DOCSLIB.ORG

B-Modes and TES Polarimeters

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
B-Modes and TES Polarimeters B-Modes and TES Polarimeters Hsiao-Mei (Sherry) Cho National Institute of Standards and Technology, Boulder, CO, USA Thursday June 27th, 2013 LTD15, Pasadena, CA Outline Part I: Current CMB polarimeter systems ● Science ● How to measure B-modes? ● Near future CMB polarimeter systems Part II: Next-generation feedhorn-coupled CMB polarimetry ● On-chip detection over a multi-octave bandwidth design ● Program directions Acknowledgements TES Polarimeter Projects Multi-Octave collaborations ● ABS ● University of Michigan ● ACTPol ● NIST-Boulder ● BICEP 2/Keck array/BICEP3 ● CLASS ● LiteBIRD* ● EBEX Special Thanks ● PIPER ● POLARBEAR I/II Dr. Kent Irwin ● SPIDER Dr. Jeff McMahon ● SPTpol /3G Dr. Brad Benson Dr. Mike Niemack Goal Searching for inflationary B-mode polarization signal in CMB Direct probe of inflation Detection of the cosmic gravity wave (g-wave) background would probe the inflationary era (10-35 s?) “De-lens” to improve inflationary gravity wave search sensitivity E-Modes and B-Modes Polarization maps broken into mathematical basis sets Density waves: “divergence”, Unique gravity wave but no “curl” signature: “curl” mode ● Similar to the fundamental theorem of vector calculus (Helmholtz theorem), but for a tensor field ● Measuring B mode polarization is a very clean way to probe gravity waves in inflation Primordial gravitational waves and B-modes TT TE EE Approx EE/BB foreground BB G-waves r=0.3 decay once inside the horizon. Reionization peak B modes from lensing of E modes (not (zr=10) Horizon size at primordial). decoupling (zdec=1089) Measurements before TESs Decision, decision and decisions 1. Optics Off axis Gregorian, Crossed- Dragone or Refractor 2. Polarization modulation TES polarimeter projects: HWP or VPM ABS ACTPol 3. Beam forming BICEP 2/Keck array/BICEP3 Feeds, Lenses, or Phased-arrays CLASS EBEX EBEX6K 4. Multichroic LiteBIRD* 90/150GHz or 90/150/220GHz PIPER POLARBEAR I/II 5. Readout Simons array TDM or FDM SPIDER SPTpol SPT-3G Off axis Gregorian: POLARBEAR-1 Sky Huan Tran Telescope Primary Primary Secondary Receiver Secondary Receiver Crossed-Dragone: Atacama B-Mode Search (ABS) Cold (~4 K) crossed-Dragone optics with ~60 cm diameter mirrors and an aperture diameter of ~25 cm 60 cm Refractor: SPIDER Suborbital Polarimeter for Inflation Dust and the Epoch of Reionization Spider Instrument Insert (one of six) Half-Wave Plate (HWP): The E and B Experiment (EBEX) ● Continuous 1.24 Hz rotation at 4 K 150 150 ● 1,000,000 rotations during 2012 flight 250 ● 15 mWatt power dissipation 250 410 150 5 mm gap Variable-Delay Polarization Modulator (VPM): Cosmology Large Angular Scale Surveyor (CLASS) Variable-Delay Polarization Modulator (VPM): Cosmology Large Angular Scale Surveyor (CLASS) Feedhorn-Coupled: SPTPol 95 GHz 150 GHz Contoured feed horn; maintains polarization angle Detector in wave- guide section with ࣅ/4 backshort Crossed absorbers 6 cm 1 cm Lens Coupled & Multichroic: POLARBEAR-2 Incident light AR coated lens Si lens 90/150 GHz Planar Detector antenna wafer Phased Array: BICEP2/Keck Array/BICEP3/SPIDER Background