2013/03/31 by Planck Collaboration, P. A. R. Ade, N. Aghanim +250 · 1 citation
Physics and Astronomy · #Anisotropy #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Calibration #Channel (broadcasting) #Cosmic microwave background #Detector #Galaxies: Formation, Evolution, Phenomena #Microwave #Noise (video) #Optics #Physics #Planck #Radio spectrum #Remote sensing #Scientific Research and Discoveries #Sky #Telecommunications #astro-ph.CO #astro-ph.IM
paper · pdf · doi:10.1051/0004-6361/201321570
published as A&A 571, A6 (2014) · Accepted (revised) version by AA; 47 pages, 42 figures, 4 tables. It now includes an additional annex devoted to further & conclusive tests at 217GHz. This paper is one of a set associated with the 2013 release of data from the Planck mission
openalex publication_date 2014/07/22 · arxiv created 2014/07/23 · arxiv updated 2014/10/29 · openalex created_date 2017/05/26 · openalex updated_date 2026/08/06
Wedescribe 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 857GHz with an angular resolution ranging from 9.́7 to 4.́6. The detector noise per (effective) beam solid angle is respectively, 10, 6 , 12, and 39 μK in the four lowest HFI frequency channels (100−353GHz) 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%.