Issue |
A&A
Volume 571, November 2014
Planck 2013 results
|
|
---|---|---|
Article Number | A8 | |
Number of page(s) | 25 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361/201321538 | |
Published online | 29 October 2014 |
Planck 2013 results. VIII. HFI photometric calibration and mapmaking
1
APC, AstroParticule et Cosmologie, Université Paris Diderot,
CNRS/IN2P3, CEA/lrfu, Observatoire de Paris, Sorbonne Paris Cité, 10 rue Alice Domon et Léonie
Duquet, 75205
Paris Cedex 13,
France
2
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Science and Engineering, PO Box
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AALTO,
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Town, 7701
Rondebosh, South
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UK
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Juan, 1, planta 2, 44001
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Laboratory, Berkeley,
California,
USA
15
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Gif-sur-Yvette Cedex,
France
16
DTU Space, National Space Institute, Technical University of
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327, 2800
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Denmark
17
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Genève, 24 quai E.
Ansermet, 1211
Genève 4,
Switzerland
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Universidad de Salamanca, 37008
Salamanca,
Spain
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Toronto, Ontario,
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9010, 6500 GL
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26
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Helsinki,
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Princeton, New Jersey, USA
28
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29
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Santa Barbara, California, USA
30
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31
Dipartimento di Fisica e Astronomia G. Galilei, Università degli
Studi di Padova, via Marzolo
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Padova,
Italy
32
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Ferrara, via Saragat
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Ferrara,
Italy
33
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P.le A. Moro 2, 00185
Roma,
Italy
34
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Milano, via Celoria
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Milano,
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35
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Trieste, via A. Valerio
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Trieste,
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36
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Roma,
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37
Discovery Center, Niels Bohr Institute, Blegdamsvej 17, 2100
Copenhagen,
Denmark
38
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19001
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Chile
39
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Castillo, s/n, Urbanización Villafranca del Castillo, Villanueva de la
Cañada, Madrid,
Spain
40
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Netherlands
41
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42
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51
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Université Joseph Fourier, Grenoble 1/CNRS-INSU, UMR 5274, 38041
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Laboratory, Prince Consort
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SW7 2AZ,
UK
55
Infrared Processing and Analysis Center, California Institute of
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CA
91125,
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56
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I, 25 rue des
Martyrs, Grenoble,
France
57
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58
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Paris-Sud 11, Bâtiment
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France
59
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60
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61
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63
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64
Instituto de Física de Cantabria (CSIC-Universidad de
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65
Jet Propulsion Laboratory, California Institute of
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Drive, Pasadena,
California,
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66
Jodrell Bank Centre for Astrophysics, Alan Turing Building, School
of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13
9PL, UK
67
Kavli Institute for Cosmology Cambridge,
Madingley Road, Cambridge, CB3 0HA, UK
68
LAL, Université Paris-Sud, CNRS/IN2P3, 91898
Orsay,
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69
LERMA, CNRS, Observatoire de Paris, 61 avenue de
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Paris,
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70
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Joseph Fourier Grenoble I, CNRS/IN2P3, Institut National Polytechnique de
Grenoble, 53 rue des
Martyrs, 38026
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74
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CNRS, Bâtiment 210,
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75
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76
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80
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81
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Gower Street, London, UK
82
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83
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85
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Moscow,
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Berkeley, California, USA
87
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Karachai-Cherkessian Republic,
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88
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89
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Keble Road, Oxford
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90
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91
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Paris,
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92
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93
University of Granada, Departamento de Física Teórica y del Cosmos,
Facultad de Ciencias, 18071
Granada,
Spain
94
Warsaw University Observatory, Aleje Ujazdowskie 4, 00-478
Warszawa,
Poland
Received:
21
March
2013
Accepted:
8
March
2014
This paper describes the methods used to produce photometrically calibrated maps from the Planck High Frequency Instrument (HFI) cleaned, time-ordered information. HFI observes the sky over a broad range of frequencies, from 100 to 857 GHz. To obtain the best calibration accuracy over such a large range, two different photometric calibration schemes have to be used. The 545 and 857 GHz data are calibrated by comparing flux-density measurements of Uranus and Neptune with models of their atmospheric emission. The lower frequencies (below 353 GHz) are calibrated using the solar dipole. A component of this anisotropy is time-variable, owing to the orbital motion of the satellite in the solar system. Photometric calibration is thus tightly linked to mapmaking, which also addresses low-frequency noise removal. By comparing observations taken more than one year apart in the same configuration, we have identified apparent gain variations with time. These variations are induced by non-linearities in the read-out electronics chain. We have developed an effective correction to limit their effect on calibration. We present several methods to estimate the precision of the photometric calibration. We distinguish relative uncertainties (between detectors, or between frequencies) and absolute uncertainties. Absolute uncertainties lie in the range from 0.54% to 10% from 100 to 857 GHz. We describe the pipeline used to produce the maps from the HFI timelines, based on the photometric calibration parameters, and the scheme used to set the zero level of the maps a posteriori. We also discuss the cross-calibration between HFI and the SPIRE instrument on board Herschel. Finally we summarize the basic characteristics of the set of HFI maps included in the 2013 Planck data release.
Key words: cosmic background radiation / cosmology: observations / surveys / methods: data analysis
© ESO, 2014
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