Planck 2015 results. IX. Diffuse component separation: CMB maps
Creators: name: Planck Collaboration
name: Adam, R.
name: Ade, P. A. R.
name: Aghanim, N.
name: Arnaud, M.
name: Ashdown, M.
name: Aumont, J.
name: Baccigalupi, C.
name: Banday, A. J.
name: Barreiro, R. B.
name: Bartlett, J. G.
name: Bartolo, N.
name: Basak, S.
name: Battaner, E.
name: Benabed, K.
name: Benoît, A.
name: Benoit-Lévy, A.
name: Bernard, J. -P.
name: Bersanelli, M.
name: Bielewicz, P.
name: Bonaldi, A.
name: Bonavera, L.
name: Bond, J. R.
name: Borrill, J.
name: Bouchet, F. R.
name: Boulanger, F.
name: Bucher, M.
name: Burigana, C.
name: Butler, R. C.
name: Calabrese, E.
name: Cardoso, J. -F.
name: Casaponsa, B.
name: Castex, G.
name: Catalano, A.
name: Challinor, A.
name: Chamballu, A.
name: Chary, R. -R.
name: Chiang, H. C.
name: Christensen, P. R.
name: Clements, D. L.
name: Colombi, S.
name: Colombo, L. P. L.
name: Combet, C.
name: Couchot, F.
name: Coulais, A.
name: Crill, B. P.
name: Curto, A.
name: Cuttaia, F.
name: Danese, L.
name: Davies, R. D.
name: Davis, R. J.
name: de Bernardis, P.
name: de Rosa, A.
name: de Zotti, G.
name: Delabrouille, J.
name: Désert, F. -X.
name: Dickinson, C.
name: Diego, J. M.
name: Dole, H.
name: Donzelli, S.
name: Doré, O.
name: Douspis, M.
name: Ducout, A.
name: Dupac, X.
name: Efstathiou, G.
name: Elsner, F.
name: Enßlin, T. A.
name: Eriksen, H. K.
name: Falgarone, E.
name: Fantaye, Y.
name: Fergusson, J.
name: Finelli, F.
name: Forni, O.
name: Frailis, M.
name: Fraisse, A. A.
name: Franceschi, E.
name: Frejsel, A.
name: Galeotta, S.
name: Galli, S.
name: Ganga, K.
name: Ghosh, T.
name: Giard, M.
name: Giraud-Héraud, Y.
name: Gjerløw, E.
name: González-Nuevo, J.
name: Górski, K. M.
name: Gratton, S.
name: Gregorio, A.
name: Gruppuso, A.
name: Gudmundsson, J. E.
name: Hansen, F. K.
name: Hanson, D.
name: Harrison, D. L.
name: Helou, G.
name: Henrot-Versillé, S.
name: Hernández-Monteagudo, C.
name: Herranz, D.
name: Hildebrandt, S. R.
name: Hivon, E.
name: Hobson, M.
name: Holmes, W. A.
name: Hornstrup, A.
name: Hovest, W.
name: Huffenberger, K. M.
name: Hurier, G.
name: Jaffe, A. H.
name: Jaffe, T. R.
name: Jones, W. C.
name: Juvela, M.
name: Keihänen, E.
name: Keskitalo, R.
name: Kisner, T. S.
name: Kneissl, R.
name: Knoche, J.
name: Krachmalnicoff, N.
name: Kunz, M.
name: Kurki-Suonio, H.
name: Lagache, G.
name: Lamarre, J. -M.
name: Lasenby, A.
name: Lattanzi, M.
name: Lawrence, C. R.
name: Jeune, M. Le
name: Leonardi, R.
name: Lesgourgues, J.
name: Levrier, F.
name: Liguori, M.
name: Lilje, P. B.
name: Linden-Vørnle, M.
name: López-Caniego, M.
name: Lubin, P. M.
name: Macías-Pérez, J. F.
name: Maggio, G.
name: Maino, D.
name: Mandolesi, N.
name: Mangilli, A.
name: Marshall, D. J.
name: Martin, P. G.
name: Martínez-González, E.
name: Masi, S.
name: Matarrese, S.
name: Mazzotta, P.
name: McGehee, P.
name: Meinhold, P. R.
name: Melchiorri, A.
name: Mendes, L.
name: Mennella, A.
