Difference between revisions of "Appendix of HFI DPC paper"

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This page is intented to gather figures that are not inserted in the 2017 DPC paper  ({{PlanckPapers|planck2016-l03}}) for readability reasons.
 
This page is intented to gather figures that are not inserted in the 2017 DPC paper  ({{PlanckPapers|planck2016-l03}}) for readability reasons.
  
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<span style="font-size:150%">'''Section 3.1.2. Mask of the very bright regions where the sub-pixel effect in the foreground templates creates problems and prevent them to be used for cosmology or astrophysics analysis''' </span>
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<span style="font-size:150%">'''Section 3.1.2: masks of the very bright regions where the sub-pixel effect in the foreground templates prevent them to be used for cosmology or astrophysics analysis''' </span>
  
 
Those masks are provided in the PLA.<!-- LVLV -->
 
Those masks are provided in the PLA.<!-- LVLV -->
 
   
 
   
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{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
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{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:center" width=800px
 
|+ '''CO and dust templates '''
 
|+ '''CO and dust templates '''
 
|- bgcolor="ffdead"
 
|- bgcolor="ffdead"
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<span style="font-size:150%">'''Section 3.2: Complementary figures of Fig. 11''' </span>
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<span style="font-size:150%">'''Section 3.2: complementary figures of Fig. 11''' </span>
  
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
+
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:centert" width=800px
 
|+ '''Comparaison of 2015 and 2017 I, Q and U maps and their difference. '''
 
|+ '''Comparaison of 2015 and 2017 I, Q and U maps and their difference. '''
 
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<span style="font-size:150%">'''Section 5.3.10. For convenience, we reproduce here Figures 6, 7 and 8 of Rosset et al.''' </span>
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<span style="font-size:150%">'''Section 5.3.10: for convenience, we reproduce here Figures 6, 7 and 8 of Rosset et al.''' </span>
  
  
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This paper is published as Rosset et al. Planck pre-launch status: High Frequency Instrument polarization calibration. 2010b, A&A, 520, A13.
+
This paper is published as Rosset et al. Planck pre-launch status: High Frequency Instrument polarization calibration. 2010b, A&A, 520, A13. ({{PlanckPapers|Planck-PreLaunch-IX}})
 
The figures 6, 7 et 8 reproduced hereunder are given in the version on ArXiv 1004.2595
 
The figures 6, 7 et 8 reproduced hereunder are given in the version on ArXiv 1004.2595
  
  
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{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
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{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:centert" width=800px
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
 
! gain errors (1)|| polarization efficiency errors (2)|| orientation errors (3)
 
! gain errors (1)|| polarization efficiency errors (2)|| orientation errors (3)
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(1) Delta Cl in rms due to gain errors from 0.01% to 1% for E-mode (top) and B-mode (bottom) compared to initial spectrum (solid black lines). Cosmic variance for E-mode is plotted in dashed black line.
+
(1) <math>\Delta C_{\ell}</math> in rms due to gain errors from 0.01% to 1% for E-mode (top) and B-mode (bottom) compared to initial spectrum (solid black lines). Cosmic variance for E-mode is plotted in dashed black line.
  
−
(2) Delta Cl in rms due to polarization effi?ciency errors from 0.1% to 4% for E-mode (top) and B-mode (bottom) compared to initial spectrum (solid black lines). Cosmic variance for E-mode is plotted in dashed black line.
+
(2) <math>\Delta C_{\ell}</math> in rms due to polarization efficiency errors from 0.1% to 4% for E-mode (top) and B-mode (bottom) compared to initial spectrum (solid black lines). Cosmic variance for E-mode is plotted in dashed black line.
  
−
(3) Delta Cl in rms due to various orientation errors from 0.25 to 2 degrees for E-mode (top) and B-mode (bottom) compared to initial spectrum (solid black lines). Cosmic variance for E-mode is plotted in dashed black line.
+
(3) <math>\Delta C_{\ell}</math> in rms due to various orientation errors from 0.25 to 2 degrees for E-mode (top) and B-mode (bottom) compared to initial spectrum (solid black lines). Cosmic variance for E-mode is plotted in dashed black line.
  
  
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<span style="font-size:150%">'''Section 5.5: Complementary figures of Fig. 29''' </span>
+
<span style="font-size:150%">'''Section 5.5: complementary figures of Fig. 29''' </span>
  
−
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
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{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:center" width=800px
 
|+ '''Map and power spectra from E2E simulations difference with and without 4K lines. '''
 
|+ '''Map and power spectra from E2E simulations difference with and without 4K lines. '''
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   
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<span style="font-size:150%">'''Section 5.13: complementary figures of Fig. 47''' </span>
 
<span style="font-size:150%">'''Section 5.13: complementary figures of Fig. 47''' </span>
  
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{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:left" width=800px
+
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:center" width=800px
 
|+ '''ADCNL induced gain time variation as a function of ring numbers. Blue line shows the solved gain variation for the data and grey ones show 10 realizations drawn within the uncertainties of the ADC model. '''
 
|+ '''ADCNL induced gain time variation as a function of ring numbers. Blue line shows the solved gain variation for the data and grey ones show 10 realizations drawn within the uncertainties of the ADC model. '''
 
|- bgcolor="ffdead"   
 
|- bgcolor="ffdead"   

Revision as of 13:38, 6 October 2017

This page is intented to gather figures that are not inserted in the 2017 DPC paper (Planck-2020-A3[1]) for readability reasons.

