Difference between revisions of "Summary LFI"
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{{DISPLAYTITLE:Summary of LFI data characteristics}} | {{DISPLAYTITLE:Summary of LFI data characteristics}} | ||
| − | The LFI performance are summarized in Table 1 below. All the details can be found in the LFI data processing paper | + | 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. | ||
| − | <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 | + | <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. | ||
| − | <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> | + | <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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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].
| Parameter | 30 GHz | 44 GHz | 70 GHz |
|---|---|---|---|
| Center frequency [GHz] | 28.4 | 44.1 | 70.4 |
| Scanning beam FWHM [arcmin] | 33.10 | 27.94 | 13.08 |
| Scanning beam ellipticity | 1.37 | 1.25 | 1.27 |
| Effective beam FWHM [arcmin] | 32.29 | 27.00 | 13.21 |
| White noise level in map [K] | *TBD | *TBD | *TBD |
| White noise level in timelines [K] | 148.1 | 174.2 | 152.0 |
| f [mHz] | 114.1 | 52.4 | 19.7 |
| 1/ slope | -0.92 | -0.88 | -1.20 |
| Overall calibration uncertainty [%] | 0.35 | 0.26 | 0.29 |
| Systematic effects uncertainty in Stokes [K] | 0.88 | 1.97 | 1.87 |
| Systematic effects uncertainty in Stokes [K] | 1.11 | 1.14 | 2.25 |
| Systematic effects uncertainty in Stokes [K] | 0.95 | 1.29 | 2.22 |
Determined by fitting Jupiter observations directly in the timelines.
Calculated from the main beam solid angle of the effective beam, . These values are used in the source extraction pipeline Planck-2015-A35[2].
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.
Values derived from fitting noise spectra.
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 , see Planck-2015-A05[3].
Peak-to-peak difference between 99% and 1% quantities in the pixel value distributions from simulated maps, see Planck-2015-A03[1].
References[edit]
- ↑ 1.01.1 Planck 2015 results. II. LFI processing, Planck Collaboration, 2016, A&A, 594, A2.
- ↑ Planck 2015 results. XXVI. The second Planck catalogue of compact sources, Planck Collaboration, 2016, A&A, 594, A26.
- ↑ 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
