Fact-checked by Grok 2 weeks ago

Cosmological principle

The cosmological principle is a foundational assumption in modern cosmology stating that, on the largest scales, the universe is both homogeneous—meaning the distribution of matter and energy is uniform, with no preferred location—and isotropic—appearing the same in all directions, with no preferred orientation.^[1] This principle extends the Copernican idea that observers occupy no special position in the cosmos, implying that physical laws and constants are the same everywhere and unchanging over time.^[2] Formulated by Albert Einstein in his 1917 paper "Kosmologische Betrachtungen zur allgemeinen Relativitätstheorie," the principle was applied to general relativity to model the universe as a whole, assuming a static, finite structure with uniform matter density.^[3] To balance gravitational contraction and achieve this static state, Einstein introduced the cosmological constant term (Λ) into his field equations, estimating the universe's radius at approximately 10^7 light-years based on a matter density of about 10^{-22} g/cm³.^[4] However, Edwin Hubble's 1929 observations of galactic redshifts revealed an expanding universe, prompting Einstein to abandon the static model and cosmological constant, which he later called his "greatest blunder."^[4] The cosmological principle forms the basis for the Friedmann-Lemaître-Robertson-Walker (FLRW) metric, which describes a dynamically expanding universe consistent with the Big Bang theory and enables predictions of cosmic evolution through the Friedmann equations.^[2] Inflation, a brief period of rapid early expansion, helps realize the cosmological principle by smoothing out initial irregularities.^[1] Empirical support for the principle is robust, primarily from the cosmic microwave background (CMB) radiation, the remnant heat from the early universe discovered in 1964 and measured at 2.725 K.^[1] CMB observations by satellites like COBE (1989) and WMAP show temperature uniformity to 1 part in 10^5 across the sky, with isotropic distribution filling the universe and variations arising from primordial density fluctuations rather than directional biases.^[5] Large-scale galaxy surveys, such as the Sloan Digital Sky Survey (SDSS), further confirm homogeneity on scales of hundreds of millions of light-years, aligning with predictions from the principle.^[1] While the principle holds well on cosmic scales, tensions arise on smaller scales or in interpreting phenomena like the CMB dipole (due to our motion relative to the CMB rest frame) and potential large-scale anisotropies probed by modern missions like Planck.^[6] Nonetheless, it remains essential for interpreting cosmological data and parameterizing the universe's composition, including dark matter and dark energy.^[2]

Definition and Historical Origins

Definition

The cosmological principle is the foundational assumption in modern cosmology that the universe is homogeneous—meaning matter and energy are uniformly distributed on large scales—and isotropic—meaning it appears the same in all directions from any given point—on scales exceeding approximately 100 megaparsecs (Mpc).^[7] This principle implies that there is no preferred location or direction in the universe, allowing observers anywhere to describe the cosmos in a similar manner.^[8] The principle exists in weak and strong forms. The weak form posits statistical or observational uniformity, where homogeneity and isotropy hold approximately on large scales due to averaging over cosmic structures, supported by empirical evidence from galaxy distributions and cosmic microwave background radiation.^[9] In contrast, the strong form asserts exact uniformity everywhere in space, without statistical approximations, though this is generally considered an idealization not fully realized in observations.^[10] Etymologically, the principle traces its roots to the Copernican idea that Earth holds no privileged position in the cosmos, extending this philosophical stance to the entire universe by rejecting any central or special viewpoint.^[2] Early proponent Albert Einstein formalized a related assumption in 1917, stating that "the density of the ponderable matter may be assumed to be the same throughout all space," to construct a static cosmological model within general relativity.

Historical Development

The cosmological principle was first explicitly introduced by Albert Einstein in his 1917 paper, where he applied general relativity to model the universe as a whole, assuming spatial homogeneity and isotropy to construct a static, closed universe. To achieve this static configuration and counteract the attractive force of gravity, Einstein introduced the cosmological constant term into his field equations, marking the initial formulation of the principle as a foundational symmetry assumption in relativistic cosmology.^[11] Shortly thereafter, Willem de Sitter proposed an alternative model in 1917, describing an empty universe with positive cosmological constant that exhibited hyperbolic geometry and inherent expansion, influencing subsequent discussions by highlighting solutions without matter content while preserving the symmetry assumptions of the cosmological principle.^[12] Edwin Hubble's 1929 observations of redshifted spectra from distant galaxies provided empirical evidence for universal expansion, with velocities proportional to distance, which contradicted static models and prompted the abandonment of Einstein's static universe in favor of dynamic solutions aligned with the cosmological principle. In the 1930s, Howard Percy Robertson and Arthur Geoffrey Walker independently derived the general form of metrics satisfying the cosmological principle's homogeneity and isotropy, establishing it as a rigorous symmetry condition for cosmological solutions in general relativity, with key works in 1935 and 1934 respectively. Following World War II, the principle became integral to the emerging Big Bang theory, as articulated by George Gamow, Ralph Alpher, and Robert Herman in 1948, who incorporated it into models of an evolving, expanding universe and predicted the existence of cosmic microwave background radiation as a relic of the hot early phase.

Fundamental Assumptions

Homogeneity

The homogeneity assumption within the cosmological principle posits that the universe exhibits spatial uniformity in the distribution of matter and energy, implying that the average density observed by any observer is independent of their position in space on sufficiently large scales. This uniformity arises from the idea that local irregularities, such as variations in galaxy densities, average out over vast distances, leading to a statistically consistent cosmic backdrop. Seminal formulations of this concept emphasize that homogeneity is not absolute but emerges as an effective property when probing the universe beyond the scales of individual structures. This homogeneity becomes apparent only on scales exceeding approximately 100 Mpc, where the universe transitions from clustered configurations—such as galaxies, clusters, and voids dominating smaller regions—to a more uniform distribution. On sub-100 Mpc scales, the matter distribution shows significant inhomogeneities due to gravitational clustering, but beyond this threshold, the density fluctuations diminish, supporting the notion of a smooth cosmic fabric. Observational analyses of galaxy distributions confirm this scale dependence, with the Sloan Digital Sky Survey (SDSS) revealing a shift to uniformity around 60–70 h⁻¹ Mpc, consolidating the empirical basis for large-scale homogeneity.^[13]^[14] The physical foundation of homogeneity relies on statistical measures that average out local fluctuations, ensuring that the universe behaves as if uniform when examined through ensemble averages. A key indicator is the two-point correlation function ξ(r), which quantifies the excess probability of finding a pair of galaxies separated by distance r compared to a random distribution; in a homogeneous universe, ξ(r) approaches zero as r increases to cosmic scales, signaling the absence of preferred positions. This statistical homogeneity underpins the reliability of cosmological models by allowing global properties, like expansion rates, to be inferred without location-specific biases.^[15] Galaxy redshift surveys serve as primary observational proxies for verifying homogeneity, mapping the three-dimensional distribution of galaxies across vast volumes and demonstrating that average densities converge to uniformity on Gpc scales. For instance, surveys like SDSS and the 2dF Galaxy Redshift Survey have shown that while local voids and filaments introduce anisotropies, the overall matter budget evens out, aligning with the cosmological principle's expectations. These datasets provide robust evidence that the universe's large-scale structure adheres to homogeneous statistics, enabling accurate predictions of cosmic evolution.^[13]^[16] Under the homogeneity assumption, the evolution of matter density is governed by the continuity equation in an expanding universe:

