First Season QUaD CMB Temperature and Polarization Power Spectra

Ade, Peter A. R.; Bock, J. J.; Bowden, M.; Brown, Michael L.; Cahill, G.; Carlstrom, J. E.; Castro, Paulo Francisco de; Church, S.; Culverhouse, T.; Friedman, Robert; Ganga, K.; Gear, Walter Kieran; Hinderks, J.; Kovac, J. M.; Lange, A. E.; Leitch, E. M.; Melhuish, S. J.; Murphy, John A.; Orlando, A.; Schwarz, R.; O’Sullivan, C.; Piccirillo, L.; Pryke, C.; Rajguru, N.; Rusholme, B.; Taylor, Abigail Helen; Thompson, K. L.; Wu, Emily; Zemcov, Michael

doi:10.1086/524922

Cited by 62 publications

(60 citation statements)

References 25 publications

(18 reference statements)

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“…It has already led to spectacular results concerning the cosmological model (Kovac et al 2002;Readhead et al 2004;Nolta et al 2009;Ade et al 2008) describing our Universe. Even more challenging is the detection of the so-called B-modes in the CMB polarization, associated with pure tensor modes originating from primordial gravitational waves enhanced by inflation.…”

Section: Introductionmentioning

confidence: 99%

An efficient phase-shifting scheme for bolometric additive interferometry

Charlassier¹,

Hamilton²,

Bréelle³

et al. 2009

A&A

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Context. Most upcoming CMB polarization experiments will use direct imaging to search for primordial gravitational waves through the B-modes. Bolometric interferometry is an appealing alternative to direct imaging that combines the advantages of interferometry in terms of systematic effects handling and those of bolometric detectors in terms of sensitivity. Aims. We calculate the signal from a bolometric interferometer in order to investigate its sensitivity to the Stokes parameters paying particular attention to the choice of the phase shifting scheme applied to the input channels in order to modulate the signal. Methods. The signal is expressed as a linear combination of the Stokes parameter visibilities whose coefficients are functions of the phase shifts. Results. We show that the signal to noise ratio on the reconstructed visibilities can be maximized provided the fact that the phase shifting scheme is chosen in a particular way called "coherent summation of equivalent baselines". As a result, a bolometric interferometer is competitive with an imager having the same number of horns, but only if the coherent summation of equivalent baselines is performed. We confirm our calculations using a Monte-Carlo simulation. We also discuss the impact of the uncertainties on the relative calibration between bolometers and propose a way to avoid this systematic effect.

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Section: Introductionmentioning

confidence: 99%

An efficient phase-shifting scheme for bolometric additive interferometry

Charlassier¹,

Hamilton²,

Bréelle³

et al. 2009

A&A

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“…Over the past years, CMB polarization has been measured by several experiments and is being measured by the Planck surveyor Leitch et al 2002;Pryke et al 2002a,b Halverson et al 2002Leitch et al 2005;Ade & et al 2008;Pryke & et al 2009;Hinderks et al 2009;Brown & et al 2009;The Planck Collaboration 2006). CMB polarization pattern may be considered as the sum of gradient-like E mode and curllike B mode (Zaldarriaga & Seljak 1997;Kamionkowski et al 1997).…”

Section: Introductionmentioning

confidence: 99%

E/B decomposition of CMB polarization pattern of incomplete sky: a pixel space approach

Kim¹,

Naselsky²

2010

A&A

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CMB polarization pattern may be decomposed into gradient-like (E) and curl-like (B) mode, which provide invaluable information respectively. We have investigated E/B decomposition in pixel space. We find E/B mixing due to incomplete sky is localized in pixel-space, and negligible in the regions far away from the masked area. By estimating the expected local leakage power, we have diagnosed ambiguous pixels. Our criteria for ambiguous pixels (i.e. r c ) is associated with the tensor-to-scalar ratio of B mode power spectrum, which the leakage power is comparable to. By setting r c to a lower value, we may reduce leakage level, but reduce sky fraction at the same time. Therefore, we have solved ∂ΔC l /∂r c = 0, and obtained the optimal r c , which minimizes the estimation uncertainty, given a foreground mask and noise level. We have applied our method to a simulated map blocked by a foreground (diffuse + point source) mask. Our simulation shows leakage power is smaller than primordial (i.e. unlensed) B mode power spectrum of tensor-to-scalar ratio r ∼ 1 × 10 −3 at wide range of multipoles (50 l 2000), while allowing us to retain sky fraction ∼0.48.

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“…Adding the statistical and systematic errors in quadrature and averaging over Wilkinson Microwave Anisotropy Probe (WMAP; Komatsu et al 2010), QUaD (Ade et al 2008), and BICEP (Chiang et al 2010; see Komatsu et al 2010 for more details) with inverse variance weighting, the limits obtained were α = −0.…”

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confidence: 99%

Constraining Primordial Magnetic Fields Through Large-Scale Structure

Kahniashvili

Maravin

Natarajan

et al. 2013

ApJ

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We study primordial magnetic field effects on the matter perturbations in the universe. We assume magnetic field generation prior to the big bang nucleosynthesis (BBN), i.e., during the radiation-dominated epoch of the universe expansion, but do not limit analysis by considering a particular magnetogenesis scenario. Contrary to previous studies, we limit the total magnetic field energy density and not the smoothed amplitude of the magnetic field at large (of the order of 1 Mpc) scales. We review several cosmological signatures, such as halo abundance, thermal Sunyaev-Zel'dovich effect, and Lyα data. For a cross-check, we compare our limits with that obtained through the cosmic microwave background faraday rotation effect and BBN. The limits range between 1.5 nG and 4.5 nG for n B ∈ (−3; −1.5).

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First Season QUaD CMB Temperature and Polarization Power Spectra

Cited by 62 publications

References 25 publications

An efficient phase-shifting scheme for bolometric additive interferometry

An efficient phase-shifting scheme for bolometric additive interferometry

E/B decomposition of CMB polarization pattern of incomplete sky: a pixel space approach

Constraining Primordial Magnetic Fields Through Large-Scale Structure

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