DOCSLIB.ORG

The POLARBEAR Experiment Probing the Cosmic Microwave Background Polarization

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The POLARBEAR Experiment Probing the Cosmic Microwave Background Polarization The POLARBEAR experiment probing the cosmic microwave background polarization Davide Poletti (APC, Paris) on behalf of the POLARBEAR Collaboration 14 Dec 2015 ! 28th Texas Symposium on Relativistic Astrophysics POLARBEAR Collaboration UC Berkeley UC San Diego KEK McGill University SISSA Brian Barch Chris Aleman Yoshiki Akiba Matt Dobbs Carlo Baccigalupi Yuji Chinone Kam Arnold Takaho Hamada Adam Gilbert Giulio Fabbian Ari Cukierman Matt Atlas Masaya Hasegawa Josh Montgomery Giuseppe Puglisi Tijmen de Haan Darcy Barron Kaori Hattori Graeme Smecher Josquin Errard Tucker Elleflot Masashi Hazumi JAXA Neil Goeckner-Wald George Fuller Yuki Inoue Dalhousie Tomotake Matsumura John Groh Logan Howe Haruki Nishino Scott Chapman UC Irvine Grantland Hall Jon Kaufman Yuuko Segawa Colin Ross Chang Feng Charles Hill Kavon Kazemzadeh Jun-ichi Suzuki Kaja Rotermund William Holzapfel Brian Keating Osamu Tajima Alexei Tikhomirov National Institute Yasuto Hori David Leon Satoru Takakura for Fusion Science Oliver Jeong Lindsay Lowry Sayuri Takatori Lawrence Suguru Takada Adrian Lee Frederick Matsuda Takayuki Tomaru Berkeley NL Mike Myers Martin Navaroli Julian Borrill Reijo Keskitalo Cardiff University Chris Raum Hans Paar Laboratoire Peter Ade Paul Richards Gabriel Rebeiz Astroparticule & Theodore Kisner Blake Sherwin Praween Siritanasak Cosmologie Akito Kusaka NASA Goddard Ian Shirley Nathan Stebor Maude Le Jeune Eric Linder Nathan Miller Julien Peloton Bryan Steinbach Brandon Wilson Kavli IPMU Aritoki Suzuki Amit Yadav Davide Poletti Princeton Radek Stompor Takuro Fujino Zigmund Kermish Nathan Whitehorn Alex Zahn Fumiya Irie Oliver Zahn Nobuhiko Katayama CU Boulder Argonne NL Católica (PUC) Kuniyoshi Mizukami Imperial College Nils Halverson Amy Bender David Boettger Tetsu Yamashita Anne Ducout Greg Jaehnig Rolando Dunner Stephen Feeney David Schenck U. Melbourne Andrew Jaffe Christian Reichardt And many more in years past ✦ B-modes science and measurements ✦ The POLARBEAR experiment ✦ First season’s results ✦ POLARBEAR 2 and Simons array Davide Poletti - POLARBEAR collaboration 3 The Cosmic Microwave Background The CMB: • picture of the 380,000 years old universe • information on the inflationary phase Adapted from NASA/WMAP Temperature anisotropies: • ΛCDM confirmed • Cosmological information exploited Planck Collaboration Davide Poletti - POLARBEAR collaboration 4 The CMB polarization Polarization field ➱ Q, U Stokes parameters ! y Q < 0 ! U > 0 x ! ! Q > 0 ! U < 0 ! ➱ Decomposed in E and B modes Davide Poletti - POLARBEAR collaboration 5 Primordial B-modes Perturbations at the last scattering surface: • Scalar ➱ E only (to linear order) • Tensor ➱ E and B Tensor perturbation after inflation: • r! Energy scale of inflation ( ~1016 GeV for r~0.1)! • nt" Consistency relation (r = - 8 nt) Davide Poletti - POLARBEAR collaboration 6 Lensing B-Modes ESA/Planck Acquaviva and Baccigalupi (2006) D D φ(nˆ)= 2 dD s − (Dnˆ,D) − DDs Different dark! Z energy scenarios d = φ r δE(l; l0)= [E(l0) cos 2' B(l0)sin2' ][l (l l0)]φ(l l0) − l0l − l0l · − − δB(l; l0)= [E(l0)sin2' + B(l0) cos 2' ][l (l l0)]φ(l l0) − l0l