Planck 2018 results

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Journal ISSN
Volume Title
A1 Alkuperäisartikkeli tieteellisessä aikakauslehdessä
Date
2020-09-01
Department
Leiden University
University of Cambridge
Université Paul Sabatier
International School for Advanced Studies
University of the Western Cape
IRAP
Universidad de Cantabria
University of Padova
Indian Institute of Science Education and Research Thiruvananthapuram
Institut d 'Astrophysique de Paris
University of Milano
University of Toronto
Lawrence Berkeley National Laboratory
Université Paris-Sud
Université Pierre et Marie Curie
University of Ferrara
Cardiff University
University of Sussex
University of KwaZulu-Natal
Institut national de physique nucléaire et de physique des particules
California Institute of Technology
Sapienza University of Rome
INAF - Osservatorio Astronomico di Padova
University of Manchester
University of Tokyo
European Space Astronomy Centre
Max-Planck-Institut für Astrophysik
UMR7095
African Institute for Mathematical Sciences
National Research Council of Italy
Osservatorio Astronomico di Trieste
Princeton University
Simon Fraser University
University of Chicago
University of La Laguna
University of Oviedo
Jet Propulsion Laboratory
University of Oslo
Sun Yat-Sen University
Imperial College London
University of Helsinki
University of California Santa Barbara
Department of Applied Physics
University College London
University of Rome Tor Vergata
Université Paris-Saclay
Agenzia Spaziale Italiana
Radboud University Nijmegen
National Institute for Nuclear Physics
University of British Columbia
Max Planck Institute for Astronomy
European Space Research and Technology Centre
Università Degli Studi di Trieste
Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna
University of California San Diego
Major/Subject
Mcode
Degree programme
Language
en
Pages
33
Series
Astronomy and Astrophysics, Volume 641
Abstract
The study of polarized dust emission has become entwined with the analysis of the cosmic microwave background (CMB) polarization in the quest for the curl-like B-mode polarization from primordial gravitational waves and the low-multipole E-mode polarization associated with the reionization of the Universe. We used the new Planck PR3 maps to characterize Galactic dust emission at high latitudes as a foreground to the CMB polarization and use end-to-end simulations to compute uncertainties and assess the statistical significance of our measurements. We present Planck EE, BB, and TE power spectra of dust polarization at 353 GHz for a set of six nested high-Galactic-latitude sky regions covering from 24 to 71% of the sky. We present power-law fits to the angular power spectra, yielding evidence for statistically significant variations of the exponents over sky regions and a difference between the values for the EE and BB spectra, which for the largest sky region are αEE = -2.42 ± 0.02 and αBB = -2.54 ± 0.02, respectively. The spectra show that the TE correlation and E/B power asymmetry discovered by Planck extend to low multipoles that were not included in earlier Planck polarization papers due to residual data systematics. We also report evidence for a positive TB dust signal. Combining data from Planck and WMAP, we have determined the amplitudes and spectral energy distributions (SEDs) of polarized foregrounds, including the correlation between dust and synchrotron polarized emission, for the six sky regions as a function of multipole. This quantifies the challenge of the component-separation procedure that is required for measuring the low-ℓ reionization CMB E-mode signal and detecting the reionization and recombination peaks of primordial CMB B modes. The SED of polarized dust emission is fit well by a single-temperature modified black-body emission law from 353 GHz to below 70 GHz. For a dust temperature of 19.6 K, the mean dust spectral index for dust polarization is βdP = 1.53±0.02. The difference between indices for polarization and total intensity is βdP-βdI = 0.05±0.03. By fitting multi-frequency cross-spectra between Planck data at 100, 143, 217, and 353 GHz, we examine the correlation of the dust polarization maps across frequency. We find no evidence for a loss of correlation and provide lower limits to the correlation ratio that are tighter than values we derive from the correlation of the 217- and 353 GHz maps alone. If the Planck limit on decorrelation for the largest sky region applies to the smaller sky regions observed by sub-orbital experiments, then frequency decorrelation of dust polarization might not be a problem for CMB experiments aiming at a primordial B-mode detection limit on the tensor-to-scalar ratio r≃ 0.01 at the recombination peak. However, the Planck sensitivity precludes identifying how difficult the component-separation problem will be for more ambitious experiments targeting lower limits on r.
Description
Keywords
Cosmic background radiation, Dust, Extinction, ISM: magnetic fields, ISM: structure, Polarization, Submillimeter: diffuse background
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Citation
Akrami , Y , Ashdown , M , Aumont , J , Baccigalupi , C , Ballardini , M , Banday , A J , Barreiro , R B , Bartolo , N , Basak , S , Benabed , K , Bernard , J P , Bersanelli , M , Bielewicz , P , Bond , J R , Borrill , J , Bouchet , F R , Boulanger , F , Bracco , A , Bucher , M , Burigana , C , Calabrese , E , Cardoso , J F , Carron , J , Chiang , H C , Combet , C , Crill , B P , De Bernardis , P , De Zotti , G , Delabrouille , J , Delouis , J M , Di Valentino , E , Dickinson , C , Diego , J M , Ducout , A , Dupac , X , Efstathiou , G , Elsner , F , Enßlin , T A , Falgarone , E , Fantaye , Y , Ferrière , K , Finelli , F , Forastieri , F , Frailis , M , Fraisse , A A , Franceschi , E , Frolov , A , Galeotta , S , Galli , S , Ganga , K , Génova-Santos , R T , Ghosh , T , González-Nuevo , J , Górski , K M , Gruppuso , A , Gudmundsson , J E , Guillet , V , Handley , W , Hansen , F K , Herranz , D , Huang , Z , Jaffe , A H , Jones , W C , Keihänen , E , Keskitalo , R , Kiiveri , K , Kim , J , Krachmalnicoff , N , Kunz , M , Kurki-Suonio , H , Lamarre , J M , Lasenby , A , Le Jeune , M , Levrier , F , Liguori , M , Lilje , P B , Lindholm , V , López-Caniego , M , Lubin , P M , Ma , Y Z , Maciás-Pérez , J F , Maggio , G , Maino , D , Mandolesi , N , Mangilli , A , Martin , P G , Martínez-González , E , Matarrese , S , McEwen , J D , Meinhold , P R , Melchiorri , A , Migliaccio , M , Miville-Deschênes , M A , Molinari , D , Moneti , A , Montier , L , Morgante , G , Natoli , P , Pagano , L , Paoletti , D , Pettorino , V , Piacentini , F , Polenta , G , Puget , J L , Rachen , J P , Reinecke , M , Remazeilles , M , Renzi , A , Rocha , G , Rosset , C , Roudier , G , Rubiño-Martín , J A , Ruiz-Granados , B , Salvati , L , Sandri , M , Savelainen , M , Scott , D , Soler , J D , Spencer , L D , Tauber , J A , Tavagnacco , D , Toffolatti , L , Tomasi , M , Trombetti , T , Valiviita , J , Vansyngel , F , Van Tent , B , Vielva , P , Villa , F , Vittorio , N , Wehus , I K , Zacchei , A & Zonca , A 2020 , ' Planck 2018 results : XI.Polarized dust foregrounds ' , Astronomy and Astrophysics , vol. 641 , 11 . https://doi.org/10.1051/0004-6361/201832618