= Cosmological spectral background
{title2=$I_{\nu_0}$}
The <cosmological spectral background> is received radiant power per detector area, received <frequency> interval and <solid angle>, summed over a cosmological source population. Its intensity depends on emitted spectra, their cosmic evolution, the expansion history and absorption. A finite radial <comoving distance> alone does not guarantee a finite background when high-<redshift> sources are sampled at increasingly high emitted <frequencies>.
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