l0l · − − Davide Poletti - POLARBEAR collaboration 7 Lensing B-Modes ESA/Planck Acquaviva and Baccigalupi (2006) D D φ(nˆ)= 2 dD s − (Dnˆ,D) − DDs Different dark! Z energy scenarios d = φ r δE(l; l0)= [E(l0) cos 2' B(l0)sin2' ][l (l l0)]φ(l l0) − l0l − l0l · − − δB(l; l0)= [E(l0)sin2' + B(l0) cos 2' ][l (l l0)]φ(l l0) − l0l l0l · − − Davide Poletti - POLARBEAR collaboration 8 Measurements of the BB power spectrum Mar 2014 2015 102 DASI WMAP-9yr CBI QUaD MAXIPOL QUIET-Q BOOMERanG QUIET-W CAPMAP BICEP1-3yr 1 ) 10 2 K µ ) 2 K )( ! 0 π 10 ) ( (2 / /(2 BB l BB ` -1 C 10 l(l+1)C + 1) ⇥ ( ⇥ 10-2 r=0.2 r=0.025 10-3 10 100 1000 Multipole Moment, ell Davide Poletti - POLARBEAR collaboration 9 Measurements of the BB power spectrum Mar 2014 2015 POLARBEAR! 10 Mar 102 DASI QUaD CBI QUIET-Q MAXIPOL QUIET-W BOOMERanG BICEP1-3yr CAPMAP POLARBEAR 1 WMAP-9yr ) 10 2 K µ ) 2 K )( ! 0 π 10 ) ( (2 / /(2 BB l BB ` -1 C 10 l(l+1)C + 1) POLARBEAR ⇥ ( ⇥ 10-2 r=0.2 r=0.025 10-3 10 100 1000 Multipole Moment, ell Davide Poletti - POLARBEAR collaboration 10 Measurements of the BB power spectrum Mar 2014 2015 BICEP2! 17 Mar 102 DASI QUaD CBI QUIET-Q MAXIPOL QUIET-W BOOMERanG BICEP1-3yr CAPMAP BICEP2-3yr 1 WMAP-9yr POLARBEAR ) 10 2 K µ ) 2 K )( ! 0 π 10 ) ( (2 / /(2 BB l BB ` -1 C 10 l(l+1)C + 1) BICEP2 POLARBEAR ⇥ ( ⇥ 10-2 r=0.2 r=0.025 10-3 10 100 1000 Multipole Moment, ell Davide Poletti - POLARBEAR collaboration 11 Measurements of the BB power spectrum Mar 2014 2015 ACTPol! 21 May 102 DASI QUIET-Q CBI QUIET-W MAXIPOL BICEP1-3yr BOOMERanG ACTPol 1 CAPMAP BICEP2-3yr 10 WMAP-9yr POLARBEAR ACTPol ) QUaD 2 K µ ) 0 2 10 K )( ! π ) ( (2 / -1 /(2 10 BB l BB ` C BICEP2 POLARBEAR -2 l(l+1)C 10 r=0.20 + 1) ⇥ ( ⇥ 10-3 r=0.025 10-4 10 100 1000 Multipole Moment, ell Davide Poletti - POLARBEAR collaboration 12 Measurements of the BB power spectrum Mar 2014 2015 BICEP2 - Keck Array - Planck! 2 Feb 102 DASI QUIET-Q CBI QUIET-W MAXIPOL BICEP1-3yr BOOMERanG ACTPol 1 CAPMAP BKP 10 WMAP-9yr POLARBEAR ACTPol ) QUaD 2 K µ ) 0 2 10 K )( ! π ) ( (2 / -1 /(2 10 BB l BB ` C POLARBEAR -2 BKP l(l+1)C 10 + 1) ⇥ ( ⇥ 10-3 10-4 10 100 1000 Multipole Moment, ell Davide Poletti - POLARBEAR collaboration 13 Measurements of the BB power spectrum Mar 2014 2015 SPTPol! 8 Mar 102 DASI QUIET-Q CBI QUIET-W MAXIPOL BICEP1-3yr BOOMERanG ACTPol 1 CAPMAP BKP 10 WMAP-9yr SPTpol ACTPol ) QUaD POLARBEAR 2 K µ ) 0 2 10 K )( ! π ) ( (2 / -1 /(2 10 SPTpol BB l BB ` C POLARBEAR -2 BKP l(l+1)C 10 + 1) ⇥ ( r=0.09 ⇥ 10-3 10-4 10 100 1000 Multipole Moment, ell Davide Poletti - POLARBEAR collaboration 14 Measurements of the BB power spectrum Mar 2014 2015 BICEP2 / Keck! 30 Oct 102 DASI QUIET-Q CBI QUIET-W MAXIPOL BICEP1-3yr BOOMERanG ACTPol 1 CAPMAP BK14 10 WMAP-9yr SPTpol ) QUaD POLARBEAR 2 K ACTPol µ ) 0 2 10 K )( ! π ) ( (2 / -1 /(2 10 SPTpol BB l BB ` C POLARBEAR -2 BK14 l(l+1)C 10 + 1) ⇥ ( ⇥ r=0.07 10-3 10-4 10 100 1000 Multipole Moment, ell Davide Poletti - POLARBEAR collaboration 15 Measurements of the BB power spectrum Mar 2014 2015 BICEP2 / Keck! 30 Oct 102 DASI QUIET-Q CBI QUIET-W MAXIPOL BICEP1-3yr BOOMERanG ACTPol 1 CAPMAP BK14 10 WMAP-9yr SPTpol ) QUaD POLARBEAR 2 K ACTPol µ ) 0 2 10 K )( ! π ) ( (2 / -1 /(2 10 SPTpol BB l BB ` Plus measurementsC through! POLARBEAR cross-correlation!-2 ! BK14 l(l+1)C 10 • SPTPol+ 1) ! ⇥ ( • POLARBEAR⇥ ! r=0.07 -3 • ACTPol! 