For a radial null geodesic in the FRW metric, define . Two successive wave crests emitted and received at the same comoving positions obey
Subtracting and keeping the first order in the wave periods gives . Thus the cosmological time dilation and the cosmological redshift have the same factor:
Here the emitter and observer are comoving; an additional peculiar velocity would supply a separate kinematic redshift. The derivation uses the null geodesic propagation of the crests rather than interpreting a finite cosmological distance as an ordinary Doppler effect.
The luminosity distance is defined by , where is the bolometric luminosity and the received radiative flux. In the FRW metric a sphere through the observer around a comoving source has area . The cosmological redshift reduces each photon's energy by , and cosmological time dilation reduces their arrival rate by another such factor. Hence
The positive radial lookback integral is . The printed time limits are reversed; also the factor is required unless units are adopted. The areal coordinate and the radial comoving distance agree only when .
For an Einstein-de Sitter universe, the Friedmann equation gives . Using the redshift-time relation in the radial null geodesic integral yields
Thus the Einstein-de Sitter luminosity-distance relation is
Its small-redshift expansion recovers Hubble's law.
A Type Ia supernova can be standardized as a standard candle by correcting its peak brightness using the light curve shape and colour index. Its host spectrum gives the redshift; the corrected apparent magnitude and calibrated absolute magnitude give the distance modulus
The resulting Hubble diagram measures the shape of the luminosity distance as a function of redshift. A spatially flat matter-and-vacuum model, for example, predicts
Nonzero cosmological spatial curvature changes both the expansion rate and the conversion from radial to transverse comoving distance. Comparing the observed Hubble diagram with these predictions constrains the matter density parameter, cosmological constant and cosmological spatial curvature; a single low-redshift observation cannot separate them. The nearby sample calibrates the common intercept, while distant Type Ia supernovae supply the redshift-dependent shape. Relative faintness at a specified redshift means a greater inferred luminosity distance.
Type Ia supernova cosmology requires correction for interstellar extinction, possible evolution of the standardized luminosity, and selection bias. The absolute magnitude–Hubble constant degeneracy means that an uncalibrated sample constrains the shape rather than independently determining .
Use the luminosity convention in the supplied flux relation: , where is the total spectral luminosity. For a general spectrum , the cosmological spectral flux-density relation gives
In a spatially flat universe, a shell subtending the solid angle contains sources, because is their comoving number density. The cosmological spectral background intensity per unit solid angle is consequently
This is the cosmological background intensity from comoving emissivity specialized to identical, nonevolving sources in an Einstein-de Sitter universe. For the integrand reduces to , or directly . The finite comoving particle horizon therefore gives
For , instead,
The emitted frequency grows with redshift, and the rising spectral luminosity now defeats the redshift dimming. The Einstein-de Sitter spectral-background convergence criterion is ; equality produces a logarithmic divergence. This divergence describes the unbounded power-law, eternal-population model. A finite formation epoch, a high-frequency spectral break or absorption changes that model and can make its background finite.

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