Large-scale polarization of the cosmic microwave background radiation

Ng, Ka Lok; Ng, Kin-Wang

doi:10.1103/physrevd.51.364

Cited by 21 publications

(21 citation statements)

References 24 publications

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“…The polarization power spectrum, C Π ℓ , is highly dependent on the cosmological details of the model used to generate the anisotropy spectrum, C α ℓ . For this reason, the ratio of polarization to anisotropy is often calculated in order to predict observable levels of polarization for particular observations (Ng & Ng 1995;Crittenden, Davis, & Steinhardt 1993). In practice, the polarization spectra are normalized to the appropriate anisotropy spectra, which are in turn normalized to the low ℓ values of C α ℓ measured by the COBE DMR.…”

Section: Polarization Power Spectrummentioning

confidence: 99%

Large Angular Scale Polarization of the Cosmic Microwave Background Radiation and the Feasibility of Its Detection

Keating

Timbie

Polnarev

et al. 1998

ApJ

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In addition to its spectrum and temperature anisotropy, the 2.7 K Cosmic Microwave Background (CMB) is also expected to exhibit a low level of polarization. The spatial power spectrum of the polarization can provide details about the formation of structure in the universe as well as its ionization history. Here we calculate the magnitude of the CMB polarization in various cosmological scenarios, with both an analytic and a numerical method. We then outline the fundamental challenges to measuring these signals and focus on two of them: achieving adequate sensitivity and removing contamination from foreground sources. We describe the design of a ground-based instrument (POLAR) that could detect polarization of the CMB at large angular scales in the next few years.

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Section: Polarization Power Spectrummentioning

confidence: 99%

Large Angular Scale Polarization of the Cosmic Microwave Background Radiation and the Feasibility of Its Detection

Keating

Timbie

Polnarev

et al. 1998

ApJ

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“…The first computations were performed in homogeneous but anisotropically expanding universes [2,[4][5][6][7][8]. Energy-density fluctuations [9][10][11][12][13][14][15] and long wavelength gravitational waves [16,17,12,13,18] were also considered as the source of the anisotropy that leads to polarization. Typically, at least within standard recombination histories, the degree of linear polarization turns out to be almost two orders of magnitude smaller than the large scale temperature anisotropy.…”

Section: Introductionmentioning

confidence: 99%

Analytic approach to the polarization of the cosmic microwave background in flat and open universes

1995

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We develop an analytic method and approximations to compute the polarization induced in the cosmic microwave background radiation on a wide range of angular scales by anisotropic Thomson scattering in the presence of adiabatic scalar (energy-density) linear fluctuations. The formalism is an extension to the polarized case of the analytic approach recently developed by Hu and Sugiyama to evaluate the (unpolarized) temperature correlation function. The analytic approach helps to highlight the dependence of potentially measurable polarization properties of the cosmic microwave background radiation upon various parameters of the cosmological model. We show, for instance, that the ratio between the multipoles of the temperature and polarization correlation functions depends very sensitively upon the value of Ro, the matter density in units of the critical, in an open universe.PACS number(s): 98.70.Vc, 98.80.E~

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“…Another possibility is that one may distinguish the scalar and tensor contributions to the multipole moments by examining the polarization of the CBR. This has been examined by Harari and Zaldarriaga [40], by Crittenden, Davis and Steinhardt [39], and by Ng and Ng [41].…”

Section: Introductionmentioning

confidence: 99%

CBR anisotropy from primordial gravitational waves in inflationary cosmologies

Allen

Koranda

1994

Phys. Rev. D

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We examine stochastic temperature fluctuations of the cosmic background radiation (CBR) arising via the Sachs-Wolfe effect from gravitational wave perturbations produced in the early Universe. These temperature fluctuations are described by an angular correlation function C(γ). A new (more concise and general) derivation of C(γ) is given, and evaluated for inflationary-universe cosmologies. This yields standard results for angles γ greater than a few degrees, but new results for smaller angles, because we do not make standard long-wavelength approximations to the gravitational wave mode functions. The function C(γ) may be expanded in a series of Legendre polynomials; we use numerical methods to compare the coefficients of the resulting expansion in our exact calculation with standard (approximate) results. We also report some progress towards finding a closed form expression for C(γ)

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Large-scale polarization of the cosmic microwave background radiation

Cited by 21 publications

References 24 publications

Large Angular Scale Polarization of the Cosmic Microwave Background Radiation and the Feasibility of Its Detection

Large Angular Scale Polarization of the Cosmic Microwave Background Radiation and the Feasibility of Its Detection

Analytic approach to the polarization of the cosmic microwave background in flat and open universes

CBR anisotropy from primordial gravitational waves in inflationary cosmologies

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