Planck intermediate results: XLIV. Structure of the Galactic magnetic field from dust polarization maps of the southern Galactic cap

Research output: Contribution to journalArticleScientificpeer-review

Researchers

  • N. Aghanim
  • M. I R Alves
  • D. Arzoumanian
  • J. Aumont
  • C. Baccigalupi
  • M. Ballardini
  • A. J. Banday
  • R. B. Barreiro
  • N. Bartolo
  • S. Basak
  • K. Benabed
  • J. P. Bernard
  • M. Bersanelli
  • P. Bielewicz
  • L. Bonavera
  • J. R. Bond
  • J. Borrill
  • F. R. Bouchet
  • F. Boulanger
  • A. Bracco
  • M. Bucher
  • C. Burigana
  • E. Calabrese
  • J. F. Cardoso
  • H. C. Chiang
  • L. P L Colombo
  • C. Combet
  • B. Comis
  • F. Couchot
  • A. Coulais
  • B. P. Crill
  • A. Curto
  • F. Cuttaia
  • R. J. Davis
  • P. De Bernardis
  • A. De Rosa
  • G. De Zotti
  • J. Delabrouille
  • J. M. Delouis
  • E. Di Valentino
  • C. Dickinson
  • J. M. Diego
  • O. Doré
  • M. Douspis
  • A. Ducout
  • X. Dupac
  • S. Dusini
  • G. Efstathiou
  • F. Elsner
  • T. A. Enßlin
  • H. K. Eriksen
  • E. Falgarone
  • Y. Fantaye
  • K. Ferrière
  • F. Finelli
  • M. Frailis
  • A. A. Fraisse
  • E. Franceschi
  • A. Frolov
  • S. Galeotta
  • S. Galli
  • K. Ganga
  • R. T. Génova-Santos
  • M. Gerbino
  • T. Ghosh
  • J. González-Nuevo
  • K. M. Górski
  • S. Gratton
  • A. Gregorio
  • A. Gruppuso
  • J. E. Gudmundsson
  • V. Guillet
  • F. K. Hansen
  • G. Helou
  • S. Henrot-Versillé
  • D. Herranz
  • E. Hivon
  • Z. Huang
  • A. H. Jaffe
  • T. R. Jaffe
  • W. C. Jones
  • E. Keihänen
  • R. Keskitalo
  • T. S. Kisner
  • N. Krachmalnicoff
  • M. Kunz
  • H. Kurki-Suonio
  • G. Lagache
  • J. M. Lamarre
  • M. Langer
  • A. Lasenby
  • M. Lattanzi
  • M. Le Jeune
  • F. Levrier
  • M. Liguori
  • P. B. Lilje
  • M. López-Caniego
  • P. M. Lubin
  • J. F. MacIás-Pérez
  • G. Maggio
  • D. Maino
  • N. Mandolesi
  • A. Mangilli
  • M. Maris
  • P. G. Martin
  • E. Martínez-González
  • S. Matarrese
  • N. Mauri
  • J. D. McEwen
  • A. Melchiorri
  • A. Mennella
  • M. Migliaccio
  • M. A. Miville-Deschênes
  • D. Molinari
  • A. Moneti
  • L. Montier
  • G. Morgante
  • A. Moss
  • P. Naselsky
  • P. Natoli
  • J. Neveu
  • H. U. Nørgaard-Nielsen
  • N. Oppermann
  • C. A. Oxborrow
  • L. Pagano
  • D. Paoletti
  • B. Partridge
  • O. Perdereau
  • L. Perotto
  • V. Pettorino
  • F. Piacentini
  • S. Plaszczynski
  • G. Polenta
  • J. P. Rachen
  • R. Rebolo
  • M. Reinecke
  • M. Remazeilles
  • A. Renzi
  • I. Ristorcelli
  • G. Rocha
  • M. Rossetti
  • G. Roudier
  • B. Ruiz-Granados
  • L. Salvati
  • M. Sandri
  • D. Scott
  • C. Sirignano
  • J. D. Soler
  • A. S. Suur-Uski
  • J. A. Tauber
  • D. Tavagnacco
  • M. Tenti
  • L. Toffolatti
  • M. Tomasi
  • M. Tristram
  • T. Trombetti
  • J. Valiviita
  • F. Vansyngel
  • F. Van Tent
  • P. Vielva
  • F. Villa
  • B. D. Wandelt
  • I. K. Wehus
  • A. Zacchei
  • A. Zonca