\frac{\partial \rho}{\partial t} + 3 \frac{\dot{a}}{a} \rho = 0,

where ρ denotes the average density, a is the scale factor, and the dot indicates time derivative; this equation enforces uniform dilution of density with expansion, reflecting the principle's role in maintaining spatial invariance across the cosmos.^[17]

Isotropy

The isotropy component of the cosmological principle asserts that, on sufficiently large scales, the universe appears identical in all directions from the perspective of any observer, with no preferred axis or directional bias in the distribution of matter, radiation, or other physical properties. This assumption implies rotational symmetry in the large-scale structure, ensuring that measurements of cosmic quantities, such as expansion rates or density fluctuations, yield the same results regardless of orientation.^[18] Isotropy at every point in the universe, when combined with the Copernican principle—that no observer occupies a privileged position—logically entails spatial homogeneity, as any directional uniformity observed locally must hold universally without special locations. However, the converse does not necessarily follow: a homogeneous universe could, in principle, exhibit anisotropies if symmetries allow for directional variations that average out spatially. This one-way implication underscores isotropy's role as a stronger constraint in deriving the full cosmological principle.^[19] Geometrically, isotropy manifests as the rotational invariance of the spacetime metric, meaning the metric tensor remains unchanged under arbitrary rotations of spatial coordinates, preserving the form of physical laws across directions. In an ideal isotropic universe, this invariance would eliminate directional signals, such as dipole (ℓ=1) or higher-order multipole contributions, in the expansion of cosmic fields like the density or temperature distributions. A brief illustration arises in the cosmic microwave background (CMB), where perfect isotropy would confine the angular power spectrum C_\ell to a constant monopole term at ℓ=0, with all higher ℓ suppressed to zero, reflecting uniform temperature without angular variations. Empirical support for isotropy comes from the CMB, whose temperature is uniform to approximately 1 part in $10^5 across the full sky, as measured by satellites like COBE and Planck, indicating near-perfect directional symmetry on scales exceeding the horizon at recombination. Galaxy distributions further corroborate this, with large-scale surveys revealing no significant anisotropies in number counts or clustering patterns beyond ~100 Mpc, after correcting for local peculiar velocities, consistent with rotational invariance on gigaparsec scales. These tests affirm isotropy as a foundational pillar, though subtle deviations at low multipoles continue to be probed for potential refinements.^[20]^[21]

Mathematical and Theoretical Framework

Role in General Relativity

The Einstein field equations of general relativity, G_{\mu\nu} = 8\pi G T_{\mu\nu}, where G_{\mu\nu} is the Einstein tensor describing spacetime curvature and T_{\mu\nu} is the stress-energy tensor representing matter and energy content, form a system of 10 coupled nonlinear partial differential equations for the 10 independent components of the metric tensor g_{\mu\nu}.^[22] Solving these equations for the entire universe without additional assumptions is computationally intractable due to their complexity and the vast number of possible configurations.^[22] The cosmological principle addresses this by imposing symmetries of homogeneity and isotropy on large scales, corresponding to invariance under spatial translations and rotations, respectively.^[23] These symmetries generate a Lie group action that ensures maximal spatial symmetry, reducing the 10 independent components of the metric tensor, thereby simplifying the 10 field equations to a solvable form consistent with the principle's assumptions.^[23] Homogeneity implies that the universe appears identical at every spatial point, while isotropy means it looks the same in all directions from any point, collectively simplifying the geometry to a form amenable to analytical solution.^[24] To derive the appropriate spacetime metric, one assumes a line element ds^2 = g_{\mu\nu} \, dx^\mu \, dx^\nu that remains invariant under the full group of spatial translations and rotations.^[23] This invariance constrains the functional form of g_{\mu\nu}, eliminating degrees of freedom and ensuring the metric respects the cosmological principle's symmetries, thereby allowing the Einstein field equations to be solved in a cosmological context.^[23] Historically, the cosmological principle first played a pivotal role in Albert Einstein's 1917 application of general relativity to the universe, yielding his static universe model as the initial solution. In this model, Einstein introduced the cosmological constant \Lambda into the field equations, G_{\mu\nu} + \Lambda g_{\mu\nu} = 8\pi [G](/page/G) T_{\mu\nu}, to balance gravitational attraction with repulsive effects and maintain a finite, static, homogeneous, and isotropic universe.^[25] This marked the earliest use of symmetry assumptions to apply general relativity on cosmic scales, though the model was later superseded by evidence of expansion.^[26]

Friedmann–Lemaître–Robertson–Walker (FLRW) Metric

The cosmological principle, assuming spatial homogeneity and isotropy, constrains the geometry of spacetime such that the most general metric compatible with these symmetries is the Friedmann–Lemaître–Robertson–Walker (FLRW) metric. This form arises from the requirement that the metric be invariant under spatial translations and rotations at any fixed cosmic time t, leading to a diagonal line element in comoving coordinates where observers move with the expansion. The symmetries eliminate off-diagonal terms and impose that the spatial part scales uniformly with a time-dependent factor a(t), known as the scale factor, which describes the relative expansion of the universe.^[27]^[28] The explicit form of the FLRW metric in spherical coordinates is

ds^2 = -c^2 \, dt^2 + a(t)^2 \left[ \frac{dr^2}{1 - k r^2} + r^2 \, d\theta^2 + r^2 \sin^2\theta \, d\phi^2 \right],

where c is the speed of light, r is the dimensionless comoving radial coordinate (ranging from 0 to infinity for k \leq 0 and from 0 to $1 / \sqrt{|k|} for k > 0), and d\Omega^2 = d\theta^2 + \sin^2\theta \, d\phi^2 is the metric on the unit sphere. The parameter k characterizes the spatial curvature: k = +1 for a closed (spherical) geometry, k = 0 for flat (Euclidean), and k = -1 for open (hyperbolic). Observations from the cosmic microwave background indicate that the universe is nearly flat, with k consistent with zero within measurement precision.^[29]^[30]^[31] Substituting the FLRW metric into the Einstein field equations of general relativity yields the Friedmann equations, which govern the dynamics of the scale factor. The first Friedmann equation relates the Hubble parameter H(t) = \dot{a}/a to the total energy density \rho and curvature:

