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. J. Banday, R. B. Barreiro, E. Battaner, K. Benabed, A. Benoît, A. Benoit-Lévy, J. -P. Bernard, M. Bersanelli, P. Bielewicz, J. Bobin, Jacob Bock, J. R. BondJ. Borrill, F. R. Bouchet, F. Boulanger, J. W. Bowyer, M. Bridges, M. Bucher, C. Burigana, J. -F. Cardoso, A. Catalano, A. Chamballu, R. -R. Chary, X. Chen, Lung-Yih Chiang, H. C. Chiang, P. R. Christensen, S. Church, D. L. Clements, S. Colombi, L. P. L. Colombo, C. Combet, F. Couchot, A. Coulais, B. P. Crill, A. Curto, F. Cuttaia, L. Danese, R. D. Davies, Rebecca Davis, P. de Bernardis, A. de Rosa, G. de Zotti, J. Delabrouille, J. -M. Delouis, F. -X. Désert, C. Dickinson, J. M. Diego, H. Dole, S. Donzelli, O. Doré, M. Douspis, J. Dunkley, X. Dupac, G. Efstathiou, T. A. Enßlin, H. K. Eriksen, F. Finelli, O. Forni, M. Frailis, A. A. Fraisse, E. Franceschi, S. Galeotta, K. Ganga, M. Giard, G. Giardino, D. Girard, Y. Giraud-Héraud, J. González-Nuevo, K. M. Górski, S. Gratton, A. Gregorio, A. Gruppuso, J. E. Gudmundsson, F. K. Hansen, D. Hanson, D. Harrison, G. Helou, S. Henrot-Versillé, O. Herent, C. Hernández-Monteagudo, D. Herranz, Steen Hildebrandt, E. Hivon, M. Hobson, W. A. Holmes, Allan Hornstrup, Z. Hou, W. Hovest, K. M. Huffenberger, G. Hurier, T. R. Jaffe, A. H. Jaffe, W. C. Jones, M. Juvela, E. Keihänen, R. Keskitalo, T. S. Kisner, R. Kneissl, J. Knoche, L. Knox, M. Kunz, H. Kurki-Suonio, G. Lagache, J. -M. Lamarre, A. Lasenby, R. J. Laureijs, C. R. Lawrence, M. Le Jeune, R. Leonardi, C. Leroy, J. Lesgourgues, M. Liguori, P. B. Lilje, Michael Linden-Vørnle, M. López-Caniego, P. M. Lubin, J. F. Macías-Pérez, C. J. MacTavish, B. Maffei, N. Mandolesi, M. Maris, D. J. Marshall, P. G. Martin, E. Martínez-González, S. Masi, S. Matarrese, F. Matthai, P. Mazzotta, P. McGehee, P. R. Meinhold, A. Melchiorri, L. Mendes, A. Mennella, M. Migliaccio, S. Mitra, M. -A. Miville-Deschênes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, S. Mottet, D. Munshi, P. Naselsky, F. Nati, P. Natoli, C. B. Netterfield, Hans Ulrik Nørgaard-Nielsen, Chris North, F. Noviello, D. Novikov, Igor Dmitrievich Novikov, F. Orieux, S. Osborne, Carol Anne 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. W. Pratt, G. Prézeau, S. Prunet, J. -L. Puget, J. P. Rachen, B. Racine, W. T. 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. P. S. Shellard, L. D. Spencer, J. -L. Starck, V. Stolyarov, R. Stompor, R. Sudiwala, F. Sureau, D. Sutton, A. -S. Suur-Uski, J. -F. Sygnet, J. A. Tauber, D. Tavagnacco, S. Techene, L. Terenzi, M. Tomasi, M. Tristram, M. Tucci, G. Umana, L. Valenziano, J. Valiviita, B. Van Tent, L. Vibert, P. Vielva, Frank Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, S. D. M. White, D. Yvon, A. Zacchei, A. Zonca

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    Abstract

    We describe the processing of the 531 billion raw data samples from the High Frequency Instrument (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 9.07 to 4.06. The detector noise per (effective) beam solid angle is respectively,10, 6 , 12, and 39 µK in the four lowest HFI frequency channels (100-353 GHz) and 13 and 14 kJy sr-1 in the 545 and 857 GHz channels. Relativeto the 143 GHz channel, these two high frequency channels are calibrated to within 5% and the 353 GHz channel to the percent level. The 100 and217 GHz channels, which together with the 143 GHz channel determine the high-multipole part of the CMB power spectrum (50 < ∫ < 2500), are calibrated relative to 143 GHz to better than 0.2%.
    Original languageEnglish
    Article numberA6
    JournalAstronomy & Astrophysics
    Volume571
    Number of pages44
    ISSN0004-6361
    DOIs
    Publication statusPublished - 2013

    Keywords

    • Methods: data analysis
    • Cosmic background radiation
    • Cosmology: observations
    • Surveys

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