Morgante G, Mortlock D, Moss A, Munshi D, Murphy JA, Naselsky P, Nati F, Natoli P, Netterfield CB, Nguyen HT, Nørgaard-Nielsen HU, Noviello F, Novikov D, Novikov I, O'Brient R, Ogburn RW, Orlando A, Pagano L, Pajot F, Paladini R, Paoletti D, Partridge B, Pasian F, Patanchon G, Pearson TJ, Perdereau O, Perotto L, Pettorino V, Piacentini F, Piat M, Pietrobon D, Plaszczynski S, Pointecouteau E, Polenta G, Ponthieu N, Pratt GW, Prunet S, Pryke C, Puget JL, Rachen JP, Reach WT, 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 JA, Rusholme B, Sandri M, Santos D, Savelainen M, Savini G, Schwarz R, Scott D, Seiffert MD, Sheehy CD, Spencer LD, Staniszewski ZK, Stolyarov V, Sudiwala R, Sunyaev R, Sutton D, Suur-Uski AS, Sygnet JF, Tauber JA, Teply GP, Terenzi L, Thompson KL, Toffolatti L, Tolan JE, Tomasi M, Tristram M, Tucci M, Turner AD, Valenziano L, Valiviita J, Van Tent B, Vibert L, Vielva P, Vieregg AG, Villa F, Wade LA, Wandelt BD, Watson R, Weber AC, Wehus IK, White M, White SDM, Willmert J, Wong CL, Yoon KW, Yvon D, Zacchei A, Zonca A. Joint analysis of BICEP2/keck array and Planck Data. PHYSICAL REVIEW LETTERS 2015; 114:101301. [PMID: 25815919 DOI: 10.1103/physrevlett.114.101301] [Citation(s) in RCA: 52] [Impact Index Per Article: 5.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/21/2015] [Indexed: 06/04/2023]
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 deg^{2} 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 r_{0.05}<0.12 at 95% confidence. Marginalizing over dust and r, lensing B modes are detected at 7.0σ significance.
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Affiliation(s)
- P A R Ade
- School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff, CF24 3AA, United Kingdom
| | - N Aghanim
- Institut d'Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France
| | - Z Ahmed
- Department of Physics, Stanford University, Stanford, California 94305, USA
| | - R W Aikin
- California Institute of Technology, Pasadena, California, USA
| | - K D Alexander
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA
| | - M Arnaud
- Laboratoire AIM, IRFU/Service d'Astrophysique-CEA/DSM-CNRS-Université Paris Diderot, Bâtiment 709, CEA-Saclay, F-91191 Gif-sur-Yvette Cedex, France
| | - J Aumont
- Institut d'Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France
| | - C Baccigalupi
- SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy
| | - A J Banday
- Université de Toulouse, UPS-OMP, IRAP, F-31028 Toulouse cedex 4, France
- CNRS, IRAP, 9 Avenue colonel Roche, BP 44346, F-31028 Toulouse cedex 4, France
| | - D Barkats
- Joint ALMA Observatory, Vitacura, Santiago, Chile
| | - R B Barreiro
- Instituto de Física de Cantabria (CSIC-Universidad de Cantabria), Avenida de los Castros s/n, Santander, Spain
| | - J G Bartlett
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/lrfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | - N Bartolo
- Dipartimento di Fisica e Astronomia G. Galilei, Università degli Studi di Padova, via Marzolo 8, 35131 Padova, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Padova, via Marzolo 8, I-35131 Padova, Italy
| | - E Battaner
- University of Granada, Departamento de Física Teórica y del Cosmos, Facultad de Ciencias, Granada, Spain
- University of Granada, Instituto Carlos I de Física Teórica y Computacional, Granada, Spain
| | - K Benabed
- Institut d'Astrophysique de Paris, CNRS (UMR7095), 98 bis Boulevard Arago, F-75014, Paris, France
- UPMC Université de Paris 06, UMR7095, 98 bis Boulevard Arago, F-75014, Paris, France
| | - A Benoît
- Institut Néel, CNRS, Université Joseph Fourier Grenoble I, 25 rue des Martyrs, Grenoble, France
| | - A Benoit-Lévy
- Institut d'Astrophysique de Paris, CNRS (UMR7095), 98 bis Boulevard Arago, F-75014, Paris, France
- UPMC Université de Paris 06, UMR7095, 98 bis Boulevard Arago, F-75014, Paris, France
- Department of Physics and Astronomy, University College London, London WC1E 6BT, United Kingdom
| | - S J Benton
- Department of Physics, University of Toronto, Toronto, Ontario, M5S 1A7, Canada
| | - J-P Bernard
- Université de Toulouse, UPS-OMP, IRAP, F-31028 Toulouse cedex 4, France
- CNRS, IRAP, 9 Avenue colonel Roche, BP 44346, F-31028 Toulouse cedex 4, France
| | - M Bersanelli
- Dipartimento di Fisica, Università degli Studi di Milano, Via Celoria, 16, Milano, Italy
- INAF/IASF Milano, Via E. Bassini 15, Milano, Italy
| | - P Bielewicz
- SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy
- Université de Toulouse, UPS-OMP, IRAP, F-31028 Toulouse cedex 4, France
- CNRS, IRAP, 9 Avenue colonel Roche, BP 44346, F-31028 Toulouse cedex 4, France
| | - C A Bischoff
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA
| | - J J Bock
- California Institute of Technology, Pasadena, California, USA
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | - A Bonaldi
- Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, United Kingdom
| | - L Bonavera
- Instituto de Física de Cantabria (CSIC-Universidad de Cantabria), Avenida de los Castros s/n, Santander, Spain
| | - J R Bond
- CITA, University of Toronto, 60 St. George Street, Toronto, Ontario M5S 3H8, Canada
| | - J Borrill
- Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, California, USA
- Space Sciences Laboratory, University of California, Berkeley, California, USA
| | - F R Bouchet
- Institut d'Astrophysique de Paris, CNRS (UMR7095), 98 bis Boulevard Arago, F-75014, Paris, France
- Sorbonne Université-UPMC, UMR7095, Institut d'Astrophysique de Paris, 98 bis Boulevard Arago, F-75014, Paris, France
| | - F Boulanger
- Institut d'Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France
| | - J A Brevik
- California Institute of Technology, Pasadena, California, USA
| | - M Bucher
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/lrfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
| | - I Buder
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA
| | - E Bullock
- Minnesota Institute for Astrophysics, University of Minnesota, Minneapolis, Minnesota 55455, USA
| | - C Burigana
- INAF/IASF Bologna, Via Gobetti 101, Bologna, Italy
- Dipartimento di Fisica e Scienze della Terra, Università di Ferrara, Via Saragat 1, 44122 Ferrara, Italy
- INFN, Sezione di Bologna, Via Irnerio 46, I-40126, Bologna, Italy
| | - R C Butler
- INAF/IASF Bologna, Via Gobetti 101, Bologna, Italy
| | - V Buza
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA
| | - E Calabrese
- Sub-Department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, United Kingdom
| | - J-F Cardoso
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/lrfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
- Institut d'Astrophysique de Paris, CNRS (UMR7095), 98 bis Boulevard Arago, F-75014, Paris, France
- Laboratoire Traitement et Communication de l'Information, CNRS (UMR 5141) and Télécom ParisTech, 46 rue Barrault F-75634 Paris Cedex 13, France
| | - A Catalano
- Laboratoire de Physique Subatomique et Cosmologie, Université Grenoble-Alpes, CNRS/IN2P3, 53, rue des Martyrs, 38026 Grenoble Cedex, France
- LERMA, CNRS, Observatoire de Paris, 61 Avenue de l'Observatoire, Paris, France
| | - A Challinor
- Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, United Kingdom
- Kavli Institute for Cosmology Cambridge, Madingley Road, Cambridge, CB3 0HA, United Kingdom
- Centre for Theoretical Cosmology, DAMTP, University of Cambridge, Wilberforce Road, Cambridge CB3 0WA, United Kingdom
| | - R-R Chary
- Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, California 91125, USA
| | - H C Chiang
- Department of Physics, Princeton University, Princeton, New Jersey, USA
- Astrophysics & Cosmology Research Unit, School of Mathematics, Statistics & Computer Science, University of KwaZulu-Natal, Westville Campus, Private Bag X54001, Durban 4000, South Africa
| | - P R Christensen
- Niels Bohr Institute, Blegdamsvej 17, Copenhagen, Denmark
- Discovery Center, Niels Bohr Institute, Blegdamsvej 17, Copenhagen, Denmark
| | - L P L Colombo
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
- Department of Physics and Astronomy, Dana and David Dornsife College of Letter, Arts and Sciences, University of Southern California, Los Angeles, California 90089, USA
| | - C Combet
- Laboratoire de Physique Subatomique et Cosmologie, Université Grenoble-Alpes, CNRS/IN2P3, 53, rue des Martyrs, 38026 Grenoble Cedex, France
| | - J Connors
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA
| | - F Couchot
- LAL, Université Paris-Sud, CNRS/IN2P3, Orsay, France
| | - A Coulais
- LERMA, CNRS, Observatoire de Paris, 61 Avenue de l'Observatoire, Paris, France
| | - B P Crill
- California Institute of Technology, Pasadena, California, USA
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | - A Curto
- Instituto de Física de Cantabria (CSIC-Universidad de Cantabria), Avenida de los Castros s/n, Santander, Spain
