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 (Planck-2020-A3[1]).




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

The difference between the downgraded (at Nside=128) and the full resolution (at Nside=2048) CO simulated maps provides the level of the 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.

The table displays the maps of the logarithm of the ratio of the variance, in each Nside=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. It can also be noted that very few pixels close to the Galactic centre have been biased at the level comparable to the noise.

Those bias maps are provided in the PLA.

The table also gives the sky fraction masked by thresholding at 100, 10, and 1 % the rms noise of the CO bandpass correction at Nside=2048 inside the pixel at Nside=128 referred to the rms of the noise at Nside=2048 inside the pixel at Nside=128.

CO templates
100 GHz 143 GHz 217 GHz 353 GHz
I Q U I Q U I Q U I Q U
bias maps 100-I CO Subpix.png 100-Q CO Subpix.png 100-U CO Subpix.png . . . 217-I CO Subpix.png 217-Q CO Subpix.png 217-U CO Subpix.png 353-I CO Subpix.png 353-Q CO Subpix.png 353-U CO Subpix.png
100% 0.01 0.01 0.07 . . . 0.00 0.01 0.01 0.00 0.01 0.01
10% 0.55 0.97 1.80 . . . 0.04 0.29 0.19 0.01 0.38 0.29
1% 7.39 8.63 10.81 . . . 0.90 4.98 2.79 0.46 5.81 3.38





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)
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(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]

(Planck) High Frequency Instrument

Data Processing Center

Planck Legacy Archive

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

analog to digital converter