TY - JOUR
T1 - First year Wilkinson micro wave anisotropy probe observations
T2 - Dark energy induced correlation with radio sources
AU - Nolta, M. R.
AU - Wright, E. L.
AU - Page, L.
AU - Bennett, C. L.
AU - Halpern, M.
AU - Hinshaw, G.
AU - Jarosik, N.
AU - Kogut, A.
AU - Limon, M.
AU - Meyer, S. S.
AU - Spergel, D. N.
AU - Tucker, G. S.
AU - Wollack, E.
PY - 2004/6/10
Y1 - 2004/6/10
N2 - The first-year Wilkinson Microwave Anisotropy Probe (WMAP) data, in combination with any one of a number of other cosmic probes, show that we live in a flat Λ-dominated cold dark matter (CDM) universe with Ωm ≈ 0.27 and ΩΛ ≈ 0.73. In this model the late-time action of the dark energy, through the integrated Sachs-Wolfe effect, should produce cosmic microwave background (CMB) anisotropies correlated with matter density fluctuations at z ≲ 2 (Crittenden & Turok 1996). The measurement of such a signal is an important independent check of the model. We cross-correlate the NRAO VLA Sky Survey (NVSS) radio source catalog (Condon et al. 1998) with the WMAP data in search of this signal, and see indications of the expected correlation. Assuming a flat ACDM cosmology, we find ΩΛ > 0 (95% CL, statistical errors only) with the peak of the likelihood at ΩΛ = 0.68, consistent with the preferred WMAP value. A closed model with Ωm = 1.28, h = 0.33, and no dark energy component (ΩΛ = 0), marginally consistent with the WMAP CMB TT angular power spectrum, would produce an anticorrelation between the matter distribution and the CMB. Our analysis of the cross-correlation of the WMAP data with the NVSS catalog rejects this cosmology at the 3 σ level.
AB - The first-year Wilkinson Microwave Anisotropy Probe (WMAP) data, in combination with any one of a number of other cosmic probes, show that we live in a flat Λ-dominated cold dark matter (CDM) universe with Ωm ≈ 0.27 and ΩΛ ≈ 0.73. In this model the late-time action of the dark energy, through the integrated Sachs-Wolfe effect, should produce cosmic microwave background (CMB) anisotropies correlated with matter density fluctuations at z ≲ 2 (Crittenden & Turok 1996). The measurement of such a signal is an important independent check of the model. We cross-correlate the NRAO VLA Sky Survey (NVSS) radio source catalog (Condon et al. 1998) with the WMAP data in search of this signal, and see indications of the expected correlation. Assuming a flat ACDM cosmology, we find ΩΛ > 0 (95% CL, statistical errors only) with the peak of the likelihood at ΩΛ = 0.68, consistent with the preferred WMAP value. A closed model with Ωm = 1.28, h = 0.33, and no dark energy component (ΩΛ = 0), marginally consistent with the WMAP CMB TT angular power spectrum, would produce an anticorrelation between the matter distribution and the CMB. Our analysis of the cross-correlation of the WMAP data with the NVSS catalog rejects this cosmology at the 3 σ level.
KW - Cosmic microwave background
KW - Cosmology: observations
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U2 - 10.1086/386536
DO - 10.1086/386536
M3 - Article
AN - SCOPUS:3142781525
SN - 0004-637X
VL - 608
SP - 10
EP - 15
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1 I
ER -