- Astrophysics Group, Cavendish Laboratory, University of Cambridge, J J Thomson Avenue, Cambridge CB3 0HE, United Kingdom
| | - F Cuttaia
- INAF/IASF Bologna, Via Gobetti 101, Bologna, Italy
| | - L Danese
- SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy
| | - R D Davies
- Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, United Kingdom
| | - R J Davis
- Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, United Kingdom
| | - P de Bernardis
- Dipartimento di Fisica, Università La Sapienza, Piazzale Aldo Moro 2, Roma, Italy
| | - A de Rosa
- INAF/IASF Bologna, Via Gobetti 101, Bologna, Italy
| | - G de Zotti
- SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy
- INAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padova, Italy
| | - J Delabrouille
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/lrfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
| | - J-M Delouis
- Institut d'Astrophysique de Paris, CNRS (UMR7095), 98 bis Boulevard Arago, F-75014, Paris, France
- UPMC Université de Paris 06, UMR7095, 98 bis Boulevard Arago, F-75014, Paris, France
| | - F-X Désert
- IPAG: Institut de Planétologie et d'Astrophysique de Grenoble, Université Grenoble Alpes, IPAG, F-38000 Grenoble, France, CNRS, IPAG, F-38000 Grenoble, France
| | - C Dickinson
- Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, United Kingdom
| | - J M Diego
- Instituto de Física de Cantabria (CSIC-Universidad de Cantabria), Avenida de los Castros s/n, Santander, Spain
| | - H Dole
- Institut d'Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France
- Institut Universitaire de France, 103, bd Saint-Michel, 75005, Paris, France
| | - S Donzelli
- INAF/IASF Milano, Via E. Bassini 15, Milano, Italy
| | - O Doré
- California Institute of Technology, Pasadena, California, USA
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | - M Douspis
- Institut d'Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France
| | - C D Dowell
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | - L Duband
- Service des Basses Températures, Commissariat à l'Energie Atomique, 38054 Grenoble, France
| | - A Ducout
- Institut d'Astrophysique de Paris, CNRS (UMR7095), 98 bis Boulevard Arago, F-75014, Paris, France
- Imperial College London, Astrophysics group, Blackett Laboratory, Prince Consort Road, London, SW7 2AZ, United Kingdom
| | - J Dunkley
- Sub-Department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, United Kingdom
| | - X Dupac
- European Space Agency, ESAC, Planck Science Office, Camino bajo del Castillo, s/n, Urbanización Villafranca del Castillo, Villanueva de la Cañada, Madrid, Spain
| | - C Dvorkin
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA
| | - G Efstathiou
- Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, United Kingdom
| | - F Elsner
- Institut d'Astrophysique de Paris, CNRS (UMR7095), 98 bis Boulevard Arago, F-75014, Paris, France
- UPMC Université de Paris 06, UMR7095, 98 bis Boulevard Arago, F-75014, Paris, France
- Department of Physics and Astronomy, University College London, London WC1E 6BT, United Kingdom
| | - T A Enßlin
- Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, 85741 Garching, Germany
| | - H K Eriksen
- Institute of Theoretical Astrophysics, University of Oslo, Blindern, Oslo, Norway
| | - E Falgarone
- LERMA, CNRS, Observatoire de Paris, 61 Avenue de l'Observatoire, Paris, France
| | - J P Filippini
- California Institute of Technology, Pasadena, California, USA
- Department of Physics, University of Illinois at Urbana-Champaign, 1110 West Green Street, Urbana, Illinois, USA
| | - F Finelli
- INAF/IASF Bologna, Via Gobetti 101, Bologna, Italy
- INFN, Sezione di Bologna, Via Irnerio 46, I-40126, Bologna, Italy
| | - S Fliescher
- School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455, USA
| | - O Forni
- Université de Toulouse, UPS-OMP, IRAP, F-31028 Toulouse cedex 4, France
- CNRS, IRAP, 9 Avenue colonel Roche, BP 44346, F-31028 Toulouse cedex 4, France
| | - M Frailis
- INAF-Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, Trieste, Italy
| | - A A Fraisse
- Department of Physics, Princeton University, Princeton, New Jersey, USA
| | - E Franceschi
- INAF/IASF Bologna, Via Gobetti 101, Bologna, Italy
| | - A Frejsel
- Niels Bohr Institute, Blegdamsvej 17, Copenhagen, Denmark
| | - S Galeotta
- INAF-Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, Trieste, Italy
| | - S Galli
- Institut d'Astrophysique de Paris, CNRS (UMR7095), 98 bis Boulevard Arago, F-75014, Paris, France
| | - K Ganga
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/lrfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
| | - T Ghosh
- Institut d'Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France
| | - M Giard
- Université de Toulouse, UPS-OMP, IRAP, F-31028 Toulouse cedex 4, France
- CNRS, IRAP, 9 Avenue colonel Roche, BP 44346, F-31028 Toulouse cedex 4, France
| | - E Gjerløw
- Institute of Theoretical Astrophysics, University of Oslo, Blindern, Oslo, Norway
| | - S R Golwala
- California Institute of Technology, Pasadena, California, USA
| | - J González-Nuevo
- SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy
- Instituto de Física de Cantabria (CSIC-Universidad de Cantabria), Avenida de los Castros s/n, Santander, Spain
| | - K M Górski
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
- Warsaw University Observatory, Aleje Ujazdowskie 4, 00-478 Warszawa, Poland
| | - S Gratton
- Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, United Kingdom
- Kavli Institute for Cosmology Cambridge, Madingley Road, Cambridge, CB3 0HA, United Kingdom
| | - A Gregorio
- INAF-Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, Trieste, Italy
- Dipartimento di Fisica, Università degli Studi di Trieste, via Alfonso Valerio 2, Trieste, Italy
- INFN/National Institute for Nuclear Physics, Via Valerio 2, I-34127 Trieste, Italy
| | - A Gruppuso
- INAF/IASF Bologna, Via Gobetti 101, Bologna, Italy
| | - J E Gudmundsson
- Department of Physics, Princeton University, Princeton, New Jersey, USA
| | - M Halpern
- Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia, Canada
| | - F K Hansen
- Institute of Theoretical Astrophysics, University of Oslo, Blindern, Oslo, Norway
| | - D Hanson
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
- CITA, University of Toronto, 60 St. George Street, Toronto, Ontario M5S 3H8, Canada
- McGill Physics, Ernest Rutherford Physics Building, McGill University, 3600 rue University, Montréal, Quebec, H3A 2T8, Canada
| | - D L Harrison
- Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, United Kingdom
- Kavli Institute for Cosmology Cambridge, Madingley Road, Cambridge, CB3 0HA, United Kingdom
| | - M Hasselfield
- Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia, Canada
| | - G Helou
- California Institute of Technology, Pasadena, California, USA
| | | | - D Herranz
- Instituto de Física de Cantabria (CSIC-Universidad de Cantabria), Avenida de los Castros s/n, Santander, Spain
| | - S R Hildebrandt
- California Institute of Technology, Pasadena, California, USA
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | - G C Hilton
- National Institute of Standards and Technology, Boulder, Colorado 80305, USA
| | - E Hivon
- Institut d'Astrophysique de Paris, CNRS (UMR7095), 98 bis Boulevard Arago, F-75014, Paris, France
- UPMC Université de Paris 06, UMR7095, 98 bis Boulevard Arago, F-75014, Paris, France
| | - M Hobson
- Astrophysics Group, Cavendish Laboratory, University of Cambridge, J J Thomson Avenue, Cambridge CB3 0HE, United Kingdom
| | - W A Holmes
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | - W Hovest
- Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, 85741 Garching, Germany
| | - V V Hristov
- California Institute of Technology, Pasadena, California, USA
| | - K M Huffenberger
- Department of Physics, Florida State University, Keen Physics Building, 77 Chieftan Way, Tallahassee, Florida, USA
| | - H Hui
- California Institute of Technology, Pasadena, California, USA
| | - G Hurier
- Institut d'Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France
| | - K D Irwin
- Department of Physics, Stanford University, Stanford, California 94305, USA
- National Institute of Standards and Technology, Boulder, Colorado 80305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, California 94025, USA
| | - A H Jaffe
- Imperial College London, Astrophysics group, Blackett Laboratory, Prince Consort Road, London, SW7 2AZ, United Kingdom
| | - T R Jaffe
- Université de Toulouse, UPS-OMP, IRAP, F-31028 Toulouse cedex 4, France
- CNRS, IRAP, 9 Avenue colonel Roche, BP 44346, F-31028 Toulouse cedex 4, France
| | - J Jewell
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | - W C Jones
- Department of Physics, Princeton University, Princeton, New Jersey, USA