Imaging of Cosmic Extragalactic Polarization (BICEP) Multichroic: ACTPOL A polarization sensitive receiver for the 6- meter Atacama Cosmology Telescope (ACT) 90/150 GHz Feed array wafers Time-Division Multiplexer (TDM): Primordial Inflation Polarization Explorer (PIPER) 1,280-pixel SQUID Multiplexer Frequency Domain Multiplexer (FDM): POLARBEAR-1 R1 Bias comb L1 L2 L3 Ln ΣVi(fi) RB C1 C2 C3 Cn RS RS RS RS Nulling comb R R 2 I1 fb Σ-Vi(fi) L&Cs I2 SQUIDs Demodulator Updates Atacama B-Mode Search (ABS) Currently in second year of observation Princeton, Johns Hopkins, NIST, UBC, U. Chile ACTPOL Currently on the telescope! 150 GHz array (PA1) BICEP2 (2010-12)/Keck Array (2011- )/BICEP3 (2014- ) Background Imaging of Cosmic Extragalactic Polarization (BICEP) BICEP MOUNT EXISTING DASI MOUNT BICEP MOUNT CLASS Status Deploying telescopes 2014-2015 Polarbear ACT/ABS CLASS The E and B Experiment (EBEX) 12 days of data collected in 1/2013 and are being analyzed 150 150 250 250 410 150 150 30 cm PIPER Plan to fly in 2015! POLARBEAR-1 APC, Cardiff , C.U. Boulder, Dalhousie, Imperial, IPMU, KEK, LBNL, McGill, UC Berkeley, UCSD E-mode polarization Observing since 2012 1 year of data -- CMB Polarization Map today ~15x deeper than Planck POLARBEAR-2 Plan to deploy 2014 250 mK 350 mK 4 K 300 K modulator Digital demodulat Vbias Lin o SPIDER Suborbital Polarimeter for Inflation Dust and the Epoch of Reionization ● Currently, Spider is in the field, at the CSBF facility in Palestine, TX, with five of her 6 telescopes installed. ● Will launch this fall, probably in the air around Christmas (depending on, among other things, the winds). The goal is to get a 24 day flight (two trips). SPTPol 2012 to mid-2013: Observed 100 deg2 SPTpol “deep” field 2013-2015: Observe 500 deg2 KECK field and “de-lens” large scales to constrain primordial gravity waves from inflation 150GHz 95GHz Near Future Projects ● EBEX6K: 90/150/220 GHz, FDM, 2016, ? ● Simons array: 3 x Polarbear2, FDM, 2016 ● SPT-3G: 100/150/220 GHz, FDM, 2016 ● LiteBIRD*: Lite (Light) Satellite for the Studies of B-mode Polarization and Inflation from Cosmic Background Radiation Detection, 60/78/100GHz and 140/195/280GHz, FDM, 2020 Next-generation feedhorn-coupled CMB polarimetry (nearly) Multi-Octave Horn Coupled Architecture Prototype feed Ring Loaded (cross-section) Corrugated Feed Round to Quad- Ridge Transition cross-section of Prototype quad-ridge Quad Transition waveguide OMT Design Next Steps –Microwave SQUID Multiplexer feedline Single channel detail rf-SQUID resonator Microwave SQUID Multiplexer chip ● Read out 100s – 1000s of TESs with 6 lines (2 coax, 2 flux ramp, 2 TES bias) ● First on sky demo Mustang1.5 on GBT anticipated fall 2013 Take Home Messages ● Every system is complicated ● Many talks and posters on CMB today ● Stay tuned! Many more results are coming!! ● Multichroic detectors are welcome ● Multiplexer readout are needed Thank local organizing committee!! ☺ TES polarimeter projects On-going observation Will deploy in 2013-2014 Will deploy 2015-2020 ABS BICEP3 EBEX6K (balloon)? ACTPol CLASS LiteBIRD*(Satellite) BICEP 2 POLARBEAR II PIPER(ballon) EBEX (balloon) SPIDER Simons array Keck array SPT-3G POLARBEAR SPTpol.
