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• LFI design, qualification, and performance
  ...me gain variations in the two amplifier chains as the sky signal, the true sky power can be recovered. In each radiometer the sky signal coming from the OMT output is continuously compared with a stable 4
  50 KB (7,843 words) - 15:28, 4 July 2018
• Simulation data
  The FFP10 dataset is made of several full-sky map sets in FITS format: * separated input sky components per HFI bolometer and LFI radiometer
  114 KB (17,146 words) - 09:49, 21 February 2022
• Specially processed maps
  ...sents an estimate of the CMB lensing potential on approximately 70% of the sky, and also forms the basis for the Planck 2014 lensing likelihood. It is pro | dat_klm.fits || HEALPix FITS format alm, with <math>L_{\rm max}=2048</math> || Contains the estimated lensing convergence <math> \hat
  14 KB (2,181 words) - 06:56, 26 April 2016
• CMB spectrum & Likelihood Code
  ...Planck 2018 temperature data between 30 and 857 GHz, including 86% of the sky ({{PlanckPapers|planck2016-l06}}). The asymmetric error bars associated wit ...e Galactic centre and plane are masked and we retain only about 50% of the sky. The mask is built by applying a threshold on the 353-GHz map and combined
  118 KB (17,535 words) - 10:05, 11 May 2021
• CMB maps
  : The Commander sky maps have different angular resolutions depending on data products: ...Virgo and Coma clusters, as well as the Crab nebula. A total of 88% of the sky is admitted for analysis.
  124 KB (18,807 words) - 18:58, 20 March 2023
• Lensing
  ...sents an estimate of the CMB lensing potential on approximately 70% of the sky. | mask.fits.gz || HEALPix FITS format map, with <math>N_{\rm side}=2048</math> || Lens reconstruction analysis mask.
  37 KB (5,494 words) - 12:25, 10 July 2019
• Pre-processing
  ...N_{\rm blanck,} bc}- O_{bc}}{F1_{bc}} \times \frac{G_{\rm amp, ETAL}}{G_{{\rm amp}, bc}} </math>. ...} (-1)^{{\rm parity}_{n}} Signal\_{N\!D}\_V_{bc} [n] - \frac{1}{4} (-1)^{{\rm parity}_{n+1}} Signal\_{N\!D}\_V_{bc} [n+1]</math>,
  13 KB (1,990 words) - 07:23, 5 July 2018
• TOI processing LFI
  ...f the horn is corrected for systematic effects. Next, measurements of the sky and the 4-K load are differenced, then the signals from one diode are combi :<math> V = V'R'(V') = G(t)T_{\rm sys} </math>.
  37 KB (6,274 words) - 16:09, 4 July 2018
• Pre-processing LFI
  ...switch configuration, the output can be a sequence of either <i>V</i>_sky or <i>V</i>_load signals. V_{\rm out} = G_{\rm DAE}(V_{\rm in} + O_{\rm DAE}) + Z_{\rm DAE},
  15 KB (2,441 words) - 15:41, 4 July 2018
• Map-making LFI
  ...it the information contained in the large-scale structure of the microwave sky, pixel-pixel covariances are needed in the maximum likelihood estimation of ...entire mission (noise parameters are listed in Table 1), and one for each sky survey (SS1 and SS2).
  21 KB (3,331 words) - 16:04, 6 July 2018
• Beams LFI
  LFI observed the sky with 11 pairs of beams associated with the 22 pseudo-correlation radiometer ...the (<i>u</i>,<i>v</i>) plane is shown. The polarizations direction on the sky are highlighted by the coloured arrows. The M-polarization is shown in gree
  23 KB (3,593 words) - 15:15, 9 November 2018
• LFI-Validation
  ...son. We can use FFP10 noise simulations, identical to the data in terms of sky sampling and with matching time domain noise characteristics, to make stati ...n coolers), or related to intrinsic instrument properties coupled with the sky signal, such as stray light contamination.
  6 KB (891 words) - 11:09, 6 July 2018
• Effective Beams
  ...etry of the beam and the uneven distribution of scanning angles across the sky. ..., the objects whose convolution with the true CMB sky produce the observed sky map.
  67 KB (9,735 words) - 02:01, 22 March 2018
• Summary LFI
  [[File:Lfi_perf.jpg|thumb|center|655px|<math>^{ \rm a \, }</math> White noise per pixel computed from half-ring difference maps <math>^{ \rm b \, }</math> FWHM and ellipticity from scanning beam evaluated fitting Jup
  3 KB (411 words) - 16:00, 5 July 2018
• LFIAppendix
  ...(1−A) \frac{z}{L_{\rm s}} + A \, \sin^\beta \, (\frac{\pi \, z}{2 \, L_{\rm s}})) </math> : <math> 0 ≤ z ≤ L_{\rm s}
  60 KB (9,314 words) - 08:48, 2 January 2015
• Frequency maps angular power spectra
  {{DISPLAYTITLE:Sky temperature power spectra}} Angular power spectra of cut sky CMB dominated maps are provided to allow independent cosmological analysis
  25 KB (3,718 words) - 15:37, 18 July 2014
• HFI data compression
  strip on the sky about 8&deg; long. The mean <<i>S</i>_REU> of the data within <math>S_{{\rm demod},i} = (S_{{\rm REU},i} - \langle S_{\rm REU} \rangle) \ast(-1)^{i}</math>,
  8 KB (1,269 words) - 09:45, 10 December 2014
• Astrophysical component separation
  ...al linear combination" method with weighting coefficients varying over the sky and over the multipole range up to &#8467;=3200, and it does so using "need ...rds, the weights are computed over a masked sky, but are applied to a full sky (excluding point sources). In a final step, the pixels masked due to point
  16 KB (2,572 words) - 10:22, 10 July 2018
• Beams
  ...ope and the mapmaking procedure, and varies from pixel to pixel across the sky. ...see {{PlanckPapers|planck2016-l03}}). This affects a small fraction of the sky in a negligible way.
  53 KB (8,689 words) - 15:07, 2 July 2018
• CMB and astrophysical component maps
  : The Commander sky maps have different angular resolutions depending on data products: * The components of the full astrophysical sky model derived from the complete data combination (Planck, WMAP, 408 MHz) ha
  73 KB (10,660 words) - 08:15, 21 August 2016

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