DOCSLIB.ORG

Probing Cosmology with Quad: Scientific Optimization of an Experiment to Measure the Polarization of the Cosmic Microwave Background

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Probing Cosmology with Quad: Scientific Optimization of an Experiment to Measure the Polarization of the Cosmic Microwave Background Probing cosmology with QUaD: Scientific optimization of an experiment to measure the polarization of the Cosmic Microwave Background. by Melanie Bowden A thesis submitted to the University of Wales for the degree of Doctor of Philosophy UMI Number: U584672 All rights reserved INFORMATION TO ALL USERS The quality of this reproduction is dependent upon the quality of the copy submitted. In the unlikely event that the author did not send a complete manuscript and there are missing pages, these will be noted. Also, if material had to be removed, a note will indicate the deletion. Dissertation Publishing UMI U584672 Published by ProQuest LLC 2013. Copyright in the Dissertation held by the Author. Microform Edition © ProQuest LLC. All rights reserved. This work is protected against unauthorized copying under Title 17, United States Code. ProQuest LLC 789 East Eisenhower Parkway P.O. Box 1346 Ann Arbor, Ml 48106-1346 DECLARATION This work has not previously been accepted in substance for any degree and is not being concurrentlylcurrentiy submittedsubmitted inp candidaturecan for any degree. Signed D ate.... STATEMENT 1 The QUaD project is a collaboration between a number of instutioos involving a large number of people involved in the instrument design and manufacture and the data analysis pipeline. 1 have been involved only in the data analysis and science analysis and have played no part in the experimental side of the project. The work presented in this thesis is all my own work carried out under the supervision of Prof. Walter Gear (and in close collaboration with Dr. Andy Thylor and Dr. Ken Ganga) with the exception of the following: The sensitivity calculation was based on previous calculations by Prof. Walter Gear, Dr. Jamie Bode and Prof. Sarah Church. Initial versions of the Fortran code for the area optimization and parameter estimation were given to me by Dr. Andy Taylor. The code for plotting error ellipses was written by Dr. Andy Taylor. An initial version of the time-ordered data simulation code was given to me by Dr. Ken Ganga. The estimated foreground maps and sky coverage plots were made by Dr. Ken Ganga (although these have been modified slightly). The IDL software to plot the maps was written by Dr. Ken Ganga. I acknowledge the use of the CMBFAST code for making realizations of the CMB power spectra and the HEALPix CMB package was used extensively for the work in Chapters 6 and 7. I also acknowledge the use of foreground prediction code available at http://w^ ^ b ^ .upenp^edu/^max/foregrounds.html. D ate....... STATEMENT 2 I hereby give consent for my thesis, if accepted, to be available for photocopying and for inter-library loan, and for the title and summary to be made available to outside organisations. l Signed .......... Date <^£2.0..t./A£.-........ Acknowledgements This work has carried as part of the QUaD project and throughout the course of my PhD I have received help and advice from many people within the collaboration. I thank my supervisor Walter Gear for his support, particularly in the initial stages of the work, and for reading through the drafts of this thesis under tight time constraints. This work would not have been possible without the help of Andy Taylor who provided the ideas for the survey area and parameter estimation calculations and has given me numerous crash courses on cosmology, data analysis and statistics and invaluable help with applying for jobs and writing papers. Ken Ganga has given me continual help with the survey design and data simulations and has also been a constant source of moral support. I thank Mike Zemcov for his help with the data simulations, for letting me use the results of his map-making code and for useful discussions throughout the last year, Si­ mon Melhuish for looking after my computer and for his tips on how to use the English language, Tim Waskett for help with formatting this thesis and Ian Bacchus for bringing me Diet Coke. Phil Mauskopf has provided me with the motivation to still be interested in cosmology when it has started to fade away. Finally, I would like to thank Douglas for his emotional support throughout the last three years and for explaining to me how instrumentation works. Contents 1 Introduction 3 1.1 The CM B .................................................................................................................. 4 1.1.1 The CMB in a smooth U niverse ............................................................... 4 1.1.2 The CMB temperature anisotropies ........................................................ 