Introduction to microwave background polarization

Kosowsky, Arthur

doi:10.1016/s1387-6473(99)00009-3

Cited by 49 publications

(44 citation statements)

References 36 publications

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“…We then introduce the quantity C E;B = 0.5 · (C E + C B ), which will be used in the following best-fit analysis. On the contrary, the E and B modes of the primordial CMB anisotropies differ largely as they are induced by different mechanisms (e.g., Seljak & Zaldarriaga 1997;Kosowsky 1999). In the case of C TI , C synch e −(σ b ) 2 and c src e −(σ b ) 2 are also displayed.…”

Section: Selected Areas and Data Analysismentioning

confidence: 99%

An angular power spectrum analysis of the DRAO 1.4 GHz polarization survey: implications for CMB observations

Porta¹,

Burigana

Reich³

et al. 2006

A&A

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Aims. The aim of the present analysis is to improve the knowledge of the statistical properties of the Galactic diffuse synchrotron emission, which constrains sensitive CMB anisotropy measurements. Methods. We have analysed the new DRAO 1.4 GHz polarization survey together with the Stockert 1.4 GHz total intensity survey and derived the angular power spectra (APSs) of the total intensity, the polarized emission, and their cross-correlation for the entire surveys and for three low-intensity regions.Results. The APSs of the diffuse synchrotron emission are modelled by power laws. For the E and B modes, a slope of α ∼ [−3.0, −2.5] for the multipole range ∼[30, 300] is found. By the extrapolation of these results to 70 GHz, we can estimate the Galactic synchrotron contamination of CMB anisotropies, and we find results that are compatible with the ones coming from WMAP 3-yr data. In the low-intensity regions, the cosmological primordial B mode peak at ∼ 100 should be clearly observable for a tensor-to-scalar ratio T/S > ∼ 0.5 and a synchrotron temperature spectral index β ∼ −3. Its detection is also possible for T/S > ∼ 0.005 and β ∼ −3, in case a separation of the foreground from the CMB signal could be achieved with an accuracy of ∼5−10%. For the TE mode, a mask excluding |b gal | ≤ 5• (for β ∼ −3.0) or |b gal | ≤ 20• (for β ∼ −2.8) from the surveys is sufficient to render the foreground contamination negligible, thus confirming the ability of WMAP to have a clear view of the temperature-polarization correlation peak and antipeak series.

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Section: Selected Areas and Data Analysismentioning

confidence: 99%

An angular power spectrum analysis of the DRAO 1.4 GHz polarization survey: implications for CMB observations

Porta¹,

Burigana

Reich³

et al. 2006

A&A

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“…In addition, a linearly polarized component of the CMB arises from any quadrupolar variation in the photons scattered from electrons at the last scattering surface (Rees 1968;Hu & White 1997). Polarization data will complement other CMB data (e.g., Kosowsky 1999). Current cosmological models predict that polarization anisotropies are 10-20 times smaller than temperature anisotropies.…”

Section: Introductionmentioning

confidence: 99%

A Limit on the Polarized Anisotropy of the Cosmic Microwave Background at Subdegree Angular Scales

Hedman

Barkats

Gundersen

et al. 2001

The Astrophysical Journal

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A ground-based polarimeter, PIQUE, operating at 90 GHz has set a new limit on the magnitude of any polarized anisotropy in the cosmic microwave background. The combination of the scan strategy and full width halfmaximum beam of 0Њ .24 gives broad window functions with and for the E-and ϩ294 ϩ229Al S p 211 Al S p 212B-mode window functions, respectively. A joint likelihood analysis yields simultaneous 95% confidence level flat band power limits of 14 and 13 mK on the amplitudes of the E-and B-mode angular power spectra, respectively. Assuming no B-modes, a 95% confidence limit of 10 mK is placed on the amplitude of the E-mode angular power spectrum alone.

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“…The CMB radiation can be polarized due to the gravitational waves called the B-mode of CMB [43][44][45]. The angular power spectrum of the B-mode of CMB is given by [46,47] …”

Section: Bb-mode Angular Power Spectrum Of Cmbmentioning

confidence: 99%