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    Planck 2015 results III. LFI systematic uncertainties

    Ade, P.A.R. and Aumont, J. and Baccigalupi, C. and Banday, A.J. and Barreiro, R.B. and Bartolo, N. and Basak, S. and Battaglia, P. and Battaner, E. and Benabed, K. and Benoit-Lévy, A. and Bernard, J.-P. and Bersanelli, M. and Bielewicz, P. and Bonaldi, A. and Bonavera, L. and Bond, J.R. and Borrill, J. and Burigana, C. and Butler, R.C. and Calabrese, E. and Catalano, A. and Christensen, P.R. and Colombo, L.P.L. and Cruz, M. and Curto, A. and Cuttaia, F. and Danese, L. and Davies, R.D. and Davis, R.J. and De Bernardis, P. and de Rosa, A. and de Zotti, G. and Delabrouille, J. and Dickinson, C. and Diego, J.M. and Dore, O. and Ducout, A. and Dupac, X. and Elsner, F. and Enßlin, T.A. and Eriksen, H.K. and Finelli, F. and Frailis, M. and Franceschet, C. and Franceschi, E. and Galeotta, S. and Galli, S. and Ganga, K. and Ghosh, T. and Giard, M. and Giraud-Héraud, Y. and Gjerløw, E. and Gonzalez-Nuevo, J. and Gorski, K.M. and Gregorio, A. and Gruppuso, A. and Hansen, F.K. and Harrison, D. and Hernandez-Monteagudo, C. and Herranz, D. and Hildebrandt, S.R. and Hivon, E. and Hobson, M. and Hornstrup, A. and Hovest, W. and Huffenberger, K.M. and Hurier, G. and Jaffe, A.H. and Jaffe, T.R. and Keihanen, E. and Keskitalo, R. and Kiiveri, K. and Kisner, T.S. and Knoche, J. and Krachmalnicoff, N. and Kunz, M. and Kurki-Suonio, H. and Lagache, G. and Lamarre, J.-M. and Lasenby, A. and Lattanzi, M. and Lawrence, C.R. and Leahy, J.P. and Leonardi, R. and Levrier, F. and Liguori, M. and Lilje, P.B. and Linden-Vornle, M. and Lindholm, V. and Lopez-Caniego, M. and Lubin, P.M. and Macias-Perez, J.F. and Maffei, B. and Maggio, G. and Maino, D. and Mandolesi, N. and Mangilli, A. and Maris, M. and Martin, P.G. and Martinez-Gonzalez, E. and Masi, S. and Matarrese, S. and Meinhold, P.R. and Mennella, A. and Migliaccio, M. and Mitra, S. and Montier, L. and Morgante, G. and Mortlock, D. and Munshi, D. and Murphy, J.Anthony and Nati, F. and Natoli, P. and Noviello, F. and Paci, F. and Pagano, L. and Pajot, F. and Paoletti, D. and Partridge, B. and Pasian, F. and Pearson, T.J. and Perdereau, O. and Pettorino, V. and Piacentini, F. and Pointecouteau, E. and Polenta, G. and Pratt, G.W. and Puget, J.-L. and Rachen, J.P. and Reinecke, M. and Remazeilles, M. and Renzi, A. and Ristorcelli, I. and Rocha, G. and Rosset, C. and Rossetti, M. and Roudier, G. and Rubino-Martin, J.A. and Rusholme, B. and Sandri, M. and Santos, D. and Savelainen, M. and Scott, D. and Stolyarov, V. and Stompor, R. and Suur-Uski, A.-S. and Sygnet, J.-F. and Tauber, J.A. and Tavagnacco, D. and Terenzi, L. and Toffolatti, L. and Tomasi, M. and Tristram, M. and Tucci, M. and Umana, G. and Valenziano, L. and Valiviita, J. and Van Tent, B. and Vassallo, T. and Vielva, P. and Villa, F. and Wade, L.A. and Wandelt, B.D. and Yvon, D. and Zacchei, A. and Zibin, J.P. and Zonca, A. (2016) Planck 2015 results III. LFI systematic uncertainties. Astronomy & Astrophysics, 594 (A3). ISSN 0004-6361

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    We present the current accounting of systematic effect uncertainties for the Low Frequency Instrument (LFI) that are relevant to the 2015 release of the Planck cosmological results, showing the robustness and consistency of our data set, especially for polarization analysis. We use two complementary approaches: (i) simulations based on measured data and physical models of the known systematic effects; and (ii) analysis of difference maps containing the same sky signal (“null-maps”). The LFI temperature data are limited by instrumental noise. At large angular scales the systematic effects are below the cosmic microwave background (CMB) temperature power spectrum by several orders of magnitude. In polarization the systematic uncertainties are dominated by calibration uncertainties and compete with the CMB E-modes in the multipole range 10–20. Based on our model of all known systematic effects, we show that these effects introduce a slight bias of around 0.2σ on the reionization optical depth derived from the 70GHz EE spectrum using the 30 and 353GHz channels as foreground templates. At 30GHz the systematic effects are smaller than the Galactic foreground at all scales in temperature and polarization, which allows us to consider this channel as a reliable template of synchrotron emission. We assess the residual uncertainties due to LFI effects on CMB maps and power spectra after component separation and show that these effects are smaller than the CMB amplitude at all scales. We also assess the impact on non-Gaussianity studies and find it to be negligible. Some residuals still appear in null maps from particular sky survey pairs, particularly at 30 GHz, suggesting possible straylight contamination due to an imperfect knowledge of the beam far sidelobes.

    Item Type: Article
    Keywords: Planck Collaboration; cosmic background radiation; cosmology: observations; space vehicles: instruments; methods: data analysis;
    Academic Unit: Faculty of Science and Engineering > Experimental Physics
    Item ID: 14346
    Identification Number:
    Depositing User: Dr. Anthony Murphy
    Date Deposited: 15 Apr 2021 16:08
    Journal or Publication Title: Astronomy & Astrophysics
    Publisher: EDP Sciences
    Refereed: Yes

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