Section 3.1.2: masks of the very bright regions where the sub-pixel effect in the foreground templates prevent them to be used for cosmology or astrophysics analysis

Those masks are provided in the PLA.

CO and dust templates
100 GHz 143 GHz 217 GHz 353 GHz
CO template TEMPLATE RES CO 100.png . TEMPLATE RES CO 217.png TEMPLATE RES CO 353.png
Dust template TEMPLATE RES DUST 100.png TEMPLATE RES DUST 143.png TEMPLATE RES DUST 217.png TEMPLATE RES DUST 353.png


Section 3.2: complementary figures of Fig. 11

Comparaison of 2015 and 2017 I, Q and U maps and their difference.
2015 maps 2017 maps difference
I Q U I Q U I Q U
100 GHz 100GHz DX11 I.pdf.pdf 100GHz DX11 Q.pdf.pdf 100GHz DX11 U.pdf.pdf 100GHz I.pdf 100GHz Q.pdf 100GHz U.pdf 100GHz diff I.pdf.pdf 100GHz diff Q.pdf.pdf 100GHz diff U.pdf.pdf
143 GHz 143GHz DX11 I.pdf.pdf 143GHz DX11 Q.pdf.pdf 143GHz DX11 U.pdf.pdf 143GHz I.pdf 143GHz Q.pdf 143GHz U.pdf 143GHz diff I.pdf.pdf 143GHz diff Q.pdf.pdf 143GHz diff U.pdf.pdf
217 GHz 217GHz DX11 I.pdf.pdf 217GHz DX11 Q.pdf.pdf 217GHz DX11 U.pdf.pdf 217GHz I.pdf 217GHz Q.pdf 217GHz U.pdf 217GHz diff I.pdf.pdf 217GHz diff Q.pdf.pdf 217GHz diff U.pdf.pdf
353 GHz 353GHz DX11 I.pdf.pdf 353GHz DX11 Q.pdf.pdf 353GHz DX11 U.pdf.pdf 353GHz I.pdf 353GHz Q.pdf 353GHz U.pdf 353GHz diff I.pdf.pdf 353GHz diff Q.pdf.pdf 353GHz diff U.pdf.pdf
545 GHz 545GHz DX11 I.pdf.pdf . . 545GHz I.pdf . . 545GHz diff I.pdf.pdf . .
857 GHz 857GHz DX11 I.pdf.pdf . . 857GHz I.pdf . . 857GHz diff I.pdf.pdf . .


Section 5.3.10: for convenience, we reproduce here Figures 6, 7 and 8 of Rosset et al.


This paper is published as Rosset et al. Planck pre-launch status: High Frequency Instrument polarization calibration. 2010b, A&A, 520, A13. ([2]) The figures 6, 7 et 8 reproduced hereunder are given in the version on ArXiv 1004.2595


gain errors (1) polarization efficiency errors (2) orientation errors (3)
Error creating thumbnail: convert: unable to extend cache `/tmp/magick-2955jBnw-VcVoJ8T': File too large @ error/cache.c/OpenPixelCache/4091.
Error creating thumbnail: convert: unable to extend cache `/tmp/magick-2962UX91cw4swIhf': File too large @ error/cache.c/OpenPixelCache/4091.
Error creating thumbnail: convert: unable to extend cache `/tmp/magick-2969jAi2gZbHpEyL': File too large @ error/cache.c/OpenPixelCache/4091.

(1) [math]\Delta C_{\ell}[/math] in rms due to gain errors from 0.01% to 1% for E-mode (top) and B-mode (bottom) compared to initial spectrum (solid black lines). Cosmic variance for E-mode is plotted in dashed black line.

(2) [math]\Delta C_{\ell}[/math] in rms due to polarization efficiency errors from 0.1% to 4% for E-mode (top) and B-mode (bottom) compared to initial spectrum (solid black lines). Cosmic variance for E-mode is plotted in dashed black line.

(3) [math]\Delta C_{\ell}[/math] in rms due to various orientation errors from 0.25 to 2 degrees for E-mode (top) and B-mode (bottom) compared to initial spectrum (solid black lines). Cosmic variance for E-mode is plotted in dashed black line.


