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@article{Ade:2014:0004-6361/201321538,
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 Battaner, E and Benabed, K and Benoit, A and Benoit-Levy, A and Bernard, J-P and Bersanelli, M and Bertincourt, B and Bielewicz, P and Bobin, J and Bock, JJ and Bond, JR and Borrill, J and Bouchet, FR and Boulanger, F and Bridges, M and Bucher, M and Burigana, C and Cardoso, J-F and Catalano, A and Challinor, 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 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 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, TA and Eriks},
doi = {0004-6361/201321538},
journal = {ASTRONOMY & ASTROPHYSICS},
title = {Planck 2013 results. VIII. HFI photometric calibration and mapmaking},
url = {http://dx.doi.org/10.1051/0004-6361/201321538},
volume = {571},
year = {2014}
}

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TY  - JOUR
AB  - This paper describes the methods used to produce photometrically calibrated maps from the Planck High Frequency Instrument (HFI) cleaned, time-ordered information. HFI observes the sky over a broad range of frequencies, from 100 to 857  GHz. To obtain the best calibration accuracy over such a large range, two different photometric calibration schemes have to be used. The 545 and 857 GHz data are calibrated by comparing flux-density measurements of Uranus and Neptune with models of their atmospheric emission. The lower frequencies (below 353  GHz) are calibrated using the solar dipole. A component of this anisotropy is time-variable, owing to the orbital motion of the satellite in the solar system. Photometric calibration is thus tightly linked to mapmaking, which also addresses low-frequency noise removal. By comparing observations taken more than one year apart in the same configuration, we have identified apparent gain variations with time. These variations are induced by non-linearities in the read-out electronics chain. We have developed an effective correction to limit their effect on calibration. We present several methods to estimate the precision of the photometric calibration. We distinguish relative uncertainties (between detectors, or between frequencies) and absolute uncertainties. Absolute uncertainties lie in the range from 0.54% to 10% from 100 to 857  GHz. We describe the pipeline used to produce the maps from the HFI timelines, based on the photometric calibration parameters, and the scheme used to set the zero level of the maps a posteriori. We also discuss the cross-calibration between HFI and the SPIRE instrument on board Herschel. Finally we summarize the basic characteristics of the set of HFI maps included in the 2013 Planck data release.
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  - Battaner,E
AU  - Benabed,K
AU  - Benoit,A
AU  - Benoit-Levy,A
AU  - Bernard,J-P
AU  - Bersanelli,M
AU  - Bertincourt,B
AU  - Bielewicz,P
AU  - Bobin,J
AU  - Bock,JJ
AU  - Bond,JR
AU  - Borrill,J
AU  - Bouchet,FR
AU  - Boulanger,F
AU  - Bridges,M
AU  - Bucher,M
AU  - Burigana,C
AU  - Cardoso,J-F
AU  - Catalano,A
AU  - Challinor,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  - 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  - 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  - Filliard,C
AU  - Finelli,F
AU  - Forni,O
AU  - Frailis,M
AU  - Franceschi,E
AU  - Galeotta,S
AU  - Ganga,K
AU  - Giard,M
AU  - Giardino,G
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  - Lamarre,J-M
AU  - Lasenby,A
AU  - Laureijs,RJ
AU  - Lawrence,CR
AU  - Le,Jeune M
AU  - Lellouch,E
AU  - Leonardi,R
AU  - Leroy,C
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  - 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  - Maurin,L
AU  - Mazzotta,P
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  - Moneti,A
AU  - Montier,L
AU  - Moreno,R
AU  - Morgante,G
AU  - Mortlock,D
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  - Oxborrow,CA
AU  - Paci,F
AU  - Pagano,L
AU  - Pajot,F
AU  - Paladini,R
AU  - Paoletti,D
AU  - Partridge,B
AU  - Pasian,F
AU  - Patanchon,G
AU  - Pearson,TJ
AU  - Pe
DO  - 0004-6361/201321538
PY  - 2014///
SN  - 1432-0746
TI  - Planck 2013 results. VIII. HFI photometric calibration and mapmaking
T2  - ASTRONOMY & ASTROPHYSICS
UR  - http://dx.doi.org/10.1051/0004-6361/201321538
UR  - http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000345282600011&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=1ba7043ffcc86c417c072aa74d649202
UR  - http://hdl.handle.net/10044/1/60472
VL  - 571
ER  -

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