| | - M Juvela
- Department of Physics, Gustaf Hällströmin katu 2a, University of Helsinki, Helsinki, Finland
| | - A Karakci
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/lrfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
| | - K S Karkare
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA
| | - J P Kaufman
- Department of Physics, University of California at San Diego, La Jolla, California 92093, USA
| | - B G Keating
- Department of Physics, University of California at San Diego, La Jolla, California 92093, USA
| | - S Kefeli
- California Institute of Technology, Pasadena, California, USA
| | - E Keihänen
- Department of Physics, Gustaf Hällströmin katu 2a, University of Helsinki, Helsinki, Finland
| | - S A Kernasovskiy
- Department of Physics, Stanford University, Stanford, California 94305, USA
| | - R Keskitalo
- Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, California, USA
| | - T S Kisner
- Lawrence Berkeley National Laboratory, Berkeley, California, USA
| | - R Kneissl
- European Southern Observatory, ESO Vitacura, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago, Chile
- Atacama Large Millimeter/submillimeter Array, ALMA Santiago Central Offices, Alonso de Cordova 3107, Vitacura, Casilla 763 0355, Santiago, Chile
| | - J Knoche
- Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, 85741 Garching, Germany
| | - L Knox
- Department of Physics, University of California, One Shields Avenue, Davis, California, USA
| | - J M Kovac
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA
| | - N Krachmalnicoff
- Dipartimento di Fisica, Università degli Studi di Milano, Via Celoria, 16, Milano, Italy
| | - M Kunz
- Institut d'Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France
- Département de Physique Théorique, Université de Genève, 24, Quai E. Ansermet, 1211 Genève 4, Switzerland
- African Institute for Mathematical Sciences, 6-8 Melrose Road, Muizenberg, Cape Town, South Africa
| | - C L Kuo
- Department of Physics, Stanford University, Stanford, California 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, California 94025, USA
| | - H Kurki-Suonio
- Department of Physics, Gustaf Hällströmin katu 2a, University of Helsinki, Helsinki, Finland
- Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of Helsinki, Helsinki, Finland
| | - G Lagache
- Institut d'Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France
- Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France
| | - A Lähteenmäki
- Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of Helsinki, Helsinki, Finland
- Aalto University Metsähovi Radio Observatory and Department of Radio Science and Engineering, P.O. Box 13000, FI-00076 AALTO, Finland
| | - J-M Lamarre
- LERMA, CNRS, Observatoire de Paris, 61 Avenue de l'Observatoire, Paris, France
| | - A Lasenby
- Kavli Institute for Cosmology Cambridge, Madingley Road, Cambridge, CB3 0HA, United Kingdom
- Astrophysics Group, Cavendish Laboratory, University of Cambridge, J J Thomson Avenue, Cambridge CB3 0HE, United Kingdom
| | - M Lattanzi
- Dipartimento di Fisica e Scienze della Terra, Università di Ferrara, Via Saragat 1, 44122 Ferrara, Italy
| | - C R Lawrence
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | - E M Leitch
- University of Chicago, Chicago, Illinois 60637, USA
| | - R Leonardi
- European Space Agency, ESAC, Planck Science Office, Camino bajo del Castillo, s/n, Urbanización Villafranca del Castillo, Villanueva de la Cañada, Madrid, Spain
| | - F Levrier
- LERMA, CNRS, Observatoire de Paris, 61 Avenue de l'Observatoire, Paris, France
| | - A Lewis
- Department of Physics and Astronomy, University of Sussex, Brighton BN1 9QH, United Kingdom
| | - M Liguori
- Dipartimento di Fisica e Astronomia G. Galilei, Università degli Studi di Padova, via Marzolo 8, 35131 Padova, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Padova, via Marzolo 8, I-35131 Padova, Italy
| | - P B Lilje
- Institute of Theoretical Astrophysics, University of Oslo, Blindern, Oslo, Norway
| | - M Linden-Vørnle
- DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, DK-2800 Kongens Lyngby, Denmark
| | - M López-Caniego
- Instituto de Física de Cantabria (CSIC-Universidad de Cantabria), Avenida de los Castros s/n, Santander, Spain
- European Space Agency, ESAC, Planck Science Office, Camino bajo del Castillo, s/n, Urbanización Villafranca del Castillo, Villanueva de la Cañada, Madrid, Spain
| | - P M Lubin
- Department of Physics, University of California, Santa Barbara, California, USA
| | - M Lueker
- California Institute of Technology, Pasadena, California, USA
| | - J F Macías-Pérez
- Laboratoire de Physique Subatomique et Cosmologie, Université Grenoble-Alpes, CNRS/IN2P3, 53, rue des Martyrs, 38026 Grenoble Cedex, France
| | - B Maffei
- Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, United Kingdom
| | - D Maino
- Dipartimento di Fisica, Università degli Studi di Milano, Via Celoria, 16, Milano, Italy
- INAF/IASF Milano, Via E. Bassini 15, Milano, Italy
| | - N Mandolesi
- INAF/IASF Bologna, Via Gobetti 101, Bologna, Italy
- Dipartimento di Fisica e Scienze della Terra, Università di Ferrara, Via Saragat 1, 44122 Ferrara, Italy
| | - A Mangilli
- Institut d'Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France
- LAL, Université Paris-Sud, CNRS/IN2P3, Orsay, France
| | - M Maris
- INAF-Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, Trieste, Italy
| | - P G Martin
- CITA, University of Toronto, 60 St. George Street, Toronto, Ontario M5S 3H8, Canada
| | - E Martínez-González
- Instituto de Física de Cantabria (CSIC-Universidad de Cantabria), Avenida de los Castros s/n, Santander, Spain
| | - S Masi
- Dipartimento di Fisica, Università La Sapienza, Piazzale Aldo Moro 2, Roma, Italy
| | - P Mason
- California Institute of Technology, Pasadena, California, USA
| | - S Matarrese
- Dipartimento di Fisica e Astronomia G. Galilei, Università degli Studi di Padova, via Marzolo 8, 35131 Padova, Italy
- Istituto Nazionale di Fisica Nucleare, Sezione di Padova, via Marzolo 8, I-35131 Padova, Italy
- Gran Sasso Science Institute, INFN, viale F. Crispi 7, 67100L'Aquila, Italy
| | - K G Megerian
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | - P R Meinhold
- Department of Physics, University of California, Santa Barbara, California, USA
| | - A Melchiorri
- Dipartimento di Fisica, Università La Sapienza, Piazzale Aldo Moro 2, Roma, Italy
- INFN, Sezione di Roma 1, Università di Roma Sapienza, Piazzale Aldo Moro 2, 00185, Roma, Italy
| | - L Mendes
- European Space Agency, ESAC, Planck Science Office, Camino bajo del Castillo, s/n, Urbanización Villafranca del Castillo, Villanueva de la Cañada, Madrid, Spain
| | - A Mennella
- Dipartimento di Fisica, Università degli Studi di Milano, Via Celoria, 16, Milano, Italy
- INAF/IASF Milano, Via E. Bassini 15, Milano, Italy
| | - M Migliaccio
- Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, United Kingdom
- Kavli Institute for Cosmology Cambridge, Madingley Road, Cambridge, CB3 0HA, United Kingdom
| | - S Mitra
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
- IUCAA, Post Bag 4, Ganeshkhind, Pune University Campus, Pune 411 007, India
| | - M-A Miville-Deschênes
- Institut d'Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France
- CITA, University of Toronto, 60 St. George Street, Toronto, Ontario M5S 3H8, Canada
| | - A Moneti
- Institut d'Astrophysique de Paris, CNRS (UMR7095), 98 bis Boulevard Arago, F-75014, Paris, France
| | - L Montier
- Université de Toulouse, UPS-OMP, IRAP, F-31028 Toulouse cedex 4, France
- CNRS, IRAP, 9 Avenue colonel Roche, BP 44346, F-31028 Toulouse cedex 4, France
| | - G Morgante
- INAF/IASF Bologna, Via Gobetti 101, Bologna, Italy
| | - D Mortlock
- Imperial College London, Astrophysics group, Blackett Laboratory, Prince Consort Road, London, SW7 2AZ, United Kingdom
| | - A Moss
- School of Physics and Astronomy, University of Nottingham, Nottingham NG7 2RD, United Kingdom
| | - D Munshi
- School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff, CF24 3AA, United Kingdom
| | - J A Murphy
- National University of Ireland, Department of Experimental Physics, Maynooth, County Kildare, Ireland
| | - P Naselsky
- Niels Bohr Institute, Blegdamsvej 17, Copenhagen, Denmark
- Discovery Center, Niels Bohr Institute, Blegdamsvej 17, Copenhagen, Denmark
| | - F Nati
- Department of Physics, Princeton University, Princeton, New Jersey, USA
| | - P Natoli
- INAF/IASF Bologna, Via Gobetti 101, Bologna, Italy
- Dipartimento di Fisica e Scienze della Terra, Università di Ferrara, Via Saragat 1, 44122 Ferrara, Italy
- Agenzia Spaziale Italiana Science Data Center, Via del Politecnico snc, 00133, Roma, Italy
| | - C B Netterfield
- Department of Astronomy and Astrophysics, University of Toronto, 50 Saint George Street, Toronto, Ontario, Canada
