Planck 2013 results

Ade, P. A. R.; Aghanim, N.; Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; 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.; Boulanger, F.; Bowyer, J. W.; Bridges, M.; Bucher, M.; Burigana, C.; Cardoso, J. -F.; Catalano, A.; Chamballu, A.; Chary, R. -R.; Chen, X.; Chiang, H. C.; Chiang, L. -Y; Christensen, P. R.; Church, S.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Combet, C.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rose, A.; , Planck Collaboration

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Planck 2013 results

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Title:	Planck 2013 results
Author(s):	Ade, P. A. R. ; Aghanim, N. ; Armitage-Caplan, C. ; Arnaud, M. ; Ashdown, M. ; Atrio-Barandela, F. ; 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. ; Boulanger, F. ; Bowyer, J. W. ; Bridges, M. ; Bucher, M. ; Burigana, C. ; Cardoso, J. -F. ; Catalano, A. ; Chamballu, A. ; Chary, R. -R. ; Chen, X. ; Chiang, H. C. ; Chiang, L. -Y ; Christensen, P. R. ; Church, S. ; Clements, D. L. ; Colombi, S. ; Colombo, L. P. L. ; Combet, C. ; Couchot, F. ; Coulais, A. ; Crill, B. P. ; Curto, A. ; Cuttaia, F. ; Danese, L. ; Davies, R. D. ; Davis, R. J. ; de Bernardis, P. ; de Rose, A. ; , Planck Collaboration
Date:	2014-11
Language:	en
Pages:	44
Department:	Cardiff University University of Paris Sud 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 Observatoire de Paris University of Manchester Sapienza University of Rome
Series:	ASTRONOMY AND ASTROPHYSICS, Volume 571
ISSN:	0004-6361 1432-0746
DOI-number:	10.1051/0004-6361/201321570
Keywords:	methods: data analysis, cosmic background radiation, cosmology: observations, surveys, PRE-LAUNCH STATUS, MODEL, CALIBRATION, BEAMS
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Citation: Ade , P A R , Aghanim , N , Armitage-Caplan , C , Arnaud , M , Ashdown , M , Atrio-Barandela , F , 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 , Boulanger , F , Bowyer , J W , Bridges , M , Bucher , M , Burigana , C , Cardoso , J -F , Catalano , A , Chamballu , A , Chary , R -R , Chen , X , Chiang , H C , Chiang , L -Y , Christensen , P R , Church , S , Clements , D L , Colombi , S , Colombo , L P L , Combet , C , Couchot , F , Coulais , A , Crill , B P , Curto , A , Cuttaia , F , Danese , L , Davies , R D , Davis , R J , de Bernardis , P , de Rose , A & Planck Collaboration 2014 , ' Planck 2013 results : VI. High Frequency Instrument data processing ' , Astronomy and Astrophysics , vol. 571 , A6 . https://doi.org/10.1051/0004-6361/201321570
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%.

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