10 1.1.3 Observing the CMB ................................................................................... 21 1.1.4 Initial conditions - inflation ..................................................................... 24 1.1.5 Status of CMB temperature observations............................................... 28 1.1.6 Key p o in ts ....................................................................................................... 31 1.2 The polarization of the CMB .............................................................................. 33 1.2.1 The Stokes p a ra m e te rs ................................................................................ 33 1.2.2 E-B decom position ...................................................................................... 35 1.2.3 Generation of CMB polarization ............................................................... 40 1.2.4 Calculating the polarization at recombination ......................................... 43 1.2.5 Secondary polarization anisotropies ......................................................... 43 1.2.6 Degeneracy b re a k in g ................................................................................... 48 1.2.7 Key p o in ts ....................................................................................................... 50 1.3 Thesis overview ......................................................................................................... 51 2 The QUaD experiment 53 2.1 Measuring CMB polarization with QUaD ............................................................. 53 2.2 The QUaD in s tru m e n t........................................................................................... 57 2.2.1 Telescope and o p t i c s ................................................................................... 57 2.2.2 Focal plane and feed horns ......................................................................... 58 2.2.3 Cryogenics ....................................................................................................... 59 2.2.4 Detectors ....................................................................................................... 62 2.2.5 Electronics ....................................................................................................... 64 2.3 Other CMB polarization experiments ................................................................. 66 2.3.1 Detections and upper l i m i t s ...................................................................... 66 2.3.2 Experiments currently in operation ............................................................. 69 CONTENTS 2.3.3 Upcoming experiments ................................................................................ ‘u 2.3.4 Planned next generation experiments ..................................................... 71 3 Astrophysical foregrounds 73 3.1 D u s t ............................................................................................................................. 76 3.2 Synchrotron ................................................................................................................ 79 3.3 Free-free em ission....................................................................................................... 82 3.4 Point sources ............................................................................................................. 82 3.5 Conclusions and Outlook ......................................................................................... 64 4 Sensitivity calculation 87 4.1 Formalism for describing random no ise ................................................................ 87 4.2 Contribution to the NEP for a bolometric experiment ........................................ 90 4.3 Derivation of photon noise for a P S B .................................................................. 91 4.4 Calculating QUaD sensitivity ................................................................................... 94 4.5 Results.......................................................................................................................... 97 5 Forecasting performance of QUaD 101 5.1 Parameter estimation theory ..................................................................................... 101 5.1.1 The likelihood function ..................................................................................101 5.1.2 Confidence limits and the Fisher matrix .................................................103 5.2 Application to CMB polarization ........................................................................... 107 5.3 Multipole coverage ..................................................................................................... 110 5.4 Including foreground models .....................................................................................I l l 5.5 Determining area of sky to observe ......................................................................