| | - H T Nguyen
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | - H U Nørgaard-Nielsen
- DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, DK-2800 Kongens Lyngby, Denmark
| | - F Noviello
- Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, United Kingdom
| | - D Novikov
- Lebedev Physical Institute of the Russian Academy of Sciences, Astro Space Centre, 84/32 Profsoyuznaya st., Moscow, GSP-7, 117997, Russia
| | - I Novikov
- Niels Bohr Institute, Blegdamsvej 17, Copenhagen, Denmark
- Lebedev Physical Institute of the Russian Academy of Sciences, Astro Space Centre, 84/32 Profsoyuznaya st., Moscow, GSP-7, 117997, Russia
| | - R O'Brient
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | - R W Ogburn
- Department of Physics, Stanford University, Stanford, California 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, California 94025, USA
| | - A Orlando
- Department of Physics, University of California at San Diego, La Jolla, California 92093, USA
| | - L Pagano
- Dipartimento di Fisica, Università La Sapienza, Piazzale Aldo Moro 2, Roma, Italy
- INFN, Sezione di Roma 1, Università di Roma Sapienza, Piazzale Aldo Moro 2, 00185, Roma, Italy
| | - F Pajot
- Institut d'Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France
| | - R Paladini
- Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, California 91125, USA
| | - D Paoletti
- INAF/IASF Bologna, Via Gobetti 101, Bologna, Italy
- INFN, Sezione di Bologna, Via Irnerio 46, I-40126, Bologna, Italy
| | - B Partridge
- Haverford College Astronomy Department, 370 Lancaster Avenue, Haverford, Pennsylvania, USA
| | - F Pasian
- INAF-Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, Trieste, Italy
| | - G Patanchon
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/lrfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
| | - T J Pearson
- California Institute of Technology, Pasadena, California, USA
- Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, California 91125, USA
| | - O Perdereau
- LAL, Université Paris-Sud, CNRS/IN2P3, Orsay, France
| | - L Perotto
- Laboratoire de Physique Subatomique et Cosmologie, Université Grenoble-Alpes, CNRS/IN2P3, 53, rue des Martyrs, 38026 Grenoble Cedex, France
| | - V Pettorino
- HGSFP and University of Heidelberg, Theoretical Physics Department, Philosophenweg 16, 69120, Heidelberg, Germany
| | - F Piacentini
- Dipartimento di Fisica, Università La Sapienza, Piazzale Aldo Moro 2, Roma, Italy
| | - M Piat
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/lrfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
| | - D Pietrobon
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | | | - E Pointecouteau
- Université de Toulouse, UPS-OMP, IRAP, F-31028 Toulouse cedex 4, France
- CNRS, IRAP, 9 Avenue colonel Roche, BP 44346, F-31028 Toulouse cedex 4, France
| | - G Polenta
- Agenzia Spaziale Italiana Science Data Center, Via del Politecnico snc, 00133, Roma, Italy
- INAF-Osservatorio Astronomico di Roma, via di Frascati 33, Monte Porzio Catone, Italy
| | - N Ponthieu
- Institut d'Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France
- IPAG: Institut de Planétologie et d'Astrophysique de Grenoble, Université Grenoble Alpes, IPAG, F-38000 Grenoble, France, CNRS, IPAG, F-38000 Grenoble, France
| | - G W Pratt
- Laboratoire AIM, IRFU/Service d'Astrophysique-CEA/DSM-CNRS-Université Paris Diderot, Bâtiment 709, CEA-Saclay, F-91191 Gif-sur-Yvette Cedex, France
| | - S Prunet
- Institut d'Astrophysique de Paris, CNRS (UMR7095), 98 bis Boulevard Arago, F-75014, Paris, France
- UPMC Université de Paris 06, UMR7095, 98 bis Boulevard Arago, F-75014, Paris, France
| | - C Pryke
- Minnesota Institute for Astrophysics, University of Minnesota, Minneapolis, Minnesota 55455, USA
- School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455, USA
| | - J-L Puget
- Institut d'Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France
| | - J P Rachen
- Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, 85741 Garching, Germany
- Department of Astrophysics/IMAPP, Radboud University Nijmegen, P.O. Box 9010, 6500 GL Nijmegen, The Netherlands
| | - W T Reach
- Universities Space Research Association, Stratospheric Observatory for Infrared Astronomy, MS 232-11, Moffett Field, California 94035, USA
| | - R Rebolo
- Instituto de Astrofísica de Canarias, C/Vía Láctea s/n, La Laguna, Tenerife, Spain
- Consejo Superior de Investigaciones Científicas (CSIC), Madrid, Spain
- Departamento Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain
| | - M Reinecke
- Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, 85741 Garching, Germany
| | - M Remazeilles
- Institut d'Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/lrfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
- Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, United Kingdom
| | - C Renault
- Laboratoire de Physique Subatomique et Cosmologie, Université Grenoble-Alpes, CNRS/IN2P3, 53, rue des Martyrs, 38026 Grenoble Cedex, France
| | - A Renzi
- Dipartimento di Matematica, Università di Roma Tor Vergata, Via della Ricerca Scientifica, 1, Roma, Italy
- INFN, Sezione di Roma 2, Università di Roma Tor Vergata, Via della Ricerca Scientifica, 1, Roma, Italy
| | - S Richter
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA
| | - I Ristorcelli
- Université de Toulouse, UPS-OMP, IRAP, F-31028 Toulouse cedex 4, France
- CNRS, IRAP, 9 Avenue colonel Roche, BP 44346, F-31028 Toulouse cedex 4, France
| | - G Rocha
- California Institute of Technology, Pasadena, California, USA
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | - M Rossetti
- Dipartimento di Fisica, Università degli Studi di Milano, Via Celoria, 16, Milano, Italy
- INAF/IASF Milano, Via E. Bassini 15, Milano, Italy
| | - G Roudier
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/lrfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
- LERMA, CNRS, Observatoire de Paris, 61 Avenue de l'Observatoire, Paris, France
| | - M Rowan-Robinson
- Imperial College London, Astrophysics group, Blackett Laboratory, Prince Consort Road, London, SW7 2AZ, United Kingdom
| | - J A Rubiño-Martín
- Instituto de Astrofísica de Canarias, C/Vía Láctea s/n, La Laguna, Tenerife, Spain
- Departamento Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain
| | - B Rusholme
- Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, California 91125, USA
| | - M Sandri
- INAF/IASF Bologna, Via Gobetti 101, Bologna, Italy
| | - D Santos
- Laboratoire de Physique Subatomique et Cosmologie, Université Grenoble-Alpes, CNRS/IN2P3, 53, rue des Martyrs, 38026 Grenoble Cedex, France
| | - M Savelainen
- Department of Physics, Gustaf Hällströmin katu 2a, University of Helsinki, Helsinki, Finland
- Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of Helsinki, Helsinki, Finland
| | - G Savini
- Optical Science Laboratory, University College London, Gower Street, London, United Kingdom
| | - R Schwarz
- School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455, USA
| | - D Scott
- Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia, Canada
| | - M D Seiffert
- California Institute of Technology, Pasadena, California, USA
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | - C D Sheehy
- School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455, USA
- Kavli Institute for Cosmological Physics, University of Chicago, Chicago, Illinois 60637, USA
| | - L D Spencer
- School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff, CF24 3AA, United Kingdom
| | - Z K Staniszewski
- California Institute of Technology, Pasadena, California, USA
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | - V Stolyarov
- Kavli Institute for Cosmology Cambridge, Madingley Road, Cambridge, CB3 0HA, United Kingdom
- Astrophysics Group, Cavendish Laboratory, University of Cambridge, J J Thomson Avenue, Cambridge CB3 0HE, United Kingdom
- Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnij Arkhyz, Zelenchukskiy region, Karachai-Cherkessian Republic, 369167, Russia
| | - R Sudiwala
- School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff, CF24 3AA, United Kingdom
| | - R Sunyaev
- Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, 85741 Garching, Germany
- Space Research Institute (IKI), Russian Academy of Sciences, Profsoyuznaya Street, 84/32, Moscow, 117997, Russia
| | - D Sutton
- Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, United Kingdom
- Kavli Institute for Cosmology Cambridge, Madingley Road, Cambridge, CB3 0HA, United Kingdom
| | - A-S Suur-Uski
- Department of Physics, Gustaf Hällströmin katu 2a, University of Helsinki, Helsinki, Finland
- Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of Helsinki, Helsinki, Finland
| | - J-F Sygnet
- Institut d'Astrophysique de Paris, CNRS (UMR7095), 98 bis Boulevard Arago, F-75014, Paris, France
