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 <cite>#planck2013-p02</cite> {{P2013|2}}.
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Quantification of the performance of LFI is summarized in Table 1 below. All the details can be found in the LFI data processing paper {{PlanckPapers|planck2014-a03}}.
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<!-- {{PlanckPapers|planck2013-p02}} -->
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 +
 
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{| border="1" cellspacing="0" cellpadding="2" align="center"
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|+ '''Table 1. LFI performance parameters'''
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|-
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!scope="col"| Parameter
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!scope="col"| 30 GHz
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!scope="col"| 44 GHz
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!scope="col"| 70 GHz
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|-
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|width="320" | Centre frequency [GHz]
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|width="100" | 28.4
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|width="100" | 44.1
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|width="100" | 70.4
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|-
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|width="320" | Scanning beam FWHM<sup>a</sup> [arcmin]
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|width="100" | 33.10
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|width="100" | 27.94
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|width="100" | 13.08
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|-
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|width="320" | Scanning beam ellipticity<sup>a</sup>
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|width="100" | 1.37
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|width="100" | 1.25
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|width="100" | 1.27
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|-
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|width="320" | Effective beam FWHM<sup>b</sup> [arcmin]
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|width="100" | 32.29
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|width="100" | 27.00
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|width="100" | 13.21
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|-
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|width="320" | White noise level in map<sup>c</sup> [&mu;K<sub>CMB</sub>]
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|width="100" | *TBD
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|width="100" | *TBD
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|width="100" | *TBD
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|-
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|width="320" | White noise level in timelines<sup>d</sup> [&mu;K<sub>CMB</sub> s<sup>1/2</sup>]
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|width="100" | 148.1
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|width="100" | 174.2
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|width="100" | 152.0
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|-
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|width="320" | <i>f</i><sub>knee</sub><sup>d</sup> [mHz]
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|width="100" | 114.1
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|width="100" | 52.4
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|width="100" | 19.7
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|-
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|width="320" | 1/<i>f</i> slope<sup>d</sup>
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|width="100" | -0.92
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|width="100" | -0.88
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|width="100" | -1.20
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|-
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|width="320" | Overall calibration uncertainty<sup>e</sup> [%]
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|width="100" | 0.35
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|width="100" | 0.26
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|width="100" | 0.29
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|-
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|width="320" | Systematic effects uncertainty in Stokes <i>I</i> <sup>f</sup> [&mu;K<sub>CMB</sub>]
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|width="100" | 0.88
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|width="100" | 1.97
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|width="100" | 1.87
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|-
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|width="320" | Systematic effects uncertainty in Stokes <i>Q</i> <sup>f</sup> [&mu;K<sub>CMB</sub>]
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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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|-
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|width="320" | Systematic effects uncertainty in Stokes <i>U</i> <sup>f</sup> [&mu;K<sub>CMB</sub>]
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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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|-
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|}
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<sup>a</sup> Determined by fitting Jupiter observations directly in the timelines.
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<sup>b</sup> Calculated from the main beam solid angle of the effective beam, &Omega;<sub>eff</sub> = mean(&Omega;). These values are used in the source extraction pipeline ({{PlanckPapers|planck2014-a35||Planck-2015-A35}}).
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<!-- {{PlanckPapers|planck2013-p05}} -->
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<sup>c</sup> 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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<sup>d</sup> Values derived from fitting noise spectra.
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<sup>e</sup> 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 < &#8467; < 250, see {{PlanckPapers|planck2014-a05}}.
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<!-- {{PlanckPapers|planck2013-p02b}} -->
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<sup>f</sup> Peak-to-peak difference between 99% and 1% quantities in the pixel value distributions from simulated maps, see {{PlanckPapers|planck2014-a03}}.
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<!-- {{PlanckPapers|planck2013-p02a}} -->
  
  
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<center>
 
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'''Table 1. Summary of the LFI performance parameters'''
 
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[[File:tab_perf2.jpg|thumb|center|600px|
 
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<math>^{ \rm a \, }</math> FWHM and ellipticity from scanning beam evaluated fitting Jupiter directly in the timelines. <math>\hspace{480mm} </math>
 
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<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}}.
 
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<math>^{ \rm c \, }</math> White noise per pixel computed from half-ring difference maps. Those values are within the 1% with the white noise sensitivity computed directly on the timelines, taking in account the actual mission time minus the manoeuvres and bad-science flagged data.
 
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]]
 
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</center>
 
  
 
<!--
 
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'''Table 1. Summary of the LFI performance parameters'''
 
'''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
 
[[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
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<math>^{ \rm b \, }</math> FWHM and ellipticity from scanning beam evaluated fitting Jupiter directly in the timelines. <math>\hspace{50mm} </math>
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<math>^{ \rm b \, }</math> FWHM and ellipticity from scanning beam evaluated fitting Jupiter directly in the timelines. <math>\hspace{49mm} </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 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}}
 
<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}}
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== References ==
 
== References ==
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<references />
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<biblio force=false>
 
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#[[References]]
 
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</biblio>
 
  
 
[[Category:LFI data processing|008]]
 
[[Category:LFI data processing|008]]

Latest revision as of 10:09, 26 September 2016

Quantification of the performance of LFI is summarized in Table 1 below. All the details can be found in the LFI data processing paper Planck-2015-A02[1].


Table 1. LFI performance parameters
Parameter 30 GHz 44 GHz 70 GHz
Centre frequency [GHz] 28.4 44.1 70.4
Scanning beam FWHMa [arcmin] 33.10 27.94 13.08
Scanning beam ellipticitya 1.37 1.25 1.27
Effective beam FWHMb [arcmin] 32.29 27.00 13.21
White noise level in mapc [μKCMB] *TBD *TBD *TBD
White noise level in timelinesd [μKCMB s1/2] 148.1 174.2 152.0
fkneed [mHz] 114.1 52.4 19.7
1/f sloped -0.92 -0.88 -1.20
Overall calibration uncertaintye [%] 0.35 0.26 0.29
Systematic effects uncertainty in Stokes I f [μKCMB] 0.88 1.97 1.87
Systematic effects uncertainty in Stokes Q f [μKCMB] 1.11 1.14 2.25
Systematic effects uncertainty in Stokes U f [μKCMB] 0.95 1.29 2.22

a Determined by fitting Jupiter observations directly in the timelines.

b Calculated from the main beam solid angle of the effective beam, Ωeff = mean(Ω). These values are used in the source extraction pipeline (Planck-2015-A35[2]).

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.

d Values derived from fitting noise spectra.

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 < ℓ < 250, see Planck-2015-A04[3].

f Peak-to-peak difference between 99% and 1% quantities in the pixel value distributions from simulated maps, see Planck-2015-A02[1].



References[edit]

  1. ↑ 1.01.1 Planck 2015 results. II. LFI processing, Planck Collaboration, 2016, A&A, 594, A2.
  2. ↑ Planck 2015 results. XXVI. The second Planck catalogue of compact sources, Planck Collaboration, 2016, A&A, 594, A26.
  3. ↑ 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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