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An accelerating universe has $\ddot{a}>0$, equivalently $q<0$ while expansion continues.

Here $a$ is the scale factor and $q=-a\ddot{a}/{\dot{a}}^2$ the deceleration parameter. Accelerating expansion means $\dot{a}>0$ and $\ddot{a}>0$; the Hubble parameter $H=\dot{a}/a$ can still decrease. The observational challenge is to reconstruct that history from a past light cone, rather than watch a distant galaxy speed up over the observing campaign.

The cosmological principle assumes that the universe is statistically homogeneous and isotropic on sufficiently large spatial scales. It applies to a coarse-grained description, not to each galaxy or local void. Combined with the Copernican principle, cosmological isotropy around us supports a homogeneous description rather than a specially centred model. It motivates an FRW metric, whose expansion is governed by a few time-dependent quantities. Observations sample only a finite past light cone, so they support this hypothesis without proving global spatial homogeneity beyond the observed region.

Use units $c=1$, and let $r$ be the areal radial coordinate of the FRW metric, rather than the radial comoving distance when $k\ne 0$. On a constant-cosmic time slice the spatial metric tensor isThe determinant of the spatial metric tensor supplies the factor $(1-k{r}^2{)}^{-1/2}$. Integrating over the solid angle gives $d{V}_{\mathrm{shell}}=4\pi a^3{r}^2|dr|/\sqrt{1-k{r}^2}$. An incoming radial null geodesic obeysConsequently the proper shell volume sampled by an emission-time interval of positive width $dt$ is $4\pi a^2{r}^{2}dt$. Multiplying by the proper number density proves the source counts on an FLRW past light cone:Here $r(t)$ is evaluated on the observer's past light cone, not along a fixed source worldline. The curvature factor cancels between the spatial volume and the radial light speed; it has not been set to one.

The strongest evidence for large-scale cosmological isotropy is the nearly direction-independent blackbody temperature of the cosmic microwave background. After removing the dipole associated mainly with our peculiar velocity, its residual temperature fluctuations are of order $10^{-5}$. Nearly isotropic counts of distant radio sources and galaxies, after correcting for sky coverage and selection effects, provide independent evidence. Local galaxies, clusters and voids clearly are not isotropic structures; the claim concerns a statistical description on sufficiently large scales.

Large redshift surveys show that the mean galaxy density stabilizes as increasingly large volumes are sampled, and that the excess pair correlations weaken at large separations. This supports statistical homogeneity beyond the characteristic clustering scales. The consistency of large-scale observations in different directions and the success of a common FRW metric description are additional checks.

Isotropy around one observer does not alone prove spatial homogeneity: a radially varying distribution centered on that observer could look isotropic. The Copernican principle supplies the assumption that we occupy no preferred position; comparable isotropy about typical locations then supports the cosmological principle. Surveys observe a finite past light cone, with source evolution and selection, so they cannot establish homogeneity everywhere on a simultaneous spatial slice. The evidence supports large-scale statistical isotropy and homogeneity, with substantial small-scale structure and an explicit typical-observer assumption.

The cosmological principle assumes statistical spatial homogeneity and cosmological isotropy on sufficiently large scales. Spatial homogeneity means that coarse-grained statistical properties do not depend on location; cosmological isotropy means that they do not depend on direction. The claim concerns a large-scale description, allowing individual galaxies, clusters and voids. It motivates the FRW metric and makes cosmic expansion describable by a single scale factor and a small number of matter variables.

Its adoption combines empirical large-scale regularity with the Copernican principle, the assumption that our location is typical. The resulting models provide a coherent account of cosmic expansion, the cosmic microwave background and primordial abundances. Neither the Einstein field equations alone nor cosmological isotropy around just one observer proves global spatial homogeneity: a spherically symmetric universe specially centred on that observer would also look isotropic. Observations of a finite past light cone support the principle over sampled scales without establishing it beyond the observed region.

Three supporting observations probe complementary aspects. First, after the observer-motion dipole and local foregrounds are removed, the cosmic microwave background is extremely isotropic, with intrinsic temperature fluctuations of order $10^{-5}$ and a nearly identical thermal spectrum across the sky. Second, suitably corrected all-sky counts of distant radio sources and extragalactic background intensities show no large preferred direction; Galactic obscuration and survey selection must be accounted for. Third, three-dimensional galaxy redshift surveys show that clustering and voids average toward statistically similar distributions in sufficiently large regions: large-volume number counts approach volume scaling and correlations weaken on large separation scales. The first two primarily test cosmological isotropy, while the third adds evidence for large-scale spatial homogeneity. The principle is a well-supported large-scale working hypothesis whose observational and typicality assumptions remain explicit.

Write the electromagnetic field tensor as $F^{\mu \nu }={\partial }^{\mu }{A}^{\nu }-{\partial }^{\nu }{A}^{\mu }$. Substitution into the Covariant Maxwell equation with the minus-plus-plus-plus metric givesChoose the Lorenz gauge ${\partial }_{\mu }{A}^{\mu }=0$. Since ${\partial }_{\mu }{\partial }^{\mu }={\nabla }^2-c^{-2}{\partial }_t^2$, the electromagnetic four-potential obeysConvolution with the outgoing retarded Green function gives the retarded electromagnetic potential

For the point particle, ${\tau }_{\ast }(x)$ is its unique retarded proper time, characterized byThus $y({\tau }_{\ast })$ is where the particle's worldline intersects the past light cone of the observation event $x$; the displayed expression is the covariant form of the Lienard-Wiechert potentials.

On the $z$-axis put $D=\sqrt{R^2+z^2}$. The retarded time is $t_{\ast }=t-D/c$. For the circular orbit, the spatial velocity at that time isBecause the displacement from the retarded source point to the observation point is orthogonal to this velocity, $|R^{\nu }{\dot{y}}_{\nu }|=\gamma cD$, while ${\dot{y}}^{\mu }=\gamma (c,\mathbf{v})$. The factors of $\gamma$ cancel, leaving

The past light cone of a spacetime event $O$ is the past-directed part of its light cone. In Minkowski spacetime, its spacetime events satisfy $|\Delta \mathbf{x}|=-c\Delta t$ with $\Delta t<0$. They are the possible emission events of light rays arriving at $O$. The interior also contains events that can send slower signals to $O$. The retarded potential of a moving point electric charge, given by the Liénard–Wiechert potential, uses the emission event where the source's world line intersects this boundary.

For proper number density $n(t)$ in an FLRW metric $d{s}^2=d{t}^2-a^2[d{r}^2/(1-k{r}^2)+r^{2}d{\Omega }^2]$, a radial shell has proper volume $4\pi a^3{r}^2|dr|/\sqrt{1-k{r}^2}$. A radial null geodesic obeys $|dr|=\sqrt{1-k{r}^2}dt/a$. Multiplication gives the displayed shell count on a local radial branch of the past light cone. Spatially uniform number density need not be time independent or have conserved comoving number density.