| | - J A Tauber
- European Space Agency, ESTEC, Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands
| | - G P Teply
- California Institute of Technology, Pasadena, California, USA
| | - L Terenzi
- INAF/IASF Bologna, Via Gobetti 101, Bologna, Italy
- Facoltà di Ingegneria, Università degli Studi e-Campus, Via Isimbardi 10, Novedrate (CO), 22060, Italy
| | - K L Thompson
- Department of Physics, Stanford University, Stanford, California 94305, USA
| | - L Toffolatti
- Instituto de Física de Cantabria (CSIC-Universidad de Cantabria), Avenida de los Castros s/n, Santander, Spain
- INAF/IASF Bologna, Via Gobetti 101, Bologna, Italy
- Departamento de Física, Universidad de Oviedo, Avda. Calvo Sotelo s/n, Oviedo, Spain
| | - J E Tolan
- Department of Physics, Stanford University, Stanford, California 94305, USA
| | - M Tomasi
- Dipartimento di Fisica, Università degli Studi di Milano, Via Celoria, 16, Milano, Italy
- INAF/IASF Milano, Via E. Bassini 15, Milano, Italy
| | - M Tristram
- LAL, Université Paris-Sud, CNRS/IN2P3, Orsay, France
| | - M Tucci
- Département de Physique Théorique, Université de Genève, 24, Quai E. Ansermet, 1211 Genève 4, Switzerland
| | - A D Turner
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
- University of Chicago, Chicago, Illinois 60637, USA
| | - L Valenziano
- INAF/IASF Bologna, Via Gobetti 101, Bologna, Italy
| | - J Valiviita
- Department of Physics, Gustaf Hällströmin katu 2a, University of Helsinki, Helsinki, Finland
- Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of Helsinki, Helsinki, Finland
| | - B Van Tent
- Laboratoire de Physique Théorique, Université Paris-Sud 11 & CNRS, Bâtiment 210, 91405 Orsay, France
| | - L Vibert
- Institut d'Astrophysique Spatiale, CNRS (UMR8617) Université Paris-Sud 11, Bâtiment 121, Orsay, France
| | - P Vielva
- Instituto de Física de Cantabria (CSIC-Universidad de Cantabria), Avenida de los Castros s/n, Santander, Spain
| | - A G Vieregg
- Kavli Institute for Cosmological Physics, University of Chicago, Chicago, Illinois 60637, USA
- Department of Physics, Enrico Fermi Institute, University of Chicago, Chicago, Illinois 60637, USA
| | - F Villa
- INAF/IASF Bologna, Via Gobetti 101, Bologna, Italy
| | - L A Wade
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | - B D Wandelt
- Institut d'Astrophysique de Paris, CNRS (UMR7095), 98 bis Boulevard Arago, F-75014, Paris, France
- UPMC Université de Paris 06, UMR7095, 98 bis Boulevard Arago, F-75014, Paris, France
- Department of Physics, University of Illinois at Urbana-Champaign, 1110 West Green Street, Urbana, Illinois, USA
| | - R Watson
- Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13 9PL, United Kingdom
| | - A C Weber
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | - I K Wehus
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, USA
| | - M White
- Department of Physics, University of California, Berkeley, California, USA
| | - S D M White
- Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, 85741 Garching, Germany
| | - J Willmert
- School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455, USA
| | - C L Wong
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA
| | - K W Yoon
- Department of Physics, Stanford University, Stanford, California 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, California 94025, USA
| | - D Yvon
- DSM/Irfu/SPP, CEA-Saclay, F-91191 Gif-sur-Yvette Cedex, France
| | - A Zacchei
- INAF-Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, Trieste, Italy
| | - A Zonca
- Department of Physics, University of California, Santa Barbara, California, USA
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Durastanti C, Fantaye Y, Hansen F, Marinucci D, Pesenson I. Simple proposal for radial 3D needlets. Int J Clin Exp Med 2014. [DOI: 10.1103/physrevd.90.103532] [Citation(s) in RCA: 14] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Kamionkowski M, Kovetz ED. Statistical diagnostics to identify galactic foregrounds in B-mode maps. PHYSICAL REVIEW LETTERS 2014; 113:191303. [PMID: 25415897 DOI: 10.1103/physrevlett.113.191303] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/20/2014] [Indexed: 06/04/2023]
Abstract
Recent developments in the search for inflationary gravitational waves in the cosmic microwave background polarization motivate the search for new diagnostics to distinguish the Galactic foreground contribution to B modes from the cosmic signal. We show that B modes from these foregrounds should exhibit a local hexadecapolar departure in power from statistical isotropy (SI). We present a simple algorithm to search for a uniform SI violation of this sort, as may arise in a sufficiently small patch of sky. We then show how to search for these effects if the orientation of the SI violation varies across the survey region, as is more likely to occur in surveys with more sky coverage. If detected, these departures from Gaussianity would indicate some level of Galactic foreground contamination in the B-mode maps. Given uncertainties about foreground properties, though, caution should be exercised in attributing a null detection to an absence of foregrounds.
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Affiliation(s)
- Marc Kamionkowski
- Department of Physics and Astronomy, Johns Hopkins University, Baltimore, Maryland 21218, USA
| | - Ely D Kovetz
- Department of Physics and Astronomy, Johns Hopkins University, Baltimore, Maryland 21218, USA and Theory Group, Department of Physics and Texas Cosmology Center, The University of Texas at Austin, Austin, Texas 78712, USA
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34
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Essinger-Hileman T, Ali A, Amiri M, Appel JW, Araujo D, Bennett CL, Boone F, Chan M, Cho HM, Chuss DT, Colazo F, Crowe E, Denis K, Dünner R, Eimer J, Gothe D, Halpern M, Harrington K, Hilton GC, Hinshaw GF, Huang C, Irwin K, Jones G, Karakla J, Kogut AJ, Larson D, Limon M, Lowry L, Marriage T, Mehrle N, Miller AD, Miller N, Moseley SH, Novak G, Reintsema C, Rostem K, Stevenson T, Towner D, U-Yen K, Wagner E, Watts D, Wollack EJ, Xu Z, Zeng L. CLASS: the cosmology large angular scale surveyor. ACTA ACUST UNITED AC 2014. [DOI: 10.1117/12.2056701] [Citation(s) in RCA: 75] [Impact Index Per Article: 7.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022]
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35
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Ade PAR, Akiba Y, Anthony AE, Arnold K, Atlas M, Barron D, Boettger D, Borrill J, Chapman S, Chinone Y, Dobbs M, Elleflot T, Errard J, Fabbian G, Feng C, Flanigan D, Gilbert A, Grainger W, Halverson NW, Hasegawa M, Hattori K, Hazumi M, Holzapfel WL, Hori Y, Howard J, Hyland P, Inoue Y, Jaehnig GC, Jaffe A, Keating B, Kermish Z, Keskitalo R, Kisner T, Le Jeune M, Lee AT, Linder E, Leitch EM, Lungu M, Matsuda F, Matsumura T, Meng X, Miller NJ, Morii H, Moyerman S, Myers MJ, Navaroli M, Nishino H, Paar H, Peloton J, Quealy E, Rebeiz G, Reichardt CL, Richards PL, Ross C, Schanning I, Schenck DE, Sherwin B, Shimizu A, Shimmin C, Shimon M, Siritanasak P, Smecher G, Spieler H, Stebor N, Steinbach B, Stompor R, Suzuki A, Takakura S, Tomaru T, Wilson B, Yadav A, Zahn O. Measurement of the cosmic microwave background polarization lensing power spectrum with the POLARBEAR experiment. PHYSICAL REVIEW LETTERS 2014; 113:021301. [PMID: 25062161 DOI: 10.1103/physrevlett.113.021301] [Citation(s) in RCA: 13] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/11/2014] [Indexed: 06/03/2023]
Abstract
Gravitational lensing due to the large-scale distribution of matter in the cosmos distorts the primordial cosmic microwave background (CMB) and thereby induces new, small-scale B-mode polarization. This signal carries detailed information about the distribution of all the gravitating matter between the observer and CMB last scattering surface. We report the first direct evidence for polarization lensing based on purely CMB information, from using the four-point correlations of even- and odd-parity E- and B-mode polarization mapped over ∼30 square degrees of the sky measured by the POLARBEAR experiment. These data were analyzed using a blind analysis framework and checked for spurious systematic contamination using null tests and simulations. Evidence for the signal of polarization lensing and lensing B modes is found at 4.2σ (stat+sys) significance. The amplitude of matter fluctuations is measured with a precision of 27%, and is found to be consistent with the Lambda cold dark matter cosmological model. This measurement demonstrates a new technique, capable of mapping all gravitating matter in the Universe, sensitive to the sum of neutrino masses, and essential for cleaning the lensing B-mode signal in searches for primordial gravitational waves.
