M. R. Nolta et al. 2009 ApJS 180 296 doi:10.1088/0067-0049/180/2/296
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
Show affiliationsWe 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 ℓ/(2π) < 0.15 μK2 (95% CL).
cosmic microwave background; cosmological parameters; cosmology: observations; early universe; large-scale structure of universe; space vehicles: instruments
Issue 2 (2009 February)
Received 2008 March 4, accepted for publication 2008 June 20
Published 2009 February 11
M. R. Nolta et al. 2009 ApJS 180 296
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G S Hall 2003 Class. Quantum Grav. 20 4067
Jens Bolte and Jonathan Harrison 2003 J. Phys. A: Math. Gen. 36 2747
Raffaele Rani et al 2003 Class. Quantum Grav. 20 1929
E. L. Wright et al. 2009 ApJS 180 283
E Minguzzi 2003 Class. Quantum Grav. 20 2443
Markus J Buehler et al 2004 Modelling Simul. Mater. Sci. Eng. 12 S391
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