Planck 2015 results: IV. Low Frequency Instrument beams and window functions

Tutkimustuotos: Lehtiartikkelivertaisarvioitu

Tutkijat

  • Planck Collaboration

Organisaatiot

  • University of California at Berkeley
  • University of Oxford
  • Télécom ParisTech
  • University of Granada
  • Université Joseph Fourier Grenoble I
  • Nicolaus Copernicus Astronomical Center
  • CNRS UMR 5141
  • INAF, Osservatorio Astronomico di Padova
  • Institut Universitaire de France
  • Cardiff University
  • CNRS/IN2P3
  • Kavli Institute for Cosmology Cambridge
  • University of Cambridge
  • International School for Advanced Studies
  • IRAP
  • Universidad de Cantabria
  • Università Degli Studi di Padova
  • INFN, Sezione di Padova
  • UMR7095
  • University College London
  • INAF/IASF Milano
  • Università degli Studi di Milano
  • California Institute of Technology
  • University of Manchester
  • University of Toronto
  • Lawrence Berkeley National Laboratory
  • AstroParticule et Cosmologie
  • INAF/IASF Bologna
  • University of Ferrara
  • INFN, Sezione di Bologna
  • CNRS/IN2P3
  • LERMA - Laboratoire d'Etudes du Rayonnement et de la Matiere en Astrophysique et Atmospheres
  • CNRS Centre National de la Recherche Scientifique
  • Laboratoire AIM, Service d’Astrophysique, DSM\IRFU, CEA\Saclay
  • Niels Bohr Institute
  • University of Southern California
  • Università La Sapienza
  • Imperial College London
  • University of Helsinki

Kuvaus

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). The structure of the paper is similar to that presented in the 2013 Planck release; the main differences concern the beam normalization and the delivery of the window functions to be used for polarization analysis. The in-flight assessment of the LFI main beams relies on measurements performed during observations of Jupiter. By stacking data from seven Jupiter transits, the main beam profiles are measured down to -25 dB at 30 and 44 GHz, and down to -30 dB at 70 GHz. It has been confirmed that the agreement between the simulated beams and the measured beams is better than 1% at each LFI frequency band (within the 20 dB contour from the peak, the rms values are 0.1% at 30 and 70 GHz; 0.2% at 44 GHz). Simulated polarized beams are used for the computation of the effective beam window functions. The error budget for the window functions is estimated from both main beam and sidelobe contributions, and accounts for the radiometer band shapes. The total uncertainties in the effective beam window functions are 0.7% and 1% at 30 and 44 GHz, respectively (at ℓ ≈ 600); and 0.5% at 70 GHz (at ℓ ≈ 1000).

Yksityiskohdat

AlkuperäiskieliEnglanti
ArtikkeliA4
Sivumäärä22
JulkaisuAstronomy and Astrophysics
Vuosikerta594
TilaJulkaistu - 1 lokakuuta 2016
OKM-julkaisutyyppiA1 Julkaistu artikkeli, soviteltu

Lataa tilasto

Ei tietoja saatavilla

ID: 9202860