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@article{Adam:2016:0004-6361/201525936,
author = {Adam, R and Ade, PAR and Aghanim, N and Arnaud, M and Ashdown, M and Aumont, J and Baccigalupi, C and Banday, AJ and Barreiro, RB and Bartlett, JG and Bartolo, N and Basak, S and Battaner, E and Benabed, K and Benoit, A and Benoit-Levy, A and Bernard, J-P and Bersanelli, M and Bielewicz, P and Bock, JJ and Bonaldi, A and Bonavera, L and Bond, JR and Borrill, J and Bouchet, FR and Boulanger, F and Bucher, M and Burigana, C and Butler, RC and Calabrese, E and Cardoso, J-F and Casaponsa, B and Castex, G and Catalano, A and Challinor, A and Chamballu, A and Chary, R-R and Chiang, HC and Christensen, PR and Clements, DL and Colombi, S and Colombo, LPL and Combet, C and Couchot, F and Coulais, A and Crill, BP and Curto, A and Cuttaia, F and Danese, L and Davies, RD and Davis, RJ and de, Bernardis P and de, Rosa A and de, Zotti G and Delabrouille, J and Desert, F-X and Dickinson, C and Diego, JM and Dole, H and Donzelli, S and Dore, O and Douspis, M and Ducout, A and Dupac, X and Efstathiou, },
doi = {0004-6361/201525936},
journal = {Astronomy and Astrophysics},
title = {Planck 2015 results IX. Diffuse component separation: CMB maps},
url = {http://dx.doi.org/10.1051/0004-6361/201525936},
volume = {594},
year = {2016}
}

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TY  - JOUR
AB  - We present foreground-reduced cosmic microwave background (CMB) maps derived from the full Planck data set in both temperature and polarization. Compared to the corresponding Planck 2013 temperature sky maps, the total data volume is larger by a factor of 3.2 for frequencies between 30 and 70 GHz, and by 1.9 for frequencies between 100 and 857 GHz. In addition, systematic errors in the forms of temperature-to-polarization leakage, analogue-to-digital conversion uncertainties, and very long time constant errors have been dramatically reduced, to the extent that the cosmological polarization signal may now be robustly recovered on angular scales   40. On the very largest scales, instrumental systematic residuals are still non-negligible compared to the expected cosmological signal, and modes with < 20 are accordingly suppressed in the current polarization maps by high-pass filtering. As in 2013, four different CMB component separation algorithms are applied to these observations, providing a measure of stability with respect to algorithmic and modelling choices. The resulting polarization maps have rms instrumental noise ranging between 0.21 and 0.27μK averaged over 55′ pixels, and between 4.5 and 6.1μK averaged over  pixels. The cosmological parameters derived from the analysis of temperature power spectra are in agreement at the 1σ level with the Planck 2015 likelihood. Unresolved mismatches between the noise properties of the data and simulations prevent a satisfactory description of the higher-order statistical properties of the polarization maps. Thus, the primary applications of these polarization maps are those that do not require massive simulations for accurate estimation of uncertainties, for instance estimation of cross-spectra and cross-correlations, or stacking analyses. However, the amplitude of primordial non-Gaussianity is consistent with zero within 2σ for all local, equilateral, and orthogonal configuration
