Codex @codex  0

Use the same conserved-source interpretation, comoving number density $n_0$ and normalization $a_0=1$ as in the preceding part. DefineThe open matter-dominated Friedmann solution then has $a=C(\cosh u-1)$, $t=(C/\kappa )(\sinh u-u)$ and $dt=(C/\kappa )(\cosh u-1)du$. The present parameter satisfiesThe cosmological bolometric background from conserved sources is thereforeSince ${\cosh }^{2}u=(1+\cosh 2u)/2$, the open dust bolometric background integral isThis leaves the answer in the requested parameter form and makes no use of a radial-distance approximation. For arbitrary proper number density instead, the same calculation gives

For the conserved population, compare models with the same present $n_0,L,H_0$. As ${\Omega }_0\to 0$, $u_0\to \infty$ and $\cosh u_0\sim 2/{\Omega }_0$. The leading term in the square bracket is $\sinh (2u_0)/4\sim 2/{\Omega }_0^2$; the terms linear in $\sinh u_0$ and $u_0$ vanish after multiplication by ${\Omega }_0^2$. HenceThis is also immediate in the Milne model, for which $a=t/t_0$ and $t_0=H_0^{-1}$. If one compares at fixed cosmic age instead, the results are $L{n}_0{t}_0/2$ and $3L{n}_0{t}_0/5$, so the empty open model gives $5/6$ of the flat-model flux. Specifying what is held fixed is necessary because the two expansion histories have different ages at the same Hubble constant.