Efficient decomposition of cosmic microwave background polarization maps into pure<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>E</mml:mi></mml:math>, pure<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>B</mml:mi></mml:math>, and ambiguous components

Bunn, Emory F.

doi:10.1103/physrevd.83.083003

Cited by 24 publications

(23 citation statements)

References 41 publications

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“…In this paper we would like to highlight a novel method based on decomposition of the Stokes parameters Q and U into the (Q E , U E ) and (Q B , U B ) families, associated with the E and B modes respectively, 1 which satisfy (Q, U ) = (Q E , U E ) + (Q B , U B ). Based on this representation we will investigate the polarization intensity maps for the E family and the B family,…”

Section: Introductionmentioning

confidence: 99%

E and B families of the Stokes parameters in the polarized synchrotron and thermal dust foregrounds

Liu

Creswell²,

Naselsky³

2018

J. Cosmol. Astropart. Phys.

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Better understanding of Galactic foregrounds is one of the main obstacles to detection of primordial gravitational waves through measurement of the B mode in the polarized microwave sky. We generalize the method proposed in [1] and decompose the polarization signals into the E and B families directly in the domain of the Stokes Q, U parameters asThis also enables an investigation of the morphology and the frequency dependence of these two families, which has been done in the WMAP K, Ka (tracing synchrotron emission) and Planck 2015 HFI maps (tracing thermal dust). The results reveal significant differences in spectra between the E and B families. The spectral index of the E family fluctuates less across the sky than that of the B family, and the same tendency occurs for the polarization angles of the dust and synchrotron channels. The new insight from WMAP and Planck data on the North Polar Spur and BICEP2 zones through our method clearly indicates that these zones are characterized by very low polarization intensity of the B family compared to the E family. We have detected global structure of the B family polarization angles at high Galactic latitudes which cannot be attributed to the cosmic microwave background or instrumental noise. However, we cannot exclude instrumental systematics as a partial contributor to these anomalies.

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Section: Introductionmentioning

confidence: 99%

E and B families of the Stokes parameters in the polarized synchrotron and thermal dust foregrounds

Liu

Creswell²,

Naselsky³

2018

J. Cosmol. Astropart. Phys.

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“…The E/B-mode decomposition can be done either on the shear field itself (e.g. Bunn et al 2003;Bunn 2011), or at the level of correlation functions (e.g. ).…”

Section: Condition Of 3pt E/b Decompositionmentioning

confidence: 99%

Relations between three-point configuration space shear and convergence statistics

Shi

Schneider

Joachimi

2011

A&A

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With the growing interest in and ability of using weak lensing studies to probe the non-Gaussian properties of the matter density field, there is an increasing need for the study of suitable statistical measures, e.g. shear three-point statistics. In this paper we establish the relations between the three-point configuration space shear and convergence statistics, which are an important missing link between different weak lensing three-point statistics and provide an alternative way of relating observation and theory. The method we use also allows us to derive the relations between other two-and three-point correlation functions. We show the consistency of the relations obtained with already established results and demonstrate how they can be evaluated numerically. As a direct application, we use these relations to formulate the condition for E/B-mode decomposition of lensing three-point statistics, which is the basis for constructing new three-point statistics which allow for exact E/B-mode separation. Our work applies also to other two-dimensional polarization fields such as that of the cosmic microwave background.

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“…However, it is important to stress, that component separation and extraction of the primordial CMB polarised signal usually takes place in Q, U domain and only then is converted into E/B components. This conversion is not local and for different masks is accompanied by the presence of different E-to-B leakage terms [5][6][7][8][9].…”

Section: Introductionmentioning

confidence: 99%

Statistics of CMB polarization angles

Creswell

Dachlythra

Liu

et al. 2020

J. Cosmol. Astropart. Phys.

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We study the distribution functions of the CMB polarization angle ψ, focusing on the Planck 2018 CMB maps. We extend the model of Preece & Battye (2014) of Gaussian correlated Q and U Stokes parameters to allow nonzero means. When the variances of Q and U are equal and their covariance and means are zero, the polarization angle is uniformly distributed. Otherwise the uniform distribution will be modulated by harmonics with 2ψ and 4ψ phases. These modulations are visible in the Planck 2018 CMB maps. Furthermore, the mean value of U is peculiar compared to the power spectrum.

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Efficient decomposition of cosmic microwave background polarization maps into pureE, pureB, and ambiguous components

Cited by 24 publications

References 41 publications

E and B families of the Stokes parameters in the polarized synchrotron and thermal dust foregrounds

E and B families of the Stokes parameters in the polarized synchrotron and thermal dust foregrounds

Relations between three-point configuration space shear and convergence statistics

Statistics of CMB polarization angles

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