Research units

  • CNRS/IN2P3
  • IRAP
  • Service d'Astrophysique CEA
  • International School for Advanced Studies
  • Universit'a di Rome Sapienza
  • Instituto de Física de Cantabria (CSIC-Universidad de Cantabria)
  • UMR7095
  • INAF/IASF Milano
  • University of Toronto
  • University of California at Berkeley
  • Institut d 'Astrophysique de Paris
  • Université Pierre and Marie Curie
  • University of Oxford
  • Télécom ParisTech
  • Princeton University
  • Jet Propulsion Laboratory, California Institute of Technology
  • CNRS/IN2P3
  • Universite Paris-Sud
  • LERMA - Laboratoire d'Etudes du Rayonnement et de la Matiere en Astrophysique et Atmospheres
  • Kavli Institute for Cosmology Cambridge
  • Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna
  • University of Manchester
  • Università La Sapienza
  • CNRS Centre National de la Recherche Scientifique
  • Urbanización Villafranca Del Castillo
  • University of Cambridge
  • Max-Planck-Institut für Astrophysik
  • University of Oslo
  • Università di Roma Tor Vergata
  • Osservatorio Astronomico di Trieste
  • Simon Fraser University
  • University of Chicago
  • Instituto Astrofisico de Canarias
  • Stockholm University
  • University of Warsaw
  • California Institute of Technology
  • Imperial College London
  • University of Helsinki
  • Lawrence Berkeley National Laboratory
  • University of Milano
  • University of California at Santa Barbara
  • University College London
  • University of Nottingham
  • Niels Bohr Institute
  • Danmarks Tekniske Universitet
  • Haverford College
  • Institut für Theoretische Astrophysik
  • Osservatorio Astronomico Roma
  • Facultad de Ciencias
  • University of British Columbia
  • ESTEC - European Space Research and Technology Centre

Abstract

Using data from the Planck satellite, we study the statistical properties of interstellar dust polarization at high Galactic latitudes around the south pole (b <-60°). Our aim is to advance the understanding of the magnetized interstellar medium (ISM), and to provide a modelling framework of the polarized dust foreground for use in cosmic microwave background (CMB) component-separation procedures. We examine the Stokes I, Q, and U maps at 353 GHz, and particularly the statistical distribution of the polarization fraction (p) and angle (ψ), in order to characterize the ordered and turbulent components of the Galactic magnetic field (GMF) in the solar neighbourhood. The Q and U maps show patterns at large angular scales, which we relate to the mean orientation of the GMF towards Galactic coordinates (l0,b0) = (70° ± 5°,24° ± 5°). The histogram of the observed p values shows a wide dispersion up to 25%. The histogram of ψ has a standard deviation of 12° about the regular pattern expected from the ordered GMF. We build a phenomenological model that connects the distributions of p and ψ to a statistical description of the turbulent component of the GMF, assuming a uniform effective polarization fraction (p0) of dust emission. To compute the Stokes parameters, we approximate the integration along the line of sight (LOS) as a sum over a set of N independent polarization layers, in each of which the turbulent component of the GMF is obtained from Gaussian realizations of a power-law power spectrum. We are able to reproduce the observed p and ψ distributions using a p0 value of 26%, a ratio of 0.9 between the strengths of the turbulent and mean components of the GMF, and a small value of N. The mean value of p (inferred from the fit of the large-scale patterns in the Stokes maps) is 12 ± 1%. We relate the polarization layers to the density structure and to the correlation length of the GMF along the LOS. We emphasize the simplicity of our model (involving only a few parameters), which can be easily computed on the celestial sphere to produce simulated maps of dust polarization. Our work is an important step towards a model that can be used to assess the accuracy of component-separation methods in present and future CMB experiments designed to search the B mode CMB polarization from primordial gravity waves.

Details

Original languageEnglish
Article numberA105
JournalAstronomy and Astrophysics
Volume596
Publication statusPublished - 1 Dec 2016
MoE publication typeA1 Journal article-refereed

    Research areas

  • Cosmic background radiation, Dust, extinction, ISM: magnetic fields, Magnetohydrodynamics (MHD), Methods: data analysis, Polarization

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