Load more

Recommended publications
  • 19 International Workshop on Low Temperature Detectors
    19th International Workshop on Low Temperature Detectors Program version 1.24 - British Summer Time 1 Date Time Session Monday 19 July 14:00 - 14:15 Introduction and Welcome 14:15 - 15:15 Oral O1: Devices 1 15:15 - 15:25 Break 15:25 - 16:55 Oral O1: Devices 1 (continued) 16:55 - 17:05 Break 17:05 - 18:00 Poster P1: MKIDs and TESs 1 Tuesday 20 July 14:00 - 15:15 Oral O2: Cold Readout 15:15 - 15:25 Break 15:25 - 16:55 Oral O2: Cold Readout (continued) 16:55 - 17:05 Break 17:05 - 18:30 Poster P2: Readout, Other Devices, Supporting Science 1 20:00 - 21:00 Virtual Tour of NIST Quantum Sensor Group Labs Wednesday 21 July 14:00 - 15:15 Oral O3: Instruments 15:15 - 15:25 Break 15:25 - 16:55 Oral O3: Instruments (continued) 16:55 - 17:05 Break 17:05 - 18:30 Poster P3: Instruments, Astrophysics and Cosmology 1 18:00 - 19:00 Vendor Exhibitor Hour Thursday 22 July 14:00 - 15:15 Oral O4A: Rare Events 1 Oral O4B: Material Analysis, Metrology, Other 15:15 - 15:25 Break 15:25 - 16:55 Oral O4A: Rare Events 1 (continued) Oral O4B: Material Analysis, Metrology, Other (continued) 16:55 - 17:05 Break 17:05 - 18:30 Poster P4: Rare Events, Materials Analysis, Metrology, Other Applications 20:00 - 21:00 Virtual Tour of NIST Cleanoom Monday 26 July 23:00 - 00:15 Oral O5: Devices 2 00:15 - 00:25 Break 00:25 - 01:55 Oral O5: Devices 2 (continued) 01:55 - 02:05 Break 02:05 - 03:30 Poster P5: MMCs, SNSPDs, more TESs Tuesday 27 July 23:00 - 00:15 Oral O6: Warm Readout and Supporting Science 00:15 - 00:25 Break 00:25 - 01:55 Oral O6: Warm Readout and Supporting Science
    [Show full text]
  • CMB Telescopes and Optical Systems to Appear In: Planets, Stars and Stellar Systems (PSSS) Volume 1: Telescopes and Instrumentation
    CMB Telescopes and Optical Systems To appear in: Planets, Stars and Stellar Systems (PSSS) Volume 1: Telescopes and Instrumentation Shaul Hanany ([email protected]) University of Minnesota, School of Physics and Astronomy, Minneapolis, MN, USA, Michael Niemack ([email protected]) National Institute of Standards and Technology and University of Colorado, Boulder, CO, USA, and Lyman Page ([email protected]) Princeton University, Department of Physics, Princeton NJ, USA. March 26, 2012 Abstract The cosmic microwave background radiation (CMB) is now firmly established as a funda- mental and essential probe of the geometry, constituents, and birth of the Universe. The CMB is a potent observable because it can be measured with precision and accuracy. Just as importantly, theoretical models of the Universe can predict the characteristics of the CMB to high accuracy, and those predictions can be directly compared to observations. There are multiple aspects associated with making a precise measurement. In this review, we focus on optical components for the instrumentation used to measure the CMB polarization and temperature anisotropy. We begin with an overview of general considerations for CMB ob- servations and discuss common concepts used in the community. We next consider a variety of alternatives available for a designer of a CMB telescope. Our discussion is guided by arXiv:1206.2402v1 [astro-ph.IM] 11 Jun 2012 the ground and balloon-based instruments that have been implemented over the years. In the same vein, we compare the arc-minute resolution Atacama Cosmology Telescope (ACT) and the South Pole Telescope (SPT). CMB interferometers are presented briefly. We con- clude with a comparison of the four CMB satellites, Relikt, COBE, WMAP, and Planck, to demonstrate a remarkable evolution in design, sensitivity, resolution, and complexity over the past thirty years.
