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Published September 2020 | Published + Accepted Version
Journal Article Open

Planck 2018 results. XI. Polarized dust foregrounds

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.
Macías-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.
Planck Collaboration


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 α_(EE) = −2.42 ± 0.02 and α_(BB) = −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 β_d^P = 1.53±0.02. The difference between indices for polarization and total intensity is β_d^P−β_d^I = 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.

Additional Information

© 2020 Planck Collaboration. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Received 11 January 2018; Accepted 14 September 2018; Published online 11 September 2020. Planck (http://www.esa.int/Planck) is a project of the European Space Agency (ESA) with instruments provided by two scientific consortia funded by ESA member states and led by Principal Investigators from France and Italy, telescope reflectors provided through a collaboration between ESA and a scientific consortium led and funded by Denmark, and additional contributions from NASA (USA). The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. This research has received funding by the Agence Nationale de la Recherche (ANR-17-CE31-0022).

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August 19, 2023
August 19, 2023