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• Main Page
  ##[[LFI overview|LFI design, qualification, and performance]]<span style="color:red"></span> ###[[LFI design, qualification, and performance#LFIDescription| Instrument descripti
  6 KB (669 words) - 21:21, 6 August 2018
• LFI design, qualification, and performance
  ...to the warm (roughly 300 K) back-end unit (BEU) containing a further radio frequency amplification stage, detector diodes, and all the electronics for data acqu 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 ...scanning direction, in order to provide finer sky sampling for the highest frequency detectors when combining two years of observations.
  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 ...ze:150%">'''Level 2: converting temporal information into clean calibrated maps'''</span>
  4 KB (627 words) - 13:09, 7 July 2015
• The LFI DPC
  ...telemetry handling|Housekeeping telemetry handling]] • [[Pre-processing LFI#Auxiliary data handling|Auxiliary data handling]]'' ...Calibration]] • [[TOI_processing LFI#Noise|Noise]] • [[TOI_processing LFI#References|References]] ''
  8 KB (1,072 words) - 20:27, 4 February 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
• Product Table for PLAv2
  ...color in the products category name, e.g. <span style="color:Blue">1 year maps</span>). Please check this in the tables and let me know whether there are |rowspan="3" align="center" | LFI
  83 KB (8,209 words) - 12:21, 5 February 2015
• Catalogues
  ...single-frequency source catalogues extracted from the Planck full-mission maps in intensity and polarization (LFI_SkyMap_0??_1024_R2.01_full.fits and HFI_ ...4 observations for HFI channels. The relevant properties of the frequency maps and main parameters used to generate the catalogues are summarized in Table
  72 KB (10,038 words) - 08:40, 24 October 2016
• CMB spectrum & Likelihood Code
  ...f Planck 2015 temperature data between 30 and 857 GHz, the 9-year WMAP sky maps, and the 408-MHz Haslam et al. (1982) survey, including 93% of the sky ({{P ...{{PlanckPapers|planck2014-a13}} by optimally combining the spectra in the frequency range 100-217 GHz, and correcting them for unresolved foregrounds using the
  61 KB (9,011 words) - 08:06, 15 May 2017
• Glossary
  **''LFI'' - absolute calibration refers to the 0th order calibration for each chann * '''DMC''': Data Management Component, the databases used at the HFI and LFI DPCs.
  7 KB (1,093 words) - 13:07, 7 July 2015
• Timelines
  ...the value of that quantity as a function of time during the mission. For LFI, refer to {{PlanckPapers|planck2014-a03}}, and for HFI, to {{PlanckPapers|p ...here are sampled regularly at the (instrument dependent) detector sampling frequency and span the full science mission. They thus consist of a large amount of
  28 KB (4,415 words) - 18:43, 21 August 2015
• Single detector maps
  ! There are no single detector maps in the first release. ...of 1024 for LFI, in Galactic coordinates, and Nested ordering. The three maps will be packaged into a FITS files with a single ''BINTABLE'' extension con
  5 KB (484 words) - 10:47, 18 October 2012
• Sky temperature maps
  {{DISPLAYTITLE:2015 Sky temperature and polarization maps}} ...are provided for the full Planck mission using all valid detectors in each frequency channel, and also for various subsets by splitting the mission in various t
  45 KB (6,681 words) - 11:55, 16 May 2017
• HelpForBook
  ...user interested in frequency maps may also be interested in other types of maps. Where DPC is one of HFI or LFI, x_x_x_x the section number for the page where the image will be displayed
  31 KB (5,455 words) - 18:41, 16 March 2013
• The RIMO
  ...th the released data products. It is described in detail in ''The HFI and LFI RIMO ICD'' (ref). See also {{PlanckPapers|planck2014-a03}} and {{PlanckPap ; LFI 2015 RIMO: {{PLASingleFile|fileType=rimo|name=LFI_RIMO_R2.50.fits|link=LFI_
  14 KB (2,168 words) - 09:15, 8 March 2017
• 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
• Scanning Beams
  == LFI beams == ...assuming a flat spectrum of the incoming radiation. The Stokes parameters maps contain the complete information about the field intensity and polarization
  6 KB (827 words) - 14:33, 15 April 2015
• References
  title = {Planck 2013 results: The Low Frequency Instrument data processing (p02)}, title = {Planck 2013 results: LFI systematic uncertainties (p02a)},
  173 KB (25,381 words) - 15:29, 4 June 2014
• LFI-Validation
  ...validation is critical at each step of the analysis pipeline. Much of the LFI data validation is based on null tests. Here we present some examples from ...ion and half-ring levels, for single detectors, horns, horn pairs and full frequency complements. Where possible, map differences are generated in <i>I</i>, <i
  10 KB (1,699 words) - 13:37, 19 September 2016
• 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) - 10:45, 5 February 2015
• 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
  25 KB (3,934 words) - 15:07, 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
• Main Page3
  ##[[LFI design, qualification, and performance|LFI design, qualification, and performance]]<span style="color:red">(Gregorio)< ##[[The LFI DPC|LFI data processing: Introduction]] <span style="color:red">(Zacchei)</span>
  6 KB (770 words) - 17:33, 29 January 2013
• Summary LFI
  {{DISPLAYTITLE:Summary of LFI data characteristics}} ...of LFI is summarized in Table 1 below. All the details can be found in the LFI data processing paper {{PlanckPapers|planck2014-a03}}.
