Difference between revisions of "Summary LFI"

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|width="300" | Overall calibration uncertainty<math>^{\rm e}</math> [%]
 
|width="300" | Overall calibration uncertainty<math>^{\rm e}</math> [%]
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|width="100" | *TBD
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|width="100" | 0.35
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|width="100" | *TBD
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|width="100" | 0.26
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|width="100" | *TBD
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|width="100" | 0.29
 
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|width="300" | Systematic effects uncertainty<math>^{\rm f}</math> [<math>\mu</math>K<math>_{CMB}</math>]
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|width="300" | Systematic effects uncertainty in Stokes <math>I^{\rm f}</math> [<math>\mu</math>K<math>_{CMB}</math>]
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|width="100" | *TBD
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|width="100" | 0.88
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|width="100" | *TBD
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|width="100" | 1.97
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|width="100" | *TBD
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|width="100" | 1.87
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|width="300" | Systematic effects uncertainty in Stokes <math>Q^{\rm f}</math> [<math>\mu</math>K<math>_{CMB}</math>]
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|width="100" | 1.11
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|width="100" | 1.14
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|width="100" | 2.25
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|width="300" | Systematic effects uncertainty in Stokes <math>U^{\rm f}</math> [<math>\mu</math>K<math>_{CMB}</math>]
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|width="100" | 0.95
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|width="100" | 1.29
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|width="100" | 2.22
 
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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}}.  
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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}} .  
  
 
<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.

Revision as of 16:15, 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-2013-II[1]Planck-2015-A03[2].

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

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

[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 Planck-2013-XXVIII[3] .

[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 d}[/math] Values derived from fitting noise spectra.

[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 \lt \ell \lt 250 [/math] (see Planck-2013-V[4].

[math]^{\rm f}[/math] Peak-to-peak difference between 99% and 1% quantities in the pixel value distributions from simulated maps (see Planck-2013-III[5].


References[edit]

  1. ↑ Planck 2013 results. II. Low Frequency Instrument data processing, Planck Collaboration, 2014, A&A, 571, A2
  2. ↑ Planck 2015 results. II. LFI processing, Planck Collaboration, 2016, A&A, 594, A2.
  3. ↑ Planck 2013 results. XXVIII. The Planck Catalogue of Compact Sources, Planck Collaboration, 2014, A&A, 571, A28
  4. ↑ Planck 2013 results. V. LFI Calibration, Planck Collaboration, 2014, A&A, 571, A5
  5. ↑ Planck 2013 results. III. Low Frequency Instrument systematic uncertainties, Planck Collaboration, 2014, A&A, 571, A3

(Planck) Low Frequency Instrument

Full-Width-at-Half-Maximum

Cosmic Microwave background

To be defined / determined

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