    [Show full text]
  • The Design of the Ali CMB Polarization Telescope Receiver
    The design of the Ali CMB Polarization Telescope receiver M. Salatinoa,b, J.E. Austermannc, K.L. Thompsona,b, P.A.R. Aded, X. Baia,b, J.A. Beallc, D.T. Beckerc, Y. Caie, Z. Changf, D. Cheng, P. Chenh, J. Connorsc,i, J. Delabrouillej,k,e, B. Doberc, S.M. Duffc, G. Gaof, S. Ghoshe, R.C. Givhana,b, G.C. Hiltonc, B. Hul, J. Hubmayrc, E.D. Karpela,b, C.-L. Kuoa,b, H. Lif, M. Lie, S.-Y. Lif, X. Lif, Y. Lif, M. Linkc, H. Liuf,m, L. Liug, Y. Liuf, F. Luf, X. Luf, T. Lukasc, J.A.B. Matesc, J. Mathewsonn, P. Mauskopfn, J. Meinken, J.A. Montana-Lopeza,b, J. Mooren, J. Shif, A.K. Sinclairn, R. Stephensonn, W. Sunh, Y.-H. Tsengh, C. Tuckerd, J.N. Ullomc, L.R. Valec, J. van Lanenc, M.R. Vissersc, S. Walkerc,i, B. Wange, G. Wangf, J. Wango, E. Weeksn, D. Wuf, Y.-H. Wua,b, J. Xial, H. Xuf, J. Yaoo, Y. Yaog, K.W. Yoona,b, B. Yueg, H. Zhaif, A. Zhangf, Laiyu Zhangf, Le Zhango,p, P. Zhango, T. Zhangf, Xinmin Zhangf, Yifei Zhangf, Yongjie Zhangf, G.-B. Zhaog, and W. Zhaoe aStanford University, Stanford, CA 94305, USA bKavli Institute for Particle Astrophysics and Cosmology, Stanford, CA 94305, USA cNational Institute of Standards and Technology, Boulder, CO 80305, USA dCardiff University, Cardiff CF24 3AA, United Kingdom eUniversity of Science and Technology of China, Hefei 230026 fInstitute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049 gNational Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 hNational Taiwan University, Taipei 10617 iUniversity of Colorado Boulder, Boulder, CO 80309, USA jIN2P3, CNRS, Laboratoire APC, Universit´ede Paris, 75013 Paris, France kIRFU, CEA, Universit´eParis-Saclay, 91191 Gif-sur-Yvette, France lBeijing Normal University, Beijing 100875 mAnhui University, Hefei 230039 nArizona State University, Tempe, AZ 85004, USA oShanghai Jiao Tong University, Shanghai 200240 pSun Yat-Sen University, Zhuhai 519082 ABSTRACT Ali CMB Polarization Telescope (AliCPT-1) is the first CMB degree-scale polarimeter to be deployed on the Tibetan plateau at 5,250 m above sea level.
    [Show full text]
  • Clover: Measuring Gravitational-Waves from Inflation
    ClOVER: Measuring gravitational-waves from Inflation Executive Summary The existence of primordial gravitational waves in the Universe is a fundamental prediction of the inflationary cosmological paradigm, and determination of the level of this tensor contribution to primordial fluctuations is a uniquely powerful test of inflationary models. We propose an experiment called ClOVER (ClObserVER) to measure this tensor contribution via its effect on the geometric properties (the so-called B-mode) of the polarization of the Cosmic Microwave Background (CMB) down to a sensitivity limited by the foreground contamination due to lensing. In order to achieve this sensitivity ClOVER is designed with an unprecedented degree of systematic control, and will be deployed in Antarctica. The experiment will consist of three independent telescopes, operating at 90, 150 or 220 GHz respectively, and each of which consists of four separate optical assemblies feeding feedhorn arrays arrays of superconducting detectors with phase as well as intensity modulation allowing the measurement of all three Stokes parameters I, Q and U in every pixel. This project is a combination of the extensive technical expertise and experience of CMB measurements in the Cardiff Instrumentation Group (Gear) and Cavendish Astrophysics Group (Lasenby) in UK, the Rome “La Sapienza” (de Bernardis and Masi) and Milan “Bicocca” (Sironi) CMB groups in Italy, and the Paris College de France Cosmology group (Giraud-Heraud) in France. This document is based on the proposal submitted to PPARC by the UK groups (and funded with 4.6ML), integrated with additional information on the Dome-C site selected for the operations. This document has been prepared to obtain an endorsement from the INAF (Istituto Nazionale di Astrofisica) on the scientific quality of the proposed experiment to be operated in the Italian-French base of Dome-C, and to be submitted to the Commissione Scientifica Nazionale Antartica and to the French INSU and IPEV.
