TY - JOUR
T1 - Five-year wilkinson microwave anisotropy probe observations
T2 - Angular power spectra
AU - Nolta, M. R.
AU - Dunkley, J.
AU - Hill, R. S.
AU - Hinshaw, G.
AU - Komatsu, E.
AU - Larson, D.
AU - Page, L.
AU - Spergel, D. N.
AU - Bennett, C. L.
AU - Gold, B.
AU - Jarosik, N.
AU - Odegard, N.
AU - Weiland, J. L.
AU - Wollack, E.
AU - Halpern, M.
AU - Kogut, A.
AU - Limon, M.
AU - Meyer, S. S.
AU - Tucker, G. S.
AU - Wright, E. L.
PY - 2009
Y1 - 2009
N2 - 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 ACDM model has a reduced χ2 for ℓ = 33-1000 of χ2/ = 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)CBBℓ/(2π) < 0.15 μK2 (95% CL).
AB - 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 ACDM model has a reduced χ2 for ℓ = 33-1000 of χ2/ = 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)CBBℓ/(2π) < 0.15 μK2 (95% CL).
KW - Cosmic microwave background
KW - Cosmological parameters
KW - Cosmology: observations
KW - Early universe
KW - Large-scale structure of universe
KW - Space vehicles: instruments
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U2 - 10.1088/0067-0049/180/2/296
DO - 10.1088/0067-0049/180/2/296
M3 - Article
AN - SCOPUS:63249119477
SN - 0067-0049
VL - 180
SP - 296
EP - 305
JO - Astrophysical Journal, Supplement Series
JF - Astrophysical Journal, Supplement Series
IS - 2
ER -