Bandpass mismatch error for satellite CMB experiments II: correcting for the spurious signal

Banerji, R.; Patanchon, G.; Delabrouille, J.; Hazumi, M.; Hoang, Duc Thuong; Ishino, H.; Matsumura, Tomotake

doi:10.1088/1475-7516/2019/07/043

Cited by 8 publications

(12 citation statements)

References 51 publications

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“…In the companion paper Ref. [19] we explore paths to correct for and mitigate bandpass mismatch error with a dedicated data processing step.…”

Section: Discussionmentioning

confidence: 99%

“…In section 2 we model the bandpass mismatch effect, and in section 3 we evaluate the impact on B mode measurements and relate the mismatch errors to the "crossing moment maps", that provide a measure of uniformity of polarizer angle coverage in each pixel. Correction methods are developed in a companion publication [20].…”

Section: Jcap12(2017)015mentioning

confidence: 99%

“…In this paper, we focus our analysis on a frequency channel centered at ν 0 = 140 GHz, and so we restrict ourselves to the dominant galactic component, namely the thermal dust emission. More galactic components are included in the companion paper discussing the correction of the mismatch [20].…”

Section: Jcap12(2017)015mentioning

confidence: 99%

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Bandpass mismatch error for satellite CMB experiments I: estimating the spurious signal

Hoang

Patanchon

Bucher

et al. 2017

J. Cosmol. Astropart. Phys.

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Future Cosmic Microwave Background (CMB) satellite missions aim to use the B mode polarization to measure the tensor-to-scalar ratio r with a sensitivity σ r < ∼ 10 −3 . Achieving this goal will not only require sufficient detector array sensitivity but also unprecedented control of all systematic errors inherent to CMB polarization measurements. Since polarization measurements derive from differences between observations at different times and from different sensors, detector response mismatches introduce leakages from intensity to polarization and thus lead to a spurious B mode signal. Because the expected primordial B mode polarization signal is dwarfed by the known unpolarized intensity signal, such leakages could contribute substantially to the final error budget for measuring r. Using simulations we estimate the magnitude and angular spectrum of the spurious B mode signal resulting from bandpass mismatch between different detectors. It is assumed here that the detectors are calibrated, for example using the CMB dipole, so that their sensitivity to the primordial CMB signal has been perfectly matched. Consequently the mismatch in the frequency bandpass shape between detectors introduces differences in the relative calibration of galactic emission components. We simulate this effect using a range of scanning patterns being considered for future satellite missions. We find that the spurious contribution to r from reionization bump on large angular scales ( < 10) is ≈ 10 −3 assuming large detector arrays and 20 percent of the sky masked. We show how the amplitude of the leakage depends on the angular coverage per pixels that results from the scan pattern. IntroductionMeasurements of the cosmic microwave background (CMB) provide a rich data set for studying cosmology and astrophysics and for placing stringent constraints on cosmological models. In particular, the ESA Planck satellite mission has produced full sky maps in both temperature and polarization at unprecedented sensitivity in nine broad (∆ν/ν ≈ 0.3) microwave frequency bands [1].Conventional cosmological models predict that the CMB is linearly polarized, so that the fourth Stokes parameter V vanishes. CMB polarization patterns can be decomposed in two components known as the E and B modes, respectively of even and odd parity. In linear cosmological perturbation theory, scalar perturbations produce E mode polarization but are unable to produce any B mode polarization at linear order. The E mode polarization angular power spectrum can be predicted from a model fitted to the measured T anisotropies. The WMAP [2] and Planck [3] space missions, complemented on smaller angular scales by ACT [4] and SPT [5], have already measured the E mode polarization power spectrum up to high multipole number , even if the accuracy of the measurement can still be substantially improved. On the other hand, the odd parity (or pseudo-scalar) polarization pattern called the B mode arises either from primordial tensor perturbations, or equivalently primordial gravitational wa...