10 • Planck 10-4 10 100 1000 Multipole Moment, ell Davide Poletti - POLARBEAR collaboration 16 ✦ B-modes science and measurements ✦ The POLARBEAR experiment! ✦ First season’s results ✦ POLARBEAR 2 and Simons array Davide Poletti - POLARBEAR collaboration 17 POLARBEAR experiment • CMB B-modes dedicated experiment • Atacama desert (~5200 m altitude) ‣ Access to 80% of the sky ‣ Dry atmosphere ‣ Targeting both primordial and lensing B-modes Crab Nebula Planck 857GHz (TauA) FIRST SEASON polarization angles calibrator • Period: May 2012 to June 2013 PB1-RA23 HA • Target: PB1-RA12 HA Overlap w/ QUIET, deep integration of Overlap w/ Herschel Herschel Atlas PB1-RA4p5 3 patches 5 deg x 5 deg Overlap w/ QUIET, BOSS Davide Poletti - POLARBEAR collaboration 18 ⇣.✏⇧⌃⌦↵↵⌅↵ ⇤⌥↵⌃↵⇥⌃⌃ 197 IA: azimuth encoder zero-point IE: elevation encoder zero-point TF: telescope flexure that describes the mechanical non-idealities affecting the telescope pointing. The parameters are reconstructed through a linear model assuming similar to the standard mapmaking equation ∆az d = As + n (9.1) ∆el ⇥ where the vector s contains the parameter to be estimated and the noise term is such that its noise correlation is the identity matrix nT n = 1.(9.2) This is equivalent to the assumption that the source does not move during Instrumentalthe design raster scan. Details on the role of each parameter and on the pointing matrix A are discussed in more detail in Errard (2012). The rms residual with between the telescope pointing after the pointing model correction is applied has an amplitude of 17arcsec in both azimuth and elevation, lead- ing to a total rms error of 25arcsec. Measurements of the product of the integrated bandwidth and fractional Array performance throughput, ⇥⇤ were also made from the beam maps observation previ- ously discussed, as well as from earlier test of the receiver in the lab and from elevation nods of the telescope. The fractional throughput is a mea- sure of the percentage of the power seen by a detector from a source at the input of the receiver compared to what would be seen if the detector had perfect efficiency to2.5 Meters that same source. The overall loss is due to expected efficiencies of the detectors and optical componentsPrimary: along the 3.5m optical path. Laboratory measurements of ⇥⇤ are consistent with a ⇥ = 37% given the measured 37GHz integrated bandwidth. Measurements of ⇥⇤ made in the field are consistent with these values. The design bolometer noise equivalent temperatures (NET) of table 9.1 are slightly degraded due to bolometer saturation powers and atmospheric con- ditions. Once the relative gain calibration for a pair of detector is available we can compute the timestream noise in polarization and temperature for the Q or U stokes parameters in individual pixels. Since the two orthogonal antennas in a focal plane pixelHuan (from now Tran on referredTelescope to as top (t) and bottom (b) ) measure two orthogonal polarization, their timestream model is t Hex Module d (t)=gtop [I(nˆ (t)) + Q(nˆ (t)) cos(2⌅(t)) + U(nˆ (t)) sin(2⌅(t))] b d (t)=gbot [I(nˆ (t)) Q(nˆ (t)) cos(2⌅(t)) U(nˆ (t)) sin(2⌅(t))] (9.3) 6mm lenslet Fourier transforming the semi-differenceMicrostrip of the top and bottom detectors Antenna allows us to see how well the unpolarizedFilter atmosphere is suppressed at low frequencies.
