부산대학교 도서관

Properly interpreted data from nearby galaxies $(z\simeq 0.01)$ lead to $\Omega \simeq 0.082$. Data from farther away galaxies $(z\simeq 1)$ with type Ia supernovae to $\Omega =0.153$. Data to be expected from very high redshifted galaxies $(z\simeq 10.1)$ to $\Omega =0.500$. And actual data from the CBR, emitted at the time at which the universe became transparent $(z\simeq 1422)$ to $\Omega \simeq 0.992$. All these data are simultaneously consistent with the standard big-bang picture (no inflation), in which $ \Omega $ is time dependent and it is given by $\Omega (y)=1/\cosh ^{2}(y)$, being $y\equiv \sinh ^{-1}(T_{+}/T)^{1/2}$
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