Difference between revisions of "Appendix of HFI DPC paper"

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This page is intented to provide complementary figures to those of the 2017 HFI DPC paper ({{PlanckPapers|planck2016-l03}}).
 
This page is intented to provide complementary figures to those of the 2017 HFI DPC paper ({{PlanckPapers|planck2016-l03}}).
  
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<span style="font-size:150%">'''Section 3.1.2: Very bright regions where the sub-pixel effect in the SRoll CO foreground templates prevent them to be used for cosmology or astrophysics analysis''' </span>
 
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We simulated the effect to evaluate its level. The difference between the simulated downgraded (at N<sub>side</sub>=128) CO simulated maps and the input full resolution (at N<sub>side</sub>=2048) CO simulated maps gives the simulated bias introduced by this downgrading for each bolometer. For each frequency channel, these bias maps are converted to HPRs, multiplied by the corresponding CO bandpass coefficients computed by SRoll, and projected onto a frequency map of the bias for the channel. Those frequency averaged bias maps are displayed in the table and given in PLA (LVLV).  <!-- LVLV -->
 
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For convenience, we also provide the maps of the logarithm of the ratio of the variance, in each N<sub>side</sub>=128 pixel, between the bias map and the noise level estimated from the End-to-End simulations. This bias is well determined and specific masks adapted to each scientific analysis can be computed at the appropriate level. Those bias maps are also provided in the PLA.<!-- LVLV -->
 
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The table also gives the sky fraction to be masked for thresholding the bias at 100, 10, and 1 % the rms of the bias at N<sub>side</sub>=2048 inside the pixel at N<sub>side</sub>=128 referred to the rms of the noise at N<sub>side</sub>=2048 inside the same pixel at N<sub>side</sub>=128.
 
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The effects are largest at 100 GHz. It can also be noted that, for polarization, only less than 10-3 of the sky is affected by this bias at the noise level. For intensity, the biais is an order of magnitude lower. If the user wants to reduce the bias below 10 % of the noise in polarization, 2% of the sky will be affected. Users can also refer to the absolute value of the bias with respect to the
 
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CO maps to build the relevant mask.
 
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{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:center" width=800px
 
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|+ '''CO templates '''
 
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!colspan="3" | 100 GHz
 
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!colspan="3" | 143 GHz
 
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!colspan="3" | 217 GHz
 
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!colspan="3" | 353 GHz
 
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|bias maps in muK
 
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|[[File:100-I_CO_Subpix.png|100px]]
 
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|bias noise ratio maps
 
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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>
 
<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. ({{PlanckPapers|Planck-PreLaunch-IX}})
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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 {{PlanckPapers|rosset2010}}. The figures 6, 7 et 8 reproduced hereunder are given in the version on ArXiv 1004.2595
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The figures 6, 7 et 8 reproduced hereunder are given in the version on ArXiv 1004.2595
 
  
 
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:centert" width=800px
 
{| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:centert" width=800px

Latest revision as of 11:31, 28 November 2017

This page is intented to provide complementary figures to those of the 2017 HFI DPC paper (Planck-2020-A3[1]).





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 Planck-PreLaunch-XIII[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-30434MV1u70kOAU06': File too large @ error/cache.c/OpenPixelCache/4091.
Error creating thumbnail: convert: unable to extend cache `/tmp/magick-30441hF9Axg5ibRSB': File too large @ error/cache.c/OpenPixelCache/4091.
Error creating thumbnail: convert: unable to extend cache `/tmp/magick-30448zev0R7LilI8V': 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
100px 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. ↑ Planck pre-launch status: High Frequency Instrument polarization calibration, C. Rosset, M. Tristram, N. Ponthieu, et al. , A&A, 520, A13+, (2010).

(Planck) High Frequency Instrument

Data Processing Center

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

analog to digital converter

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