Load more

Recommended publications
  • Analysis and Measurement of Horn Antennas for CMB Experiments
    Analysis and Measurement of Horn Antennas for CMB Experiments Ian Mc Auley (M.Sc. B.Sc.) A thesis submitted for the Degree of Doctor of Philosophy Maynooth University Department of Experimental Physics, Maynooth University, National University of Ireland Maynooth, Maynooth, Co. Kildare, Ireland. October 2015 Head of Department Professor J.A. Murphy Research Supervisor Professor J.A. Murphy Abstract In this thesis the author's work on the computational modelling and the experimental measurement of millimetre and sub-millimetre wave horn antennas for Cosmic Microwave Background (CMB) experiments is presented. This computational work particularly concerns the analysis of the multimode channels of the High Frequency Instrument (HFI) of the European Space Agency (ESA) Planck satellite using mode matching techniques to model their farfield beam patterns. To undertake this analysis the existing in-house software was upgraded to address issues associated with the stability of the simulations and to introduce additional functionality through the application of Single Value Decomposition in order to recover the true hybrid eigenfields for complex corrugated waveguide and horn structures. The farfield beam patterns of the two highest frequency channels of HFI (857 GHz and 545 GHz) were computed at a large number of spot frequencies across their operational bands in order to extract the broadband beams. The attributes of the multimode nature of these channels are discussed including the number of propagating modes as a function of frequency. A detailed analysis of the possible effects of manufacturing tolerances of the long corrugated triple horn structures on the farfield beam patterns of the 857 GHz horn antennas is described in the context of the higher than expected sidelobe levels detected in some of the 857 GHz channels during flight.
    [Show full text]
  • Rhodri Evans
    Rhodri Evans The Cosmic Microwave Background How It Changed Our Understanding of the Universe Astronomers’ Universe More information about this series at http://www.springer.com/series/6960 Rhodri Evans The Cosmic Microwave Background How It Changed Our Understanding of the Universe 123 Rhodri Evans School of Physics & Astronomy Cardiff University Cardiff United Kingdom ISSN 1614-659X ISSN 2197-6651 (electronic) ISBN 978-3-319-09927-9 ISBN 978-3-319-09928-6 (eBook) DOI 10.1007/978-3-319-09928-6 Springer Cham Heidelberg New York Dordrecht London Library of Congress Control Number: : 2014957530 © Springer International Publishing Switzerland 2015 This work is subject to copyright. All rights are reserved by the Publisher, whether the whole or part of the material is concerned, specifically the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfilms or in any other physical way, and transmission or information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed. Exempted from this legal reservation are brief excerpts in connection with reviews or scholarly analysis or material supplied specifically for the purpose of being entered and executed on a computer system, for exclusive use by the purchaser of the work. Duplication of this publication or parts thereof is permitted only under the provisions of the Copyright Law of the Publisher’s location, in its current version, and permission for use must always be obtained from Springer. Permissions for use may be obtained through RightsLink at the Copyright Clearance Center. Violations are liable to prosecution under the respective Copyright Law.
    [Show full text]
  • The EBEX Balloon Borne Experiment-Optics, Receiver, and Polarimetry
    The EBEX Balloon Borne Experiment - Optics, Receiver, and Polarimetry The EBEX Collaboration: Asad M. Aboobaker1, Peter Ade2, Derek Araujo3, Fran¸cois Aubin4, Carlo Baccigalupi5;6, Chaoyun Bao4, Daniel Chapman3, Joy Didier3, Matt Dobbs7;8, Christopher Geach4, Will Grainger9, Shaul Hanany4;∗, Kyle Helson10, Seth Hillbrand3, Johannes Hubmayr11, Andrew Jaffe12, Bradley Johnson3, Terry Jones4, Jeff Klein4, Andrei Korotkov10, Adrian Lee13, Lorne Levinson14, Michele Limon3, Kevin MacDermid7, Tomotake Matsumura4;15, Amber D. Miller3, Michael Milligan4, Kate Raach4, Britt Reichborn-Kjennerud3, Ilan Sagiv14, Giorgio Savini16, Locke Spencer2;17, Carole