Planck 2013 results: VI. High Frequency Instrument data processing

Research output: Contribution to journalArticle

Researchers

  • P. A. R. Ade
  • N. Aghanim
  • C. Armitage-Caplan
  • M. Arnaud
  • M. Ashdown
  • F. 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
  • F. Boulanger
  • J. W. Bowyer
  • M. Bridges
  • M. Bucher
  • C. Burigana
  • J. -F. Cardoso
  • A. Catalano
  • A. Chamballu
  • R. -R. Chary
  • X. Chen
  • H. C. Chiang
  • L. -Y Chiang
  • P. R. Christensen
  • S. Church
  • D. L. Clements
  • S. Colombi
  • L. P. L. Colombo
  • C. Combet
  • F. Couchot
  • A. Coulais
  • B. P. Crill
  • A. Curto
  • F. Cuttaia
  • L. Danese
  • R. D. Davies
  • R. J. Davis
  • P. de Bernardis
  • A. de Rose
  • 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, UMR8617
  • 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, Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University Paris, University of Paris Diderot - Paris VII, PRES University Sorbonne Paris Cite, National Institute of Nuclear & Particle Physics (IN2P3), Sorbonne Paris Cite, CNRS, IN2P3,CEA Irfu,Observ Paris,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

We describe the processing of the 531 billion raw data samples from the High Frequency Instrument (HFI), which we performed to produce six temperature maps from the first 473 days of Planck-HFI survey data. These maps provide an accurate rendition of the sky emission at 100, 143, 217, 353, 545, and 857 GHz with an angular resolution ranging from 9. 0 7 to 4. 0 6. The detector noise per (effective) beam solid angle is respectively, 10, 6, 12, and 39 K in the four lowest HFI frequency channels (100-353 GHz) and 13 and 14 kJy sr 1 in the 545 and 857 GHz channels. Relative to the 143 GHz channel, these two high frequency channels are calibrated to within 5% and the 353 GHz channel to the percent level. The 100 and 217 GHz channels, which together with the 143 GHz channel determine the high-multipole part of the CMB power spectrum (50 <l <2500), are calibrated relative to 143 GHz to better than 0.2%.

Details

Original languageEnglish
Article numberA6
Number of pages44
JournalAstronomy and Astrophysics
Volume571
Publication statusPublished - Nov 2014
MoE publication typeA1 Journal article-refereed

    Research areas

  • methods: data analysis, cosmic background radiation, cosmology: observations, surveys, PRE-LAUNCH STATUS, MODEL, CALIBRATION, BEAMS

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