Planck 2013 results: VII. HFI time response and beams

Research output: Contribution to journalArticle

Researchers

  • P. A. R. Ade
  • N. Aghanim
  • C. Armitage-Caplan
  • M. Arnaud
  • M. Ashdown
  • E. Atrio-Barandela
  • J. Aumont
  • C. Baccigalupi
  • A. J. Banday
  • R. B. Barreiro
  • E. Battaner
  • K. Benabed
  • A. Benoit
  • A. Benoit-Levy
  • J. -P. Bernard
  • M. Bersanelli
  • P. Bielewicz
  • J. Bobin
  • J. J. Bock
  • J. R. Bond
  • J. Borrill
  • F. R. Bouchet
  • J. W. Bowyer
  • M. Bridges
  • M. Bucher
  • C. Burigana
  • J. -E Cardoso
  • A. Catalano
  • A. Challinor
  • A. Chamballu
  • R. -R. Chary
  • H. C. Chiang
  • L. -Y Chiang
  • P. R. Christensen
  • S. Church
  • D. L. Clements
  • S. Colombi
  • L. P. L. Colombo
  • F. Couchot
  • A. Coulais
  • B. P. Crill
  • A. Curto
  • E. Cuttaia
  • L. Danese
  • R. D. Davies
  • P. de Bernardis
  • A. de Rosa
  • G. de Zotti
  • J. Delabrouille
  • J. -M. Delouis
  • Planck Collaboration

Research units

  • University of Salamanca
  • University of Granada
  • Univ Grenoble 1, Centre National de la Recherche Scientifique (CNRS), Joseph Fourier University, Inst Neel
  • University of California at Berkeley
  • Telecom Paris Tech
  • Acad Sinica, Academia Sinica - Taiwan, Inst Astron & Astrophys
  • Cardiff University
  • Univ Paris 11, Centre National de la Recherche Scientifique (CNRS), University of Paris Sud - Paris XI, CNRS, Inst Astrophys Spatiale, UMR 8617)
  • University of Oxford
  • CEA Saclay, CEA, Centre National de la Recherche Scientifique (CNRS), PRES University Sorbonne Paris Cite, University of Paris Diderot - Paris VII, Univ Paris Diderot, CNRS, CEA DSM,IRFU,Serv Astrophys,Lab AIM
  • University of Cambridge
  • International School for Advanced Studies
  • Univ Toulouse, Centre National de la Recherche Scientifique (CNRS), Universite de Toulouse, PRES Universite de Toulouse, Universite Toulouse III - Paul Sabatier, UPS OMP, IRAP
  • Univ Cantabria, Consejo Superior de Investigaciones Cientificas (CSIC), Universidad de Cantabria, CSIC, Inst Fis Cantabria
  • Univ Paris 06, Pierre & Marie Curie University - Paris 6, UMR7095
  • INAF IASF Milano, Istituto Nazionale Astrofisica - Italy
  • California Institute of Technology
  • University of Toronto
  • Imperial College London
  • Univ Paris Diderot, CEA, PRES University Sorbonne Paris Cite, University of Paris Diderot - Paris VII, PSL Research University Paris, Observatoire de Paris, Centre National de la Recherche Scientifique (CNRS), Observ Paris, Sorbonne Paris Cite, CNRS IN2P3,CEA lrfu,APC
  • IASF Bologna, Istituto Nazionale Astrofisica - Italy, INAF
  • Univ Grenoble 1, Centre National de la Recherche Scientifique (CNRS), Institut National Polytechnique de Grenoble, Joseph Fourier University, National Institute of Nuclear & Particle Physics (IN2P3), Lab Phys Subatom & Cosmol, CNRS, Inst Natl Polytech Grenoble,IN2P3
  • Princeton University
  • Niels Bohr Inst, Niels Bohr Institute, University of Copenhagen
  • Stanford University
  • Univ Paris 11, Centre National de la Recherche Scientifique (CNRS), National Institute of Nuclear & Particle Physics (IN2P3), University of Paris Sud - Paris XI, CNRS, IN2P3, LAL
  • Observ Paris, Centre National de la Recherche Scientifique (CNRS)
  • Univ Manchester, Jodrell Bank Centre for Astrophysics, University of Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys
  • Sapienza University Rome

Abstract

This paper characterizes the effective beams, the effective beam window functions and the associated errors for the Planck High Frequency Instrument (HFI) detectors. The effective beam is the angular response including the effect of the optics, detectors, data processing and the scan strategy. The window function is the representation of this beam in the harmonic domain which is required to recover an unbiased measurement of the cosmic microwave background angular power spectrum. The HFI is a scanning instrument and its effective beams are the convolution of: a) the optical response of the telescope and feeds; b) the processing of the time-ordered data and deconvolution of the bolometric and electronic transfer function; and c) the merging of several surveys to produce maps. The time response transfer functions are measured using observations of Jupiter and Saturn and by minimizing survey difference residuals. The scanning beam is the post-deconvolution angular response of the instrument, and is characterized with observations of Mars. The main beam solid angles are determined to better than 0.5% at each HFI frequency band. Observations of Jupiter and Saturn limit near sidelobes (within 5 degrees) to about 0.1% of the total solid angle. Time response residuals remain as long tails in the scanning beams, but contribute less than 0.1% of the total solid angle. The bias and uncertainty in the beam products are estimated using ensembles of simulated planet observations that include the impact of instrumental noise and known systematic effects. The correlation structure of these ensembles is well-described by five errors eigenmodes that are sub-dominant to sample variance and instrumental noise in the harmonic domain. A suite of consistency tests provide confidence that the error model represents a sufficient description of the data. The total error in the effective beam window functions is below 1% at 100 GHz up to multiple l similar to 1500, below 0.5% at 143 and 217 GHz up to l similar to 2000.

Details

Original languageEnglish
Article numberA7
Pages (from-to)31
Number of pages31
JournalAstronomy and Astrophysics
Volume571
Issue numberid. A7
Publication statusPublished - Nov 2014
MoE publication typeA1 Journal article-refereed

    Research areas

  • cosmic background radiation, cosmology: observations, instrumentation: detectors, surveys, pre-launch status, power spectrum, map-making, microwave, calibrartion, planets, CMB

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