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“…In the companion paper Ref. [19] we explore paths to correct for and mitigate bandpass mismatch error with a dedicated data processing step.…”

Section: Discussionmentioning

confidence: 99%

Section: Jcap12(2017)015mentioning

confidence: 99%

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Bandpass mismatch error for satellite CMB experiments I: estimating the spurious signal

Hoang

Patanchon

Bucher

et al. 2017

J. Cosmol. Astropart. Phys.

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“…Some of these effects result from well-understood phenomena, such as imperfect inter-calibration of detectors, inaccurate correction for time constants of detectors and for electronic cross-talk, ADC conversion, unmasked glitches, etc. Other systematic effects have been discovered during data processing, such as the spurious contributions from molecular gas spectral lines in the signal [22] and bandpass mismatch between detectors [23,24], both of which were encountered in the Planck data and required dedicated complex treatment [25]. Another example is the effect of the Gore-Tex membrane in front of the JCMT which requires special treatment ( [26]).…”

Section: Introductionmentioning

confidence: 99%

Performance of the polarization leakage correction in the PILOT data

Bernard,

Roussel

et al. 2022

Preprint

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The Polarized Instrument for Long-wavelength Observation of the Tenuous interstellar medium (PILOT) is a balloon-borne experiment that aims to measure the polarized emission of thermal dust at a wavelength of 240 µm (1.2 THz). The PILOT experiment flew from Timmins, Ontario, Canada in 2015 and 2019 and from Alice Springs, Australia in April 2017. The in-flight performance of the instrument during the second flight was described in [1]. In this paper, we present data processing steps that were not presented in [1] and that we have recently implemented to correct for several remaining instrumental effects. The additional data processing concerns corrections related to detector cross-talk and readout circuit memory effects, and leakage from total intensity to polarization. We illustrate the above effects and the performance of our corrections using data obtained during the third flight of PILOT, but the methods used to assess the impact of these effects on the final science-ready data, and our strategies for correcting them will be applied to all PILOT data. We show that the above

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“…Although an important issue for precise CMB polarization measurements, we do not discuss the impact of instrumental systematic effects, and in particular of those systematic effects that induce T -E and T -B mixing. We refer the reader to some relevant dedicated studies (Kaplan & Delabrouille 2002;Hu et al 2003;Rosset et al 2007;MacTavish et al 2008;Shimon et al 2008;Keating et al 2013;Bicep2 Collaboration 2015;Natoli et al 2018;Thuong Hoang et al 2017;Banerji et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Testing the analytical blind separation method in simulated CMB polarization maps

Santos

Yao

et al. 2021

A&A

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Context. Multi-frequency observations are needed to separate the cosmic microwave background (CMB) from foreground emission and accurately extract cosmological information from the data. The analytical blind separation (ABS) method is dedicated to extracting the CMB power spectrum from multi-frequency observations in the presence of contamination from astrophysical foreground emission and instrumental noise. Aims. In this study, we apply the ABS method to simulated sky maps as could be observed with a future space-borne survey in order to test its capability of determining the CMB polarization E- and B-mode power spectra. Methods. We present the ABS method performance on simulations for both a full-sky analysis and for an analysis concentrating on sky regions less impacted by Galactic foreground emission. Results. We discuss the origin and minimization of biases in the estimated CMB polarization angular power spectra. We find that the ABS method performs quite well for the analysis of full-sky observations at intermediate and small angular scales, in spite of strong foreground contamination. On the largest scales, extra work is still required to reduce biases of various origins and the impact of confusion between CMB E and B polarization for partial sky analyses.

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Bandpass mismatch error for satellite CMB experiments II: correcting for the spurious signal

Cited by 8 publications

References 51 publications

Bandpass mismatch error for satellite CMB experiments I: estimating the spurious signal

Bandpass mismatch error for satellite CMB experiments I: estimating the spurious signal

Performance of the polarization leakage correction in the PILOT data

Testing the analytical blind separation method in simulated CMB polarization maps

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