    [Show full text]
  • The Cℓover Experiment
    Invited Paper The CℓOVER Experiment L. Piccirillo1, P. Ade2, M. D. Audley3, C. Baines1, R. Battye1, M. Brown3, P. Calisse2, A. Challinor5,6, W. D. Duncan7, P. Ferreira4, W. Gear2, D. M. Glowacka3, D. Goldie3, P.K. Grimes4, M. Halpern8, V. Haynes1, G. C. Hilton7, K. D. Irwin7, B. Johnson4, M. Jones4, A. Lasenby3, P. Leahy1, J. Leech4, S. Lewis1, B. Maffei1, L. Martinis1, P. D. Mauskopf2, S. J. Melhuish1, C. E. North4, D. O'Dea3, S. Parsley2, G. Pisano1, C. D. Reintsema7, G. Savini2, R.V. Sudiwala2, D. Sutton4, A. Taylor4, G. Teleberg2, D. Titterington3, V. N. Tsaneva3, C. Tucker2, R. Watson1, S. Withington3, G. Yassin4, J. Zhang2 1 School of Physics and Astronomy, University of Manchester, UK 2 School of Physics and Astronomy, Cardiff University, UK 3 Cavendish Laboratory, University of Cambridge, Cambridge, UK 4 Astrophysics, University of Oxford, Oxford, UK 5 Institute of Astronomy, University of Cambridge, Cambridge, UK 6 DAMTP, University of Cambridge, Cambridge, UK 7 National Institute of Standards and Technology, USA 8 University of British Columbia, Canada CℓOVER is a multi-frequency experiment optimised to measure the Cosmic Microwave Background (CMB) polarization, in particular the B- mode component. CℓOVER comprises two instruments observing respectively at 97 GHz and 150/225 GHz. The focal plane of both instruments consists of an array of corrugated feed-horns coupled to TES detectors cooled at 100 mK. The primary science goal of CℓOVER is to be sensitive to gravitational waves down to r ~ 0.03 (at 3σ) in two years of operations. 1 Introduction The Cosmic Microwave Background (CMB) Radiation is a very powerful tool to study the origin and evolution of the Universe.
    [Show full text]
  • Far Sidelobes from Baffles and Telescope Support Structures in the Atacama Cosmology Telescope
    Far Sidelobes from Baffles and Telescope Support Structures in the Atacama Cosmology Telescope Patricio A. Gallardoa, Nicholas F. Cothardb, Roberto Pudduc, Rolando Dünnerd, Brian J. Koopmana, Michael D. Niemacka, Sara M. Simone, and Edward J. Wollackf aDepartment of Physics, Cornell University, Ithaca, NY 14853 USA bDepartment of Applied and Engineering Physics, Cornell University, Ithaca, NY 14853 USA cInstituto de Astrofísica, Pontificia Universidad Católica de Chile, Macul, Santiago, Chile dInstituto de Astrofísica y Centro de Astroingeniería, Facultad de Física, Pontificia Universidad Católica de Chile, 7820436 Macul, Santiago, Chile eDepartment of Physics, University of Michigan, Ann Arbor, MI, 48103 fNASA/Goddard Space Flight Center, Greenbelt, MD, USA ABSTRACT The Atacama Cosmology Telescope (ACT) is a 6 m telescope located in the Atacama Desert, designed to measure the cosmic microwave background (CMB) with arcminute resolution. ACT, with its third generation polarization sensitive array, Advanced ACTPol, is being used to measure the anisotropies of the CMB in five frequency bands in large areas of the sky (∼ 15; 000 deg2). These measurements are designed to characterize the large scale structure of the universe, test cosmological models and constrain the sum of the neutrino masses. As the sensitivity of these wide surveys increases, the control and validation of the far sidelobe response becomes increasingly important and is particularly challenging as multiple reflections, spillover, diffraction and scattering become difficult to model and characterize at the required levels. In this work, we present a ray trace model of the ACT upper structure which is used to describe much of the observed far sidelobe pattern. This model combines secondary mirror spillover measurements with a 3D CAD model based on photogrammetry measurements to simulate the beam of the camera and the comoving ground shield.