Tucker2, Gregory S. Tucker10, Benjamin Westbrook11, Karl Young4, Kyle Zilic4 ABSTRACT The E and B Experiment (EBEX) was a long-duration balloon-borne cosmic mi- crowave background polarimeter that flew over Antarctica in 2013. We describe the experiment's optical system, receiver, and polarimetric approach, and report on their in-flight performance. EBEX had three frequency bands centered on 150, 250, and 1Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 2School of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA, United Kingdom 3Physics Department, Columbia University, New York, NY 10027 4University of Minnesota School of Physics and Astronomy, Minneapolis, MN 55455 5Astrophysics Sector, SISSA, Trieste, 34014, Italy 6INFN, Sezione di Trieste, Via Valerio 2, I-34127 Trieste, Italy 7McGill University, Montreal, Quebec, H3A 2T8, Canada 8Canadian Institute for
    [Show full text]
  • Introduction to the Special Issue on Scientific Balloon Capabilities and Instrumentation
    INTRODUCTION TO THE SPECIAL ISSUE ON SCIENTIFIC BALLOON CAPABILITIES AND INSTRUMENTATION J. A. GASKIN1, I. S., SMITH2, AND W. V. JONES3 1 X-Ray Astronomy Group, NASA Marshall Space Flight Center, Huntsville, AL 35812, USA, [email protected]. 2Space Science and Engineering Division/15, Southwest Research Institute, 6220 Culebra Rd, San Antonio, TX 78238, USA, [email protected] 3Science Mission Directorate, Astrophysics Division DH000 NASA Headquarters, Washington, DC 20546, USA, [email protected] Received (to be inserted by publisher); Revised (to be inserted by publisher); Accepted (to be inserted by publisher); In 1783, the Montgolfier brothers ushered in a new era of transportation and exploration when they used hot air to drive an un- tethered balloon to an altitude of ~2 km. Made of sackcloth and held together with cords, this balloon challenged the way we thought about human travel, and it has since evolved into a robust platform for performing novel science and testing new technologies. Today, high-altitude balloons regularly reach altitudes of 40 km, and they can support payloads that weigh more than 3,000 kg. Long-duration balloons can currently support mission durations lasting ~55 days, and developing balloon technologies (i.e. Super-Pressure Balloons) are expected to extend that duration to 100 days or longer; competing with satellite payloads. This relatively inexpensive platform supports a broad range of science payloads, spanning multiple disciplines (astrophysics, heliophysics, planetary and earth science.) Applications extending beyond traditional science include testing new technologies for eventual space-based application and stratospheric airships for planetary applications. Keywords: balloon payloads, scientific ballooning, balloon flight operations.
    [Show full text]
  • Telescope Design Considerations
    CMB S-4: Telescope Design Considerations September 12, 2016 T. Essinger-Hileman, N. Halverson, S. Hanany, M. D. Niemack, S. Padin, S. Parshley, C. Pryke, T. Suzuki, E. Switzer, K. Thompson, et al. Institutions DRAFT Contents 1 Introduction 1 1.1 Optics benchmarks . .2 2 Current CMB telescope designs and maturity 3 2.1 Current small aperture telescope designs . .4 2.2 Current large aperture telescope designs . .5 2.3 Concept for high throughput large aperture telescope design . .6 3 Telescope engineering to improve systematics 9 3.1 Monolithic mirrors . .9 3.2 Boresight rotation . 10 3.3 Shields and baffles . 10 4 Potential future studies and development areas 13 A Optics designs for current projects 16 A.1 Advanced ACTPol . 16 A.2 BICEP3 . 17 A.3 CLASS . 18 A.4 EBEX . 19 A.5 Keck/Spider . 20 A.6 Piper . 21 A.7 Simons Array . 22 A.8 SPT-3G . 23 B Projects using crossed-Dragone telescopes 24 B.1 ABS . 24 B.2 QUIET . 25 B.3 CCAT-prime . 26 DRAFT i 1 Introduction CHARGE: Summarize the current state of the technology and identify R&D efforts neces- sary to advance it for possible use in CMB-S4. CMB-S4 will likely require a scale-up in number of elements, frequency coverage, and bandwidth relative to current instruments. Because it is searching for lower magnitude signals, it will also require stronger control of systematic uncertainties. Current landscape • Existing CMB experiments have a range of telescope sizes (∼ 0:3 to 10 m) and styles (cold refractors and offset Gregory and crossed Dragone reflectors).
