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The 46 pages that link to Cosmological principle, each with the reason it gives.

• Dark matterRelated: It underlies cosmological models that infer dark matter from the universe’s expansion and structure.

• Cosmic inflationRelated: Inflation offers a possible physical account of the large-scale uniformity this principle describes.

• Big BangRelated: It lets cosmological models describe the universe with large-scale averages rather than individual galaxies.

• Cosmological redshiftRelated: It underlies the uniform expansion model used to interpret cosmological redshift.

• CosmologyRelated: It makes the universe-wide models described by cosmology mathematically tractable.

• Friedmann equationsRelated: It motivates the symmetries that reduce Einstein’s equations to this pair.

• Peculiar velocityRelated: It motivates treating large-scale expansion as a smooth background rather than individual motion.

• Observable universeRelated: It lets observations from our location support estimates of the universe’s large-scale structure.

• Fred HoyleRelated: The steady-state proposal added an unchanging-cosmos condition beyond this spatial uniformity.

• Georges LemaîtreRelated: This simplifying assumption underlies the class of cosmological models Lemaître studied.

• Friedmann–Lemaître–Robertson–Walker metricRelated: It supplies the symmetry assumptions that single out the FLRW form.

• Scale factorRelated: It motivates the symmetric cosmological models in which the scale factor is defined.

• Alexander FriedmannRelated: This large-scale symmetry makes Friedmann’s cosmological equations tractable.

• Cosmic voidRelated: It supplies the cosmic average against which void underdensities are judged.

• Age of the universeRelated: It lets cosmologists describe expansion with a single cosmic history.

• Mach's principleRelated: Machian arguments often invoke large-scale cosmic matter, whose distribution this principle idealizes.

• Particle horizonRelated: Horizon limits raise the question of how distant regions acquired similar large-scale conditions.

• Flatness problemRelated: It lets cosmology describe space with a single global curvature parameter.

• Local VoidRelated: The Local Void illustrates why large local underdensities can coexist with large-scale uniformity.

• Hubble Ultra-Deep FieldRelated: Deep-field comparisons test whether galaxy populations differ substantially between sky regions.

• Nicholas of CusaRelated: It offers a later framework for comparing Cusa's decentered cosmos with modern cosmology.

• Universe (cosmology)Related: It makes the universe’s global geometry tractable despite its lumpy local structure.

• BOSS Great WallRelated: An exceptionally large structure raises questions about the scale at which cosmic uniformity applies.

• Physical cosmologyRelated: It lets cosmologists model the universe with a small set of averaged quantities.

• Huge-LQGRelated: Huge-LQG's reported size was discussed as a possible challenge to this assumption.

• Observational cosmologyRelated: It lets observations from our location support models of the universe as a whole.

• Tired lightRelated: Any alternative cosmology must explain observations interpreted using this large-scale symmetry.

• Heinrich Wilhelm Matthias OlbersRelated: A spatially uniform distribution of stars is one assumption behind the classical paradox.

• Hubble volumeRelated: It helps make a spherical cosmic region a meaningful large-scale comparison.

• Recessional velocityRelated: It underlies interpreting recession as a general property of cosmic expansion rather than a central-point motion.

• Shape of the universeRelated: It reduces possible cosmic geometries to highly symmetric cases.

• Timeline of cosmological theoriesRelated: It makes the universe-wide models in this timeline mathematically tractable.