AU  - Adam,R
AU  - Ade,PAR
AU  - Aghanim,N
AU  - Arnaud,M
AU  - Ashdown,M
AU  - Aumont,J
AU  - Baccigalupi,C
AU  - Banday,AJ
AU  - Barreiro,RB
AU  - Bartlett,JG
AU  - Bartolo,N
AU  - Basak,S
AU  - Battaner,E
AU  - Benabed,K
AU  - Benoit,A
AU  - Benoit-Levy,A
AU  - Bernard,J-P
AU  - Bersanelli,M
AU  - Bielewicz,P
AU  - Bock,JJ
AU  - Bonaldi,A
AU  - Bonavera,L
AU  - Bond,JR
AU  - Borrill,J
AU  - Bouchet,FR
AU  - Boulanger,F
AU  - Bucher,M
AU  - Burigana,C
AU  - Butler,RC
AU  - Calabrese,E
AU  - Cardoso,J-F
AU  - Casaponsa,B
AU  - Castex,G
AU  - Catalano,A
AU  - Challinor,A
AU  - Chamballu,A
AU  - Chary,R-R
AU  - Chiang,HC
AU  - Christensen,PR
AU  - Clements,DL
AU  - Colombi,S
AU  - Colombo,LPL
AU  - Combet,C
AU  - Couchot,F
AU  - Coulais,A
AU  - Crill,BP
AU  - Curto,A
AU  - Cuttaia,F
AU  - Danese,L
AU  - Davies,RD
AU  - Davis,RJ
AU  - de,Bernardis P
AU  - de,Rosa A
AU  - de,Zotti G
AU  - Delabrouille,J
AU  - Desert,F-X
AU  - Dickinson,C
AU  - Diego,JM
AU  - Dole,H
AU  - Donzelli,S
AU  - Dore,O
AU  - Douspis,M
AU  - Ducout,A
AU  - Dupac,X
AU  - Efstathiou,G
AU  - Elsner,F
AU  - Ensslin,TA
AU  - Eriksen,HK
AU  - Falgarone,E
AU  - Fantaye,Y
AU  - Fergusson,J
AU  - Finelli,F
AU  - Forni,O
AU  - Frailis,M
AU  - Fraisse,AA
AU  - Francescht,E
AU  - Frejsel,A
AU  - Galeotta,S
AU  - Galli,S
AU  - Ganga,K
AU  - Ghosh,T
AU  - Giard,M
AU  - Giraud-Heraud,Y
AU  - Gjerlow,E
AU  - Gonzalez-Nuevo,J
AU  - Gorski,KM
AU  - Gratton,S
AU  - Gregorio,A
AU  - Gruppuso,A
AU  - Gudmundsson,JE
AU  - Hansen,FK
AU  - Hanson,D
AU  - Harrison,DL
AU  - Helou,G
AU  - Henrot-Versille,S
AU  - Hernandez-Monteagudo,C
AU  - Herranz,D
AU  - Hildebrandt,SR
AU  - Hivon,E
AU  - Hobson,M
AU  - Holmes,WA
AU  - Hornstrup,A
AU  - Hovest,W
AU  - Huffenberger,KM
AU  - Hurier,G
AU  - Jaffe,AH
AU  - Jaffe,TR
AU  - Jones,WC
AU  - Juvela,M
AU  - Keihanen,E
AU  - Keskitalo,R
AU  - Kisner,TS
AU  - Kneissl,R
AU  - Knoche,J
AU  - Krachmalnicoff,N
AU  - Kunz,M
AU  - Kurki-Suonio,H
AU  - Lagache,G
AU  - Lamarre,J-M
AU  - Lasenby,A
AU  - Lattanzi,M
AU  - Lawrence,CR
AU  - Le,Jenne M
AU  - Leonardi,R
AU  - Lesgourgues,J
AU  - Levrier,F
AU  - Liguori,M
AU  - Lilje,PB
AU  - Linden-Vornle,M
AU  - Lopez-Caniego,M
AU  - Lubin,PM
AU  - Macias-Perez,JF
AU  - Maggio,G
AU  - Maino,D
AU  - Mandolesi,N
AU  - Mangilli,A
AU  - Maris,M
AU  - Marshall,DJ
AU  - Martin,PG
AU  - Martinez-Gonzalez,E
AU  - Masi,S
AU  - Matarrese,S
AU  - McGehee,P
AU  - Meinhold,PR
AU  - Melchiorri,A
AU  - Mendes,L
AU  - Mennella,A
AU  - Migliaccio,M
AU  - Mitra,S
AU  - Miville-Deschenes,M-A
AU  - Molinari,D
AU  - Moneti,A
AU  - Montier,L
AU  - Morgante,G
AU  - Mortlock,D
AU  - Moss,A
AU  - Munshi,D
AU  - Murphy,JA
AU  - Naselsky,P
AU  - Nati,F
AU  - Natoli,P
AU  - Netterfield,CB
AU  - Norgaard-Nielsen,HU
AU  - Noviello,F
AU  - Novikov,D
AU  - Novikov,I
AU  - Oxborrow,CA
AU  - Paci,F
AU  - Pa
DO  - 0004-6361/201525936
PY  - 2016///
SN  - 0004-6361
TI  - Planck 2015 results IX. Diffuse component separation: CMB maps
T2  - Astronomy and Astrophysics
UR  - http://dx.doi.org/10.1051/0004-6361/201525936
UR  - http://hdl.handle.net/10044/1/54337
VL  - 594
ER  -

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