    [Show full text]
  • Task Force on Cosmic Microwave Background Research
    Task Force On Cosmic Microwave Background Research Final Report July 11, 2005 -1- MEMBERS OF THE CMB TASK FORCE James Bock Caltech/JPL Sarah Church Stanford University Mark Devlin University of Pennsylvania Gary Hinshaw NASA/GSFC Andrew Lange Caltech Adrian Lee University of California at Berkeley/LBNL Lyman Page Princeton University Bruce Partridge Haverford College John Ruhl Case Western Reserve University Max Tegmark Massachusetts Institute of Technology Peter Timbie University of Wisconsin Rainer Weiss (chair) Massachusetts Institute of Technology Bruce Winstein University of Chicago Matias Zaldarriaga Harvard University AGENCY OBSERVERS Beverly Berger National Science Foundation Vladimir Papitashvili National Science Foundation Michael Salamon NASA/HDQTS Nigel Sharp National Science Foundation Kathy Turner US Department of Energy -2- Table of Contents Executive Summary ...........................................................................................4 1 Outline of Report ................................................................................................8 sidebar “Some History and Perspective..............................................................10 2 Cosmology and Inflation ..................................................................................11 sidebar “Direct Measurement of Primeval Gravitational Waves” ....................18 3 Theory of CMB Polarization and Gravitational Waves ....................................19 4 Astrophysical Disturbances in Measuring the CMB Polarization: Gravitational
    [Show full text]
  • NASA Stratospheric Balloons Science at the Edge of Space
    National Aeronautics and Space Administration NASA Stratospheric Balloons Science at the edge of Space REPORT OF THE SCIENTIFIC BALLOONING ASSESSMENT GROUP The Scientific Ballooning Assessment Group Martin Israel Washington University in St. Louis, Chair Steven Boggs University of California, Berkeley Michael Cherry Louisiana State University Mark Devlin University of Pennsylvania Jonathan Grindlay Harvard University Bruce Lites National Center for Astrophysics Research James Margitan Jet Propulsion Laboratory Jonathan Ormes University of Denver Carol Raymond Jet Propulsion Laboratory Eun-Suk Seo University of Maryland, College Park Eliot Young Southwest Research Institute, Boulder Vernon Jones NASA Headquarters, Executive Secretary Ex Officio: Vladimir Papitashvili NSF, Office of Polar Programs David Pierce NASA, GSFC/WFF Balloon Program Office, Chief Debora Fairbrother NASA, GSFC/WFF Balloon Program Office, Technologist Jack Tueller NASA GSFC, Balloon Program Project Scientist John Mitchell NASA GSFC, Balloon Program Deputy Project Scientist Cover Photo: The Balloon-borne Experiment with Superconducting Spectrometer, BESS Polar II at Williams Field, McMurdo, Antarctica. Facing Page Photo: The International ocusingF Optics Collaboration for micro-Crab Sensitivity (InFOCmS), a hard x-ray telescope with CdZnTe pixel detector as a focal plane imager. NASA Stratospheric Balloons Science at the edge of Space Report of the Scientific Ballooning Assessment Group January 2010 Table of Contents Executive Summary 3 Scientific Ballooning has Made Important Contributions to NASA’s Program 9 Balloon-borne Instruments Will Continue to Contribute to NASA’s Objectives 15 Many Scientists with Leading Roles in NASA were Trained in the Balloon Program 35 The Balloon Program has Substantial Capability for Achieving Quality Science 37 Findings 41 Acronyms 46 References 49 The Cosmic Ray Energetics And Mass instrument (CREAM) hangs on the launch vehicle at Williams Field near McMurdo base Antarctica.
