Issue |
A&A
Volume 571, November 2014
Planck 2013 results
|
|
---|---|---|
Article Number | A4 | |
Number of page(s) | 22 | |
Section | Astronomical instrumentation | |
DOI | https://doi.org/10.1051/0004-6361/201321544 | |
Published online | 29 October 2014 |
Planck 2013 results. IV. Low Frequency Instrument beams and window functions
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,
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2
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Kylmälä,
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African Institute for Mathematical Sciences,
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Africa
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DTU Space, National Space Institute, Technical University of
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Universidad de Salamanca, 37008
Salamanca,
Spain
18
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Avda. Calvo Sotelo s/n,
Oviedo,
Spain
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Toronto, 50 Saint George Street,
Toronto, Ontario,
Canada
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Nijmegen, PO Box
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Nijmegen, The
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University of California, Berkeley, California, USA
22
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Vancouver, British
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of Letter, Arts and Sciences, University of Southern California,
Los Angeles, CA
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London, London
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UK
25
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Keen Physics Building, 77 Chieftan
Way, Tallahassee,
Florida,
USA
26
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Princeton, New Jersey, USA
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Santa Barbara, California, USA
30
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Padova,
Italy
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Ferrara, via Saragat
1, 44122
Ferrara,
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P.le A. Moro 2, Roma, Italy
34
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16, Milano,
Italy
35
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2, Trieste,
Italy
36
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Vergata, via della Ricerca Scientifica,
1, Roma,
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37
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38
Dpto. Astrofísica, Universidad de La Laguna (ULL),
38206, La Laguna, Tenerife,
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39
European Space Agency, ESAC, Planck Science Office, Camino bajo del
Castillo, s/n, Urbanización
Villafranca del Castillo, Villanueva de la Cañada, Madrid, Spain
40
European Space Agency, ESTEC, Keplerlaan 1, 2201 AZ
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41
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42
Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University
of Helsinki, Helsinki,
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via S. Sofia 78, Catania, Italy
44
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52
IPAG: Institut de Planétologie et d’Astrophysique de Grenoble,
Université Joseph Fourier, Grenoble 1/CNRS-INSU, UMR 5274, 38041
Grenoble,
France
53
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Geneva, Ch. d’Ecogia
16, Versoix,
Switzerland
54
IUCAA, Post Bag 4, Ganeshkhind, Pune University
Campus, 411 007
Pune,
India
55
Imperial College London, Astrophysics group, Blackett
Laboratory, Prince Consort
Road, London,
SW7 2AZ,
UK
56
Infrared Processing and Analysis Center, California Institute of
Technology, Pasadena,
CA
91125,
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57 Institut Néel, CNRS, Université
Joseph Fourier Grenoble I, 25 rue des
Martyrs, Grenoble,
France
58
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Paris,
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59
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60
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61
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Institute of Astronomy and Astrophysics, Academia
Sinica, Taipei,
Taiwan
63
Institute of Astronomy, University of Cambridge,
Madingley Road, Cambridge
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64 Institute of Theoretical
Astrophysics, University of Oslo, Blindern, Oslo,
Norway
65
Instituto de Astrofísica de Canarias, C/Vía Láctea s/n, La Laguna, Tenerife, Spain
66
Instituto de Física de Cantabria (CSIC-Universidad de
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67
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Association, via R. Cozzi
53, Milano,
Italy
68
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California,
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69
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of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester, M13
9PL, UK
70
Kavli Institute for Cosmology Cambridge,
Madingley Road, Cambridge, CB3 0HA, UK
71
LAL, Université Paris-Sud, CNRS/IN2P3, Orsay, France
72
LERMA, CNRS, Observatoire de Paris, 61 avenue de l’Observatoire, Paris, France
73
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74
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Joseph Fourier Grenoble I, CNRS/IN2P3, Institut National Polytechnique de
Grenoble, 53 rue des
Martyrs, 38026
Grenoble Cedex,
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76
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77
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University, 3600 rue
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81
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82
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83
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84
SISSA, Astrophysics Sector, via Bonomea 265, 34136
Trieste,
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85
School of Physics and Astronomy, Cardiff University,
Queens Buildings, The Parade,
Cardiff, CF24 3AA, UK
86
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87
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Berkeley, California, USA
88
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90
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Keble Road, Oxford
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91
Theory Division, PH-TH, CERN, 1211
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92
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Paris,
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93
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Toulouse Cedex 4,
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94
University of Granada, Departamento de Física Teórica y del Cosmos,
Facultad de Ciencias, Granada, Spain
95
Warsaw University Observatory, Aleje Ujazdowskie 4, 00-478
Warszawa,
Poland
Received:
22
March
2013
Accepted:
1
March
2014
This paper presents the characterization of the in-flight beams, the beam window functions, and the associated uncertainties for the Planck Low Frequency Instrument (LFI). Knowledge of the beam profiles is necessary for determining the transfer function to go from the observed to the actual sky anisotropy power spectrum. The main beam distortions affect the beam window function, complicating the reconstruction of the anisotropy power spectrum at high multipoles, whereas the sidelobes affect the low and intermediate multipoles. The in-flight assessment of the LFI main beams relies on the measurements performed during Jupiter observations. By stacking the datafrom multiple Jupiter transits, the main beam profiles are measured down to –20 dB at 30 and 44 GHz, and down to –25 dB at 70 GHz. The main beam solid angles are determined to better than 0.2% at each LFI frequency band. The Planck pre-launch optical model is conveniently tuned to characterize the main beams independently of any noise effects. This approach provides an optical model whose beams fully reproduce the measurements in the main beam region, but also allows a description of the beams at power levels lower than can be achieved by the Jupiter measurements themselves. The agreement between the simulated beams and the measured beams is better than 1% at each LFI frequency band. The simulated beams are used for the computation of the window functions for the effective beams. The error budget for the window functions is estimated from both main beam and sidelobe contributions, and accounts for the radiometer bandshapes. The total uncertainties in the effective beam window functions are: 2% and 1.2% at 30 and 44 GHz, respectively (at ℓ ≈ 600), and 0.7% at 70 GHz (at ℓ ≈ 1000).
Key words: methods: data analysis / cosmic background radiation / telescopes
© ESO, 2014
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