H^2 = \left( \frac{\dot{a}}{a} \right)^2 = \frac{8\pi G}{3} \rho - \frac{k c^2}{a^2} + \frac{\Lambda c^2}{3},

where G is Newton's gravitational constant and \Lambda is the cosmological constant. The second Friedmann equation describes the acceleration:

\frac{\ddot{a}}{a} = -\frac{4\pi G}{3} \left( \rho + \frac{3p}{c^2} \right) + \frac{\Lambda c^2}{3},

with p denoting the isotropic pressure. These equations were first derived by applying the field equations to homogeneous, isotropic spacetimes filled with matter.^[29]^[30] Under the symmetries of the FLRW metric, the conservation of the energy-momentum tensor T^{\mu\nu} for a perfect fluid (with T^{\mu\nu} = (\rho + p/c^2) u^\mu u^\nu + p g^{\mu\nu}/c^2, where u^\mu is the four-velocity) leads to the continuity equation, or fluid equation:

\dot{\rho} + 3 H (\rho + p/c^2) = 0.

This expresses local energy conservation and implies that the density evolves with the expansion, such as \rho \propto a^{-3(1 + w)} for a constant equation-of-state parameter w = p/(\rho c^2).^[30]^[31]

Cosmological Implications

Universe Expansion

The cosmological principle, through its implications for the Friedmann–Lemaître–Robertson–Walker (FLRW) metric, predicts that the universe expands uniformly on large scales, with the scale factor a(t) governing the relative distances between comoving observers over cosmic time t. This expansion manifests as a recession of galaxies, where the velocity v of a galaxy at proper distance d follows Hubble's law: v = H_0 d, with H_0 the present-day Hubble constant, approximately 70 km/s/Mpc. This relation arises directly from the FLRW framework, where the Hubble parameter H(t) = \dot{a}/a describes the instantaneous expansion rate, and in the low-redshift limit, the recession velocity is v = H_0 d for nearby objects.^[32]^[33] The interpretation of Hubble's law under the cosmological principle emphasizes that there is no preferred center to the expansion; every observer sees distant galaxies receding proportionally to their distance, reflecting the homogeneous and isotropic stretching of space itself rather than peculiar motions through space. This global expansion rate H(t) evolves with time, decreasing as the universe ages due to the dilution of energy density, and distances to remote objects are computed via lookback time integrals that account for the changing H(t). For instance, the comoving distance \chi to an object at redshift z is given by \chi = \int_0^z \frac{[c](/page/Speed_of_light) \, dz'}{H(z')}, where c is the speed of light, and the luminosity distance d_L = (1+z) \chi (assuming a flat universe with a_0 = 1) relates observed fluxes to intrinsic luminosities.^[34]^[35] The expansion rate H(t) varies across cosmic epochs dominated by different components. In the early radiation-dominated era, when relativistic particles and photons contributed most to the energy density, H(t) \propto 1/(2t), leading to a scale factor a(t) \propto t^{1/2}. Later, during the matter-dominated era, non-relativistic matter (baryons and dark matter) slowed the expansion to H(t) \propto 2/(3t) and a(t) \propto t^{2/3}, reflecting the transition as radiation density dilutes faster than matter density with expansion. These phases establish the context for the universe's decelerating expansion until the recent onset of dark energy influence, though the principle ensures uniformity across scales.

Big Bang Model

The Big Bang model describes the evolution of the universe from an initial singularity at time t = 0, where general relativity predicts infinite density and temperature, marking the origin of space, time, and matter. This singularity arises as an extrapolation of the universe's expansion backward in time using the Friedmann equations derived under the cosmological principle. The current age of the universe, as determined from measurements of the cosmic microwave background (CMB) and the Hubble constant, is approximately 13.8 billion years.^[31] The model's timeline unfolds through distinct epochs governed by the dominant physical processes. The Planck epoch, lasting until about $10^{-43} seconds, represents the regime where quantum gravity effects are expected to dominate, beyond the reach of current theories. This is followed by the inflationary epoch, from roughly $10^{-36} seconds to $10^{-32} seconds, during which the universe undergoes rapid exponential expansion driven by a hypothetical inflaton field. Subsequent stages include Big Bang nucleosynthesis, occurring over the first few minutes when the temperature allows fusion of light nuclei, and recombination at about 380,000 years after the singularity, when electrons combine with protons to form neutral atoms, releasing the CMB photons.^[36] In the standard \LambdaCDM framework, consistent with the cosmological principle's implications for a homogeneous and isotropic universe, the energy content is divided into baryonic matter (approximately 5%), cold dark matter (approximately 25%), and dark energy (approximately 70%). These fractions, derived from CMB anisotropies and large-scale structure data, dictate the universe's expansion history and structure formation.^[31] The Big Bang model yields key predictions, including a perfect blackbody spectrum for the CMB, as anticipated from the thermal equilibrium in the early hot phase. Additionally, Big Bang nucleosynthesis accurately forecasts the primordial abundances of light elements, such as hydrogen (~75%), helium-4 (~25%), and trace amounts of deuterium, helium-3, and lithium-7, based on the neutron-to-proton ratio and reaction rates at early times. The age of the universe t_0 in a flat, matter-dominated model is approximated by t_0 \approx \frac{2}{3 H_0}, where H_0 is the present Hubble constant; in the full \LambdaCDM case, it requires numerical evaluation of the integral t_0 = \int_0^1 \frac{da}{a H(a)}, with H(a)^2 = H_0^2 \left( \Omega_m a^{-3} + \Omega_\Lambda \right) for a flat universe.^[37]^[38]

Observational Evidence and Tests

Cosmic Microwave Background (CMB)