    [Show full text]
  • Development and Preliminary Results of Point Source Observations
    The Atacama Cosmology Telescope: Development and Preliminary Results of Point Source Observations Ryan P. Fisher A DISSERTATION PRESENTED TO THE FACULTY OF PRINCETON UNIVERSITY IN CANDIDACY FOR THE DEGREE OF DOCTOR OF PHILOSOPHY RECOMMENDED FOR ACCEPTANCE BY THE DEPARTMENT OF PHYSICS [Adviser: Joseph W. Fowler] November 2009 c Copyright by Ryan Patrick Fisher, 2009. All rights reserved. Abstract The Atacama Cosmology Telescope (ACT) is a six meter diameter telescope designed to measure the millimeter sky with arcminute angular resolution. The instrument is cur- rently conducting its third season of observations from Cerro Toco in the Chilean Andes. The primary science goal of the experiment is to expand our understanding of cosmology by mapping the temperature fluctuations of the Cosmic Microwave Background (CMB) at angular scales corresponding to multipoles up to ` ∼ 10000: The primary receiver for current ACT observations is the Millimeter Bolometer Ar- ray Camera (MBAC). The instrument is specially designed to observe simultaneously at 148 GHz, 218 GHz and 277 GHz. To accomplish this, the camera has three separate de- tector arrays, each containing approximately 1000 detectors. After discussing the ACT experiment in detail, a discussion of the development and testing of the cold readout elec- tronics for the MBAC is presented. Currently, the ACT collaboration is in the process of generating maps of the microwave sky using our first and second season observations. The analysis used to generate these maps requires careful data calibration to produce maps of the arcminute scale CMB tem- perature fluctuations. Tests and applications of several elements of the ACT calibrations are presented in the context of the second season observations.
    [Show full text]
  • THE ATACAMA Cosi'vl0logy TELESCOPE: the RECEIVER and INSTRUMENTATION L2 D
    https://ntrs.nasa.gov/search.jsp?R=20120002550 2019-08-30T19:06:35+00:00Z CORE Metadata, citation and similar papers at core.ac.uk Provided by NASA Technical Reports Server THE ATACAMA COSi'vl0LOGY TELESCOPE: THE RECEIVER AND INSTRUMENTATION L2 D. S. SWETZ , P. A. R. ADE\ j'vI. A !\fIRrl, J. \V'. ApPEL" E. S. BATTISTELLlfi,j, B. BURGERI, J. CHERVENAK', 2 lVI. J. DEVLIN], S. R. DICKER]. \V. B. DORIESE , R. DUNNER', T. ESSINGER-HILEMAN'. R. P. FISHER:', J. \V. FOWLER'. 4 2 1 lVI. HALPERN ,!.VI. HASSELFIELD4, G. C. HILTON , A. D. HINCKS\ K. D. IRWIN2. N. JAROSIK', M. KAlIL', J. KLEIN , . ull 11 I2 l l u 1 J. J\1. LAd "" M. LIMON , T. A. l'vIARRIAGE . D. MARSDEN , K. J\IARTOCCI : , P. J\IAUSKOPF: , H. MOSELEY', I4 2 C. B. NETTERFIELD , J\1. D. NIEMACK " l'vI. R. NOLTA ,L. A. PAGE". L. PARKER'. S. T. STAGGS", O. STRYZAK', 1 U jHi E. R. SWlTZER : , R. THORNTON • C. TUCKER'], E. \VOLLACK', Y. ZHAO" Draft version July 5, 2010 ABSTRACT The Atacama Cosmology Telescope was designed to measure small-scale anisotropies in the Cosmic Microwave Background and detect galaxy clusters through the Sunyaev-Zel'dovich effect. The instru­ ment is located on Cerro Taco in the Atacama Desert, at an altitude of 5190 meters. A six-met.er off-axis Gregorian telescope feeds a new type of cryogenic receiver, the Millimeter Bolometer Array Camera. The receiver features three WOO-element arrays of transition-edge sensor bolometers for observations at 148 GHz, 218 GHz, and 277 GHz.
