Search results

Create the page "LFI data processing" on this wiki! See also the search results found.

• HFI/LFI joint data processing
  HFI/LFI common processing uses as basic input the maps at the nine frequencies covered by the two ins ...lihood code (of a particular theoretical <math>C(\ell)</math> given Planck data).
  464 bytes (69 words) - 21:13, 17 March 2013
• Beams LFI
  LFI is observing the sky with 11 pairs of beams associated with the 22 pseudo-c ...} (see also [[LFI design, qualification, and performance#Naming Convention|LFI naming convention]]).
  23 KB (3,650 words) - 15:53, 23 July 2014
• References
  title = {Planck 2013 results: The Low Frequency Instrument data processing (p02)}, title = {Planck 2013 results: LFI systematic uncertainties (p02a)},
  174 KB (25,501 words) - 09:16, 10 July 2014
• LFI-Validation
  Data validation is a step of paramount importance in the complex process of data analysis and the extraction of the final scientific goals of an experiment. The LFI approach to data validation is based upon null-tests approach and here we present
  13 KB (1,992 words) - 16:09, 23 July 2014
• Mission products
  To support the interpretation of these data, these products are accompanied by: * instrument-level data (beam properties, noise levels, bandpass profiles, and more) compiled into
  3 KB (470 words) - 22:04, 17 March 2013
• Spectral response
  ...correction coefficients will be provided here (or perhaps in the joint HFI/LFI section). There will be links to the UcCC subsection of the PLA section, b The band-average HFI spectral response data are shown in the figure below, and provided in the RIMO file ([[the RIMO|he
  18 KB (805 words) - 14:32, 23 July 2014
• Compact Source catalogues
  ...nck nominal maps. The first public version of the PCCS is derived from the data acquired by Planck between August 13 2009 and November 26 2010. The PCCS co ...r corrected. Colour corrections are available in Table 15 of [[LFIAppendix|LFI Appendix]] and [[UC CC Tables|HFI spectral response]] pages.
  12 KB (1,879 words) - 16:37, 23 July 2014
• Effective Beams
  ...essing are given in the respective pages for [[Beams|HFI]] and [[Beams_LFI|LFI]]. ...} and HFI {{PlanckPapers|planck2013-p03c}} papers. Relevant details of the processing steps are given in the [[Beams|Effective Beams]] section of this document.
  23 KB (3,381 words) - 12:28, 28 August 2014
• Survey scanning and performance
  ...angle from the spin axis. 545 GHz, 857 GHz, 143 GHz bolometers as well as LFI 25-26 radiometers have a slightly smaller bore-sight angle, while the other == Data gap recoveries ==
  16 KB (2,501 words) - 14:28, 22 July 2014
• Summary LFI
  {{DISPLAYTITLE:Summary of LFI data characteristics}} ...summarized in Table 1 below. All the details can be found in the LFI data processing paper {{PlanckPapers|planck2013-p02}}.
  2 KB (296 words) - 16:20, 23 July 2014
• List of acronyms
  * '''BEM''' : LFI warm electronics Back End Module * '''BEU''' : LFI warm electronics Back End Unit
  5 KB (589 words) - 18:06, 3 July 2014
• LFI systematic effect uncertainties
  Known systematic effects in the Planck-LFI data can be divided into two broad categories: effects independent of the sky si ...evel overview of the uncertainties due to systematic effects in the Planck-LFI CMB temperature maps and power spectra. Table 1 provides a list of these ef
  16 KB (2,578 words) - 16:05, 23 July 2014
• DatesObs
  * FITS format, with data in the first extension * NSIDE 1024 for LFI, and 2048 for HFI
  2 KB (351 words) - 17:26, 19 July 2013
• L3 LFI
  ...lude 1000 realization of both signal and noise maps consistent with Planck data. The angular response of the instrument is accounted for by using the beam == LFI specific L3 activities: masks, MCQA, etc ==
  2 KB (270 words) - 16:19, 23 July 2014
• LFIAppendix
  {{DISPLAYTITLE:LFI Annexes}} === Annexes: LFI Instrument ===
  59 KB (9,067 words) - 10:10, 23 July 2014
• Frequency maps angular power spectra
  ...the data, and therefore determine the best cosmological models fitting the data. Several examples of such high-<math>\ell</math> likelihoods are described, ...tematic effects (such as uncertainty on the beam modeling) as well as post-processing steps (such as foreground subtraction) will increase the covariance. In the
  25 KB (3,721 words) - 17:10, 23 July 2014
• Astrophysical component separation
  ...g 'needlets' which are spherical wavelets. A special procedure is used for processing the coarsest needlet scale ...applied to Planck simulations Leach et al., 2008 and to WMAP polarisation data Fernandez-Cobos et al., 2012. In the cleaning process, no assumptions about
  12 KB (1,894 words) - 16:38, 23 July 2014
• CMB Maps test
  The CMB data are in thermodynamic temperature units (uK_cmb), and the residuals are in t ...applied to Planck simulations Leach et al., 2008 and to WMAP polarisation data Fernandez-cobos et al., 2012. In the cleaning process, no assumptions about
  7 KB (1,103 words) - 18:38, 1 March 2013
• Unit conversion and Color correction
  ...is delivered as a tarfile and contains a detailed instruction manual. The data and software file requirements are provided below along with basic use inst ...ro</tt>: a routine to get the desired detector level spectral transmission data (HFI) and output in a structure format used by the other routines.
  28 KB (4,680 words) - 10:21, 2 October 2014
• Beams
  ...on to reconstruct the beam. The data are processed with the bigPlanets TOI processing (see [[Frequency_Maps#HFI_processing | here]] or Section 3.11 of {{PlanckPa The time ordered data are used to fit a two dimensional B-Spline surface using a least square min
  33 KB (5,387 words) - 14:27, 23 July 2014

View (previous 20 | next 20) (20 | 50 | 100 | 250 | 500)