The cosmic microwave background (CMB) serves as a cornerstone observational test of the cosmological principle, providing evidence for the homogeneity and isotropy of the universe on large scales through its nearly uniform radiation field. Predicted theoretically in the context of the hot Big Bang model, the CMB originates from the epoch of recombination, when the universe cooled sufficiently for protons and electrons to form neutral hydrogen atoms, allowing photons to decouple from matter and propagate freely. This relic radiation, now observed as microwaves, fills the universe uniformly, supporting the assumption that the universe appears the same in all directions and from any vantage point on sufficiently large scales. The CMB was serendipitously discovered in 1965 by Arno Penzias and Robert Wilson at Bell Laboratories, who detected a persistent excess antenna temperature of about 3.5 K at a frequency of 4.08 GHz using a horn antenna, initially attributed to possible equipment noise but later identified as cosmic origin. This observation confirmed earlier theoretical predictions from 1948 by Ralph Alpher, Hans Bethe, and George Gamow, who, in their analysis of Big Bang nucleosynthesis, foresaw a residual blackbody radiation field with a temperature around 5 K as a remnant of the early hot universe. The discovery provided direct empirical support for the expanding universe model and the uniformity implied by the cosmological principle. Key properties of the CMB include its near-perfect blackbody spectrum with a current temperature of T = 2.725 \pm 0.002 K, as precisely measured by the Far Infrared Absolute Spectrophotometer (FIRAS) instrument on the Cosmic Background Explorer (COBE) satellite, deviating from a perfect blackbody by less than 0.005%. The radiation exhibits remarkable isotropy, with temperature fluctuations at the level of \Delta T / T \sim 10^{-5}, arising from primordial density perturbations that seeded the growth of cosmic structure while preserving overall uniformity consistent with the cosmological principle. These small anisotropies, first detected by COBE's Differential Microwave Radiometer (DMR), reflect the statistical homogeneity of the early universe. The CMB formed during the decoupling epoch at a redshift of z \approx 1100, approximately 380,000 years after the Big Bang, when the plasma temperature dropped to about 3000 K, enabling recombination and rendering the universe optically thin to photons. Since then, these photons have free-streamed across the expanding universe, redshifted by the cosmic expansion to their present microwave frequencies, maintaining a snapshot of the isotropic conditions at last scattering that aligns with the homogeneity and isotropy assumptions.^[39] Analysis of the CMB angular power spectrum reveals acoustic peaks resulting from baryon-photon oscillations in the early universe's photon-baryon fluid, where sound waves in the tightly coupled plasma before decoupling imprinted oscillatory patterns in the temperature fluctuations. These peaks, prominently mapped by the Planck satellite, provide tight constraints on cosmological parameters, such as the baryon density \Omega_b h^2 \approx 0.0224 and total matter density \Omega_m h^2 \approx 0.143, reinforcing the flat, homogeneous geometry predicted by the cosmological principle.^[31] On large angular scales, the dominant temperature fluctuations are described by the Sachs-Wolfe effect, where photons climbing out of potential wells in the early universe lose energy, leading to \Delta T / T \approx \frac{1}{3} \frac{\delta \rho}{\rho}, with \frac{\delta \rho}{\rho} representing the primordial density contrast. This relation, derived from general relativistic perturbations, links observed CMB anisotropies directly to the initial conditions of homogeneity.^[40]

Large-Scale Structure Surveys

Large-scale structure surveys map the distribution of galaxies and matter across vast cosmic volumes, providing direct tests of the cosmological principle's homogeneity assumption by revealing how density variations average out on scales exceeding 100 Mpc. Early pivotal efforts include the 2dF Galaxy Redshift Survey (2dFGRS), which measured redshifts for over 220,000 galaxies and uncovered a filamentary web of structures—such as walls, filaments, and voids—but demonstrated that these features smooth into statistical uniformity on scales greater than approximately 100 Mpc, consistent with an isotropic and homogeneous matter distribution on larger scales.^[41] Similarly, the Sloan Digital Sky Survey (SDSS) has cataloged millions of galaxies, confirming the same transition to homogeneity beyond 70–100 h^{-1} Mpc (where h ≈ 0.7), where the galaxy distribution aligns with expectations from a homogeneous universe despite prominent small-scale clustering.^[42]^[43] A key statistical tool in these surveys is the two-point correlation function, ξ(r), which quantifies the excess probability of finding galaxy pairs separated by distance r relative to a random, homogeneous distribution. On small scales (r ≲ 10 Mpc), ξ(r) is positive and large, reflecting clustered structures, but it transitions to ξ(r) ≈ 0 for r ≫ 100 Mpc, indicating that density fluctuations decorrelate and the universe approaches homogeneity.^[42] This behavior is formalized through the density contrast δ, defined as

\delta = \frac{\rho - \bar{\rho}}{\bar{\rho}},

where ρ is the local density and \bar{ρ} is the mean cosmic density; surveys show that |δ| < 10^{-4} on the largest probed scales, underscoring the uniformity required by the cosmological principle.^[44] Additionally, baryon acoustic oscillations (BAO) imprint a characteristic scale of roughly 150 Mpc in the galaxy clustering pattern, arising from sound waves in the early universe plasma; this feature is clearly detected in SDSS and 2dFGRS data, providing a standard ruler that matches the scale inferred from the cosmic microwave background, further validating large-scale homogeneity. Ongoing missions in the 2020s continue to refine these tests with unprecedented precision. The Euclid space telescope, launched in July 2023, images and spectroscopically surveys billions of galaxies to map large-scale structure over 15,000 square degrees of the sky; its Quick Data Release 1 (March 2025) confirms the flat geometry of the universe through BAO and galaxy clustering analyses that align with homogeneous models.^[45]^[46] Likewise, the Dark Energy Spectroscopic Instrument (DESI), operational since 2021, has measured redshifts for tens of millions of objects in its Data Release 2 (2025), yielding BAO detections that support a flat, homogeneous cosmology with no significant deviations on scales up to several gigaparsecs, though with hints of evolving dark energy.^[47]^[48] These results collectively affirm that matter distribution adheres to the cosmological principle on cosmic scales, enabling robust constraints on parameters like the matter density Ω_m ≈ 0.3.

