Difference between revisions of "Appendix of HFI DPC paper"
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− | This page is intented to | + | This page is intented to provide complementary figures to those of the 2017 HFI DPC paper ({{PlanckPapers|planck2016-l03}}). |
− | {| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align: | + | |
− | |+ '''[ | + | |
+ | <!-- | ||
+ | {| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:center" width=800px | ||
+ | |+ '''CO and dust templates ''' | ||
+ | |- bgcolor="ffdead" | ||
+ | ! | ||
+ | !100 GHz | ||
+ | !143 GHz | ||
+ | !217 GHz | ||
+ | !353 GHz | ||
+ | |- | ||
+ | | CO template | ||
+ | |[[File:TEMPLATE_RES_CO_100.png|100px]] | ||
+ | |. | ||
+ | |[[File:TEMPLATE_RES_CO_217.png|100px]] | ||
+ | |[[File:TEMPLATE_RES_CO_353.png|100px]] | ||
+ | |- | ||
+ | | Dust template | ||
+ | |[[File:TEMPLATE_RES_DUST_100.png|100px]] | ||
+ | |[[File:TEMPLATE_RES_DUST_143.png|100px]] | ||
+ | |[[File:TEMPLATE_RES_DUST_217.png|100px]] | ||
+ | |[[File:TEMPLATE_RES_DUST_353.png|100px]] | ||
+ | |} | ||
+ | |||
+ | --> | ||
+ | |||
+ | |||
+ | |||
+ | <br> | ||
+ | ---- | ||
+ | <span style="font-size:150%">'''Section 5.3.10: for convenience, we reproduce here Figures 6, 7 and 8 of Rosset et al.''' </span> | ||
+ | |||
+ | 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 | ||
+ | |||
+ | {| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align:centert" width=800px | ||
+ | |- bgcolor="ffdead" | ||
+ | ! gain errors (1)|| polarization efficiency errors (2)|| orientation errors (3) | ||
+ | |- | ||
+ | |[[File:13054fig6.pdf]] | ||
+ | |[[File:13054fig7.pdf]] | ||
+ | |[[File:13054fig8.pdf]] | ||
+ | |} | ||
+ | |||
+ | (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. | ||
+ | |||
+ | |||
+ | <br> | ||
+ | ---- | ||
+ | <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:center" width=800px | ||
+ | |+ '''Map and power spectra from E2E simulations difference with and without 4K lines. ''' | ||
|- bgcolor="ffdead" | |- bgcolor="ffdead" | ||
!colspan="2"| 100 GHz bolometers | !colspan="2"| 100 GHz bolometers | ||
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!colspan="2"| 353 GHz bolometers | !colspan="2"| 353 GHz bolometers | ||
|- | |- | ||
− | |[[File:map_100-1a_lines4K.pdf]] | + | |[[File:map_100-1a_lines4K.pdf|100px]] |
− | |[[File:cl_fsky43_lines4K_100-1a_sroll.pdf]] | + | |[[File:cl_fsky43_lines4K_100-1a_sroll.pdf|100px]] |
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− | |[[File:cl_fsky43_lines4K_143-1a_sroll.pdf]] | + | |[[File:cl_fsky43_lines4K_143-1a_sroll.pdf|100px]] |
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− | |[[File:map_100-2a_lines4K.pdf]] | + | |[[File:map_100-2a_lines4K.pdf|100px]] |
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− | |[[File:cl_fsky43_lines4K_353-4b_sroll.pdf]] | + | |[[File:cl_fsky43_lines4K_353-4b_sroll.pdf|100px]] |
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− | |[[File:map_100-4a_lines4K.pdf]] | + | |[[File:map_100-4a_lines4K.pdf|100px]] |
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− | |[[File:map_100-4b_lines4K.pdf]] | + | |[[File:map_100-4b_lines4K.pdf|100px]] |
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|} | |} | ||
− | {| border="1" cellpadding="3" cellspacing="0" align="center" style="text-align: | + | <br> |
− | |+ ''' | + | ---- |
+ | <span style="font-size:150%">'''Section 5.13: complementary figures of Fig. 47''' </span> | ||
+ | |||
+ | {| 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. ''' | ||
|- bgcolor="ffdead" | |- bgcolor="ffdead" | ||
! 100 GHz bolometers || 143 GHz bolometers || 217 GHz bolometers || 353 GHz bolometers | ! 100 GHz bolometers || 143 GHz bolometers || 217 GHz bolometers || 353 GHz bolometers | ||
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|[[File:DEC16v1_gains_353ghz_JG_INL.pdf]] | |[[File:DEC16v1_gains_353ghz_JG_INL.pdf]] | ||
|} | |} | ||
+ | |||
+ | <br> | ||
+ | == References == | ||
+ | <References /> | ||
+ | |||
+ | [[Category:HFI data processing|004]] |
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) |
---|---|---|
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Error creating thumbnail: convert: unable to extend cache `/tmp/magick-11405iw6mMLG8tIra': File too large @ error/cache.c/OpenPixelCache/4091.
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Error creating thumbnail: convert: unable to extend cache `/tmp/magick-11412ELvJeE5wyu8y': File too large @ error/cache.c/OpenPixelCache/4091.
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(1)
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)
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)
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
100 GHz bolometers | 143 GHz bolometers | 217 GHz bolometers | 353 GHz bolometers | ||||
---|---|---|---|---|---|---|---|
100px | |||||||
. | . | ||||||
. | . | ||||||
. | . | ||||||
. | . | . | . |
Section 5.13: complementary figures of Fig. 47
References[edit]
- ↑ Planck 2018 results. III. High Frequency Instrument data processing and frequency maps, Planck Collaboration, 2020, A&A, 641, A3.
- ↑ 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