Load more

Recommended publications
  • Proceedings of Spie
    PROCEEDINGS OF SPIE SPIEDigitalLibrary.org/conference-proceedings-of-spie Survey strategy optimization for the Atacama Cosmology Telescope De Bernardis, F., Stevens, J., Hasselfield, M., Alonso, D., Bond, J. R., et al. F. De Bernardis, J. R. Stevens, M. Hasselfield, D. Alonso, J. R. Bond, E. Calabrese, S. K. Choi, K. T. Crowley, M. Devlin, J. Dunkley, P. A. Gallardo, S. W. Henderson, M. Hilton, R. Hlozek, S. P. Ho, K. Huffenberger, B. J. Koopman, A. Kosowsky, T. Louis, M. S. Madhavacheril, J. McMahon, S. Næss, F. Nati, L. Newburgh, M. D. Niemack, L. A. Page, M. Salatino, A. Schillaci, B. L. Schmitt, N. Sehgal, J. L. Sievers, S. M. Simon, D. N. Spergel, S. T. Staggs, A. van Engelen, E. M. Vavagiakis, E. J. Wollack, "Survey strategy optimization for the Atacama Cosmology Telescope," Proc. SPIE 9910, Observatory Operations: Strategies, Processes, and Systems VI, 991014 (15 July 2016); doi: 10.1117/12.2232824 Event: SPIE Astronomical Telescopes + Instrumentation, 2016, Edinburgh, United Kingdom Downloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 06 Oct 2020 Terms of Use: https://www.spiedigitallibrary.org/terms-of-use Survey strategy optimization for the Atacama Cosmology Telescope F. De Bernardisa, J. R. Stevensa, M. Hasselfieldb,c, D. Alonsod, J. R. Bonde, E. Calabresed, S. K. Choif, K. T. Crowleyf, M. Devling, J. Dunkleyd, P. A. Gallardoa, S. W. Hendersona, M. Hiltonh, R. Hlozeki, S. P. Hof, K. Huffenbergerj, B. J. Koopmana, A. Kosowskyk, T. Louisl, M. S. Madhavacherilm, J. McMahonn, S. Naessd, F. Natig, L. Newburghi, M. D. Niemacka, L. A. Pagef, M. Salatinof, A.