Violations of Homogeneity

Observed deviations from the cosmological principle's assumption of homogeneity manifest primarily through the discovery of large-scale structures that appear to exceed the expected uniform distribution of matter on scales beyond approximately 100 Mpc, where the two-point correlation function of galaxies transitions to near-zero, indicating homogeneity.^[49] These structures challenge the idea that the universe is statistically uniform on observable scales, as the correlation length—the scale at which galaxy clustering becomes negligible—is estimated at around 70–100 h⁻¹ Mpc (with h ≈ 0.7), beyond which fluctuations should average out.^[50] If confirmed as coherent features rather than projections or survey artifacts, such anomalies suggest potential breakdowns in homogeneity, prompting reevaluations of structure formation models. However, subsequent analyses in 2025 suggest these structures may arise from statistical fluctuations or projections in ΛCDM models, without necessitating a breakdown of homogeneity.^[51] Early examples include the CfA2 Great Wall, discovered in the Center for Astrophysics Redshift Survey, which spans approximately 150 Mpc at a median redshift of z ≈ 0.03 and consists of a planar assembly of galaxies connecting multiple clusters. Similarly, the Sloan Great Wall, identified in the Sloan Digital Sky Survey (SDSS), extends over about 430 Mpc (or 1.4 billion light-years) at z ≈ 0.08, representing one of the densest filamentary structures in the nearby universe and comprising several superclusters. Complementing these overdensities are vast underdensities, such as the Boötes Void, the largest known void discovered in 1981, with a diameter of roughly 100 Mpc (corresponding to a redshift extent of about 7,500 km/s) and containing far fewer galaxies than expected in a homogeneous distribution—only around 60 galaxies observed within its volume despite predictions of thousands. More recent discoveries have pushed these scales further, intensifying debates over homogeneity. The Giant Arc, serendipitously identified in 2021 through MgII absorption lines in quasar spectra, spans approximately 1 Gpc (proper size at the present epoch) at z ≈ 0.8, potentially indicating a collapsing or bound structure that defies standard Gaussian random fields in ΛCDM simulations.^[52] Likewise, the Big Ring, announced in 2024 from similar MgII catalogues, forms a circular annulus-like feature with a diameter of about 400 Mpc (1.3 billion light-years) at z ≈ 0.38, located near the Giant Arc on the sky; its non-circular, potentially non-Gaussian morphology raises questions about whether it arises from true large-scale inhomogeneities or line-of-sight alignments.^[53] These ultra-large structures, if real and coherent, exceed the homogeneity scale by factors of several, implying that matter distribution may remain inhomogeneous across observable volumes up to billions of light-years. Statistical analyses of galaxy surveys provide quantitative evidence for these mild inhomogeneities. Power-law correlations in the galaxy distribution, described by the two-point correlation function ξ(r) ∝ (r/r₀)^(-γ) with r₀ ≈ 5 h⁻¹ Mpc and γ ≈ 1.8 on small scales, weaken toward homogeneity beyond 100 Mpc but persist in showing excess clustering in certain regions.^[54] Fractal dimension estimates, such as the correlation dimension D₂, yield values around 2 on scales up to 20–70 h⁻¹ Mpc, indicating scale-invariant clustering akin to a fractal, before approaching the Euclidean value of 3 at larger distances, consistent with a transition to homogeneity around 100 Mpc.^[55] Additionally, χ² tests applied to galaxy counts in large-scale structure surveys, such as those from SDSS, assess deviations from uniform Poisson distributions, revealing statistically significant over- and under-densities that align with observed structures and suggest the homogeneity scale may vary slightly with survey depth.^[56] These tests collectively underscore that while the universe appears broadly homogeneous on the largest scales, localized violations persist, necessitating refined models to reconcile observations with theoretical expectations.

Violations of Isotropy

Observations of galaxy distributions have revealed potential directional deviations from isotropy, particularly in quasar catalogs from the Sloan Digital Sky Survey (SDSS). Analysis of SDSS quasar samples shows a dipole anisotropy in number counts with an amplitude on the order of $10^{-3}, consistent with the expected kinematic effect from our motion relative to the cosmic rest frame, but the direction suggests a possible preferred axis along the observer's velocity.^[57] This dipole arises from relativistic aberration and Doppler boosting, yet studies indicate alignments in the distribution that may hint at larger-scale anisotropies beyond the standard kinematic interpretation.^[57] Type Ia supernovae provide another probe of isotropy, with the Union2.1 compilation exhibiting a preferred direction in the deceleration parameter and expansion rate. Fits to the Union2.1 data, comprising 580 supernovae, reveal a dipole modulation pointing towards galactic coordinates (l, b) = (307.1^\circ \pm 16.2^\circ, -14.3^\circ \pm 10.1^\circ), suggesting anisotropic cosmic expansion at low redshifts.^[58] This preferred axis, detected via dipole fitting under a \LambdaCDM model, contrasts with null results from hemisphere comparisons, indicating the signal's subtlety but potential violation of large-scale isotropy.^[58] Radio source surveys, such as the NRAO VLA Sky Survey (NVSS), further suggest directional biases. The NVSS catalog of approximately 1.8 million extragalactic radio sources displays a dipole with direction (\mathrm{RA}, \mathrm{Dec}) = (154^\circ \pm 19^\circ, -2^\circ \pm 19^\circ), closely aligned with the cosmic microwave background (CMB) dipole at (\mathrm{RA}, \mathrm{Dec}) = (168^\circ, -7^\circ).^[59] However, the dipole amplitude, around $1.8 \times 10^{-2}, exceeds the kinematic expectation by a factor of about 4, implying possible non-kinematic contributions or a preferred axis in the radio source distribution.^[59] Beyond the dipole, the CMB itself shows non-dipole anisotropies in low-\ell multipoles that challenge isotropy. The quadrupole (\ell=2) and octupole (\ell=3) exhibit anomalously low power compared to \LambdaCDM predictions, with their planes of oscillation aligned at a level inconsistent with random orientations.^[60] This quadrupole-octupole alignment, along with the dipole-quadrupole-octupole configuration, occurs with a probability of less than 1% under standard cosmology, pointing to a common preferred axis perpendicular to the ecliptic.^[60] Recent analyses of Planck 2018 data confirm these mild deviations from isotropy across multiple probes, though generally within 3\sigma of \LambdaCDM expectations. The CMB temperature anisotropies display low-\ell anomalies, including the quadrupole-octupole alignment at approximately 3\sigma significance and hemispherical power asymmetry, but no compelling evidence for strong isotropy violation. These findings suggest that while preferred directions exist in the data, they may stem from statistical fluctuations or subtle cosmological effects rather than fundamental breakdowns of the principle.