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Affiliation(s)
- P A R Ade
- School of Physics and Astronomy, Cardiff University, Cardiff CF10 3XQ, United Kingdom
| | - Y Akiba
- The Graduate University for Advanced Studies, Hayama, Miura District, Kanagawa 240-0115, Japan
| | - A E Anthony
- Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, Colorado 80309, USA
| | - K Arnold
- Department of Physics, University of California, San Diego, La Jolla, California 92093-0424, USA
| | - M Atlas
- Department of Physics, University of California, San Diego, La Jolla, California 92093-0424, USA
| | - D Barron
- Department of Physics, University of California, San Diego, La Jolla, California 92093-0424, USA
| | - D Boettger
- Department of Physics, University of California, San Diego, La Jolla, California 92093-0424, USA
| | - J Borrill
- Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, California 92093-0424, USA and Space Sciences Laboratory, University of California, Berkeley, Berkeley, California 94720, USA
| | - S Chapman
- Department of Physics and Atmospheric Science, Dalhousie University, Halifax, Nova Scotia B3H 4R2, Canada
| | - Y Chinone
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan and Department of Physics, University of California, Berkeley, Berkeley, California 94720, USA
| | - M Dobbs
- Physics Department, McGill University, Montreal, Quebec H3A 0G4, Canada
| | - T Elleflot
- Department of Physics, University of California, San Diego, La Jolla, California 92093-0424, USA
| | - J Errard
- Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, California 92093-0424, USA and Space Sciences Laboratory, University of California, Berkeley, Berkeley, California 94720, USA
| | - G Fabbian
- AstroParticule et Cosmologie, Univ Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France and International School for Advanced Studies (SISSA), Trieste 34014, Italy
| | - C Feng
- Department of Physics, University of California, San Diego, La Jolla, California 92093-0424, USA
| | - D Flanigan
- Department of Physics, University of California, Berkeley, Berkeley, California 94720, USA and Columbia University, New York, New York 10027, USA
| | - A Gilbert
- Physics Department, McGill University, Montreal, Quebec H3A 0G4, Canada
| | - W Grainger
- Rutherford Appleton Laboratory, STFC, Swindon SN2 1SZ, United Kingdom
| | - N W Halverson
- Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, Colorado 80309, USA and Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, Colorado 80309, USA and Department of Physics, University of Colorado, Boulder, Colorado 80309, USA
| | - M Hasegawa
- The Graduate University for Advanced Studies, Hayama, Miura District, Kanagawa 240-0115, Japan and High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - K Hattori
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - M Hazumi
- The Graduate University for Advanced Studies, Hayama, Miura District, Kanagawa 240-0115, Japan and High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan and Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - W L Holzapfel
- Department of Physics, University of California, Berkeley, Berkeley, California 94720, USA
| | - Y Hori
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - J Howard
- Department of Physics, University of California, Berkeley, Berkeley, California 94720, USA and Department of Physics, University of Oxford, Oxford OX1 2JD, United Kingdom
| | - P Hyland
- Physics Department, Austin College, Sherman, Texas 75090, USA
| | - Y Inoue
- The Graduate University for Advanced Studies, Hayama, Miura District, Kanagawa 240-0115, Japan
| | - G C Jaehnig
- Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, Colorado 80309, USA and Department of Physics, University of Colorado, Boulder, Colorado 80309, USA
| | - A Jaffe
- Department of Physics, Imperial College London, London SW7 2AZ, United Kingdom
| | - B Keating
- Department of Physics, University of California, San Diego, La Jolla, California 92093-0424, USA
| | - Z Kermish
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - R Keskitalo
- Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, California 92093-0424, USA
| | - T Kisner
- Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, California 92093-0424, USA and Space Sciences Laboratory, University of California, Berkeley, Berkeley, California 94720, USA
| | - M Le Jeune
- AstroParticule et Cosmologie, Univ Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France
| | - A T Lee
- Department of Physics, University of California, Berkeley, Berkeley, California 94720, USA and Physics Division, Lawrence Berkeley National Laboratory, Berkeley, California 92093-0424, USA
| | - E Linder
- Space Sciences Laboratory, University of California, Berkeley, Berkeley, California 94720, USA and Physics Division, Lawrence Berkeley National Laboratory, Berkeley, California 92093-0424, USA
| | - E M Leitch
- Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, Illinois 60637, USA and Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, Illinois 60637, USA
| | - M Lungu
- Department of Physics, University of California, Berkeley, Berkeley, California 94720, USA
| | - F Matsuda
- Department of Physics, University of California, San Diego, La Jolla, California 92093-0424, USA
| | - T Matsumura
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - X Meng
- Department of Physics, University of California, Berkeley, Berkeley, California 94720, USA
| | - N J Miller
- Observational Cosmology Laboratory, Code 665, NASA Goddard Space Flight Center, Greenbelt, Maryland 20771, USA
| | - H Morii
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - S Moyerman
- Department of Physics, University of California, San Diego, La Jolla, California 92093-0424, USA
| | - M J Myers
- Department of Physics, University of California, Berkeley, Berkeley, California 94720, USA
| | - M Navaroli
- Department of Physics, University of California, San Diego, La Jolla, California 92093-0424, USA
| | - H Nishino
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - H Paar
- Department of Physics, University of California, San Diego, La Jolla, California 92093-0424, USA
| | - J Peloton
- AstroParticule et Cosmologie, Univ Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France
| | - E Quealy
- Department of Physics, University of California, Berkeley, Berkeley, California 94720, USA and Physics Department, Napa Valley College, Napa, California 94558, USA
| | - G Rebeiz
- Department of Electrical and Computer Engineering, University of California, San Diego, La Jolla, California 92093-0424, USA
| | - C L Reichardt
- Department of Physics, University of California, Berkeley, Berkeley, California 94720, USA
| | - P L Richards
- Department of Physics, University of California, Berkeley, Berkeley, California 94720, USA
| | - C Ross
- Department of Physics and Atmospheric Science, Dalhousie University, Halifax, Nova Scotia B3H 4R2, Canada
| | - I Schanning
- Department of Physics, University of California, San Diego, La Jolla, California 92093-0424, USA
| | - D E Schenck
- Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, Colorado 80309, USA and Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, Colorado 80309, USA
| | - B Sherwin
- Department of Physics, University of California, Berkeley, Berkeley, California 94720, USA and Miller Institute for Basic Research in Science, University of California, Berkeley, Berkeley, California 94720, USA
| | - A Shimizu
- The Graduate University for Advanced Studies, Hayama, Miura District, Kanagawa 240-0115, Japan
| | - C Shimmin
- Department of Physics, University of California, Berkeley, Berkeley, California 94720, USA
| | - M Shimon
- Department of Physics, University of California, San Diego, La Jolla, California 92093-0424, USA and School of Physics and Astronomy, Tel Aviv University, Tel Aviv, Israel
| | - P Siritanasak
- Department of Physics, University of California, San Diego, La Jolla, California 92093-0424, USA
| | - G Smecher
- Three-Speed Logic, Inc., Vancouver, British Columbia V6A 2J8, Canada
| | - H Spieler
- Physics Division, Lawrence Berkeley National Laboratory, Berkeley, California 92093-0424, USA
| | - N Stebor
- Department of Physics, University of California, San Diego, La Jolla, California 92093-0424, USA
| | - B Steinbach
- Department of Physics, University of California, Berkeley, Berkeley, California 94720, USA
| | - R Stompor
- AstroParticule et Cosmologie, Univ Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France
| | - A Suzuki
- Department of Physics, University of California, Berkeley, Berkeley, California 94720, USA
| | - S Takakura
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan and Osaka University, Toyonaka, Osaka 560-0043, Japan
| | - T Tomaru
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - B Wilson
- Department of Physics, University of California, San Diego, La Jolla, California 92093-0424, USA
| | - A Yadav
- Department of Physics, University of California, San Diego, La Jolla, California 92093-0424, USA
| | - O Zahn
- Physics Division, Lawrence Berkeley National Laboratory, Berkeley, California 92093-0424, USA
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36
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Ade PAR, Aikin RW, Barkats D, Benton SJ, Bischoff CA, Bock JJ, Brevik JA, Buder I, Bullock E, Dowell CD, Duband L, Filippini JP, Fliescher S, Golwala SR, Halpern M, Hasselfield M, Hildebrandt SR, Hilton GC, Hristov VV, Irwin KD, Karkare KS, Kaufman JP, Keating BG, Kernasovskiy SA, Kovac JM, Kuo CL, Leitch EM, Lueker M, Mason P, Netterfield CB, Nguyen HT, O'Brient R, Ogburn RW, Orlando A, Pryke C, Reintsema CD, Richter S, Schwarz R, Sheehy CD, Staniszewski ZK, Sudiwala RV, Teply GP, Tolan JE, Turner AD, Vieregg AG, Wong CL, Yoon KW. Detection of B-mode polarization at degree angular scales by BICEP2. PHYSICAL REVIEW LETTERS 2014; 112:241101. [PMID: 24996078 DOI: 10.1103/physrevlett.112.241101] [Citation(s) in RCA: 98] [Impact Index Per Article: 9.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/04/2014] [Indexed: 06/03/2023]
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 30 < ℓ < 150, inconsistent with the null hypothesis at a significance of >5σ. 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_(-0.05)(+0.07), 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.
