Difference between revisions of "Summary LFI"

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{{DISPLAYTITLE:Summary of LFI data characteristics}}
 
{{DISPLAYTITLE:Summary of LFI data characteristics}}
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The LFI performance are summarized in Table 1 below. All the details can be found in the LFI data processing paper {{PlanckPapers|planck2013-p02}} {{PlanckPapers|planck2014-a03||Planck-2015-A03}}.
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The LFI performance are summarized in Table 1 below. All the details can be found in the LFI data processing paper {{PlanckPapers|planck2014-a03||Planck-2015-A03}}.
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<math>^{\rm a}</math> Determined by fitting Jupiter observations directly in the timelines.
 
<math>^{\rm a}</math> Determined by fitting Jupiter observations directly in the timelines.
  
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<math>^{\rm b}</math> Calculated from the main beam solid angle of the effective beam, <math>\Omega_{\rm eff} = \hbox{mean}(\Omega)</math>. These values are used in the source extraction pipeline {{PlanckPapers|planck2013-p05}} {{PlanckPapers|planck2014-a35||Planck-2015-A35}}.  
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<math>^{\rm b}</math> Calculated from the main beam solid angle of the effective beam, <math>\Omega_{\rm eff} = \hbox{mean}(\Omega)</math>. These values are used in the source extraction pipeline {{PlanckPapers|planck2014-a35||Planck-2015-A35}}.  
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<math>^{\rm c}</math> White noise per pixel computed from half-ring difference maps. These values are within 1% of the white noise sensitivity computed directly on the timelines, taking into account the actual integration time represented in the maps.
 
<math>^{\rm c}</math> White noise per pixel computed from half-ring difference maps. These values are within 1% of the white noise sensitivity computed directly on the timelines, taking into account the actual integration time represented in the maps.
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<math>^{\rm d}</math> Values derived from fitting noise spectra.  
 
<math>^{\rm d}</math> Values derived from fitting noise spectra.  
  
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<math>^{\rm e}</math> Sum of the error on the estimation of the calibration constant (0.25 %) and the square root of the squared sum of the following errors: beam uncertainty; sidelobe convolution effect; and unknown systematics as measured from the power spectrum at <math>50 < \ell < 250 </math> (see {{PlanckPapers|planck2013-p02b}} {{PlanckPapers|planck2014-a05||Planck-2015-A05}}.
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<math>^{\rm e}</math> Sum of the error on the estimation of the calibration constant (0.25 %) and the square root of the squared sum of the following errors: beam uncertainty; sidelobe convolution effect; and unknown systematics as measured from the power spectrum at <math>50 < \ell < 250 </math>, see {{PlanckPapers|planck2014-a05||Planck-2015-A05}}.
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<math>^{\rm f}</math> Peak-to-peak difference between 99% and 1% quantities in the pixel value distributions from simulated maps, see {{PlanckPapers|planck2014-a03||Planck-2015-A03}}.
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<math>^{\rm f}</math> Peak-to-peak difference between 99% and 1% quantities in the pixel value
 
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distributions from simulated maps (see {{PlanckPapers|planck2013-p02a}} {{PlanckPapers|planck2014-a03||Planck-2015-A03}}.
 
  
  

Revision as of 16:27, 3 February 2015

The LFI performance are summarized in Table 1 below. All the details can be found in the LFI data processing paper Planck-2015-A03[1].


Table 1. LFI performance parameters
Parameter 30 GHz 44 GHz 70 GHz
Center frequency [GHz] 28.4 44.1 70.4
Scanning beam FWHM^{\rm a} [arcmin] 33.10 27.94 13.08
Scanning beam ellipticity^{\rm a} 1.37 1.25 1.27
Effective beam FWHM^{\rm b} [arcmin] 32.29 27.00 13.21
White noise level in map^{\rm c} [\muK[math]_{CMB}[/math]] *TBD *TBD *TBD
White noise level in timelines^{\rm d} [\muK[math]_{CMB} \;s^{1/2}[/math]] 148.1 174.2 152.0
f_{\rm knee}^{\rm d} [mHz] 114.1 52.4 19.7
1/f slope^{\rm d} -0.92 -0.88 -1.20
Overall calibration uncertainty^{\rm e} [%] 0.35 0.26 0.29
Systematic effects uncertainty in Stokes I^{\rm f} [\muK[math]_{CMB}[/math]] 0.88 1.97 1.87
Systematic effects uncertainty in Stokes Q^{\rm f} [\muK[math]_{CMB}[/math]] 1.11 1.14 2.25
Systematic effects uncertainty in Stokes U^{\rm f} [\muK[math]_{CMB}[/math]] 0.95 1.29 2.22

^{\rm a} Determined by fitting Jupiter observations directly in the timelines.

^{\rm b} Calculated from the main beam solid angle of the effective beam, \Omega_{\rm eff} = \hbox{mean}(\Omega). These values are used in the source extraction pipeline Planck-2015-A35[2].


^{\rm c} White noise per pixel computed from half-ring difference maps. These values are within 1% of the white noise sensitivity computed directly on the timelines, taking into account the actual integration time represented in the maps.

^{\rm d} Values derived from fitting noise spectra.

^{\rm e} Sum of the error on the estimation of the calibration constant (0.25 %) and the square root of the squared sum of the following errors: beam uncertainty; sidelobe convolution effect; and unknown systematics as measured from the power spectrum at 50 \lt \ell \lt 250 , see Planck-2015-A05[3].

^{\rm f} Peak-to-peak difference between 99% and 1% quantities in the pixel value distributions from simulated maps, see Planck-2015-A03[1].



References[edit]

  1. ↑ Jump up to: 1.01.1 Planck 2015 results. II. LFI processing, Planck Collaboration, 2016, A&A, 594, A2.
  2. Jump up ↑ Planck 2015 results. XXVI. The second Planck catalogue of compact sources, Planck Collaboration, 2016, A&A, 594, A26.
  3. Jump up ↑ Planck 2015 results. IV. LFI beams and window functions, Planck Collaboration, 2016, A&A, 594, A4.

(Planck) Low Frequency Instrument

Full-Width-at-Half-Maximum

Cosmic Microwave background

To be defined / determined

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