Specific Observational Anomalies

CMB Dipole

The Cosmic Microwave Background (CMB) dipole represents the largest-scale anisotropy in the CMB temperature map, first precisely measured by the Differential Microwave Radiometers (DMR) instrument on the Cosmic Background Explorer (COBE) satellite in 1992. The measurement revealed a temperature variation with amplitude \Delta T = 3.365 \pm 0.027 mK, corresponding to a fractional amplitude \Delta T / T \approx 1.23 \times 10^{-3} relative to the mean CMB temperature of T \approx 2.725 K, and directed toward galactic coordinates (l, b) = (264^\circ, 48^\circ), in the general direction of the Virgo constellation. This dipole is interpreted as arising from the Doppler boost effect due to the motion of the Local Group of galaxies, including the Solar System, relative to the CMB rest frame, where the universe appears isotropic on average. The implied peculiar velocity is v \approx 370 km/s in the direction (l, b) = (264^\circ, 48^\circ). The kinematic origin aligns with the cosmological principle's expectation of large-scale isotropy, as our local motion induces a directional temperature shift without implying intrinsic inhomogeneity in the CMB itself. The temperature variation follows the first-order Doppler formula:

\frac{\Delta T}{T} = \frac{v}{c} \cos \theta,

where v is the observer's velocity relative to the CMB frame, c is the speed of light, and \theta is the angle between the line of sight and the direction of motion; this is the leading term of the full relativistic Doppler effect for photon temperature in the CMB, \frac{T(\theta)}{T_0} = \frac{\sqrt{1 - \beta^2}}{1 - \beta \cos \theta} with \beta = v/c \ll 1. Under the cosmological principle, the dipole should be a pure kinematic effect from our peculiar velocity, serving as a test of isotropy: any deviation would suggest intrinsic anisotropies at the largest scales, while higher-order multipoles (\ell \geq 2) arise from primordial density fluctuations and late-time effects like the integrated Sachs-Wolfe effect. The 2018 Planck Collaboration analysis, using full-mission data across multiple frequencies, confirmed the kinematic dipole with high precision, yielding v = 369.82 \pm 0.11 km/s toward (l, b) = (264.021^\circ, 48.253^\circ), consistent with COBE and subsequent missions like WMAP.^[61] However, some analyses of Planck data have hinted at possible small non-kinematic contributions to the observed dipole, potentially from intrinsic CMB modulation or local structure effects, though these remain unconstrained at the percent level and do not contradict the overall kinematic dominance.

Other Anomalies and Tensions

One prominent modern tension challenging the cosmological principle is the discrepancy in measurements of the Hubble constant H_0, which quantifies the current expansion rate of the Universe. Analyses of the cosmic microwave background (CMB) from the Planck satellite yield H_0 \approx 67.4 \pm 0.5 km/s/Mpc under the standard \LambdaCDM model. In contrast, local distance ladder measurements using Cepheid variables and Type Ia supernovae from the SH0ES team report H_0 = 72.6 \pm 1.0 km/s/Mpc (as of 2024, incorporating James Webb Space Telescope data), with the tension exceeding 5\sigma significance and confirmed by recent JWST observations.^[62] Interpretations of this Hubble tension often invoke potential violations of the cosmological principle's assumptions of homogeneity and isotropy. For instance, anisotropic expansion models, such as those based on Bianchi type-I metrics, could reconcile the discrepancy by allowing direction-dependent Hubble rates, though such scenarios challenge large-scale uniformity. Local inhomogeneities, like underdense voids around the Milky Way, might also bias local H_0 measurements higher, effectively violating homogeneity on scales up to hundreds of megaparsecs. Beyond the Hubble tension, alignments in dipole anisotropies across multiple probes suggest unexpectedly large bulk flows. Observations of Type Ia supernovae indicate bulk flow velocities of approximately 1000 km/s aligned with the CMB dipole direction, exceeding \LambdaCDM predictions for scales beyond 270 Mpc. Similarly, quasar catalogs reveal a dipole amplitude over twice that expected from our motion relative to the CMB rest frame, with the direction closely matching the CMB dipole and implying peculiar velocities inconsistent with homogeneity, though recent analyses with catalogs like Quaia show mixed results, with some confirming the excess and others finding consistency.^[63] Recent baryon acoustic oscillation (BAO) measurements from the Dark Energy Spectroscopic Instrument (DESI) 2024 data release, spanning over 6 million galaxies and quasars up to redshift z \approx 3.5, yield H_0 \approx 67.97 km/s/Mpc when combined with CMB data, aligning with Planck and further exacerbating the tension with local measurements. James Webb Space Telescope (JWST) observations from 2023 to 2025 of early galaxies at redshifts z > 10, revealing unexpectedly massive structures forming within 300 million years post-Big Bang, hint at faster early expansion rates that could amplify the H_0 discrepancy if reconciled with standard models. Statistical assessments using Bayesian methods quantify the breakdown of the standard model in accommodating these tensions. Bayes factor analyses comparing \LambdaCDM to extended models incorporating inhomogeneities or anisotropies favor alternatives with factors exceeding 10 in some datasets, indicating substantial evidence for principle violations over statistical fluctuations alone.