    [Show full text]
  • A Millimeter-Wave Galactic Plane Survey with the BICEP Polarimeter
    A Millimeter-wave Galactic Plane Survey with the BICEP Polarimeter The Harvard community has made this article openly available. Please share how this access benefits you. Your story matters Citation Bierman, E. M, J. Kovac et al. 2011. "A Millimeter-Wave Galactic Plane Survey with the BICEP Polarimeter." The Astrophysical Journal 741: 81. Published Version doi:10.1088/0004-637X/741/2/81 Citable link http://nrs.harvard.edu/urn-3:HUL.InstRepos:12712844 Terms of Use This article was downloaded from Harvard University’s DASH repository, and is made available under the terms and conditions applicable to Other Posted Material, as set forth at http:// nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of- use#LAA The Astrophysical Journal, 741:81 (21pp), 2011 November 10 doi:10.1088/0004-637X/741/2/81 C 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. A MILLIMETER-WAVE GALACTIC PLANE SURVEY WITH THE BICEP POLARIMETER E. M. Bierman1, T. Matsumura2, C. D. Dowell2,3, B. G. Keating1,P.Ade4, D. Barkats5, D. Barron1, J. O. Battle3, J. J. Bock2,3,H.C.Chiang2,6, T. L. Culverhouse2, L. Duband7,E.F.Hivon8, W. L. Holzapfel9, V. V. Hristov2, J. P. Kaufman1, J. M. Kovac2,10,C.L.Kuo11,A.E.Lange2, E. M. Leitch3,P.V.Mason2, N. J. Miller1, H. T. Nguyen3, C. Pryke12,S.Richter2,G.M.Rocha2, C. Sheehy12, Y. D. Takahashi9, and K. W. Yoon13 1 University of California, San Diego, USA; [email protected] 2 California Institute of Technology, USA 3 Jet Propulsion Laboratory, USA 4 University of Wales, UK 5 Joint ALMA Office-NRAO,
    [Show full text]
  • Quad: a Millimeter-Wave Polarimeter for Observation of the Cosmic Microwave Background Radiation
    QUAD: A MILLIMETER-WAVE POLARIMETER FOR OBSERVATION OF THE COSMIC MICROWAVE BACKGROUND RADIATION A DISSERTATION SUBMITTED TO THE DEPARTMENT OF PHYSICS AND THE COMMITTEE ON GRADUATE STUDIES OF STANFORD UNIVERSITY IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY James R. Hinderks August 2005 c Copyright by James R. Hinderks 2005 All Rights Reserved ii I certify that I have read this dissertation and that, in my opinion, it is fully adequate in scope and quality as a dissertation for the degree of Doctor of Philosophy. Prof. Sarah E. Church Principal Adviser I certify that I have read this dissertation and that, in my opinion, it is fully adequate in scope and quality as a dissertation for the degree of Doctor of Philosophy. Prof. Giorgio Gratta I certify that I have read this dissertation and that, in my opinion, it is fully adequate in scope and quality as a dissertation for the degree of Doctor of Philosophy. Prof. Steven Kahn Approved for the University Committee on Graduate Studies. iii iv Abstract This thesis describes the design and performance of the QUaD experiment and presents some of its earliest results. QUaD is a millimeter-wavelength polarime- ter designed for observing the Cosmic Microwave Background (CMB). QUaD was commissioned at the MAPO observatory at the Amundsen-Scott South Pole Station in the Austral Summer of 2004/2005, achieved first light in Feb 2005, and began science observation in May. QUaD observes the CMB with an array of 31 polarization-sensitive Neutron Transmutation Doped (NTD) germanium bolometers split between two frequency bands centered at 100 and 150 GHz.