    [Show full text]
  • A Balloon-Borne Cosmic Microwave Background Anisotropy Probe
    The E and B EXperiment: A balloon-borne cosmic microwave background anisotropy probe Seth Hillbrand Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Graduate School of Arts and Sciences COLUMBIA UNIVERSITY 2014 c 2014 Seth Hillbrand All Rights Reserved ABSTRACT The E and B EXperiment: A balloon-borne cosmic microwave background anisotropy probe Seth Hillbrand The E and B Experiment (EBEX), is a balloon-borne sub-orbital cosmic microwave background polarimeter, designed to measure polarization levels in the microwave spectrum. EBEX recently completed an 11-day Antarctic long duration balloon (LDB) science flight in January, 2013. 1000 transition edge sensor bolometric detectors in ∼ three frequency bands centered at 150, 250 and 410 GHz sampled a large segment of the southern sky. Over 1.5TB of data were collected during the LDB flight. In this thesis, we describe the design and performance of the EBEX software components monitoring and controlling the system during the flight, including automation, telemetry, data storage and readout array management. We also describe the design and development of a novel attitude reconstruction system for a balloon-borne pointed observation platform based on a daytime star camera and 3-axis gyroscopes. The data gathered during the LDB flight are analyzed and the results presented showing attitude reconstruction error at less than 2000 RMS for an 80 second interval. Table of Contents 1 Introduction1 2 EBEX Science4 2.1 Concordance Cosmology.........................4 2.1.1 Expanding Universe.......................6 2.1.2 Flat Universe...........................9 2.1.3 Hot, Dense Early Universe....................9 2.1.4 Dark Matter Universe.....................
    [Show full text]
  • Implementation and Analysis of the 2009 Engineering Flight
    The E and B EXperiment: Implementation and Analysis of the 2009 Engineering Flight A DISSERTATION SUBMITTED TO THE FACULTY OF THE GRADUATE SCHOOL OF THE UNIVERSITY OF MINNESOTA BY Michael Bryce Milligan IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF Doctor of Philosophy Shaul Hanany May, 2011 c Michael Bryce Milligan 2011 ALL RIGHTS RESERVED Acknowledgements There are many people who have earned my lasting gratitude over the past (too many) years. To compile an exhaustive list would be both tedious and inevitably uncharitable to those I fail to mention. Forgive me, then, if I stick to generalities except for those few cases who, perhaps, don't know who they are. The EBEX project itself is a collaboration of dozens of individuals, without whom this wonderful contraption we have built could not exist. I have been delighted to call them colleagues and friends, and I especially tip my hat to those of you who shared with me the ups and downs of our field campaigns in Nevis, NY, Ft. Sumner, NM, and Palestine, TX. And behind all of us, I recognize the family and friends who cheer on our successes, lighten the setbacks, and tolerate the strange hours and long absences that come with experimental astrophysics. Not least my own family and friends, who never seem to give up on me even when I quite shamefully neglect them! I appreciate all the people who have been guideposts on the path that led me here. Early on, Moises Sandoval and later Jim Fraser nurtured in me a taste for doing an experiment to untangle the nature of the world.
    [Show full text]
  • Calibration and Design of the E and B Experiment (EBEX) Cryogenic Receiver
    Calibration and Design of the E and B EXperiment (EBEX) Cryogenic Receiver A THESIS SUBMITTED TO THE FACULTY OF THE GRADUATE SCHOOL OF THE UNIVERSITY OF MINNESOTA BY Kyle Thomas Zilic IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF Doctor of Philosophy Professor Shaul Hanany August, 2014 c Kyle Thomas Zilic 2014 ALL RIGHTS RESERVED Acknowledgements I first want to express my thanks to my advisor and mentor in experimentation through the years, Shaul Hanany. All good experimental practices I have are from him and without him I would be a “nicer” person. None of the work I’ve done, data I’ve analyzed, things I’ve designed, built, tested, broke, fixed, and experimentation I’ve done would have possible without the concerted effort of the University of Minnesota Observational Cosmology group. Without my fellow graduate students – Chaoyun Bao, Clay Hogan-Chin, Hannes Hubmayr, Jeff Klein, Michael Milligan, Dan Polsgrove, Kate Raach, and Ilan Sagiv, – our dutiful undergraduate students – Alex, Bob, Craig, Dave, Geach, Vanessa,– and our fearless post-doc leader, Asad Aboobaker, our experiment would have crumbled and my sanity surely with it. I would also like to acknowledge the fine work from everyone else in the EBEX collaboration and I would especially mention the Herculean efforts from everyone in the Nevis 2008, Fort Sumner 2009, Palestine 2011, Palestine 2012, and Antarctica 2012 campaigns. Hopefully this is the Final Countdown... i Dedication This is dedicated to the individuals that, without whom, I wouldn’t be here: To Bill Jameson, who first inspired my love of physics and taught me more than just science.
