Planck 2013 results. XXXI. Consistency of the Planck data

被引:73
作者
Ade, P. A. R. [79 ]
Arnaud, M. [67 ]
Ashdown, M. [7 ,64 ]
Aumont, J. [54 ]
Baccigalupi, C. [78 ]
Banday, A. J. [10 ,85 ]
Barreiro, R. B. [61 ]
Battaner, E. [86 ,87 ]
Benabed, K. [55 ,84 ]
Benoit-Levy, A. [22 ,55 ,84 ]
Bernard, J. -P. [10 ,85 ]
Bersanelli, M. [31 ,45 ]
Bielewicz, P. [10 ,78 ,85 ]
Bond, J. R. [9 ]
Borrill, J. [13 ,81 ]
Bouchet, F. R. [55 ,84 ]
Burigana, C. [29 ,44 ]
Cardoso, J. -F. [1 ,55 ,68 ,69 ]
Catalano, A. [66 ,70 ]
Challinor, A. [12 ,57 ,64 ]
Chamballu, A. [14 ,54 ,67 ]
Chiang, H. C. [8 ,25 ]
Christensen, P. R. [34 ,75 ]
Clements, D. L. [51 ]
Colombi, S. [55 ,84 ]
Colombo, L. P. L. [21 ,62 ]
Couchot, F. [65 ]
Coulais, A. [66 ]
Crill, B. P. [62 ,76 ]
Curto, A. [7 ,61 ]
Cuttaia, F. [44 ]
Danese, L. [78 ]
Davies, R. D. [63 ]
Davis, R. J. [63 ]
de Bernardis, P. [30 ]
de Rosa, A. [44 ]
de Zotti, G. [41 ,78 ]
Delabrouille, J. [1 ]
Desert, F. -X. [49 ]
Dickinson, C. [63 ]
Diego, J. M. [61 ]
Dole, H. [53 ,54 ]
Donzelli, S. [45 ]
Dore, O. [11 ,62 ]
Douspis, M. [54 ]
Dupac, X. [36 ]
Ensslin, T. A. [72 ]
Eriksen, H. K. [58 ]
Finelli, F. [44 ,46 ]
Forni, O. [10 ,85 ]
机构
[1] Univ Paris Diderot, Sorbonne Paris Cite, CNRS IN2P3, Observ Paris,APC,CEA Irfu, F-75205 Paris 13, France
[2] Aalto Univ, Metsahovi Radio Observ, Aalto 00076, Finland
[3] Dept Radio Sci & Engn, Aalto 00076, Finland
[4] African Inst Math Sci, ZA-7945 Cape Town, South Africa
[5] Agenzia Spaziale Italiana Sci Data Ctr, I-00133 Rome, Italy
[6] Agenzia Spaziale Italiana, Rome, Italy
[7] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England
[8] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa
[9] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada
[10] CNRS, IRAP, F-31028 Toulouse 4, France
[11] CALTECH, Pasadena, CA 91125 USA
[12] Univ Cambridge, DAMTP, Ctr Theoret Cosmol, Cambridge CB3 0WA, England
[13] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA
[14] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France
[15] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark
[16] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland
[17] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain
[18] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands
[19] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA
[20] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada
[21] Univ So Calif, Dana & David Dornsife Coll Letter Arts & Sci, Dept Phys & Astron, Los Angeles, CA 90089 USA
[22] UCL, Dept Phys & Astron, London WC1E 6BT, England
[23] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA
[24] Univ Helsinki, Dept Phys, Helsinki 00014, Finland
[25] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA
[26] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA
[27] Univ Illinois, Dept Phys, Urbana, IL USA
[28] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy
[29] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy
[30] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy
[31] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy
[32] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy
[33] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy
[34] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark
[35] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain
[36] European Space Agcy, ESAC, Planck Sci Off, Madrid 28691, Spain
[37] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands
[38] Turku Univ, Finnish Ctr Astron ESO FINCA, Piikkio 21500, Finland
[39] Haverford Coll, Dept Astron, Haverford, PA 19041 USA
[40] Univ Helsinki, Inst Phys, FIN-00014 Helsinki, Finland
[41] Osserv Astron Padova, INAF, I-35122 Padua, Italy
[42] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy
[43] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy
[44] IASF Bologna, INAF, I-40129 Bologna, Italy
[45] IASF Milano, INAF, I-20133 Milan, Italy
[46] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy
[47] Univ Roma La Sapienza, INFN, Sez Roma 1, I-00185 Rome, Italy
[48] Ist Nazl Fis Nucl, Natl Inst Nucl Phys, I-34127 Trieste, Italy
[49] Univ Grenoble 1, IPAG, CNRS INSU, UMR 5274, F-38041 Grenoble, France
[50] IUCAA, Pune 411007, Maharashtra, India
关键词
cosmology: observations; cosmic background radiation; instrumentation: detectors; MICROWAVE; MAPS;
D O I
10.1051/0004-6361/201423743
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The Planck design and scanning strategy provide many levels of redundancy that can be exploited to provide tests of internal consistency. One of the most important is the comparison of the 70 GHz (amplifier) and 100 GHz (bolometer) channels. Based on different instrument technologies, with feeds located differently in the focal plane, analysed independently by different teams using different software, and near the minimum of diffuse foreground emission, these channels are in effect two different experiments. The 143 GHz channel has the lowest noise level on Planck, and is near the minimum of unresolved foreground emission. In this paper, we analyse the level of consistency achieved in the 2013 Planck data. We concentrate on comparisons between the 70, 100, and 143 GHz channel maps and power spectra, particularly over the angular scales of the first and second acoustic peaks, on maps masked for diffuse Galactic emission and for strong unresolved sources. Difference maps covering angular scales from 8 degrees to 15 ' are consistent with noise, and show no evidence of cosmic microwave background structure. Including small but important corrections for unresolved-source residuals, we demonstrate agreement (measured by deviation of the ratio from unity) between 70 and 100 GHz power spectra averaged over 70 <= l <= 390 at the 0.8% level, and agreement between 143 and 100 GHz power spectra of 0.4% over the same l range. These values are within and consistent with the overall uncertainties in calibration given in the Planck 2013 results. We also present results based on the 2013 likelihood analysis showing consistency at the 0.35% between the 100, 143, and 217 GHz power spectra. We analyse calibration procedures and beams to determine what fraction of these differences can be accounted for by known approximations or systematic errors that could be controlled even better in the future, reducing uncertainties still further. Several possible small improvements are described. Subsequent analysis of the beams quantifies the importance of asymmetry in the near sidelobes, which was not fully accounted for initially, affecting the 70/100 ratio. Correcting for this, the 70, 100, and 143 GHz power spectra agree to 0.4% over the first two acoustic peaks. The likelihood analysis that produced the 2013 cosmological parameters incorporated uncertainties larger than this. We show explicitly that correction of the missing near sidelobe power in the HFI channels would result in shifts in the posterior distributions of parameters of less than 0.3 sigma except for As, the amplitude of the primordial curvature perturbations at 0.05 Mpc(-1), which changes by about 1 sigma. We extend these comparisons to include the sky maps from the complete nine-year mission of the Wilkinson Microwave Anisotropy Probe (WMAP), and find a roughly 2% difference between the Planck and WMAP power spectra in the region of the first acoustic peak.
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