We describe the processing of the 531 billion raw data samples from the High Frequency Instrument (hereafter HFI), which we performed to produce six temperature maps from the first 473 days of Planck-HFI survey data. These maps provide an accurate rendition of the sky emission at 100, 143, 217, 353, 545, and 857 GHz with an angular resolution ranging from 9.7 to 4.6 arcmin. The detector noise per (effective) beam solid angle is respectively, 10, 6, 12 and 39 microKelvin in HFI four lowest frequency channel (100--353 GHz) and 13 and 14 kJy/sr for the 545 and 857 GHz channels. Using the 143 GHz channel as a reference, these two high frequency channels are intercalibrated within 5% and the 353 GHz relative calibration is at the percent level. The 100 and 217 GHz channels, which together with the 143 GHz channel determine the high-multipole part of the CMB power spectrum (50 < l <2500), are intercalibrated at better than 0.2 %.
Planck 2013 results : VI. high frequency instrument data processing / P.A.R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. Banday, R. Barreiro, E. Battaner, K. Benabed, A. Benoît, A. Benoit-Lévy, J. Bernard, M. Bersanelli, P. Bielewicz, J. Bobin, J. Bock, J. Bond, J. Borrill, F. Bouchet, F. Boulanger, J. Bowyer, M. Bridges, M. Bucher, C. Burigana, J. Cardoso, A. Catalano, A. Chamballu, R. Chary, X. Chen, L. Chiang, H. Chiang, P. Christensen, S. Church, D. Clements, S. Colombi, L. Colombo, C. Combet, F. Couchot, A. Coulais, B. Crill, A. Curto, F. Cuttaia, L. Danese, R. Davies, R. Davis, P. Bernardis, A. Rosa, G. Zotti, J. Delabrouille, J. Delouis, F. Désert, C. Dickinson, J. Diego, H. Dole, S. Donzelli, O. Doré, M. Douspis, J. Dunkley, X. Dupac, G. Efstathiou, T. Enßlin, H. Eriksen, F. Finelli, O. Forni, M. Frailis, A. Fraisse, E. Franceschi, S. Galeotta, K. Ganga, M. Giard, G. Giardino, D. Girard, Y. Giraud-Héraud, J. González-Nuevo, K. Górski, S. Gratton, A. Gregorio, A. Gruppuso, J. Gudmundsson, F. Hansen, D. Hanson, D. Harrison, G. Helou, S. Henrot-Versillé, O. Herent, C. Hernández-Monteagudo, D. Herranz, S. Hildebrandt, E. Hivon, M. Hobson, W. Holmes, A. Hornstrup, Z. Hou, W. Hovest, K. Huffenberger, G. Hurier, T. Jaffe, A. Jaffe, W. Jones, M. Juvela, E. Keihänen, R. Keskitalo, T. Kisner, R. Kneissl, J. Knoche, L. Knox, M. Kunz, H. Kurki-Suonio, G. Lagache, J. Lamarre, A. Lasenby, R. Laureijs, C. Lawrence, M. Jeune, R. Leonardi, C. Leroy, J. Lesgourgues, M. Liguori, P. Lilje, M. Linden-Vørnle, M. López-Caniego, P. Lubin, J. Macías-Pérez, C. MacTavish, B. Maffei, N. Mandolesi, M. Maris, D. Marshall, P. Martin, E. Martínez-González, S. Masi, S. Matarrese, F. Matthai, P. Mazzotta, P. McGehee, P. Meinhold, A. Melchiorri, L. Mendes, A. Mennella, M. Migliaccio, S. Mitra, M. Miville-Deschênes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, S. Mottet, D. Munshi, P. Naselsky, F. Nati, P. Natoli, C. Netterfield, H. Nørgaard-Nielsen, C. North, F. Noviello, D. Novikov, I. Novikov, F. Orieux, S. Osborne, C. Oxborrow, F. Paci, L. Pagano, F. Pajot, R. Paladini, D. Paoletti, F. Pasian, G. Patanchon, O. Perdereau, L. Perotto, F. Perrotta, F. Piacentini, M. Piat, E. Pierpaoli, D. Pietrobon, S. Plaszczynski, E. Pointecouteau, G. Polenta, N. Ponthieu, L. Popa, T. Poutanen, G. Pratt, G. Prézeau, S. Prunet, J. Puget, J. Rachen, B. Racine, W. Reach, R. Rebolo, M. Reinecke, M. Remazeilles, C. Renault, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, C. Rosset, G. Roudier, M. Rowan-Robinson, B. Rusholme, L. Sanselme, D. Santos, A. Sauvé, G. Savini, E. Shellard, L. Spencer, J. Starck, V. Stolyarov, R. Stompor, R. Sudiwala, F. Sureau, D. Sutton, A. Suur-Uski, J. Sygnet, J. Tauber, D. Tavagnacco, S. Techene, L. Terenzi, M. Tomasi, M. Tristram, M. Tucci, G. Umana, L. Valenziano, J. Valiviita, B. Tent, L. Vibert, P. Vielva, F. Villa, N. Vittorio, L. Wade, B. Wandelt, S. White, D. Yvon, A. Zacchei, A. Zonca. - In: ASTRONOMY & ASTROPHYSICS. - ISSN 0004-6361. - 571(2014 Oct 29), pp. A6.1-A6.44.
Planck 2013 results : VI. high frequency instrument data processing
M. Bersanelli;L. Colombo;S. Donzelli;A. Mennella;M. Tomasi;A. Zonca
2014
Abstract
We describe the processing of the 531 billion raw data samples from the High Frequency Instrument (hereafter HFI), which we performed to produce six temperature maps from the first 473 days of Planck-HFI survey data. These maps provide an accurate rendition of the sky emission at 100, 143, 217, 353, 545, and 857 GHz with an angular resolution ranging from 9.7 to 4.6 arcmin. The detector noise per (effective) beam solid angle is respectively, 10, 6, 12 and 39 microKelvin in HFI four lowest frequency channel (100--353 GHz) and 13 and 14 kJy/sr for the 545 and 857 GHz channels. Using the 143 GHz channel as a reference, these two high frequency channels are intercalibrated within 5% and the 353 GHz relative calibration is at the percent level. The 100 and 217 GHz channels, which together with the 143 GHz channel determine the high-multipole part of the CMB power spectrum (50 < l <2500), are intercalibrated at better than 0.2 %.
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