Ade, PAR;Aghanim, N;Ansari, R;Arnaud, M;Ashdown, M;Aumont, J;Banday, AJ;Bartelmann, M;Bartlett, JG;Battaner, E;Benabed, K;Benoit, A;Bernard, JP;Bersanelli, M;Bock, JJ;Bond, JR;Borrill, J;Bouchet, FR;Boulanger, F;Bradshaw, T;Bucher, M;Cardoso, JF;Castex, G;Catalano, A;Challinor, A;Chamballu, A;Chary, RR;Chen, X;Chiang, C;Church, S;Clements, DL;Colley, JM;Colombi, S;Couchot, F;Coulais, A;Cressiot, C;Crill, BP;Crook, M;de Bernardis, P;Delabrouille, J;Delouis, JM;Desert, FX;Dolag, K;Dole, H;Dore, O;Douspis, M;Dunkley, J;Efstathiou, G;Filliard, C;Forni, O;Fosalba, P;Ganga, K;Giard, M;Girard, D;Giraud-Heraud, Y;Gispert, R;Gorski, KM;Gratton, S;Griffin, M;Guyot, G;Haissinski, J;Harrison, D;Helou, G;Henrot-Versille, S;Hernandez-Monteagudo, C;Hildebrandt, SR;Hills, R;Hivon, E;Hobson, M;Holmes, WA;Huffenberger, KM;Jaffe, AH;Jones, WC;Kaplan, J;Kneissl, R;Knox, L;Kunz, M;Lagache, G;Lamarre, JM;Lange, AE;Lasenby, A;Lavabre, A;Lawrence, CR;Le Jeune, M;Leroy, C;Lesgourgues, J;Macias-Perez, JF;MacTavish, CJ;Maffei, B;Mandolesi, N;Mann, R;Marleau, F;Marshall, DJ;Masi, S;Matsumura, T;McAuley, I;McGehee, P;Melin, JB;Mercier, C;Mitra, S;Miville-Deschenes, MA;Moneti, A;Montier, L;Mortlock, D;Murphy, A;Nati, F;Netterfield, CB;Norgaard-Nielsen, HU;North, C;Noviello, F;Novikov, D;Osborne, S;Pajot, F;Patanchon, G;Peacocke, T;Pearson, TJ;Perdereau, O;Perotto, L;Piacentini, F;Piat, M;Plaszczynski, S;Pointecouteau, E;Ponthieu, N;Prezeau, G;Prunet, S;Puget, JL;Reach, WT;Remazeilles, M;Renault, C;Riazuelo, A;Ristorcelli, I;Rocha, G;Rosset, C;Roudier, G;Rowan-Robinson, M;Rusholme, B;Saha, R;Santos, D;Savini, G;Schaefer, BM;Shellard, P;Spencer, L;Starck, JL;Stolyarov, V;Stompor, R;Sudiwala, R;Sunyaev, R;Sutton, D;Sygnet, JF;Tauber, JA;Thum, C;Torre, JP;Touze, F;Tristram, M;Van Leeuwen, F;Vibert, L;Vibert, D;Wade, LA;Wandelt, BD;White, SDM;Wiesemeyer, H;Woodcraft, A;Yurchenko, V;Yvon, D;Zacchei, A

2011

December

Astronomy and Astrophysics

Planck early results. VI. The High Frequency Instrument data processing

Published

120 ()

PRE-LAUNCH STATUS IN-FLIGHT PERFORMANCE MAP-MAKING METHOD POWER SPECTRA COMPONENT SEPARATION SKY MAPS MICROWAVE MISSION CALIBRATION NOISE

536

We describe the processing of the 336 billion raw data samples from the High Frequency Instrument (HFI) which we performed to produce six temperature maps from the first 295 days of Planck-HFI survey data. These maps provide an accurate rendition of the sky emission at 100, 143, 217, 353, 545 and 857GHz with an angular resolution ranging from 9.9 to 4.4'. The white noise level is around 1.5 mu K degree or less in the 3 main CMB channels (100-217 GHz). The photometric accuracy is better than 2% at frequencies between 100 and 353 GHz and around 7% at the two highest frequencies. The maps created by the HFI Data Processing Centre reach our goals in terms of sensitivity, resolution, and photometric accuracy. They are already sufficiently accurate and well-characterised to allow scientific analyses which are presented in an accompanying series of early papers. At this stage, HFI data appears to be of high quality and we expect that with further refinements of the data processing we should be able to achieve, or exceed, the science goals of the Planck project.

LES ULIS CEDEX A

0004-6361

10.1051/0004-6361/201116462