Section 5.5: complementary figures of Fig. 29

Map and power spectra from E2E simulations difference with and without 4K lines.
100 GHz bolometers 143 GHz bolometers 217 GHz bolometers 353 GHz bolometers
Map 100-1a lines4K.pdf Cl fsky43 lines4K 100-1a sroll.pdf Map 143-1a lines4K.pdf Cl fsky43 lines4K 143-1a sroll.pdf Map 217-1 lines4K.pdf Cl fsky43 lines4K 217-1 sroll.pdf Map 353-1 lines4K.pdf Cl fsky43 lines4K 353-1 sroll.pdf
Map 100-1b lines4K.pdf Cl fsky43 lines4K 100-1b sroll.pdf Map 143-1b lines4K.pdf Cl fsky43 lines4K 143-1b sroll.pdf Map 217-2 lines4K.pdf Cl fsky43 lines4K 217-2 sroll.pdf Map 353-2 lines4K.pdf Cl fsky43 lines4K 353-2 sroll.pdf
Map 100-2a lines4K.pdf Cl fsky43 lines4K 100-2a sroll.pdf Map 143-2a lines4K.pdf Cl fsky43 lines4K 143-2a sroll.pdf Map 217-3 lines4K.pdf Cl fsky43 lines4K 217-3 sroll.pdf Map 353-3a lines4K.pdf Cl fsky43 lines4K 353-3a sroll.pdf
Map 100-2b lines4K.pdf Cl fsky43 lines4K 100-2b sroll.pdf Map 143-2b lines4K.pdf Cl fsky43 lines4K 143-2b sroll.pdf Map 217-4 lines4K.pdf Cl fsky43 lines4K 217-4 sroll.pdf Map 353-3b lines4K.pdf Cl fsky43 lines4K 353-3b sroll.pdf
Map 100-3a lines4K.pdf Cl fsky43 lines4K 100-3a sroll.pdf Map 143-3a lines4K.pdf Cl fsky43 lines4K 143-3a sroll.pdf Map 217-5-a lines4K.pdf Cl fsky43 lines4K 217-5a sroll.pdf Map 353-4a lines4K.pdf Cl fsky43 lines4K 353-4a sroll.pdf
Map 100-3b lines4K.pdf Cl fsky43 lines4K 100-3b sroll.pdf Map 143-3b lines4K.pdf Cl fsky43 lines4K 143-3b sroll.pdf Map 217-5b lines4K.pdf Cl fsky43 lines4K 217-5b sroll.pdf Map 353-4b lines4K.pdf Cl fsky43 lines4K 353-4b sroll.pdf
Map 100-4a lines4K.pdf Cl fsky43 lines4K 100-4a sroll.pdf Map 143-4a lines4K.pdf Cl fsky43 lines4K 143-4a sroll.pdf Map 217-6a lines4K.pdf Cl fsky43 lines4K 217-6a sroll.pdf Map 353-5a lines4K.pdf Cl fsky43 lines4K 353-5a sroll.pdf
Map 100-4b lines4K.pdf Cl fsky43 lines4K 100-4b sroll.pdf Map 143-4b lines4K.pdf Cl fsky43 lines4K 143-4b sroll.pdf Map 217-6b lines4K.pdf Cl fsky43 lines4K 217-6b sroll.pdf Map 353-5b lines4K.pdf Cl fsky43 lines4K 353-5b sroll.pdf
. . Map 143-5 lines4K.pdf Cl fsky43 lines4K 143-5 sroll.pdf Map 217-7a lines4K.pdf Cl fsky43 lines4K 217-7a sroll.pdf Map 353-6a lines4K.pdf Cl fsky43 lines4K 353-6a sroll.pdf
. . Map 143-6 lines4K.pdf Cl fsky43 lines4K 143-6 sroll.pdf Map 217-7b lines4K.pdf Cl fsky43 lines4K 217-7b sroll.pdf Map 353-6b lines4K.pdf Cl fsky43 lines4K 353-6b sroll.pdf
. . Map 143-7 lines4K.pdf Cl fsky43 lines4K 143-7 sroll.pdf Map 217-8a lines4K.pdf Cl fsky43 lines4K 217-8a sroll.pdf Map 353-7 lines4K.pdf Cl fsky43 lines4K 353-7 sroll.pdf
. . . . Map 217-8b lines4K.pdf Cl fsky43 lines4K 217-8b sroll.pdf Map 353-8 lines4K.pdf Cl fsky43 lines4K 353-8 sroll.pdf


Section 5.13: complementary figures of Fig. 47

ADCNL induced gain time variation as a function of ring numbers. Blue line shows the solved gain variation for the data and grey ones show 10 realizations drawn within the uncertainties of the ADC model.
100 GHz bolometers 143 GHz bolometers 217 GHz bolometers 353 GHz bolometers
DEC16v1 gains 100ghz JG INL.pdf DEC16v1 gains 143ghz JG INL.pdf DEC16v1 gains 217ghz JG INL.pdf DEC16v1 gains 353ghz JG INL.pdf

References[edit]

  1. ↑ Planck 2018 results. III. High Frequency Instrument data processing and frequency maps, Planck Collaboration, 2020, A&A, 641, A3.
  2. ↑

Data Processing Center

Planck Legacy Archive

EMI/EMC influence of the 4K cooler mechanical motion on the bolometer readout electronics.

analog to digital converter

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