    [Show full text]
  • The Q/U Imaging Experiment (QUIET): the Q-Band Receiver Array Instrument and Observations by Laura Newburgh Advisor: Professor Amber Miller
    The Q/U Imaging ExperimenT (QUIET): The Q-band Receiver Array Instrument and Observations by Laura Newburgh Advisor: Professor Amber Miller Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Graduate School of Arts and Sciences COLUMBIA UNIVERSITY 2010 c 2010 Laura Newburgh All Rights Reserved Abstract The Q/U Imaging ExperimenT (QUIET): The Q-band Receiver Array Instrument and Observations by Laura Newburgh Phase I of the Q/U Imaging ExperimenT (QUIET) measures the Cosmic Microwave Background polarization anisotropy spectrum at angular scales 25 1000. QUIET has deployed two independent receiver arrays. The 40-GHz array took data between October 2008 and June 2009 in the Atacama Desert in northern Chile. The 90-GHz array was deployed in June 2009 and observations are ongoing. Both receivers observe four 15◦ 15◦ regions of the sky in the southern hemisphere that are expected × to have low or negligible levels of polarized foreground contamination. This thesis will describe the 40 GHz (Q-band) QUIET Phase I instrument, instrument testing, observations, analysis procedures, and preliminary power spectra. Contents 1 Cosmology with the Cosmic Microwave Background 1 1.1 The Cosmic Microwave Background . 1 1.2 Inflation . 2 1.2.1 Single Field Slow Roll Inflation . 3 1.2.2 Observables . 4 1.3 CMB Anisotropies . 6 1.3.1 Temperature . 6 1.3.2 Polarization . 7 1.3.3 Angular Power Spectrum Decomposition . 8 1.4 Foregrounds . 14 1.5 CMB Science with QUIET . 15 2 The Q/U Imaging ExperimenT Q-band Instrument 19 2.1 QUIET Q-band Instrument Overview .
    [Show full text]
  • Maturity of Lumped Element Kinetic Inductance Detectors For
    Astronomy & Astrophysics manuscript no. Catalano˙f c ESO 2018 September 26, 2018 Maturity of lumped element kinetic inductance detectors for space-borne instruments in the range between 80 and 180 GHz A. Catalano1,2, A. Benoit2, O. Bourrion1, M. Calvo2, G. Coiffard3, A. D’Addabbo4,2, J. Goupy2, H. Le Sueur5, J. Mac´ıas-P´erez1, and A. Monfardini2,1 1 LPSC, Universit Grenoble-Alpes, CNRS/IN2P3, 2 Institut N´eel, CNRS, Universit´eJoseph Fourier Grenoble I, 25 rue des Martyrs, Grenoble, 3 Institut de Radio Astronomie Millim´etrique (IRAM), Grenoble, 4 LNGS - Laboratori Nazionali del Gran Sasso - Assergi (AQ), 5 Centre de Sciences Nucl´eaires et de Sciences de la Mati`ere (CSNSM), CNRS/IN2P3, bat 104 - 108, 91405 Orsay Campus Preprint online version: September 26, 2018 ABSTRACT This work intends to give the state-of-the-art of our knowledge of the performance of lumped element kinetic inductance detectors (LEKIDs) at millimetre wavelengths (from 80 to 180 GHz). We evaluate their optical sensitivity under typical background conditions that are representative of a space environment and their interaction with ionising particles. Two LEKID arrays, originally designed for ground-based applications and composed of a few hundred pixels each, operate at a central frequency of 100 and 150 GHz (∆ν/ν about 0.3). Their sensitivities were characterised in the laboratory using a dedicated closed-cycle 100 mK dilution cryostat and a sky simulator, allowing for the reproduction of realistic, space-like observation conditions. The impact of cosmic rays was evaluated by exposing the LEKID arrays to alpha particles (241Am) and X sources (109Cd), with a read-out sampling frequency similar to those used for Planck HFI (about 200 Hz), and also with a high resolution sampling level (up to 2 MHz) to better characterise and interpret the observed glitches.
    [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]
  • 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]
  • Arxiv:1412.0626V1 [Astro-Ph.CO] 1 Dec 2014 Versity, 3400 N
    Draft: December 2, 2014 Preprint typeset using LATEX style emulateapj v. 05/12/14 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 Dunner¨ 11, Emily Grace12, Megan Gralla9, Amir Hajian1, Matthew Hasselfield13,4, Shawn Henderson7, J. Colin Hill14, Matt Hilton15, Adam D. Hincks4, Renee´ Hlozek13, Kevin M. Huffenberger16, John P. Hughes17, Brian Koopman7, Arthur Kosowsky18, Thibaut Louis5, Marius Lungu10, Mathew Madhavacheril2, Lo¨ıc Maurin11, Jeff McMahon8, Kavilan Moodley15, Charles Munson8, Sigurd Naess5, Federico Nati19, Laura Newburgh20, Michael D. Niemack7, Michael R. Nolta1, Lyman A. Page12, Christine Pappas12, Bruce Partridge21, Benjamin L. Schmitt10, Jonathan L. Sievers22,23,12, Sara Simon12, David N. Spergel13, Suzanne T. Staggs12, Eric R. Switzer24,1, Jonathan T. Ward10, Edward J. Wollack24 Draft: December 2, 2014 ABSTRACT We present a measurement of the gravitational lensing of the Cosmic Microwave Background (CMB) temperature and polarization fields obtained by cross-correlating the reconstructed convergence signal from the first season of ACTPol data at 146 GHz with Cosmic Infrared Background (CIB) fluctu- ations measured using the Planck satellite. Using an overlap area of 206 square degrees, we detect gravitational lensing of the CMB polarization by large-scale structure at a statistical significance of 4:5σ. Combining both CMB temperature and polarization data gives a lensing detection at 9:1σ sig- nificance. A B-mode polarization lensing signal is present with a significance of 3:2σ.