    [Show full text]
  • The Quad Experiment
    New Astronomy Reviews 50 (2006) 984–992 www.elsevier.com/locate/newastrev The QUaD experiment C. Pryke Kavli Institute for Cosmological Physics, Department of Astronomy and Astrophysics, The Enrico Fermi Institute, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637-1433, USA Available online 7 November 2006 For the QUaD Collaboration. Abstract QUaD is a 31 pixel array of polarization sensitive bolometer pairs coupled to a 2.6 m Cassegrain radio telescope. The telescope is attached to the mount originally built for the DASI experiment and located at the South Pole. The telescope system is described along with details of instrumental characterization studies which we have performed. A first season of CMB observations is complete and the second season underway. Details of the current status of these observations and their analysis are presented. Ó 2006 Published by Elsevier B.V. Keywords: Cosmic microwave background; Polarization Contents 1. Introduction . 985 2. The QUaD experiment. 986 2.1. Telescope.............................................................................. 986 2.2. Focalpane............................................................................. 986 2.3. Telescopescanning....................................................................... 987 3. Instrument performance and characterization . 987 3.1. Gaincalibrationandstability................................................................ 987 3.2. Atmosphericrejection..................................................................... 988 3.3.
    [Show full text]
  • The Atacama Cosmology Telescope: Lensing of CMB Temperature and Polarization Derived from Cosmic Infrared Background Cross-Correlation
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Haverford College: Haverford Scholarship Haverford College Haverford Scholarship Faculty Publications Physics 2015 The Atacama Cosmology Telescope: Lensing of CMB Temperature and Polarization Derived from Cosmic Infrared Background Cross-Correlation Alexander van Engelen Blake D. Sherwin Neelima Sehgal Graeme E. Addison Bruce Partridge Haverford College, [email protected] Follow this and additional works at: https://scholarship.haverford.edu/physics_facpubs Repository Citation van Engelen, A., et al. (2015). "The Atacama Cosmology Telescope: Lensing of CMB Temperature and Polarization Derived from Cosmic Infrared Background Cross-Correlation," Astrophysical Journal 808 (1). This Journal Article is brought to you for free and open access by the Physics at Haverford Scholarship. It has been accepted for inclusion in Faculty Publications by an authorized administrator of Haverford Scholarship. For more information, please contact [email protected]. The Astrophysical Journal, 808:7 (9pp), 2015 July 20 doi:10.1088/0004-637X/808/1/7 © 2015. The American Astronomical Society. All rights reserved. THE ATACAMA COSMOLOGY TELESCOPE: LENSING OF CMB TEMPERATURE AND POLARIZATION DERIVED FROM COSMIC INFRARED BACKGROUND CROSS-CORRELATION Alexander van Engelen1,2, Blake D. Sherwin3, Neelima Sehgal2, Graeme E. Addison4, Rupert Allison5, Nick Battaglia6, Francesco de Bernardis7, J. Richard Bond1, Erminia Calabrese5, Kevin Coughlin8, Devin Crichton9, Rahul Datta8, Mark J. Devlin10, Joanna Dunkley5, Rolando Dünner11, Patricio Gallardo7, Emily Grace12, Megan Gralla9, Amir Hajian1, Matthew Hasselfield4,13, Shawn Henderson7, J. Colin Hill14, Matt Hilton15, Adam D. Hincks4, Renée Hlozek13, Kevin M. Huffenberger16, John P. Hughes17, Brian Koopman7, Arthur Kosowsky18, Thibaut Louis5, Marius Lungu10, Mathew Madhavacheril2, Loïc Maurin11, Jeff McMahon8, Kavilan Moodley15, Charles Munson8, Sigurd Naess5, Federico Nati19, Laura Newburgh20, Michael D.
    [Show full text]