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- ...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 Mob50 KB (7,826 words) - 22:29, 4 February 2015
- 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
- ...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 Table72 KB (10,038 words) - 08:40, 24 October 2016
- ...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 the61 KB (9,011 words) - 08:06, 15 May 2017
- **''LFI'' - absolute calibration refers to the 0th order calibration for each channel, one single number, while the relative calibration refers to the component * '''DMC''': Data Management Component, the databases used at the HFI and LFI DPCs.7 KB (1,093 words) - 13:07, 7 July 2015
- ...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 of28 KB (4,415 words) - 18:43, 21 August 2015
- ! 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 con5 KB (484 words) - 10:47, 18 October 2012
- {{DISPLAYTITLE:2015 Sky temperature and polarization maps}} ...e mission in various time ranges or in subsets of the detectors in a given channel. These products are useful for the study of source variability, but they a45 KB (6,681 words) - 11:55, 16 May 2017
- ...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
- 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
- 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
- ...sts of sources, both Galactic and extragalactic, extracted from the Planck maps. ...s of sources, one list per channel at 30, 44 and 70 GHz, and two lists per channel at 100, 143, 217, 353, 545 and 857 GHz.25 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
- 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
- NILC is a linear method for combining the input frequency channels. It implements an ILC with weighting coefficients varying over the ...applied to all Planck channels from 44 to 857 GHz omitting only the 30 GHz channel.14 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