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Affiliation(s)
- P A R Ade
- School of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA, United Kingdom
| | - R W Aikin
- Department of Physics, California Institute of Technology, Pasadena, California 91125, USA
| | - D Barkats
- Joint ALMA Observatory, Vitacura, Santiago, Chile
| | - S J Benton
- Department of Physics, University of Toronto, Toronto, Ontario, M5S 1A7, Canada
| | - C A Bischoff
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA
| | - J J Bock
- Department of Physics, California Institute of Technology, Pasadena, California 91125, USA and Jet Propulsion Laboratory, Pasadena, California 91109, USA
| | - J A Brevik
- Department of Physics, California Institute of Technology, Pasadena, California 91125, USA
| | - I Buder
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA
| | - E Bullock
- Minnesota Institute for Astrophysics, University of Minnesota, Minneapolis, Minnesota 55455, USA
| | - C D Dowell
- Jet Propulsion Laboratory, Pasadena, California 91109, USA
| | - L Duband
- Service des Basses Températures, Commissariat à l'Energie Atomique, 38054 Grenoble, France
| | - J P Filippini
- Department of Physics, California Institute of Technology, Pasadena, California 91125, USA
| | - S Fliescher
- Department of Physics, University of Minnesota, Minneapolis, Minnesota 55455, USA
| | - S R Golwala
- Department of Physics, California Institute of Technology, Pasadena, California 91125, USA
| | - M Halpern
- Department of Physics and Astronomy, University of British Columbia, Vancouver, British Columbia, V6T 1Z1, Canada
| | - M Hasselfield
- Department of Physics and Astronomy, University of British Columbia, Vancouver, British Columbia, V6T 1Z1, Canada
| | - S R Hildebrandt
- Department of Physics, California Institute of Technology, Pasadena, California 91125, USA and Jet Propulsion Laboratory, Pasadena, California 91109, USA
| | - G C Hilton
- National Institute of Standards and Technology, Boulder, Colorado 80305, USA
| | - V V Hristov
- Department of Physics, California Institute of Technology, Pasadena, California 91125, USA
| | - K D Irwin
- National Institute of Standards and Technology, Boulder, Colorado 80305, USA and Department of Physics, Stanford University, Stanford, California 94305, USA and Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, California 94025, USA
| | - K S Karkare
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA
| | - J P Kaufman
- Department of Physics, University of California at San Diego, La Jolla, California 92093, USA
| | - B G Keating
- Department of Physics, University of California at San Diego, La Jolla, California 92093, USA
| | - S A Kernasovskiy
- Department of Physics, Stanford University, Stanford, California 94305, USA
| | - J M Kovac
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA
| | - C L Kuo
- Department of Physics, Stanford University, Stanford, California 94305, USA and Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, California 94025, USA
| | - E M Leitch
- University of Chicago, Chicago, Illinois 60637, USA
| | - M Lueker
- Department of Physics, California Institute of Technology, Pasadena, California 91125, USA
| | - P Mason
- Department of Physics, California Institute of Technology, Pasadena, California 91125, USA
| | - C B Netterfield
- Department of Physics, University of Toronto, Toronto, Ontario, M5S 1A7, Canada and Canadian Institute for Advanced Research, Toronto, Ontario, M5G 1Z8, Canada
| | - H T Nguyen
- Jet Propulsion Laboratory, Pasadena, California 91109, USA
| | - R O'Brient
- Jet Propulsion Laboratory, Pasadena, California 91109, USA
| | - R W Ogburn
- Department of Physics, Stanford University, Stanford, California 94305, USA and Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, California 94025, USA
| | - A Orlando
- Department of Physics, University of California at San Diego, La Jolla, California 92093, USA
| | - C Pryke
- Minnesota Institute for Astrophysics, University of Minnesota, Minneapolis, Minnesota 55455, USA and Department of Physics, University of Minnesota, Minneapolis, Minnesota 55455, USA
| | - C D Reintsema
- National Institute of Standards and Technology, Boulder, Colorado 80305, USA
| | - S Richter
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA
| | - R Schwarz
- Department of Physics, University of Minnesota, Minneapolis, Minnesota 55455, USA
| | - C D Sheehy
- Department of Physics, University of Minnesota, Minneapolis, Minnesota 55455, USA and University of Chicago, Chicago, Illinois 60637, USA
| | - Z K Staniszewski
- Department of Physics, California Institute of Technology, Pasadena, California 91125, USA and Jet Propulsion Laboratory, Pasadena, California 91109, USA
| | - R V Sudiwala
- School of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA, United Kingdom
| | - G P Teply
- Department of Physics, California Institute of Technology, Pasadena, California 91125, USA
| | - J E Tolan
- Department of Physics, Stanford University, Stanford, California 94305, USA
| | - A D Turner
- Jet Propulsion Laboratory, Pasadena, California 91109, USA
| | - A G Vieregg
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA and University of Chicago, Chicago, Illinois 60637, USA
| | - C L Wong
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS 42, Cambridge, Massachusetts 02138, USA
| | - K W Yoon
- Department of Physics, Stanford University, Stanford, California 94305, USA and Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, California 94025, USA
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37
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Dodelson S. How much can we learn about the physics of inflation? PHYSICAL REVIEW LETTERS 2014; 112:191301. [PMID: 24877925 DOI: 10.1103/physrevlett.112.191301] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/04/2014] [Indexed: 06/03/2023]
Abstract
The recent BICEP2 measurement of B modes in the polarization of the cosmic microwave background suggests that inflation was driven by a field at an energy scale of 2 × 10(16) GeV. I explore the potential of upcoming cosmic microwave radiation polarization experiments to further constrain the physics underlying inflation. If the signal is confirmed, then two sets of experiments covering a large area will shed light on inflation. Low-resolution measurements can pin down the tensor to scalar ratio at the percent level, thereby distinguishing models from one another. A high angular resolution experiment will be necessary to measure the tilt of the tensor spectrum, testing the consistency relation that relates the tilt to the amplitude.
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Affiliation(s)
- Scott Dodelson
- Fermi National Accelerator Laboratory, Batavia, Illinois 60510-0500, USA and Kavli Institute for Cosmological Physics, Enrico Fermi Institute, University of Chicago, Chicago, Illinois 60637, USA and Department of Astronomy and Astrophysics, University of Chicago, Chicago, Illinois 60637, USA
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38
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Cosmology: First light. Nature 2014; 509:276-8. [DOI: 10.1038/509276a] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/08/2022]
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39
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Ade PAR, Akiba Y, Anthony AE, Arnold K, Atlas M, Barron D, Boettger D, Borrill J, Borys C, Chapman S, Chinone Y, Dobbs M, Elleflot T, Errard J, Fabbian G, Feng C, Flanigan D, Gilbert A, Grainger W, Halverson NW, Hasegawa M, Hattori K, Hazumi M, Holzapfel WL, Hori Y, Howard J, Hyland P, Inoue Y, Jaehnig GC, Jaffe A, Keating B, Kermish Z, Keskitalo R, Kisner T, Le Jeune M, Lee AT, Leitch EM, Linder E, Lungu M, Matsuda F, Matsumura T, Meng X, Miller NJ, Morii H, Moyerman S, Myers MJ, Navaroli M, Nishino H, Paar H, Peloton J, Poletti D, Quealy E, Rebeiz G, Reichardt CL, Richards PL, Ross C, Rotermund K, Schanning I, Schenck DE, Sherwin BD, Shimizu A, Shimmin C, Shimon M, Siritanasak P, Smecher G, Spieler H, Stebor N, Steinbach B, Stompor R, Suzuki A, Takakura S, Tikhomirov A, Tomaru T, Wilson B, Yadav A, Zahn O. Evidence for gravitational lensing of the cosmic microwave background polarization from cross-correlation with the cosmic infrared background. PHYSICAL REVIEW LETTERS 2014; 112:131302. [PMID: 24745402 DOI: 10.1103/physrevlett.112.131302] [Citation(s) in RCA: 8] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/26/2013] [Indexed: 06/03/2023]
Abstract
We reconstruct the gravitational lensing convergence signal from cosmic microwave background (CMB) polarization data taken by the Polarbear experiment and cross-correlate it with cosmic infrared background maps from the Herschel satellite. From the cross spectra, we obtain evidence for gravitational lensing of the CMB polarization at a statistical significance of 4.0σ and indication of the presence of a lensing B-mode signal at a significance of 2.3σ. We demonstrate that our results are not biased by instrumental and astrophysical systematic errors by performing null tests, checks with simulated and real data, and analytical calculations. This measurement of polarization lensing, made via the robust cross-correlation channel, not only reinforces POLARBEAR auto-correlation measurements, but also represents one of the early steps towards establishing CMB polarization lensing as a powerful new probe of cosmology and astrophysics.
