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• LFI design, qualification, and performance
  ...k-end unit (BEU) containing a further radio frequency amplification stage, detector diodes, and all the electronics for data acquisition and bias supply. Best LFI noise performance is obtained with receivers based on InP High Electron Mob
  50 KB (7,826 words) - 22:29, 4 February 2015
• Survey scanning and performance
  ...e from the spin axis. 545 GHz, 857 GHz, and 143 GHz bolometers, as well as LFI radiometers 25 and 26 had a slightly smaller bore-sight angle, while the ot ...Operational Days (the unit is seconds per square degree, normalized to one detector). The first significant data gap and recovery are clearly visible.]]
  17 KB (2,543 words) - 16:31, 3 February 2015
• The HFI DPC
  ...ps at specific frequencies into more scientific products, like catalogues, maps, and spectra of astrophysical components. L3 can rely on simulation provide ...decompressing, in some cases changing data formats, computing the time of individual data samples from the time of the compression slices, but otherwise no proc
  4 KB (627 words) - 13:09, 7 July 2015
• Simulation data
  The 2015 Planck data release is supported by a set of simulated maps of the sky, by astrophysical component, and of that sky as seen by Planck ( * 18 full mission sky simulated maps: two sets of sky maps with and without bandpass corrections applied.
  46 KB (7,032 words) - 12:02, 29 March 2016
• 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.
  26 KB (3,949 words) - 15:33, 1 March 2017
• Beams LFI
  LFI observed the sky with 11 pairs of beams associated with the 22 pseudo-corre ...} (see also [[LFI design, qualification, and performance#Naming Convention|LFI naming convention]]).
  24 KB (3,748 words) - 10:02, 26 September 2016
• Effective Beams
  ...essing are given in the respective pages for [[Beams|HFI]] and [[Beams_LFI|LFI]]. ...a discussion of its application to Planck data is given in the appropriate LFI {{PlanckPapers|planck2013-p02d}}, {{PlanckPapers|planck2014-a05||Planck-201
  22 KB (3,180 words) - 10:37, 5 February 2015
• 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
• Unit conversion and Color correction
  ...SS_0" instead of "BANDPASS_F0". This makes it possible to read the current LFI RIMO structure, where the average bandpass RIMO extensions are named BANDPA ...aper {{PlanckPapers|planck2013-p03d}} for details of the derivation of the detector spectra and band-average spectra included in the RIMO files, as well as add
  29 KB (4,776 words) - 11:02, 22 February 2017
• Beams
  ...idBeamDiagram.png|thumb|500px|center|'''Figure 2:''' Scanning beam map for detector 143-6, indicating approximately the regions that are handled with a differe ..., 0.81)&times;10^-4 for 100, 143, and 217 GHz frequency-averaged maps respectively, reduced from the previous uncertainties of (61, 23, 20)&times
  52 KB (8,515 words) - 12:52, 7 July 2015
• CMB and astrophysical component maps
  {{DISPLAYTITLE:2015 CMB and astrophysical component maps}} ...These products are derived from some or all of the nine frequency channel maps described above using different techniques and, in some cases, using other
  90 KB (13,248 words) - 13:06, 21 April 2020
• Planck Added Value Tools
  ...above functionalities are available both for map cutouts and for full sky maps. ...nous format (read next section) due to the size and the multiple number of maps selected.
  30 KB (5,022 words) - 16:55, 16 March 2018