    [Show full text]
  • Muse: a Novel Experiment for CMB Polarization Measurement Using Highly Multimoded Bolometers
    The Atacama B-mode Search Status and Prospect CMB 2013 June 11th, 2013, Okinawa, Japan Akito Kusaka (Princeton University) for ABS Collaboration Before starting my talk… Atmosphere is unpolarized ABS (Atacama B-mode Search) Princeton, Johns Hopkins, NIST, UBC, U. Chile What is ABS? Ground based CMB polarization (with T sensitivity) Angular scale: l~100(~2), B-mode from GW TES bolometer at 150 GHz › 240 pixel / 480 bolometers › ~80% of channels are regularly functional › NEQ ~ 30 mKs (w/ dead channels, pol. efficiency included) Unique Systematic error mitigation › Cold optics › Continuously rotating half-wave plate Site Chile, Cerro Toco › ~5150 m. › Extremely low moisture › Year-round access › Observing throughout the year › And day and night ACT, ABS, PolarBear, CLASS Cerro Chajnantor 5612 m (5150 m) Cerro Toco 5600 m TAO, CCAT Google Earth / Google Map / Google Earth 1 km APEX QUIET, CBI ALMA (5050 m) ASTE & NANTEN2 (4800 m) Possible combined analysis among CMB experiments Many figures / pictures are from theses of ABS instrument T. Essinger-Hileman and J. W. Appel (+ K. Visnjic and L. P. Parker soon) Optics 4 K cooled side-fed Dragone dual reflector. ~60 cm diameter mirrors. 25 cm aperture diameter. Optics Aperture The optics maximize throughput for small aperture 12 radius field of view Good image quality across the wide field of view ABS focal plane Feedhorn coupled Focal plane ~300 mK Polarization sensitive TES Ex TES Inline filter OMT Ey TES 1.6 mm 5 mm ~30 cm Fabricated at NIST Focal Plane Elements Individually machined
    [Show full text]
  • Delft University of Technology Groundbird Observation of CMB
    Delft University of Technology GroundBIRD Observation of CMB Polarization with a Rapid Scanning and MKIDs Nagasaki, T.; Choi, J.; Génova-Santos, R. T.; Karatsu, K.; Lee, K.; Naruse, M.; Suzuki, J.; Taino, T.; Tomita, N.; More Authors DOI 10.1007/s10909-018-2077-y Publication date 2018 Document Version Accepted author manuscript Published in Journal of Low Temperature Physics Citation (APA) Nagasaki, T., Choi, J., Génova-Santos, R. T., Karatsu, K., Lee, K., Naruse, M., Suzuki, J., Taino, T., Tomita, N., & More Authors (2018). GroundBIRD: Observation of CMB Polarization with a Rapid Scanning and MKIDs. Journal of Low Temperature Physics, 193(5-6), 1066-1074. https://doi.org/10.1007/s10909-018- 2077-y Important note To cite this publication, please use the final published version (if applicable). Please check the document version above. Copyright Other than for strictly personal use, it is not permitted to download, forward or distribute the text or part of it, without the consent of the author(s) and/or copyright holder(s), unless the work is under an open content license such as Creative Commons. Takedown policy Please contact us and provide details if you believe this document breaches copyrights. We will remove access to the work immediately and investigate your claim. This work is downloaded from Delft University of Technology. For technical reasons the number of authors shown on this cover page is limited to a maximum of 10. Journal of Low Temperature Physics manuscript No. (will be inserted by the editor) GroundBIRD - Observation of CMB polarization with a rapid scanning and MKIDs T.
