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FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE * OBSERVATIONS: ANGULAR POWER SPECTRA

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M. R. Nolta1, J. Dunkley2,3,4, R. S. Hill5, G. Hinshaw6, E. Komatsu7, D. Larson8, L. Page3, D. N. Spergel2,9, C. L. Bennett8, B. Gold8, N. Jarosik3, N. Odegard5, J. L. Weiland5, E. Wollack6, M. Halpern10, A. Kogut6, M. Limon11, S. S. Meyer12, G. S. Tucker13 and E. L. Wright14

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We present the temperature and polarization angular power spectra of the cosmic microwave background derived from the first five years of Wilkinson Microwave Anisotropy Probe data. The five-year temperature spectrum is cosmic variance limited up to multipole ℓ = 530, and individual ℓ-modes have signal-to-noise ratio S/N >1 for ℓ < 920. The best-fitting six-parameter ΛCDM model has a reduced χ2 for ℓ = 33-1000 of χ2/ν = 1.06, with a probability to exceed of 9.3%. There is now significantly improved data near the third peak which leads to improved cosmological constraints. The temperature-polarization correlation is seen with high significance. After accounting for foreground emission, the low-ℓ reionization feature in the EE power spectrum is preferred by Δχ2 = 19.6 for optical depth τ = 0.089 by the EE data alone, and is now largely cosmic variance limited for ℓ = 2-6. There is no evidence for cosmic signal in the BB, TB, or EB spectra after accounting for foreground emission. We find that, when averaged over ℓ = 2-6, ℓ(ℓ + 1)C BB /(2π) < 0.15 μK2 (95% CL).


Footnote
WMAP is the result of a partnership between Princeton University and NASA's Goddard Space Flight Center. Scientific guidance is provided by the WMAP Science Team.
Keywords

cosmic microwave background; cosmological parameters; cosmology: observations; early universe; large-scale structure of universe; space vehicles: instruments


Dates

Issue 2 (2009 February)

Received 2008 March 4, accepted for publication 2008 June 20

Published 2009 February 11



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