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@article{Akrami:2020:0004-6361/201832618,
author = {Akrami, Y and Ashdown, M and Aumont, J and Baccigalupi, C and Ballardini, M and Banday, AJ and Barreiro, RB and Bartolo, N and Basak, S and Benabed, K and Bernard, J-P and Bersanelli, M and Bielewicz, P and Bond, JR and Borrill, J and Bouchet, FR and Boulanger, F and Bracco, A and Bucher, M and Burigana, C and Calabrese, E and Cardoso, J-F and Carron, J and Chiang, HC and Combet, C and Crill, BP and de, Bernardis P and de, Zotti G and Delabrouille, J and Delouis, J-M and Di, Valentino E and Dickinson, C and Diego, JM and Ducout, A and Dupac, X and Efstathiou, G and Elsner, F and Enßlin, TA and Falgarone, E and Fantaye, Y and Ferrière, K and Finelli, F and Forastieri, F and Frailis, M and Fraisse, AA and Franceschi, E and Frolov, A and Galeotta, S and Galli, S and Ganga, K and Génova-Santos, RT and Ghosh, T and González-Nuevo, J and Górski, KM and Gruppuso, A and Gudmundsson, JE and Guillet, V and Handley, W and Hansen, FK and Herranz, D and Huang, Z and Jaffe, AH and Jones, WC and Keih},
doi = {0004-6361/201832618},
journal = {Astronomy & Astrophysics},
pages = {A11--A11},
title = {Planck 2018 results. XI. Polarized dust foregrounds},
url = {http://dx.doi.org/10.1051/0004-6361/201832618},
volume = {641},
year = {2020}
}

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TY  - JOUR
AB  - <jats:p>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 <jats:italic>B</jats:italic>-mode polarization from primordial gravitational waves and the low-multipole <jats:italic>E</jats:italic>-mode polarization associated with the reionization of the Universe. We used the new <jats:italic>Planck</jats:italic> 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 <jats:italic>Planck</jats:italic> <jats:italic>EE</jats:italic>, <jats:italic>BB</jats:italic>, and <jats:italic>TE</jats:italic> 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 <jats:italic>EE</jats:italic> and <jats:italic>BB</jats:italic> spectra, which for the largest sky region are <jats:italic>α</jats:italic><jats:sub><jats:italic>E</jats:italic><jats:italic>E</jats:italic></jats:sub>=−2.42±0.02 and <jats:italic>α</jats:italic><jats:sub><jats:italic>B</jats:italic><jats:italic>B</jats:italic></jats:sub>=−2.54±0.02, respectively. The spectra show that the <jats:italic>TE</jats:italic> correlation and <jats:italic>E/B</jats:italic> power asymmetry discovered by <jats:italic>Planck</jats:italic> extend to low multipoles that were not included in earlier &
AU  - Akrami,Y
AU  - Ashdown,M
AU  - Aumont,J
AU  - Baccigalupi,C
AU  - Ballardini,M
AU  - Banday,AJ
AU  - Barreiro,RB
AU  - Bartolo,N
AU  - Basak,S
AU  - Benabed,K
AU  - Bernard,J-P
AU  - Bersanelli,M
AU  - Bielewicz,P
AU  - Bond,JR
AU  - Borrill,J
AU  - Bouchet,FR
AU  - Boulanger,F
AU  - Bracco,A
AU  - Bucher,M
AU  - Burigana,C
AU  - Calabrese,E
AU  - Cardoso,J-F
AU  - Carron,J
AU  - Chiang,HC
AU  - Combet,C
AU  - Crill,BP
AU  - de,Bernardis P
AU  - de,Zotti G
AU  - Delabrouille,J
AU  - Delouis,J-M
AU  - Di,Valentino E
AU  - Dickinson,C
AU  - Diego,JM
AU  - Ducout,A
AU  - Dupac,X
AU  - Efstathiou,G
AU  - Elsner,F
AU  - Enßlin,TA
AU  - Falgarone,E
AU  - Fantaye,Y
AU  - Ferrière,K
AU  - Finelli,F
AU  - Forastieri,F
AU  - Frailis,M
AU  - Fraisse,AA
AU  - Franceschi,E
AU  - Frolov,A
AU  - Galeotta,S
AU  - Galli,S
AU  - Ganga,K
AU  - Génova-Santos,RT
AU  - Ghosh,T
AU  - González-Nuevo,J
AU  - Górski,KM
AU  - Gruppuso,A
AU  - Gudmundsson,JE
AU  - Guillet,V
AU  - Handley,W
AU  - Hansen,FK
AU  - Herranz,D
AU  - Huang,Z
AU  - Jaffe,AH
AU  - Jones,WC
AU  - Keihänen,E
AU  - Keskitalo,R
AU  - Kiiveri,K
AU  - Kim,J
AU  - Krachmalnicoff,N
AU  - Kunz,M
AU  - Kurki-Suonio,H
AU  - Lamarre,J-M
AU  - Lasenby,A
AU  - Le,Jeune M
AU  - Levrier,F
AU  - Liguori,M
AU  - Lilje,PB
AU  - Lindholm,V
AU  - López-Caniego,M
AU  - Lubin,PM
AU  - Ma,Y-Z
AU  - Macías-Pérez,JF
AU  - Maggio,G
AU  - Maino,D
AU  - Mandolesi,N
AU  - Mangilli,A
AU  - Martin,PG
AU  - Martínez-González,E
AU  - Matarrese,S
AU  - McEwen,JD
AU  - Meinhold,PR
AU  - Melchiorri,A
AU  - Migliaccio,M
AU  - Miville-Deschênes,M-A
AU  - Molinari,D
AU  - Moneti,A
AU  - Montier,L
AU  - Morgante,G
AU  - Natoli,P
AU  - Pagano,L
AU  - Paoletti,D
AU  - Pettorino,V
AU  - Piacentini,F
AU  - Polenta,G
AU  - Puget,J-L
AU  - Rachen,JP
AU  - Reinecke,M
AU  - Remazeilles,M
AU  - Renzi,A
AU  - Rocha,G
AU  - Rosset,C
AU  - Roudier,G
AU  - Rubiño-Martín,JA
AU  - Ruiz-Granados,B
AU  - Salvati,L
AU  - Sandri,M
AU  - Savelainen,M
AU  - Scott,D
AU  - Soler,JD
AU  - Spencer,LD
AU  - Tauber,JA
AU  - Tavagnacco,D
AU  - Toffolatti,L
AU  - Tomasi,M
AU  - Trombetti,T
AU  - Valiviita,J
AU  - Vansyngel,F
AU  - Van,Tent B
AU  - Vielva,P
AU  - Villa,F
AU  - Vittorio,N
AU  - Wehus,IK
AU  - Zacchei,A
AU  - Zonca,A
DO  - 0004-6361/201832618
EP  - 11
PY  - 2020///
SN  - 0004-6361
SP  - 11
TI  - Planck 2018 results. XI. Polarized dust foregrounds
T2  - Astronomy & Astrophysics
UR  - http://dx.doi.org/10.1051/0004-6361/201832618
VL  - 641
ER  -

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