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• TOI processing
  ...Cs, then processed with a pipeline whose general features are given in the HFI Data Processing paper {{PlanckPapers|planck2013-p03}} for PR1 and {{Planck ...ds a flag TOI that masks the TOI samples that are not to be projected onto maps for various reasons.
  20 KB (3,054 words) - 14:18, 2 July 2018
• HFI-Validation
  The overall internal validation of the frequency maps is performed thanks to several tests: * difference between the PR2 (2015) and PR3 (2018) frequency maps,
  6 KB (1,057 words) - 08:40, 3 July 2018
• HFI sims
  {{DISPLAYTITLE:HFI simulations}} ...R3-2018 simulation (FFP10) brings for the first time the simulation of the HFI instrumental effects. Moreover these simulated systematic effects are proce
  29 KB (4,250 words) - 13:56, 2 July 2018
• Map-making LFI
  The main output consists of temperature and polarization maps. LFI maps were constructed with the MADAM mapmaking code, version 3.7.4.
  21 KB (3,331 words) - 16:04, 6 July 2018
• Beams LFI
  ..., the window function used to correct the power spectra extracted from the maps allows for this efficiency. ...ns using the GRASP physical optics code, by appropriately tuning the Radio Frequency Flight Model (RFFM, {{PlanckPapers|tauber2010b}}).
  23 KB (3,593 words) - 15:15, 9 November 2018
• Scanning Beams
  ..., assuming a flat spectrum of the incoming radiation. The Stokes parameter maps contain the complete information about the field intensity and polarization ...mation on LFI beams can be found in {{PlanckPapers|planck2014-a05}} and on HFI beams in {{PlanckPapers|planck2014-a08}}
  6 KB (866 words) - 00:02, 22 March 2018
• References
  title = {Planck 2013 results: The Low Frequency Instrument data processing (p02)}, title = {Planck 2013 results: High Frequency Instrument Data Processing (p03)},
  173 KB (25,381 words) - 15:29, 4 June 2014
• Mission products
  ...imelines''', accompanied by the relevant flags, which can be used to build maps in addition to those supplied here; * different types of '''sky maps''', i.e., maps of the signal received from the sky, accompanied by;
  3 KB (438 words) - 21:53, 4 July 2015
• HFI cold optics & spectral response
  ..._ColdOptics.png|thumb|500px|center|Mechanical and thermal structure of the HFI focal plane unit.]] A detailed description of the HFI optical design and beam performance is given in {{PlanckPapers|maffei2010}}
  25 KB (3,795 words) - 07:52, 6 July 2018
• Spectral response
  ...escriptions apply to individual detector responses and individual detector maps. Maps which are made from combinations of detectors have an effective spectral re
  23 KB (1,443 words) - 07:19, 18 January 2019
• Compact Source catalogues
  ...sts of sources, both Galactic and extragalactic, extracted from the Planck maps. ...maps used to produce these catalogues are the 2015 full mission frequency maps (LFI_SkyMap_0??_1024_R2.01_full.fits and HFI_SkyMap_???_2048_R2.00_full.fit
  26 KB (4,040 words) - 02:01, 2 July 2018
• Effective Beams
  ...ls of the beam processing are given in the respective sections for [[Beams|HFI]] and [[Beams_LFI|LFI]]. ...s|planck2013-p02d}}, {{PlanckPapers|planck2014-a05||Planck-2015-A05}}) and HFI ({{PlanckPapers|planck2013-p03c}}) papers. Relevant details of the processi
  67 KB (9,735 words) - 02:01, 22 March 2018
• Main Page3
  ##[[HFI design, qualification, and performance|HFI design, qualification, and performance]] <span style="color:red">(Lamarre/P ##[[The HFI DPC| HFI Data Processing]] <span style="color:red">(Bouchet)</span>
  6 KB (770 words) - 17:33, 29 January 2013
• HFI time response model
  Here we describe the "Low frequency excess response" 4 model. ...F(\omega)</math> is the complex intrinsic bolometer transfer function. For HFI the bolometer transfer function is modelled as the sum of four single pole
  12 KB (1,369 words) - 09:15, 22 June 2018
• DatesObs
  There are 54 files; 6 HFI bands x 5 surveys & 3 LFI bands x 8 surveys. They are named: where ''fff'' is the usual 3-digit description of the channel frequency.
  2 KB (375 words) - 02:30, 22 February 2017
• References2
  title = {Simulation of the Planck-HFI thermal control system}, title = {Planck-HFI thermal architecture: from requirements to solutions},
  39 KB (5,438 words) - 09:40, 20 May 2014
• CMB angular power spectrum
  #REDIRECT [[Frequency map angular power spectrum]] ...tector (set) maps at 100, 143 and 217GHz, masked with mask2, which are the maps used in the High-ell likelihood.
  321 bytes (52 words) - 16:39, 20 February 2013
• Frequency maps angular power spectra
  == HFI maps power spectra == Angular power spectra of cut sky CMB dominated maps are provided to allow independent cosmological analysis at high <math>\ell<
  25 KB (3,718 words) - 15:37, 18 July 2014
• HFI data compression
  HFI channels. The variations are mainly due to the time spent by the high-frequency channels in the Galactic
  8 KB (1,269 words) - 09:45, 10 December 2014
• HFI performance summary
  The HFI operated flawlessly for 30 months, the maximum autonomy expected for the he The extreme sensitivity provided by the 100 mK bolometers and the HFI architecture provided a new view of the submillimetre and millimetre sky, w
  5 KB (674 words) - 14:36, 2 July 2018

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