Planck 2013 results. III. LFI systematic uncertainties
Planck Collaboration, 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, J. J. Bock, A. Bonaldi, L. Bonavera, J. R. Bond, J. Borrill, F. R. Bouchet, M. Bridges, M. Bucher, C. Burigana, R. C. Butler, J. -F. Cardoso, A. Catalano, A. Chamballu, L. -Y Chiang, P. R. Christensen, S. Church, S. Colombi, L. P. L. Colombo, B. P. Crill, M. Cruz, A. Curto, F. Cuttaia, L. Danese, R. D. Davies, R. J. Davis, P. de Bernardis, A. de Rosa, G. de Zotti, J. Delabrouille, J. Dick, C. Dickinson, J. M. Diego, H. Dole, S. Donzelli, O. Doré, M. Douspis, X. Dupac, G. Efstathiou, T. A. Enßlin, H. K. Eriksen, F. Finelli, O. Forni, M. Frailis, E. Franceschi, T. C. Gaier, S. Galeotta, K. Ganga, M. Giard, Y. Giraud-Héraud, E. Gjerløw, J. González-Nuevo, K. M. Górski, S. Gratton, A. Gregorio, A. Gruppuso, F. K. Hansen, D. Hanson, D. Harrison, 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, T. R. Jaffe, A. H. Jaffe, J. Jewell, W. C. Jones, M. Juvela, P. Kangaslahti, E. Keihänen, R. Keskitalo, K. Kiiveri, T. S. Kisner, J. Knoche, L. Knox, M. Kunz, H. Kurki-Suonio, G. Lagache, A. Lähteenmäki, J. -M. Lamarre, A. Lasenby, R. J. Laureijs, C. R. Lawrence, J. P. Leahy, R. Leonardi, J. Lesgourgues, M. Liguori, P. B. Lilje, V. Lindholm, M. Linden-Vørnle, M. López-Caniego, P. M. Lubin, J. F. Macías-Pérez, D. Maino, N. Mandolesi, M. Maris, D. J. Marshall, P. G. Martin, E. Martínez-González, S. Masi, S. Matarrese, F. Matthai, P. Mazzotta, P. R. Meinhold, A. Melchiorri, L. Mendes, A. Mennella, M. Migliaccio, S. Mitra, A. Moneti, L. Montier, G. Morgante, D. Mortlock, A. Moss, D. Munshi, P. Naselsky, P. Natoli, C. B. Netterfield, H. U. Nørgaard-Nielsen, D. Novikov, I. Novikov, I. J. O'Dwyer, S. Osborne, F. Paci, L. Pagano, R. Paladini, D. Paoletti, B. Partridge, F. Pasian, G. Patanchon, D. Pearson, M. Peel, O. Perdereau, L. Perotto, F. Perrotta, E. Pierpaoli, D. Pietrobon, S. Plaszczynski, P. Platania, E. Pointecouteau, G. Polenta, N. Ponthieu, L. Popa, T. Poutanen, G. W. Pratt, G. Prézeau, S. Prunet, J. -L. Puget, J. P. Rachen, R. Rebolo, M. Reinecke, M. Remazeilles, S. Ricciardi, T. Riller, G. Rocha, C. Rosset, M. Rossetti, G. Roudier, J. A. Rubiño-Martín, B. Rusholme, M. Sandri, D. Santos, D. Scott, M. D. Seiffert, E. P. S. Shellard, L. D. Spencer, J. -L. Starck, V. Stolyarov, R. Stompor, F. Sureau, D. Sutton, A. -S. Suur-Uski, J. -F. Sygnet, J. A. Tauber, D. Tavagnacco, L. Terenzi, L. Toffolatti, M. Tomasi, M. Tristram, M. Tucci, J. Tuovinen, M. Türler, G. Umana, L. Valenziano, J. Valiviita, B. Van Tent, J. Varis, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, R. Watson, A. Wilkinson, D. Yvon, A. Zacchei, A. Zonca
TL;DR
Planck 2013 results III analyzes LFI systematic uncertainties for temperature maps and power spectra. The authors adopt a dual strategy: (a) null tests by differencing maps with the same sky signal to reveal residuals, and (b) end-to-end timeline simulations to propagate known effects through the analysis pipeline. They find that the overall impact of systematics is at least two orders of magnitude below the CMB temperature power spectrum, with far-sidelobe straylight and calibration as the main remaining concerns. A residual low-ell signal, particularly at 30 GHz, suggests Galactic straylight as a primary culprit and motivates further sidelobe modelling and calibration refinements for the forthcoming polarization data release. Overall, the results support the robustness of Planck-LFI temperature measurements and guide improvements for polarization.
Abstract
We present the current estimate of instrumental and systematic effect uncertainties for the Planck-Low Frequency Instrument relevant to the first release of the Planck cosmological results. We give an overview of the main effects and of the tools and methods applied to assess residuals in maps and power spectra. We also present an overall budget of known systematic effect uncertainties, which are dominated sidelobe straylight pick-up and imperfect calibration. However, even these two effects are at least two orders of magnitude weaker than the cosmic microwave background (CMB) fluctuations as measured in terms of the angular temperature power spectrum. A residual signal above the noise level is present in the multipole range $\ell<20$, most notably at 30 GHz, and is likely caused by residual Galactic straylight contamination. Current analysis aims to further reduce the level of spurious signals in the data and to improve the systematic effects modelling, in particular with respect to straylight and calibration uncertainties.