  4 KB (577 words) - 10:09, 26 September 2016
• LFI systematic effect uncertainties
  Known systematic effects in the Planck-LFI data can be divided into two broad categories: effects independent of the s ...uncertainties due to systematic effects in the Planck-LFI CMB temperature maps and power spectra. Table 1 provides a list of these effects with short indi
  20 KB (2,907 words) - 13:28, 19 September 2016
• 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) - 21:49, 29 January 2015
• L3 LFI
  ...rsion 7 ''FFP7'', which includes 1000 realization of both signal and noise maps consistent with Planck data. The angular response of the instrument is acco ...70 GHz temperature power spectra. These have been produced from frequency maps without performing component separation. Nevertheless, there is a clear agr
  2 KB (320 words) - 17:06, 4 February 2015
• CMB angular power spectrum
  #REDIRECT [[Frequency map angular power spectrum]] For LFI, these will be at all ferequecnies, albeit with differnt masks.
  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
• Astrophysical component separation
  NILC is a linear method for combining the input frequency channels. It implements an ILC with weighting coefficients varying over the : As in the SMICA processing, the input maps are internally re-beamed to a 5′ resolution, so the resulting CMB map is
  14 KB (2,212 words) - 15:15, 26 September 2016
• CMB Maps test
  ...ption of the product, including e.g. figures related to the contents (e.g. maps, tables), and some explanation of its scientific meaning. If there are scie ...for the CMB channels, and MJy/sr for the Galactic channels). As usual, all maps are in Galactic coordinate and use Nested ordering scheme.
  7 KB (1,103 words) - 18:38, 1 March 2013
• Astrophysical component maps test
  ====Low frequency foreground component==== ...uced to Nside=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution
  22 KB (2,713 words) - 18:48, 1 March 2013
• 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 ...>: a routine to get the desired detector level spectral transmission data (LFI) and output in a structure format used by the other routines.
  29 KB (4,776 words) - 11:02, 22 February 2017
• Beams
  The reconstruction of the spatial response for the Planck High Frequency Instrument (HFI) is informed by observation of planets. Furthermore, observ ...of the main beam cannot be significantly reduced without boosting the high-frequency noise. The regularization function (a low-pass filter) chosen has approxima
  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
• Changelog
  * 2013-03-27, Moneti/Cardoso, [[CMB and astrophysical component maps]]: update to correct product description, add figures, remove commented tex * 2013-04-03, Mendes. [[Sky temperature maps]]: fixed incorrect links (Ticket ID DTX-918825). <span style="color:Green">
  12 KB (1,788 words) - 08:42, 25 September 2014
• TOC WorkInProgress
  ##[[LFI overview|LFI design, qualification, and performance]]<span style="color:red"></span> ###[[LFI design, qualification, and performance#LFIDescription| Instrument descripti
  5 KB (581 words) - 09:33, 31 March 2014
• TOCV1 BackUp
  ##[[LFI overview|LFI design, qualification, and performance]]<span style="color:red"></span> ###[[LFI design, qualification, and performance#LFIDescription| Instrument descripti
  6 KB (744 words) - 09:45, 31 March 2014
• TestMassEditing
  ...ven in [[HFIpreprocessingstatics | this table]]. As a secondary product, maps with estimates of the Zodiacal light and Far-Side-Lobes contribution remove ...used extensively to investigate the (high frequency) noise properties the maps themselves and of other products described elsewhere (see e.g., the [[HFI-V
  35 KB (5,146 words) - 17:59, 3 July 2014
• Terminology
  ;calibration: [LFI meaning]: absolute calibration refers to the 0th order calibration for each ...f a sphere], {{BibCite|gorski2005}}) pixelation used to produce Planck sky maps (and HFI HPR).
  10 KB (1,539 words) - 15:11, 21 July 2014
• NoiseCovarMatrices
  ...rix is required for maximum likelihood analysis of CMB anisotropies in the maps but also for low resolution component separation. ...e-ordered information (TOI) is cleaned of signal by interpolating the full frequency, full mission map to the sample positions on the sky.
  6 KB (1,020 words) - 18:38, 19 December 2014
• Planck high dynamic range colour palette
  We are displaying the microwave frequency maps over the frequency span of 22-353 GHz. Our principal target --- the ...anisotropy, or even larger, in the noisy channels (radiometers in WMAP and LFI), and considerably smaller, of order <math>\lesssim 10~ \mu {\rm K}</math>,
  2 KB (388 words) - 09:06, 21 June 2016
• 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