Cover Image

Planck 2015 results: IX. Diffuse component separation : CMB maps

Show other versions (1)

We present foreground-reduced cosmic microwave background (CMB) maps derived from the full <i>Planck<i/> data set in both temperature and polarization. Compared to the corresponding <i>Planck<i/> 2013 temperature sky maps, the total data volume is larger by a factor of 3.2 fo...

Full description

Saved in:
Bibliographic Details
Main Authors: Adam, Rémi (Author) , Pettorino, Valeria (Author)
Format: Article (Journal)
Language:English
Published: 20 September 2016
In: Astronomy and astrophysics
Year: 2016, Volume: 594, Pages: 1-42
ISSN:1432-0746
DOI:10.1051/0004-6361/201525936
Online Access:Verlag, lizenzpflichtig, Volltext: https://doi.org/10.1051/0004-6361/201525936
Verlag, lizenzpflichtig, Volltext: https://www.aanda.org/articles/aa/abs/2016/10/aa25936-15/aa25936-15.html
Get full text
Author Notes:Planck Collaboration: R. Adam, P.A.R. Ade, N. Aghanim, M. Arnaud, M. Ashdown, J. Aumont, C. Baccigalupi, A.J. Banday, R.B. Barreiro, J.G. Bartlett, N. Bartolo, S. Basak, E. Battaner, K. Benabed, A. Benoît, A. Benoit-Lévy, J.-P. Bernard, M. Bersanelli, P. Bielewicz, J.J. Bock, A. Bonaldi, L. Bonavera, J.R. Bond, J. Borrill, F.R. Bouchet, F. Boulanger, M. Bucher, C. Burigana, R.C. Butler, E. Calabrese, J.-F. Cardoso, B. Casaponsa, G. Castex, A. Catalano, A. Challinor, A. Chamballu, R.-R. Chary, H.C. Chiang, P.R. Christensen, 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, R.J. Davis, P. de Bernardis, A. de Rosa, G. de Zotti, J. Delabrouille, F.-X. Désert, C. Dickinson, J.M. Diego, H. Dole, S. Donzelli, O. Doré, M. Douspis, A. Ducout, X. Dupac, G. Efstathiou, F. Elsner, T.A. Enßlin, H.K. Eriksen, E. Falgarone, Y. Fantaye, J. Fergusson, F. Finelli, O. Forni, M. Frailis, A.A. Fraisse, E. Franceschi, A. Frejsel, S. Galeotta, S. Galli, K. Ganga, T. Ghosh, M. Giard, Y. Giraud-Héraud, E. Gjerløw, J. González-Nuevo, K.M. Górski, S. Gratton, A. Gregorio, A. Gruppuso, J.E. Gudmundsson, F.K. Hansen, D. Hanson, D.L. Harrison, G. Helou, S. Henrot-Versillé, C. Hernández-Monteagudo, D. Herranz, S.R. Hildebrandt, E. Hivon, M. Hobson, W.A. Holmes, A. Hornstrup, W. Hovest, K.M. Huffenberger, G. Hurier, A.H. Jaffe, T.R. Jaffe, W.C. Jones, M. Juvela, E. Keihänen, R. Keskitalo, T.S. Kisner, R. Kneissl, J. Knoche, N. Krachmalnicoff, M. Kunz, H. Kurki-Suonio, G. Lagache, J.-M. Lamarre, A. Lasenby, M. Lattanzi, C.R. Lawrence, M. Le Jeune, R. Leonardi, J. Lesgourgues, F. Levrier, M. Liguori, P.B. Lilje, M. Linden-Vørnle, M. López-Caniego, P.M. Lubin, J.F. Macías-Pérez, G. Maggio, D. Maino, N. Mandolesi, A. Mangilli, M. Maris, D.J. Marshall, P.G. Martin, E. Martínez-González, S. Masi, S. Matarrese, P. McGehee, P.R. Meinhold, A. Melchiorri, L. Mendes, A. Mennella, M. Migliaccio, S. Mitra, M.-A. Miville-Deschênes, D. Molinari, A. Moneti, L. Montier, G. Morgante, D. Mortlock, A. Moss, D. Munshi, J.A. Murphy, P. Naselsky, F. Nati, P. Natoli, C.B. Netterfield, H.U. Nørgaard-Nielsen, F. Noviello, D. Novikov, I. Novikov, C.A. Oxborrow, F. Paci, L. Pagano, F. Pajot, R. Paladini, D. Paoletti, F. Pasian, G. Patanchon, T.J. Pearson, O. Perdereau, L. Perotto, F. Perrotta, V. Pettorino, F. Piacentini, M. Piat, E. Pierpaoli, D. Pietrobon, S. Plaszczynski, E. Pointecouteau, G. Polenta, 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, A. Renzi, I. Ristorcelli, G. Rocha, C. Rosset, M. Rossetti, G. Roudier, J.A. Rubiño-Martín, B. Rusholme, M. Sandri, D. Santos, M. Savelainen, G. Savini, D. Scott, M.D. Seiffert, E.P.S. Shellard, L.D. Spencer, V. Stolyarov, R. Stompor, R. Sudiwala, R. Sunyaev, D. Sutton, A.-S. Suur-Uski, J.-F. Sygnet, J.A. Tauber, L. Terenzi, L. Toffolatti, M. Tomasi, M. Tristram, T. Trombetti, M. Tucci, J. Tuovinen, L. Valenziano, J. Valiviita, F. Van Tent, P. Vielva, F. Villa, L.A. Wade, B.D. Wandelt, I.K. Wehus, D. Yvon, A. Zacchei, and A. Zonca
Description
Summary:We present foreground-reduced cosmic microwave background (CMB) maps derived from the full <i>Planck<i/> data set in both temperature and polarization. Compared to the corresponding <i>Planck<i/> 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 <i>ℓ<i/> ≳ 40. On the very largest scales, instrumental systematic residuals are still non-negligible compared to the expected cosmological signal, and modes with <i>ℓ<i/>< 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<i>μ<i/>K averaged over 55′ pixels, and between 4.5 and 6.1<i>μ<i/>K averaged over pixels. The cosmological parameters derived from the analysis of temperature power spectra are in agreement at the 1<i>σ<i/> level with the <i>Planck<i/> 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. However, the amplitude of primordial non-Gaussianity is consistent with zero within 2<i>σ<i/> for all local, equilateral, and orthogonal configurations of the bispectrum, including for polarization <i>E<i/>-modes. Moreover, excellent agreement is found regarding the lensing <i>B<i/>-mode power spectrum, both internally among the various component separation codes and with the best-fit <i>Planck<i/> 2015 Λ cold dark matter model.
Item Description:Gesehen am 10.08.2020
Physical Description:Online Resource
ISSN:1432-0746
DOI:10.1051/0004-6361/201525936

Similar Items