name: Migliaccio, M.
name: Mitra, S.
name: Miville-Deschênes, M. -A.
name: Molinari, D.
name: Moneti, A.
name: Montier, L.
name: Morgante, G.
name: Mortlock, D.
name: Moss, A.
name: Munshi, D.
name: Murphy, J. A.
name: Naselsky, P.
name: Nati, F.
name: Natoli, P.
name: Netterfield, C. B.
name: Nørgaard-Nielsen, H. U.
name: Noviello, F.
name: Novikov, D.
name: Novikov, I.
name: Oxborrow, C. A.
name: Paci, F.
name: Pagano, L.
name: Pajot, F.
name: Paladini, R.
name: Paoletti, D.
name: Pasian, F.
name: Patanchon, G.
name: Pearson, T. J.
name: Perdereau, O.
name: Perotto, L.
name: Perrotta, F.
name: Pettorino, V.
name: Piacentini, F.
name: Piat, M.
name: Pierpaoli, E.
name: Pietrobon, D.
name: Plaszczynski, S.
name: Pointecouteau, E.
name: Polenta, G.
name: Pratt, G. W.
name: Prézeau, G.
name: Prunet, S.
name: Puget, J. -L.
name: Rachen, J. P.
name: Racine, B.
name: Reach, W. T.
name: Rebolo, R.
name: Reinecke, M.
name: Remazeilles, M.
name: Renault, C.
name: Renzi, A.
name: Ristorcelli, I.
name: Rocha, G.
name: Rosset, C.
name: Rossetti, M.
name: Roudier, G.
name: Rubiño-Martín, J. A.
name: Rusholme, B.
name: Sandri, M.
name: Santos, D.
name: Savelainen, M.
name: Savini, G.
name: Scott, D.
name: Seiffert, M. D.
name: Shellard, E. P. S.
name: Spencer, L. D.
name: Stolyarov, V.
name: Stompor, R.
name: Sudiwala, R.
name: Sunyaev, R.
name: Sutton, D.
name: Suur-Uski, A. -S.
name: Sygnet, J. -F.
name: Tauber, J. A.
name: Terenzi, L.
name: Toffolatti, L.
name: Tomasi, M.
name: Tristram, M.
name: Trombetti, T.
name: Tucci, M.
name: Tuovinen, J.
name: Valenziano, L.
name: Valiviita, J.
name: Van Tent, B.
name: Vielva, P.
name: Villa, F.
name: Wade, L. A.
name: Wandelt, B. D.
name: Wehus, I. K.
name: Yvon, D.
name: Zacchei, A.
name: Zonca, A.
Publisher: name: arXiv
Year: 2015
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We present foreground-reduced CMB maps derived from the full Planck data set in both temperature and polarization. Compared to the corresponding Planck 2013 temperature sky maps, the total data volume is larger by a factor of 3.2 for frequencies between 30 and 70 GHz, and by 1.9 for frequencies between 100 and 857 GHz. In addition, systematic errors in the forms of temperature-to-polarization leakage, analogue-to-digital conversion uncertainties, and very long time constant errors have been dramatically reduced, to the extent that the cosmological polarization signal may now be robustly recovered on angular scales $\ell\gtrsim40$. On the very largest scales, instrumental systematic residuals are still non-negligible compared to the expected cosmological signal, and modes with $\ell &lt; 20$ are accordingly suppressed in the current polarization maps by high-pass filtering. As in 2013, four different CMB component separation algorithms are applied to these observations, providing a measure of stability with respect to algorithmic and modelling choices. The resulting polarization maps have rms instrumental noise ranging between 0.21 and 0.27$\,μ\textrm{K}$ averaged over 55 arcmin pixels, and between 4.5 and 6.1$\,μ\textrm{K}$ averaged over 3.4 arcmin pixels. The cosmological parameters derived from the analysis of temperature power spectra are in agreement at the $1σ$ level with the Planck 2015 likelihood. Unresolved mismatches between the noise properties of the data and simulations prevent a satisfactory description of the higher-order statistical properties of the polarization maps. Thus, the primary applications of these polarization maps are those that do not require massive simulations for accurate estimation of uncertainties, for instance estimation of cross-spectra and cross-correlations, or stacking analyses.
description: 42 pages, 36 figures. Submitted to A&amp;A