Correlations between the<i>Wilkinson Microwave Anisotropy Probe</i>and MAXIMA Cosmic Microwave Background Anisotropy Maps

Abroe, M. E.; Borrill, J.; Ferreira, Pedro G.; Hanany, Shaul; Jaffe, A. H.; Johnson, B. R.; Lee, A. T.; Rabii, B.; Richards, P. L.; Smoot, George F.; Stompor, R.; Winant, C. D.; Wu, Jiun-Huei Proty

doi:10.1086/382348

Cited by 17 publications

(16 citation statements)

References 31 publications

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“…In other words, we hope that even for the elusive CMB B-modes we will finally arrive to the same situation we have now with CMB anisotropy, where directly comparable anisotropy maps have been detected by bolometric experiments (BOOMERanG, MAXIMA, Archeops) and by radiometers (DASI, WMAP) (de Bernardis et al 2004;Abroe et al 2004;Hamilton et al 2004;Wright 2002;Bennett et al 2004).…”

Section: The Brain Instrumentsupporting

confidence: 56%

Precision CMB Polarization from Dome-C: the BRAIN experiment

Masi

Bernardis

Giordano

et al. 2005

EAS Publications Series

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Abstract. In the current cosmological scenario, part of the linearly polarized emission of the CMB is expected to be rotational (B-modes). This component is due to tensor perturbations of the metric produced by primordial gravitational waves, which are generated a split-second after the Big Bang. The signal expected is of the order of < ∼ 0.1 µK, well below the non-rotational component of the polarization signal (E-modes), and beyond the sensitivity of present generation instruments. New, more sensitive instruments are developed in several labs, with the goal to measure the B-modes. Control of systematics and foregrounds will be the key to make the results of these experiments believable. In this paper we shortly outline BRAIN, a bolometric interferometer devoted to B-modes research, and its pathfinder experiment, devoted to test the Dome-C site.

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Section: The Brain Instrumentsupporting

confidence: 56%

Precision CMB Polarization from Dome-C: the BRAIN experiment

Masi

Bernardis

Giordano

et al. 2005

EAS Publications Series

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“…We quantify the correlation by calculating the cross-spectrum between the two data sets. This idea has already been succesfully applied to temperature anisotropy data sets (Abroe et al 2004;Tristram et al 2005b). For dust intensity we use the FDS template, based on IRAS 100 µm maps and extrapolated to 353 GHz ("model number 8") (Finkbeiner et al 1999).…”

Section: Fds-archeops Correlationmentioning

confidence: 99%

Temperature and polarization angular power spectra of Galactic dust radiation at 353 GHz as measured by Archeops

Ponthieu¹,

Macías-Pérez²,

Tristram³

et al. 2005

A&A

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We present the first measurement of temperature and polarization angular power spectra of the diffuse emission of Galactic dust at 353 GHz as seen by Archeops on 20% of the sky. The temperature angular power spectrum is compatible with that provided by the extrapolation to 353 GHz of IRAS and DIRBE maps using Finkbeiner et al. (1999, ApJ, 524, 867) model number 8. For Galactic latitudes |b| ≥ 5 deg we report a 4 sigma detection of large scale (3 ≤ ≤ 8) temperature-polarization cross-correlation ( + 1)C T E /2π = 76 ± 21 µK 2 RJ and set upper limits to the E and B mode polarization at 11 µK 2 RJ . For Galactic latitudes |b| ≥ 10 deg, on the same angular scales, we report a 2 sigma detection of temperature-polarization cross-correlation ( + 1)C T E /2π = 24 ± 13 µK 2 RJ . These results are then extrapolated to 100 GHz to estimate the contamination in CMB measurements by polarized diffuse Galactic dust emission. The T E signal is then 1.7 ± 0.5 and 0.5 ± 0.3 µK 2 CMB for |b| ≥ 5 and 10 deg respectively. The upper limit on E and B mode polarization becomes 0.2 µK 2 CMB (2σ). If the physical properties of dust radiation on the fraction of the sky observed by Archeops are representative of the whole sky, and if the actual level of E and B mode polarization is close to this upper limit, then dust polarized radiation will be a major foreground for determining the polarization power spectra of the CMB at high frequencies above 100 GHz.

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“…The primary CMB anisotropies are due to the gravitational redshift at large angular scales (Sachs & Wolfe 1967) and to the evolution of the primordial photon-baryon fluid evolution under gravity and Compton scattering at lower scales (Silk 1967 (Ruhl et al 2003, Abroe et al 2004, Kuo et al 2004, Readhead et al 2004, Dickinson et al 2004). The red, dark orange and light orange lines represent the predictions from the ΛCDM model fit to the WMAP data for the best fit, the 68% and 95% confidence levels respectively.…”

Section: Introductionmentioning

confidence: 99%

Secondary anisotropies of the CMB

Aghanim¹,

Majumdar²,

Silk³

2008

Rep. Prog. Phys.

101

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Abstract.The Cosmic Microwave Background fluctuations provide a powerful probe of the dark ages of the universe through the imprint of the secondary anisotropies associated with the reionisation of the universe and the growth of structure. We review the relation between the secondary anisotropies and and the primary anisotropies that are directly generated by quantum fluctuations in the very early universe. The physics of secondary fluctuations is described, with emphasis on the ionisation history and the evolution of structure. We discuss the different signatures arising from the secondary effects in terms of their induced temperature fluctuations, polarisation and statistics. The secondary anisotropies are being actively pursued at present, and we review the future and current observational status.

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Correlations between theWilkinson Microwave Anisotropy Probeand MAXIMA Cosmic Microwave Background Anisotropy Maps

Cited by 17 publications

References 31 publications

Precision CMB Polarization from Dome-C: the BRAIN experiment

Precision CMB Polarization from Dome-C: the BRAIN experiment

Temperature and polarization angular power spectra of Galactic dust radiation at 353 GHz as measured by Archeops

Secondary anisotropies of the CMB

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