    [Show full text]
  • Litebird Lite(Light) Satellite for the Studies for B-Mode PolarizaOn and InflaOn from Cosmic Background RadiaOn DetecOn
    LiteBIRD! Lite(Light) satellite for the studies for B-mode polarizaon and Inflaon from cosmic background Radiaon Detec6on Tomotake Matsumura (ISAS/JAXA) on behalf of LiteBIRD working group! 2014/12/1-5, PLANCK2014, Ferrara! Explora(on of early Universe using CMB satellite COBE (1989) WMAP (2001) Planck (2009) Band 32−90GHz 23−94GHz 30−857GHz （353GHz） Detectors 6 radiometers 20 radiometers 11 radiometers + 52 bolometers Operaon temperature 300/140 K 90 K 100 mK Angular Resolu6no ~7° ~0.22° ~0.1° Orbit Sun Synch L2 L2 December 3, 2014 Planck2014@Ferrara, Italy 2 Explora(on of early Universe using CMB satellite Next generation B-mode probe COBE (1989) WMAP (2001) Planck (2009) Band 32−90GHz 23−94GHz 30−857GHz （353GHz） EE Detectors 6 radiometers 20 radiometers 11 radiometers + 52 bolometers Operaon temperature 300/140 K 90 K 100 mK Angular Resolu6no ~7° ~0.22° BB ~0.1° Orbit Sun Synch L2 L2 December 3, 2014 Planck2014@Ferrara, Italy 3 LiteBIRD LiteBIRD is a next generaon CMB polarizaon satellite to probe the inflaonary Universe. The science goal of LiteBIRD is to measure the tensor-to-scalar rao with the sensi6vity of δr =0.001. The design philosophy is driven to focus on the primordial B-mode signal. Primordial B-mode r = 0.2 Lensing B-mode r = 0.025 Plot made by Y. Chinone December 3, 2014 Planck2014@Ferrara, Italy 4 LiteBIRD working group >70 members, internaonal and interdisciplinary. KEK JAXA UC Berkeley Kavli IPMU MPA NAOJ Y. Chinone H. Fuke W. Holzapfel N. Katayama E. Komatsu S. Kashima K. Haori I.
    [Show full text]
  • A Bit of History Satellites Balloons Ground-Based
    Experimental Landscape ● A Bit of History ● Satellites ● Balloons ● Ground-Based Ground-Based Experiments There have been many: ABS, ACBAR, ACME, ACT, AMI, AMiBA, APEX, ATCA, BEAST, BICEP[2|3]/Keck, BIMA, CAPMAP, CAT, CBI, CLASS, COBRA, COSMOSOMAS, DASI, MAT, MUSTANG, OVRO, Penzias & Wilson, etc., PIQUE, Polatron, Polarbear, Python, QUaD, QUBIC, QUIET, QUIJOTE, Saskatoon, SP94, SPT, SuZIE, SZA, Tenerife, VSA, White Dish & more! QUAD 2017-11-17 Ganga/Experimental Landscape 2/33 Balloons There have been a number: 19 GHz Survey, Archeops, ARGO, ARCADE, BOOMERanG, EBEX, FIRS, MAX, MAXIMA, MSAM, PIPER, QMAP, Spider, TopHat, & more! BOOMERANG 2017-11-17 Ganga/Experimental Landscape 3/33 Satellites There have been 4 (or 5?): Relikt, COBE, WMAP, Planck (+IRTS!) Planck 2017-11-17 Ganga/Experimental Landscape 4/33 Rockets & Airplanes For example, COBRA, Berkeley-Nagoya Excess, U2 Anisotropy Measurements & others... It’s difficult to get integration time on these platforms, so while they are still used in the infrared, they are no longer often used for the http://aether.lbl.gov/www/projects/U2/ CMB. 2017-11-17 Ganga/Experimental Landscape 5/33 (from R. Stompor) Radek Stompor http://litebird.jp/eng/ 2017-11-17 Ganga/Experimental Landscape 6/33 Other Satellite Possibilities ● US “CMB Probe” ● CORE-like – Studying two possibilities – Discussions ongoing ● Imager with India/ISRO & others ● Spectrophotometer – Could include imager – Inputs being prepared for AND low-angular- the Decadal Process resolution spectrophotometer? https://zzz.physics.umn.edu/ipsig/
    [Show full text]
  • Beyondplanck VI. Noise Characterization and Modelling
