Title: | Planck 2013 results |
Author(s): | Ade, P. A. R. ; Aghanim, N. ; Armitage-Caplan, C. ; Arnaud, M. ; Ashdown, M. ; Atrio-Barandela, E. ; Aumont, J. ; Baccigalupi, C. ; Banday, A. J. ; Barreiro, R. B. ; Battaner, E. ; Benabed, K. ; Benoit, A. ; Benoit-Levy, A. ; Bernard, J. -P. ; Bersanelli, M. ; Bielewicz, P. ; Bobin, J. ; Bock, J. J. ; Bond, J. R. ; Borrill, J. ; Bouchet, F. R. ; Bowyer, J. W. ; Bridges, M. ; Bucher, M. ; Burigana, C. ; Cardoso, J. -E ; Catalano, A. ; Challinor, A. ; Chamballu, A. ; Chary, R. -R. ; Chiang, H. C. ; Chiang, L. -Y ; Christensen, P. R. ; Church, S. ; Clements, D. L. ; Colombi, S. ; Colombo, L. P. L. ; Couchot, F. ; Coulais, A. ; Crill, B. P. ; Curto, A. ; Cuttaia, E. ; Danese, L. ; Davies, R. D. ; de Bernardis, P. ; de Rosa, A. ; de Zotti, G. ; Delabrouille, J. ; Delouis, J. -M. ; , Planck Collaboration |
Date: | 2014-11 |
Language: | en |
Pages: | 31 |
Department: | Cardiff University University of Paris University of Oxford University of Paris Diderot University of Cambridge University of Salamanca International School for Advanced Studies Université de Toulouse Universidad de Cantabria University of Granada Pierre and Marie Curie University Joseph Fourier University Istituto Nazionale Astrofisica - Italy California Institute of Technology University of Toronto University of California Berkeley Imperial College London Telecom ParisTech Université Grenoble Alpes Princeton University Academia Sinica - Institute of Astronomy and Astrophysics Niels Bohr Institute, University of Copenhagen Stanford University University of Paris Sud Observatoire de Paris University of Manchester Sapienza University of Rome |
Series: | ASTRONOMY AND ASTROPHYSICS, Volume 571, issue id. A7 |
ISSN: | 0004-6361 1432-0746 |
DOI-number: | 10.1051/0004-6361/201321535 |
Keywords: | cosmic background radiation, cosmology: observations, instrumentation: detectors, surveys, pre-launch status, power spectrum, map-making, microwave, calibrartion, planets, CMB |
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Ade , P A R , Aghanim , N , Armitage-Caplan , C , Arnaud , M , Ashdown , M , Atrio-Barandela , E , Aumont , J , Baccigalupi , C , Banday , A J , Barreiro , R B , Battaner , E , Benabed , K , Benoit , A , Benoit-Levy , A , Bernard , J -P , Bersanelli , M , Bielewicz , P , Bobin , J , Bock , J J , Bond , J R , Borrill , J , Bouchet , F R , Bowyer , J W , Bridges , M , Bucher , M , Burigana , C , Cardoso , J -E , Catalano , A , Challinor , A , Chamballu , A , Chary , R -R , Chiang , H C , Chiang , L -Y , Christensen , P R , Church , S , Clements , D L , Colombi , S , Colombo , L P L , Couchot , F , Coulais , A , Crill , B P , Curto , A , Cuttaia , E , Danese , L , Davies , R D , de Bernardis , P , de Rosa , A , de Zotti , G , Delabrouille , J , Delouis , J -M & Planck Collaboration 2014 , ' Planck 2013 results : VII. HFI time response and beams ' , Astronomy and Astrophysics , vol. 571 , no. id. A7 , A7 , pp. 31 . https://doi.org/10.1051/0004-6361/201321535 |
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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 characterizedwith 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.
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