【摘 要】
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With large-scale homogeneity, the universe is locally inhomogeneous, clus-tering into stars, galaxies and larger structures. Such property is described by the s
【机 构】
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Department of Astronomy,Business Office, Center for High Energy Physics,Department of Physics
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With large-scale homogeneity, the universe is locally inhomogeneous, clus-tering into stars, galaxies and larger structures. Such property is described by the smoothness parameter a which is defined as the proportion of matter in the form of intergalactic medium. If we consider the inhomogeneities over a small scale, there should be modifications of the cosmological distances compared to a homogenous model. Dyer and Roeder developed a second-order ordinary differential equation (D-R equation) that describes the angular diameter distance-redshift relation for inhomogeneous cosmological models. Furthermore, we may obtain the D-R equation for observational H(z) data (OHD). The density-parameter ΩM, the state of dark energy ω, and the smoothness-parameter a are constrained by a set of OHD in a spatially flat ACDM universe as well as a spatially flat XCDM universe. By using a x2 mini-mization method, we get a = 0.81+0.19-0.20 and ΩM = 0.32+0.12-0.06 at the confidence level. If we assume a Gaussian prior of ΩM = 0.26 0.1, we get a - 0.93+0.07-0.19 and ΩM=0.31+0.06-0.05.For the XCDM model, a is constrained to a (≧) 0.80 but w is weakly constrained around - 1, where w describes the equation of state of the dark en-ergy (Px = ωpx). We conclude that OHD constrains the smoothness parameter more effectively than the data of Sne Ia and compact radio sources.
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