Criticisms and Alternatives

Theoretical Criticisms

The cosmological principle, positing the universe's homogeneity and isotropy on large scales, has faced philosophical scrutiny for its foundational assumptions. Philosopher Karl Popper critiqued the perfect cosmological principle as a form of dogma, arguing that it elevates ignorance about the universe's structure into a prescriptive principle of knowledge, thereby hindering empirical falsifiability in cosmology. This view stems from the principle's origins as a simplifying assumption rather than a directly observable fact, potentially embedding untestable biases into theoretical frameworks.^[64] A related philosophical concern ties the principle to the Copernican assumption of mediocrity, implying Earth and observers occupy no privileged position, yet this may obscure evidence of cosmic fine-tuning in physical constants that appear exquisitely balanced for life's emergence. Critics argue that the principle's emphasis on uniformity could mask such apparent design-like features, raising questions about whether it unduly constrains interpretations of the universe's habitability. The strong version of the principle, requiring exact homogeneity and isotropy everywhere, remains inherently untestable, as it demands knowledge beyond the observable horizon, rendering it more axiomatic than empirically derived.^[65] Theoretically, cosmic inflation, while posited to enforce large-scale smoothness, relies on the principle as a prior assumption and fails to rigorously prove it from generic initial conditions. Studies show that inflationary models do not universally resolve the horizon and flatness problems without presupposing near-homogeneity at the outset, leaving the principle's validity contingent on unresolved initial state dynamics. In quantum gravity regimes, such as at the Planck scale, the principle's symmetries may break down, with theories like loop quantum cosmology suggesting that homogeneity emerges only as an effective, coarse-grained property rather than a fundamental one.^[66]^[67] General relativity's application of the principle yields global solutions like the Friedmann-Lemaître-Robertson-Walker metric, which predict an initial singularity, but alternative eternal universe models avoid this by relaxing homogeneity, implying the universe could be past- or future-eternal without such a breakdown. This highlights a limitation: the principle enforces singular behaviors that quantum corrections might circumvent, challenging its universality. Debates persist on whether the principle functions as a foundational axiom in cosmology or as a hypothesis derived from limited observations, with some viewing it as indispensable for tractable models yet vulnerable to revision by more complete theories.^[68] Approaches like timescape cosmology illustrate theoretical alternatives by incorporating inhomogeneities to explain apparent acceleration without invoking dark energy, underscoring how deviations from strict homogeneity can address tensions in standard models. Recent 2025 analyses suggest timescape models perform competitively against \LambdaCDM in fitting supernova data, potentially resolving dark energy as an illusion from gravitational time dilation in voids.^[69]^[70]

Inhomogeneous and Alternative Models

Inhomogeneous cosmological models relax the strict homogeneity and isotropy assumptions of the cosmological principle by incorporating spatial variations in density and expansion rates, potentially explaining observational phenomena like cosmic acceleration without invoking dark energy. A prominent example is the Lemaître-Tolman-Bondi (LTB) model, which describes a spherically symmetric dust-filled universe with radial inhomogeneities, allowing the local Hubble rate to differ from the global average. In this framework, observers situated off-center experience an apparent acceleration due to the gradient in expansion, mimicking the effects attributed to a cosmological constant \Lambda in homogeneous models. This approach challenges the uniformity implied by the cosmological principle, suggesting that local inhomogeneities could bias global inferences from observations like type Ia supernovae.^[71] The concept of backreaction arises from averaging theorems in general relativity, which demonstrate that the average geometry \langle g \rangle of an inhomogeneous spacetime does not equal the geometry of the average g(\langle \cdot \rangle), leading to additional terms in the effective dynamical equations. Pioneered by Buchert, these theorems apply to irrotational dust cosmologies, yielding modified Friedmann-like equations where the variance in local expansion rates contributes a "backreaction" term Q, potentially accelerating the average expansion without \Lambda. This effect quantifies how small-scale fluctuations, such as those from structure formation, influence the large-scale dynamics, providing a mechanism to relax homogeneity while preserving approximate isotropy on average. Seminal formulations show that backreaction can be positive or negative depending on the epoch, with its magnitude estimated at around 10% of the deceleration parameter in the present universe. Void models, a subclass of LTB solutions, posit that we reside within an underdense spherical bubble surrounded by a denser shell, where the local underdensity induces faster expansion inside the void, replicating the luminosity distance-redshift relation observed in supernova data. This setup mimics homogeneity from an off-center observer's perspective due to the spherical symmetry, but it inherently violates full isotropy unless the observer is precisely at the center—a position that raises Copernican concerns. Motivations for these models stem from resolving tensions like the apparent acceleration without fine-tuning \Lambda, with early implementations fitting supernova and baryon acoustic oscillation data reasonably well. However, void models typically require a void radius of about 1-2 Gpc to match observations.^[72] In the 2020s, studies using James Webb Space Telescope (JWST) data, which confirm the Hubble tension through precise Cepheid-based H0 measurements (e.g., from SH0ES), have motivated further scrutiny of LTB models. For instance, 2025 analyses of LTB void models demonstrate they can alleviate the tension between local and CMB-inferred expansion rates by tuning void parameters to fit datasets like SH0ES and the Carnegie-Chicago Hubble Program (CCHP). These efforts highlight how high-redshift galaxy observations from JWST probe the transition from local voids to the global background, testing the spatial extent of inhomogeneities.^[73] Despite their appeal, LTB and void models face significant limitations in reproducing the observed isotropy of the cosmic microwave background (CMB). Spherically symmetric LTB metrics are isotropic only about the central point, implying that off-center observers—like us—would detect a strong dipole or higher multipoles in the CMB due to integrated Sachs-Wolfe effects and Doppler contributions along the line of sight. To match the CMB's near-uniformity to 1 part in $10^5, the observer must lie within a narrow radial shell near the center (typically r \lesssim 0.1 times the void radius), which strains the model's viability and indirectly challenges the cosmological principle's isotropy. Detailed calculations confirm that standard LTB voids overpredict CMB anisotropies unless supplemented by ad hoc adjustments, underscoring their tension with full-sky CMB data.^[74]

Perfect Cosmological Principle

The perfect cosmological principle posits that the universe is homogeneous and isotropic not only in space but also in time, meaning its large-scale appearance remains unchanged across cosmic epochs, with no net evolution in structure or density. This temporal uniformity contrasts with the standard cosmological principle, which allows for evolutionary changes over time while assuming spatial homogeneity and isotropy at any given epoch. This principle formed the foundation of the steady-state theory, independently developed by Hermann Bondi and Thomas Gold, and by Fred Hoyle in 1948. In their model, the universe undergoes uniform expansion, as observed through redshift, but maintains a constant average matter density ρ through the continuous creation of matter. The required creation rate balances the dilution due to expansion and equals 3Hρ, where H is the Hubble parameter.^[75] This process is incorporated into the continuity equation for the stress-energy tensor, modified to include a creation term Γ:

\frac{\partial \rho}{\partial t} + 3H\left(\rho + \frac{p}{c^2}\right) = \Gamma

For a matter-dominated universe with pressure p ≈ 0 and steady-state conditions (constant ρ), Γ = 3Hρ ensures the left-hand side vanishes.^[75] The creation rate yields approximately one hydrogen atom per cubic meter every few billion years, a minuscule flux undetectable locally but necessary on cosmic scales. The steady-state model faced observational challenges in the 1960s and 1970s, leading to its widespread rejection. Discoveries of quasars, which are far more abundant at high redshifts (indicating higher density in the early universe), demonstrated evolutionary changes incompatible with temporal uniformity. The 1965 detection of the cosmic microwave background (CMB) as uniform blackbody radiation further supported a hot, dense early phase in the Big Bang model, rather than steady creation. Echoes of the perfect principle persist in modern variants, such as quasi-steady-state cosmology (QSSC), proposed by Hoyle, Geoffrey Burbidge, and Jayant Narlikar in the 1990s. QSSC incorporates episodic matter creation events to accommodate observed evolution, including the CMB, while retaining elements of long-term uniformity between "creation epochs."^[76]

