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@article{Ade:2014:0004-6361/201321562,
author = {Ade, PAR and Aghanim, N and Armitage-Caplan, C and Arnaud, M and Ashdown, M and Atrio-Barandela, F and Aumont, J and Baccigalupi, C and Banday, AJ and Barreiro, RB and Bartlett, JG and Battaner, E and Benabed, K and Benoit, A and Benoit-Levy, A and Bernard, J-P and Bersanelli, M and Bielewicz, P and Bobin, J and Bock, JJ and Bonaldi, A and Bond, JR and Borrill, J and Bouchet, FR and Boulanger, F and Bridges, M and Bucher, M and Burigana, C and Butler, RC and Cardoso, J-F and Catalano, A and Chamballu, A and Chary, R-R and Chen, X and Chiang, HC and Chiang, L-Y and Christensen, PR and Church, S and Clements, DL and Colley, J-M and Colombi, S and Colombo, LPL and Couchot, F and Coulais, A and Crill, BP and Curto, A and Cuttaia, F and Danese, L and Davies, RD and de, Bernardis P and de, Rosa A and de, Zotti G and Delabrouille, J and Delouis, J-M and Desert, F-X and Dickinson, C and Diego, JM and Dole, H and Donzelli, S and Dore, O and Douspis, M and Dupac, X and Efstathiou, G and Ensslin,},
doi = {0004-6361/201321562},
journal = {Astronomy and Astrophysics},
title = {Planck 2013 results. XIV. Zodiacal emission},
url = {http://dx.doi.org/10.1051/0004-6361/201321562},
volume = {571},
year = {2014}
}

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TY  - JOUR
AB  - The Planck satellite provides a set of all-sky maps at nine frequencies from 30 GHz to 857 GHz. Planets, minor bodies, and diffuse interplanetary dust emission (IPD) are all observed. The IPD can be separated from Galactic and other emissions because Planck views a given point on the celestial sphere multiple times, through different columns of IPD. We use the Planck data to investigate the behaviour of zodiacal emission over the whole sky at sub-millimetre and millimetre wavelengths. We fit the Planck data to find the emissivities of the various components of the COBE zodiacal model – a diffuse cloud, three asteroidal dust bands, a circumsolar ring, and an Earth-trailing feature. The emissivity of the diffuse cloud decreases with increasing wavelength, as expected from earlier analyses. The emissivities of the dust bands, however, decrease less rapidly, indicating that the properties of the grains in the bands are different from those in the diffuse cloud. We fit the small amount of Galactic emission seen through the telescope’s far sidelobes, and place limits on possible contamination of the cosmic microwave background (CMB) results from both zodiacal and far-sidelobe emission. When necessary, the results are used in the Planck pipeline to make maps with zodiacal emission and far sidelobes removed. We show that the zodiacal correction to the CMB maps is small compared to the Planck CMB temperature power spectrum and give a list of flux densities for small solar system bodies.
AU  - Ade,PAR
AU  - Aghanim,N
AU  - Armitage-Caplan,C
AU  - Arnaud,M
AU  - Ashdown,M
AU  - Atrio-Barandela,F
AU  - Aumont,J
AU  - Baccigalupi,C
AU  - Banday,AJ
AU  - Barreiro,RB
AU  - Bartlett,JG
AU  - Battaner,E
AU  - Benabed,K
AU  - Benoit,A
AU  - Benoit-Levy,A
AU  - Bernard,J-P
AU  - Bersanelli,M
AU  - Bielewicz,P
AU  - Bobin,J
AU  - Bock,JJ
AU  - Bonaldi,A
AU  - Bond,JR
AU  - Borrill,J
AU  - Bouchet,FR
AU  - Boulanger,F
AU  - Bridges,M
AU  - Bucher,M
AU  - Burigana,C
AU  - Butler,RC
AU  - Cardoso,J-F
AU  - Catalano,A
AU  - Chamballu,A
AU  - Chary,R-R
AU  - Chen,X
AU  - Chiang,HC
AU  - Chiang,L-Y
AU  - Christensen,PR
AU  - Church,S
AU  - Clements,DL
AU  - Colley,J-M
AU  - Colombi,S
AU  - Colombo,LPL
AU  - Couchot,F
AU  - Coulais,A
AU  - Crill,BP
AU  - Curto,A
AU  - Cuttaia,F
AU  - Danese,L
AU  - Davies,RD
AU  - de,Bernardis P
AU  - de,Rosa A
AU  - de,Zotti G
AU  - Delabrouille,J
AU  - Delouis,J-M
AU  - Desert,F-X
AU  - Dickinson,C
AU  - Diego,JM
AU  - Dole,H
AU  - Donzelli,S
AU  - Dore,O
AU  - Douspis,M
AU  - Dupac,X
AU  - Efstathiou,G
AU  - Ensslin,TA
AU  - Eriksen,HK
AU  - Finelli,F
AU  - Forni,O
AU  - Frailis,M
AU  - Fraisse,AA
AU  - Franceschi,E
AU  - Galeotta,S
AU  - Ganga,K
AU  - Giard,M
AU  - Giraud-Heraud,Y
AU  - Gonzalez-Nuevo,J
AU  - Gorski,KM
AU  - Gratton,S
AU  - Gregorio,A
AU  - Gruppuso,A
AU  - Hansen,FK
AU  - Hanson,D
AU  - Harrison,D
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  - 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  - Knox,L
AU  - Kunz,M
AU  - Kurki-Suonio,H
AU  - Lagache,G
AU  - Lahteenmaki,A
AU  - Lamarre,J-M
AU  - Lasenby,A
AU  - Laureijs,RJ
AU  - Lawrence,CR
AU  - Leonardi,R
AU  - Lesgourgues,J
AU  - Liguori,M
AU  - Lilje,PB
AU  - Linden-Vornle,M
AU  - Lopez-Caniego,M
AU  - Lubin,PM
AU  - Macias-Perez,JF
AU  - Maffei,B
AU  - Maino,D
AU  - Mandolesi,N
AU  - Maris,M
AU  - Marshall,DJ
AU  - Martin,PG
AU  - Martinez-Gonzalez,E
AU  - Masi,S
AU  - Massardi,M
AU  - Matarrese,S
AU  - Matthai,F
AU  - Mazzotta,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  - Moneti,A
AU  - Montier,L
AU  - Morgante,G
AU  - Mortlock,D
AU  - Mottet,S
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  - Osborne,S
AU  - O'Sullivan,C
AU  - Oxborrow,CA
AU  - Paci,F
AU  - Pagano,L
AU  - Pajot,F
AU  - Paladini,R
AU  - Paoletti,D
AU  - Pasian,F
AU  - Patanchon,G
AU  - Perdereau,O
AU  - Perotto,L
AU  - Perrotta,F
AU  - Piacentini
DO  - 0004-6361/201321562
PY  - 2014///
SN  - 0004-6361
TI  - Planck 2013 results. XIV. Zodiacal emission
T2  - Astronomy and Astrophysics
UR  - http://dx.doi.org/10.1051/0004-6361/201321562
UR  - http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000345282600020&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=1ba7043ffcc86c417c072aa74d649202
UR  - http://hdl.handle.net/10044/1/60468
VL  - 571
ER  -

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