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Affiliation(s)
- P A R Ade
- School of Physics and Astronomy, Cardiff University, Cardiff CF10 3XQ, United Kingdom
| | - Y Akiba
- The Graduate University for Advanced Studies, Hayama, Miura District, Kanagawa 240-0115, Japan
| | - A E Anthony
- Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309, USA and Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309, USA
| | - K Arnold
- Department of Physics, University of California, San Diego, CA 92093-0424, USA
| | - M Atlas
- Department of Physics, University of California, San Diego, CA 92093-0424, USA
| | - D Barron
- Department of Physics, University of California, San Diego, CA 92093-0424, USA
| | - D Boettger
- Department of Physics, University of California, San Diego, CA 92093-0424, USA
| | - J Borrill
- Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, CA 92093-0424, USA and Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA
| | - C Borys
- California Institute of Technology, Pasadena, California, USA
| | - S Chapman
- Department of Physics and Atmospheric Science, Dalhousie University, Halifax, NS, B3H 4R2, Canada
| | - Y Chinone
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan and Department of Physics, University of California, Berkeley, CA 94720, USA
| | - M Dobbs
- Physics Department, McGill University, Montreal, QC H3A 0G4, Canada
| | - T Elleflot
- Department of Physics, University of California, San Diego, CA 92093-0424, USA
| | - J Errard
- Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, CA 92093-0424, USA and Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA
| | - G Fabbian
- AstroParticule et Cosmologie, Univ Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France and International School for Advanced Studies (SISSA), Trieste 34014, Italy
| | - C Feng
- Department of Physics, University of California, San Diego, CA 92093-0424, USA
| | - D Flanigan
- Department of Physics, University of California, Berkeley, CA 94720, USA and Department of Physics, Columbia University, New York, NY 10027, USA
| | - A Gilbert
- Physics Department, McGill University, Montreal, QC H3A 0G4, Canada
| | - W Grainger
- Rutherford Appleton Laboratory, STFC, Swindon, SN2 1SZ, United Kingdom
| | - N W Halverson
- Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309, USA and Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309, USA and Department of Physics, University of Colorado, Boulder, CO 80309, USA
| | - M Hasegawa
- The Graduate University for Advanced Studies, Hayama, Miura District, Kanagawa 240-0115, Japan and High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - K Hattori
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - M Hazumi
- The Graduate University for Advanced Studies, Hayama, Miura District, Kanagawa 240-0115, Japan and High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan and Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - W L Holzapfel
- Department of Physics, University of California, Berkeley, CA 94720, USA
| | - Y Hori
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - J Howard
- Department of Physics, University of California, Berkeley, CA 94720, USA and Department of Physics, University of Oxford, Oxford OX1 2JD, United Kingdom
| | - P Hyland
- Physics Department, Austin College, Sherman, TX 75090, USA
| | - Y Inoue
- The Graduate University for Advanced Studies, Hayama, Miura District, Kanagawa 240-0115, Japan
| | - G C Jaehnig
- Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309, USA and Department of Physics, University of Colorado, Boulder, CO 80309, USA
| | - A Jaffe
- Department of Physics, Imperial College London, London SW7 2AZ, United Kingdom
| | - B Keating
- Department of Physics, University of California, San Diego, CA 92093-0424, USA
| | - Z Kermish
- Physics Department, Princeton University, Princeton, NJ 08544, USA
| | - R Keskitalo
- Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, CA 92093-0424, USA
| | - T Kisner
- Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, CA 92093-0424, USA and Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA
| | - M Le Jeune
- AstroParticule et Cosmologie, Univ Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France
| | - A T Lee
- Department of Physics, University of California, Berkeley, CA 94720, USA and Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
| | - E M Leitch
- Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA and Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA
| | - E Linder
- Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA and Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
| | - M Lungu
- Department of Physics, University of California, Berkeley, CA 94720, USA
| | - F Matsuda
- Department of Physics, University of California, San Diego, CA 92093-0424, USA
| | - T Matsumura
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - X Meng
- Department of Physics, University of California, Berkeley, CA 94720, USA
| | - N J Miller
- Observational Cosmology Laboratory, Code 665, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - H Morii
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - S Moyerman
- Department of Physics, University of California, San Diego, CA 92093-0424, USA
| | - M J Myers
- Department of Physics, University of California, Berkeley, CA 94720, USA
| | - M Navaroli
- Department of Physics, University of California, San Diego, CA 92093-0424, USA
| | - H Nishino
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - H Paar
- Department of Physics, University of California, San Diego, CA 92093-0424, USA
| | - J Peloton
- AstroParticule et Cosmologie, Univ Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France
| | - D Poletti
- AstroParticule et Cosmologie, Univ Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France
| | - E Quealy
- Department of Physics, University of California, Berkeley, CA 94720, USA and Physics Department, Napa Valley College, Napa, CA 94558, USA
| | - G Rebeiz
- Department of Electrical and Computer Engineering, University of California, San Diego, CA 92093, USA
| | - C L Reichardt
- Department of Physics, University of California, Berkeley, CA 94720, USA
| | - P L Richards
- Department of Physics, University of California, Berkeley, CA 94720, USA
| | - C Ross
- Department of Physics and Atmospheric Science, Dalhousie University, Halifax, NS, B3H 4R2, Canada
| | - K Rotermund
- Department of Physics and Atmospheric Science, Dalhousie University, Halifax, NS, B3H 4R2, Canada
| | - I Schanning
- Department of Physics, University of California, San Diego, CA 92093-0424, USA
| | - D E Schenck
- Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309, USA and Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309, USA
| | - B D Sherwin
- Department of Physics, University of California, Berkeley, CA 94720, USA and Miller Institute for Basic Research in Science, University of California, Berkeley, CA 94720, USA
| | - A Shimizu
- The Graduate University for Advanced Studies, Hayama, Miura District, Kanagawa 240-0115, Japan
| | - C Shimmin
- Department of Physics, University of California, Berkeley, CA 94720, USA
| | - M Shimon
- Department of Physics, University of California, San Diego, CA 92093-0424, USA and School of Physics and Astronomy, Tel Aviv University, Tel Aviv, Israel
| | - P Siritanasak
- Department of Physics, University of California, San Diego, CA 92093-0424, USA
| | - G Smecher
- Three-Speed Logic, Inc., Vancouver, B.C., V6A 2J8, Canada
| | - H Spieler
- Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
| | - N Stebor
- Department of Physics, University of California, San Diego, CA 92093-0424, USA
| | - B Steinbach
- Department of Physics, University of California, Berkeley, CA 94720, USA
| | - R Stompor
- AstroParticule et Cosmologie, Univ Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France
| | - A Suzuki
- Department of Physics, University of California, Berkeley, CA 94720, USA
| | - S Takakura
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan and Osaka University, Toyonaka, Osaka 560-0043, Japan
| | - A Tikhomirov
- Department of Physics and Atmospheric Science, Dalhousie University, Halifax, NS, B3H 4R2, Canada
| | - T Tomaru
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - B Wilson
- Department of Physics, University of California, San Diego, CA 92093-0424, USA
| | - A Yadav
- Department of Physics, University of California, San Diego, CA 92093-0424, USA
| | - O Zahn
- Physics Division, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA
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40
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Dai L. Rotation of the cosmic microwave background polarization from weak gravitational lensing. PHYSICAL REVIEW LETTERS 2014; 112:041303. [PMID: 24580435 DOI: 10.1103/physrevlett.112.041303] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/13/2013] [Indexed: 06/03/2023]
Abstract
When a cosmic microwave background (CMB) photon travels from the surface of last scatter through spacetime metric perturbations, the polarization vector may rotate about its direction of propagation. This gravitational rotation is distinct from, and occurs in addition to, the lensing deflection of the photon trajectory. This rotation can be sourced by linear vector or tensor metric perturbations and is fully coherent with the curl deflection field. Therefore, lensing corrections to the CMB polarization power spectra as well as the temperature-polarization cross correlations due to nonscalar perturbations are modified. The rotation does not affect lensing by linear scalar perturbations, but needs to be included when calculations go to higher orders. We present complete results for weak lensing of the full-sky CMB power spectra by general linear metric perturbations, taking into account both deflection of the photon trajectory and rotation of the polarization. For the case of lensing by gravitational waves, we show that the B modes induced by the rotation largely cancel those induced by the curl component of deflection.
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Affiliation(s)
- Liang Dai
- Department of Physics and Astronomy, Johns Hopkins University, Baltimore, Maryland 21218, USA
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