    Astronomy & Astrophysics manuscript no. noise_paper ©ESO 2020 November 16, 2020 BeyondPlanck VI. Noise characterization and modelling H. T. Ihle11?, M. Bersanelli4; 9; 10, C. Franceschet4; 10, E. Gjerløw11, K. J. Andersen11, R. Aurlien11, R. Banerji11, S. Bertocco8, M. Brilenkov11, M. Carbone14, L. P. L. Colombo4, H. K. Eriksen11, J. R. Eskilt11, M. K. Foss11, U. Fuskeland11, S. Galeotta8, M. Galloway11, S. Gerakakis14, B. Hensley2, D. Herman11, M. Iacobellis14, M. Ieronymaki14, H. T. Ihle11, J. B. Jewell12, A. Karakci11, E. Keihänen3; 7, R. Keskitalo1, G. Maggio8, D. Maino4; 9; 10, M. Maris8, A. Mennella4; 9; 10, S. Paradiso4; 9, B. Partridge6, M. Reinecke13, M. San11, A.-S. Suur-Uski3; 7, T. L. Svalheim11, D. Tavagnacco8; 5, H. Thommesen11, D. J. Watts11, I. K. Wehus11, and A. Zacchei8 1 Computational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, California, U.S.A. 2 Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, U.S.A. 3 Department of Physics, Gustaf Hällströmin katu 2, University of Helsinki, Helsinki, Finland 4 Dipartimento di Fisica, Università degli Studi di Milano, Via Celoria, 16, Milano, Italy 5 Dipartimento di Fisica, Università degli Studi di Trieste, via A. Valerio 2, Trieste, Italy 6 Haverford College Astronomy Department, 370 Lancaster Avenue, Haverford, Pennsylvania, U.S.A. 7 Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of Helsinki, Helsinki, Finland 8 INAF - Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, Trieste, Italy 9 INAF-IASF Milano, Via E. Bassini 15, Milano, Italy 10 INFN, Sezione di Milano, Via Celoria 16, Milano, Italy 11 Institute of Theoretical Astrophysics, University of Oslo, Blindern, Oslo, Norway 12 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California, U.S.A.
    [Show full text]
  • Measuring the Polarization of the Cosmic Microwave Background
    Measuring the Polarization of the Cosmic Microwave Background CAPMAP and QUIET Dorothea Samtleben, Kavli Institute for Cosmological Physics, University of Chicago Outline Theory point of view Ø What can we learn from the Cosmic Microwave Background (CMB)? Ø How to characterize and describe the CMB Ø Why is the CMB polarized? Experiment point of view Ø CMB polarization experiments Ø CAPMAP experiment, first results Ø Future of CMB measurements Ø QUIET experiment, status and plans Where does the CMB come from? Ø Temperature cool enough that electrons and protons form first atoms => The universe became transparent Ø Photons from that ‘last scattering surface’ give direct snapshot of the infant universe Ø Still around today but cooled down (shifted to microwaves) due to expansion of the universe CMB observations Interstellar CN absorption lines 1941! Accidental discovery 1965 Blackbody Radiation, homogenous, isotropic DT £ (1- 3)x10-3 (Partridge & Wilkinson, 1967) WHY? T Rescue by Inflationary models Inflation increases volume of universe by 1063 in 10-30 seconds Consequences (observables) for CMB: Ø Homogenous, isotropic blackbody radiation Ø Scale-invariant temperature fluctuations Ø On small scales (within horizon) temperature fluctuations from ‘accoustic oscillations’ (radiation pressure vs gravitational attraction) Ø Polarization anisotropies, correlated with temperature anisotropies Ø Gravitational waves, produced by inflation, cause distinct pattern in CMB polarization anisotropy Ø Reionization period will impact the fluctuation pattern
    [Show full text]