Microwave background polarization in cosmological models

Challinor, A.

doi:10.1103/physrevd.62.043004

Cited by 72 publications

(134 citation statements)

References 29 publications

(80 reference statements)

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“…The source functions for temperature and E-polarization perturbations are given in many previous studies [21,22].…”

Section: Photon Power Spectramentioning

confidence: 99%

“…We use synchronous gauge in this paper as it is convenient for most numerical computations. The full cosmological evolution equations in this gauge are given in a number of papers [1,21], and therefore we only explicitly show the equations that need modification. In particular, using the Boltzmann equation in this gauge we find the evolution equations for the temperature perturbation, Θ I , and E-polarization, Θ E , hierarchies arė…”

Section: Cosmological Equationsmentioning

confidence: 99%

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Effects of Rayleigh scattering on the CMB and cosmic structure

2015

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During and after recombination, in addition to Thomson scattering with free electrons, photons also coupled to neutral hydrogen and helium atoms through Rayleigh scattering. This coupling influences both CMB anisotropies and the distribution of matter in the Universe. The frequencydependence of the Rayleigh cross section breaks the thermal nature of CMB temperature and polarization anisotropies and effectively doubles the number of variables needed to describe CMB intensity and polarization statistics, while the additional atomic coupling changes the matter distribution and the lensing of the CMB. We introduce a new method to capture the effects of Rayleigh scattering on cosmological power spectra. Rayleigh scattering modifies CMB temperature and polarization anisotropies at the ∼ 1% level at 353GHz (scaling ∝ ν 4 ), and modifies matter correlations by as much as ∼ 0.3%. We show the Rayleigh signal, especially the cross-spectra between the thermal (Rayleigh) E-polarization and Rayleigh (thermal) intensity signal, may be detectable with future CMB missions even in the presence of foregrounds, and how this new information might help to better constrain the cosmological parameters.

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“…The source functions for temperature and E-polarization perturbations are given in many previous studies [21,22].…”

Section: Photon Power Spectramentioning

confidence: 99%

Section: Cosmological Equationsmentioning

confidence: 99%

Effects of Rayleigh scattering on the CMB and cosmic structure

2015

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“…If we use Eqs. (27) and (28) to express the spin-weight harmonics in terms of Legendre functions, we find the following expression for b G (l2) :…”

Section: Axisymmetric Beamsmentioning

confidence: 99%

All-sky convolution for polarimetry experiments

Challinor¹,

Fosalba

Mortlock

et al. 2000

Phys. Rev. D

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We discuss all-sky convolution of the instrument beam with the sky signal in polarimetry experiments, such as the Planck mission which will map the temperature anisotropy and polarization of the cosmic microwave background (CMB). To account properly for stray light (from e.g. the galaxy, sun, and planets) in the far side-lobes of such an experiment, it is necessary to perform the beam convolution over the full sky. We discuss this process in multipole space for an arbitrary beam response, fully including the effects of beam asymmetry and cross-polarization. The form of the convolution in multipole space is such that the Wandelt-Górski fast technique for all-sky convolution of scalar signals (e.g. temperature) can be applied with little modification. We further show that for the special case of a pure co-polarized, axisymmetric beam the effect of the convolution can be described by spin-weighted window functions. In the limits of a small angle beam and large Legendre multipoles, the spin-weight 2 window function for the linear polarization reduces to the usual scalar window function used in previous analyses of beam effects in CMB polarimetry experiments. While we focus on the example of polarimetry experiments in the context of CMB studies, we emphasise that the formalism we develop is applicable to anisotropic filtering of arbitrary tensor fields on the sphere. 98.70.Vc,

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“…We hope that the generalization of our methods to polarized map-making will be useful for making maps of the polarized microwave sky. It has already been shown [22] that little modification to the WandeltGórski method of fast all-sky convolution is needed to accomodate polarization data.…”

Section: Discussionmentioning

confidence: 99%

Deconvolution map-making for cosmic microwave background observations

Armitage

Wandelt

2004

Phys. Rev. D

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We describe a new map-making code for cosmic microwave background (CMB) observations. It implements fast algorithms for convolution and transpose convolution of two functions on the sphere (Wandelt & Górski 2001) [1]. Our code can account for arbitrary beam asymmetries and can be applied to any scanning strategy. We demonstrate the method using simulated time-ordered data for three beam models and two scanning patterns, including a coarsened version of the WMAP strategy. We quantitatively compare our results with a standard map-making method and demonstrate that the true sky is recovered with high accuracy using deconvolution map-making.

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Microwave background polarization in cosmological models

Cited by 72 publications

References 29 publications

Effects of Rayleigh scattering on the CMB and cosmic structure

Effects of Rayleigh scattering on the CMB and cosmic structure

All-sky convolution for polarimetry experiments

Deconvolution map-making for cosmic microwave background observations

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