Difference between revisions of "Summary LFI"
| Line 1: | Line 1: | ||
The LFI performance are summarized in Table 1 below. All the details can be found in the LFI data processing paper <cite>#planck2013-p02</cite> {{P2013|2}}. | The LFI performance are summarized in Table 1 below. All the details can be found in the LFI data processing paper <cite>#planck2013-p02</cite> {{P2013|2}}. | ||
| + | |||
| + | <center> | ||
| + | Table 1. Summary of the LFI performance parameters | ||
| + | [[File:Lfi_perf.jpg|thumb|center|655px|<math>^{ \rm a \, }</math> White noise per pixel computed from half-ring difference maps. Those values are within the 1% with the withe noise sensitivity computed directly on the timelines, taking in account the actual mission time minus the manoeuvres and bad-science flagged data | ||
| + | <math>^{ \rm b \, }</math> FWHM and ellipticity from scanning beam evaluated fitting Jupiter directly in the timelines. <math>\hspace{50mm} </math> | ||
| + | <math>^{ \rm c \, }</math> FWHM and ellipticity from effective beam evaluated as mean from different position on the sky. <math>\hspace{42mm} </math> | ||
| + | <math>^{ \rm d \, }</math> FWHM from effective beam evaluated as FWHM<math>_{eff} = \sqrt{\frac{Ω}{2π}} · 2 · \sqrt{2 \log 2}</math>, where Ω is the mean beam solid angle of the effective beam. Those are the values used in the source extraction pipeline <cite>#planck2013-p05</cite> {{P2013|28}} | ||
| + | ]] | ||
| + | </center> | ||
| + | |||
| + | |||
| + | <!-- | ||
<center> | <center> | ||
Table 1. Summary of the LFI performance parameters | Table 1. Summary of the LFI performance parameters | ||
| − | [[File: | + | [[File:Lfi_perf.jpg|thumb|center|655px| |
<math>^{ \rm a \, }</math> FWHM and ellipticity from scanning beam evaluated fitting Jupiter directly in the timelines. <math>\hspace{50mm} </math> | <math>^{ \rm a \, }</math> FWHM and ellipticity from scanning beam evaluated fitting Jupiter directly in the timelines. <math>\hspace{50mm} </math> | ||
| − | <math>^{ \rm b \, }</math> FWHM from effective beam estimated from the main beam solid angle of the effective beam | + | <math>^{ \rm b \, }</math> FWHM from effective beam estimated from the main beam solid angle of the effective beam. Those are the values used in the source extraction pipeline <cite>#planck2013-p05</cite> {{P2013|28}}. |
| − | <math>\hspace{ | + | <math>\hspace{100mm} </math> |
<math>^{ \rm c \, }</math> White noise per pixel computed from half-ring difference maps. Those values are within the 1% with the withe noise sensitivity computed directly on the timelines, taking in account the actual mission time minus the manoeuvres and bad-science flagged data. | <math>^{ \rm c \, }</math> White noise per pixel computed from half-ring difference maps. Those values are within the 1% with the withe noise sensitivity computed directly on the timelines, taking in account the actual mission time minus the manoeuvres and bad-science flagged data. | ||
| − | |||
</center> | </center> | ||
| − | + | --> | |
== References == | == References == | ||
Revision as of 10:06, 17 March 2013
The LFI performance are summarized in Table 1 below. All the details can be found in the LFI data processing paper #planck2013-p02 Planck-2013-II .
Table 1. Summary of the LFI performance parameters
White noise per pixel computed from half-ring difference maps. Those values are within the 1% with the withe noise sensitivity computed directly on the timelines, taking in account the actual mission time minus the manoeuvres and bad-science flagged data FWHM and ellipticity from scanning beam evaluated fitting Jupiter directly in the timelines. FWHM and ellipticity from effective beam evaluated as mean from different position on the sky. FWHM from effective beam evaluated as FWHM, where Ω is the mean beam solid angle of the effective beam. Those are the values used in the source extraction pipeline #planck2013-p05 Planck-2013-XXVIII
References[edit]
<biblio force=false>
</biblio>
(Planck) Low Frequency Instrument
Full-Width-at-Half-Maximum
