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- ...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
- ...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.fit25 KB (3,934 words) - 15:07, 26 September 2016
- ...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-20122 KB (3,180 words) - 10:37, 5 February 2015
- ##[[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
- {{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
- 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 indi20 KB (2,907 words) - 13:28, 19 September 2016
- 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
- ...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 agr2 KB (320 words) - 17:06, 4 February 2015
- #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
- == 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
- 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 is14 KB (2,212 words) - 15:15, 26 September 2016
- ...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
- ====Low frequency foreground component==== ...uced to Nside=256 first. Parameters related to the foreground scaling with frequency are estimated at that resolution22 KB (2,713 words) - 18:48, 1 March 2013
- ...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
- 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 approxima52 KB (8,515 words) - 12:52, 7 July 2015
- {{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 other90 KB (13,248 words) - 13:06, 21 April 2020
- * 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
- ##[[LFI overview|LFI design, qualification, and performance]]<span style="color:red"></span> ###[[LFI design, qualification, and performance#LFIDescription| Instrument descripti5 KB (581 words) - 09:33, 31 March 2014
- ##[[LFI overview|LFI design, qualification, and performance]]<span style="color:red"></span> ###[[LFI design, qualification, and performance#LFIDescription| Instrument descripti6 KB (744 words) - 09:45, 31 March 2014
- ...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-V35 KB (5,146 words) - 17:59, 3 July 2014
