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• Frequency maps angular power spectra
  == HFI maps power spectra == ...the data, and therefore determine the best cosmological models fitting the data. Several examples of such high-<math>\ell</math> likelihoods are described,
  25 KB (3,718 words) - 15:37, 18 July 2014
• HFI performance summary
  ...ery stable conditions during the whole mission, and practically all of the data were correctly recorded. 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
• Astrophysical component separation
  ...nckPapers|planck2016-l04}} (and references therein), give details of these processing steps. Four separate component-separation methods are used, which we now d ...al observations from WMAP and Haslam. For the reduction of the Planck 2018 data set, which includes only full-frequency maps, a simpler model is employed,
  16 KB (2,572 words) - 10:22, 10 July 2018
• CMB Maps test
  The CMB data are in thermodynamic temperature units (uK_cmb), and the residuals are in t ...applied to Planck simulations Leach et al., 2008 and to WMAP polarisation data Fernandez-cobos et al., 2012. In the cleaning process, no assumptions about
  7 KB (1,103 words) - 18:38, 1 March 2013
• UC CC Tables
  == HFI Unit Conversion Tables == ...nstances), including uncertainty estimates based on the uncertainty of the HFI detector spectral response. The derivation of the unit conversion coeffici
  77 KB (2,387 words) - 14:23, 24 November 2017
• Unit conversion and Color correction
  ...is delivered as a tarfile and contains a detailed instruction manual. The data and software file requirements are provided below along with basic use inst ...>: a routine to get the desired detector level spectral transmission data (HFI) and output in a structure format used by the other routines.
  29 KB (4,821 words) - 09:34, 10 July 2018
• HFI instrument annexes
  This is a list of all annexes for the HFI instrument section. ** [[HFI_optical_efficiency|HFI spectral response optical efficiency measurements]];
  812 bytes (97 words) - 06:52, 10 December 2014
• Beams
  ...truction of the spatial response for the Planck High Frequency Instrument (HFI) is informed by observation of planets. Furthermore, observations of Uranus ...d time response function, and the software low-pass filter, applied to the data. The "effective beam" represents the averaging of the signal due to the sca
  53 KB (8,689 words) - 15:07, 2 July 2018
• CMB and astrophysical component maps
  ...it is obtained, followed by a description of the FITS file containing the data and associated information. ...his data release, to fully characterize the large-scale residuals from the data or from simulations. Therefore all results published by the Planck Collabor
  73 KB (10,660 words) - 08:15, 21 August 2016
• Planck Legacy Archive Wiki:Books/PLA ES PR1 Snapshot1
  ;HFI design, qualification and performance :[[HFI design, qualification, and performance]]
  2 KB (263 words) - 17:36, 25 March 2013
• Changelog
  * 2013-05-21, Jaffe, [[Detector_pointing|HFI Detector Pointing]]: Changes from Reijo Keskitalo and others. <span style=" ...processing]], [[Spectral response]], [[HFI-Validation]], [[Summary of HFI data characteristics]], [[Compact Source catalogues]], [[The RIMO]], [[Effective
  12 KB (1,788 words) - 08:42, 25 September 2014
• Detector pointing
  ...detectors are known exactly a priori, we must calibrate them using flight data. ...ar as our ability to predict their effects is concerned. In this delivery HFI used a model (described below) to follow the pointing drift continuously,
  5 KB (746 words) - 13:21, 12 January 2018
• TOC WorkInProgress
  ##[[HFI design, qualification, and performance|HFI design, qualification, and performance]] #[[Data processing]]
  5 KB (581 words) - 09:33, 31 March 2014
• ChangelogV2
  ...04-15: Moneti: Added info on HFI Planet TOIs in [[Timelines | Time ordered data]] (APPROVED, IN PLA, ES PAGE PUBLIC) ...ott: finished fixing style in [[Map-making]], [[Spectral_response]], and [[HFI-Validation]]
  6 KB (842 words) - 00:29, 7 April 2018
• The Planck mission WiP
  Instrument (LFI), and a SAMBA-like High Frequency Instrument (HFI), instruments, as well as the ensuing data analysis
  15 KB (2,330 words) - 12:43, 17 July 2018
• Beam Window Functions
  ...Temperature beam window functions for polarized and unpolarized detectors (HFI PSB and SWBs) ==== ...the HEALPix resolution parameter <i>N</i>_side (=2048 for Planck HFI maps).
  11 KB (1,796 words) - 11:47, 22 June 2021
• The satellite WiP
  ...diation from the sky onto a focal plane shared by detectors of the LFI and HFI, operating at 20K and 0.1K, respectively; a telescope baffle that simultane |'''On-board data storage capacity'''
  30 KB (4,647 words) - 09:23, 10 July 2018
• TOCV1 BackUp
  ##[[HFI design, qualification, and performance|HFI design, qualification, and performance]] ##[[Data flow overview|Data flow overview]] (<span style="color:red">Leonardi</span>,<span style="color
  6 KB (744 words) - 09:45, 31 March 2014
• Template:BibCite
  ...rg/abs/1303.5063 '''Planck 2013 results: The Low Frequency Instrument data processing'''], Planck Collaboration 2013 II, A&A, in press, (2014). ....5067.pdf#{{{2|1}}} '''Planck 2013 results: High Frequency Instrument Data Processing'''], Planck Collaboration 2013 VI, A&A, in press, (2014).
  128 KB (20,140 words) - 08:49, 15 May 2018
• TestReplace2
  The heart of the HFI - the detectors - are bolometers, solid-state devices in which the The HFI Focal Plane Unit accommodates sub-millimiter absorbing
  13 KB (2,128 words) - 15:29, 4 June 2014

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