    [Show full text]
  • Intensity-Coupled Polarization in Instruments with a Continuously Rotating Half-Wave Plate
    This is an Open Access document downloaded from ORCA, Cardiff University's institutional repository: http://orca.cf.ac.uk/123155/ This is the author’s version of a work that was submitted to / accepted for publication. Citation for final published version: Didier, Joy, Miller, Amber D., Araujo, Derek, Aubin, François, Geach, Christopher, Johnson, Bradley, Korotkov, Andrei, Raach, Kate, Westbrook, Benjamin, Young, Karl, Aboobaker, Asad M., Ade, Peter, Baccigalupi, Carlo, Bao, Chaoyun, Chapman, Daniel, Dobbs, Matt, Grainger, Will, Hanany, Shaul, Helson, Kyle, Hillbrand, Seth, Hubmayr, Johannes, Jaffe, Andrew, Jones, Terry J., Klein, Jeff, Lee, Adrian, Limon, Michele, MacDermid, Kevin, Milligan, Michael, Pascale, Enzo, Reichborn-Kjennerud, Britt, Sagiv, Ilan, Tucker, Carole, Tucker, Gregory S. and Zilic, Kyle 2019. Intensity-coupled polarization in instruments with a continuously rotating half-wave plate. Astrophysical Journal 876 (1) , 54. 10.3847/1538-4357/ab0f36 file Publishers page: http://dx.doi.org/10.3847/1538-4357/ab0f36 <http://dx.doi.org/10.3847/1538- 4357/ab0f36> Please note: Changes made as a result of publishing processes such as copy-editing, formatting and page numbers may not be reflected in this version. For the definitive version of this publication, please refer to the published source. You are advised to consult the publisher’s version if you wish to cite this paper. This version is being made available in accordance with publisher policies. See http://orca.cf.ac.uk/policies.html for usage policies. Copyright and moral rights for publications made available in ORCA are retained by the copyright holders. The Astrophysical Journal, 876:54 (14pp), 2019 May 1 https://doi.org/10.3847/1538-4357/ab0f36 © 2019.
    [Show full text]
  • Report of the Astroparticle Physics International Forum (Apif)
    For Official Use DSTI/STP/GSF(2016)11/FINAL Organisation de Coopération et de Développement Économiques Organisation for Economic Co-operation and Development ___________________________________________________________________________________________ English - Or. English DIRECTORATE FOR SCIENCE, TECHNOLOGY AND INNOVATION COMMITTEE FOR SCIENTIFIC AND TECHNOLOGICAL POLICY For Official Use Official For DSTI/STP/GSF(2016)11/FINAL OECD Global Science Forum REPORT OF THE ASTROPARTICLE PHYSICS INTERNATIONAL FORUM (APIF) Authors of this report are Members of the Astroparticle Physics International Forum (annex 1). Contacts: Carthage Smith ([email protected]) and Qian Dai ([email protected]). English Complete document available on OLIS in its original format - Or. English This document and any map included herein are without prejudice to the status of or sovereignty over any territory, to the delimitation of international frontiers and boundaries and to the name of any territory, city or area. REPORT OF THE ASTROPARTICLE PHYSICS INTERNATIONAL FORUM (APIF) DISCLAIMER This paper should not be reported as representing the official views of the OECD or of its member countries. The opinions expressed and arguments employed are those of the authors. It describes preliminary results or research in progress by the author(s) and is published to stimulate discussion on a broad range of issues on which the OECD works. Comments on this paper are welcomed, and may be sent to Directorate for Science, Technology and Innovation, OECD, 2 rue André-Pascal, 75775 Paris Cedex 16, France. Note to Delegations: This document is also available on OLIS under the reference code: DSTI/STP/GSF(2016)11/FINAL This document, as well as any data and map included herein, are without prejudice to the status of or sovereignty over any territory, to the delimitation of international frontiers and boundaries and to the name of any territory, city or area.
    [Show full text]