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• PSO processing
  ...L was required by MOC to prepare the lists of pointings that were uploaded to the satellite. ...e name indicates it covers long periods of time. In general it was updated to cover
  3 KB (444 words) - 16:04, 21 May 2014
• Simulation data
  == The end-to-end simulation pipeline == ...een in the following schematic. Note that while this schematic is specific to HFI, the main components in the block diagram are similar for both instrume
  114 KB (17,146 words) - 09:49, 21 February 2022
• Specially processed maps
  ...contents are described below. The convergence map "dat_klm.fits" that can be found in the tarball, has been categorized as COM_Lensing-Convergence-dat-k ...e noise in the full mission Planck <i>y</i>-maps, which are also provided. To complement this we also provide the power spectra of the noise estimate map
  14 KB (2,181 words) - 06:56, 26 April 2016
• CMB spectrum & Likelihood Code
  ...s spectrum are the 68% confidence limits and include the uncertainties due to foreground subtraction. ...pers|planck2016-l05}}, with foreground and other nuisance parameters fixed to a best fit assuming the base-ΛCDM cosmology. Associated 1&sigma; errors i
  118 KB (17,535 words) - 10:05, 11 May 2021
• CMB maps
  All the details can be found in {{PlanckPapers|planck2016-l04}} and, for earlier releases, in {{Pl ...ovide an approximate noise estimates for the full mission, but they should be used with caution. Each split has caveats in this regard: there are noise c
  124 KB (18,807 words) - 18:58, 20 March 2023
• Lensing
  ...mode map). In the second we further add CIB information at 545 GHz (GNILC) to the lensing tracer. ...used to assess the filter, as was done in {{PlanckPapers|planck2016-l08}} to produce the <i>B</i>-mode power spectrum (Fig. 14).
  37 KB (5,494 words) - 12:25, 10 July 2019
• Timelines
  ...kPapers|planck2014-a03}} and {{PlanckPapers|planck2016-l02}}, and for HFI, to {{PlanckPapers|planck2014-a08}}. ...which has been cleaned of artifacts and systematic effects, and converted to physical units.
  40 KB (6,006 words) - 11:30, 22 June 2021
• HFI Detector Spectral Response
  ...near-band spectral regions surrounding CO rotational transitions in order to support the CO extraction component separation effort <span style="color:#0 ...eter (FTS). The required accuracy to which the spectral transmission is to be recovered is 1<math>\%</math> (see §[[#Conformity with requirements|Req.]]
  58 KB (7,853 words) - 15:51, 5 October 2012
• TOI processing
  ...55 pointings (or rings) have not been used because they have been found to be affected by thermal fluctuations (see {{PlanckPapers|planck2016-l03}}). ...tails. It also adds 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
• The satellite
  |$\pm 0.6$ arcmin/sec (changes due to manoeuvers); stability during inertial pointing <math>\sim 6.5\times 10^{-5 |'''Max angle of spin axis to Sun'''
  14 KB (2,170 words) - 09:29, 21 May 2014
• HFI sims
  == The HFI end-to-end simulation pipeline == The HFI end-to-end simulation pipeline uses several software components which are describe
  29 KB (4,250 words) - 13:56, 2 July 2018
• Beams LFI
  ...labelled as LFIXXM or LFIXXS. Here "XX" is the RCA number ranging from 18 to 28, while "M" and "S" are the two polarizations, namely the main-arm and si ...{{PlanckPapers|planck2014-a05}}. Please note that many figures below refer to the Planck release {{PlanckPapers|planck2013-p02d}}, since they have not ch
  23 KB (3,593 words) - 15:15, 9 November 2018
• HL-sims
  ...O) and create sky maps and catalogues at the specified frequencies. It can be supplemented by ad-hoc simulation software for particular (theoretical) CMB ...of the actual instruments. Alternatively, the output can be used as input to a detailed simulation of the instrumental behaviour.
  5 KB (779 words) - 16:03, 21 May 2014
• HFI detection chain
  Two extra bolometers, not optically coupled to the telescope, are added to the focal plane to monitor thermal noise (dark bolometers).
  15 KB (2,424 words) - 21:36, 19 June 2018
• HFI spectral response data processing
  ...t ZPD and that each spectrum has identical frequency sampling and can thus be averaged together. An example of a combined interferogram data set is illus ...Beer 1.5 apodization function{{BibCite|NaylorApod07}} has been selected to be used for the final spectral transmission profile data set, since it represe
  8 KB (717 words) - 08:00, 10 December 2014
• Astrophysical component separation
  ...roach implements Bayesian component separation, fitting a parametric model to the data by sampling the corresponding posterior distribution. The computat ...nsidered, or 40 arcmin FWHM for Planck alone. Higher resolution could only be achieved by omitting lower frequencies from the fit. Either approach transl
  16 KB (2,572 words) - 10:22, 10 July 2018
• Beam Window Functions
  ...gular power spectrum <i>C^XX</i>_sky(&#8467;), assumed to have isotropic statistical properties, as is the case for the CMB. ...orresponding to <i>TB</i> and <i>EB</i>, since these terms are unlikely to be major sources of contamination for the other spectra.<br />
  11 KB (1,796 words) - 11:47, 22 June 2021
• TestReplace2
  Two extra bolometers not optically coupled to the telescope are added to the focal plane to monitor thermal noise (dark bolometers).
  13 KB (2,128 words) - 15:29, 4 June 2014
• Frequency maps
  ...two releases, please go to the sections at the end of this chapter related to 2013 and 2015. To help in further processing, there are also masks of the Galactic plane and
  133 KB (19,918 words) - 11:57, 14 December 2022
• Foreground maps
  All the details can be found in {{PlanckPapers|planck2016-l04}} and {{PlanckPapers|planck2016-l08} ...or these reasons, we consider the parametric foreground products from 2015 to represent a more accurate description of the true sky than the correspondin
  107 KB (15,543 words) - 17:33, 22 October 2021