Copernican Principle

The Copernican principle asserts that Earth and its inhabitants occupy no privileged position or time within the universe, serving as a foundational assumption that the observable cosmos appears similar from any typical vantage point. This idea posits that the universe has no center or special reference frame centered on humanity; instead, Earth is merely one unremarkable location among many. Formulated initially in the context of the solar system, it implies that local peculiarities, such as our planet's position, do not imply cosmic centrality but rather reflect observer-dependent perspectives. Historically, the principle traces its roots to Nicolaus Copernicus's 1543 publication De revolutionibus orbium coelestium, which proposed a heliocentric model displacing Earth from the universe's presumed center and challenging geocentric doctrines. This shift was bolstered by Galileo's telescopic observations in the early 17th century, confirming Jupiter's moons and Venus's phases, and by Johannes Kepler's laws of planetary motion around 1609–1619, which refined the orbital mechanics without privileging Earth. Albert Einstein extended this concept to cosmology in the 1910s through general relativity, envisioning a universe where gravitational laws apply uniformly without a preferred location, thereby laying the groundwork for relativistic models of cosmic expansion. In relation to the broader cosmological principle, the Copernican idea provides the philosophical and symmetry-based justification for assuming large-scale homogeneity and isotropy, which mathematically yield the Friedmann–Lemaître–Robertson–Walker (FLRW) metric describing an expanding universe. By rejecting observer bias, it enables the averaging of matter and energy distributions over vast scales, treating the universe as statistically uniform rather than structured around any single point. Violations of this principle would necessitate models with preferred frames, potentially reviving geocentric-like asymmetries incompatible with observed cosmic uniformity. Modern validations of the Copernican principle leverage the cosmic microwave background (CMB), where the observed dipole anisotropy—arising from Earth's orbital and galactic motion relative to the CMB rest frame at approximately 370 km/s—demonstrates that our velocity is a local effect rather than evidence of cosmic centrality. The preservation of the CMB's blackbody spectrum despite this motion further confirms no special frame exists, as deviations would distort the thermal equilibrium expected in a non-privileged cosmology.

References

[1]
An Exposition on Inflationary Cosmology - G.S. Watson
The Cosmological Principle (CP) is the rudimentary foundation of most standard cosmological models. The CP can be summarized by two principles of spatial ...
[2]
Cosmological Principle - University of Oregon
The clearest modern evidence for the cosmological principle is measurements of the cosmic microwave background (shown above). Briefly (we will cover the CMB ...
[3]
http://einsteinpapers.press.princeton.edu/vol6-trans/433
[4]
Albert Einstein and the origins of modern cosmology - Physics Today
Feb 3, 2017 · In 1917 Einstein published a paper that applied general relativity to the universe, changing our view of the cosmos forever.
[5]
WMAP Big Bang CMB Test
### Summary: CMB Support for the Cosmological Principle
[6]
[PDF] Testing cosmological principle under Copernican principle - arXiv
May 25, 2025 · The evolution of modern cosmology has led to a quantitative refinement of the cosmological principle. Ac- cording to predictions of the ...<|control11|><|separator|>
[7]
Lecture 40: The Curvature of the Universe
Mar 6, 2025 · The cosmological principle states that on large scales (> 100 Mpc), the universe looks the same from every vantage point.
[8]
Cosmological principles
This conclusion is called the anthropic cosmological principle: namely, that the universe must be congenial to the origin and development of intelligent life.
[9]
[PDF] Physics 133 -- Extragalactic Astronomy and Cosmology
But is the CMB radiation really a perfect blackbody spectrum? Page 58. Is ... Only the weak form of the cosmological principle applies. Page 65. Week 1 ...<|separator|>
[10]
[PDF] Cosmological principle
Oct 13, 2011 · ✦ most modern cosmology is based on the "cosmological principle," it is assumed that, on large scales, the universe is both homogeneous and ...
[11]
[PDF] Sitzungsberichte der Königlich Preussischen Akademie der ...
Page 1. 142. Sitzung der physikalisch-mathematischen Klasse vom 8. Februar 1!)I7. Kosmologische Betrachtungen zur allgemeinen. Relativitätstheorie. Von A.
[12]
On Einstein's Theory of Gravitation and its Astronomical ...
W. de Sitter; On Einstein's Theory of Gravitation and its Astronomical Consequences. Third Paper.⋆, Monthly Notices of the Royal Astronomical Society, Volu.Missing: cosmology | Show results with:cosmology
[13]
The scale of homogeneity of the galaxy distribution in SDSS DR6
Jun 18, 2009 · We find that the galaxy distribution becomes homogeneous at a length-scale between 60 and 70 h^{-1} {\rm Mpc}.<|separator|>
[14]
[1607.03418] The Homogeneity Scale of the universe - arXiv
Jul 12, 2016 · We verify that the universe becomes homogenous on scales greater than \mathcal{R}_{H} \simeq 64.3\pm1.6\ h^{-1}Mpc, consolidating the ...
[15]
The correlation function
The correlation function is the expected 2-point function of this statistic. Equation 2, (2). From statistical homogeneity and isotropy, we have that. Equation ...
[16]
[PDF] the Cosmological Principle: the Evidence
Prime Evidence for an Isotropic Universe: 1) Isotropy Cosmic Microwave Background. 2) Isotropy X-ray Background. 3) Isotropy Gamma Ray Bursts (GRBs). 4 ...
[17]
[PDF] Lecture XXX: Dynamics of cosmic expansion - Caltech (Tapir)
Apr 11, 2012 · Continuity provides a strong constraint on the possible behavior of matter in cosmology. ... The continuity equation, Eq. (12), then tells us that.
[18]
[1205.3309] The Scale of Cosmic Isotropy - arXiv
The most fundamental premise to the standard model of the universe, the Cosmological Principle (CP), states that the large-scale properties of the universe are ...
[19]
Does the Isotropy of the CMB Imply a Homogeneous Universe ...
We demonstrate that the high isotropy of the Cosmic Microwave Background (CMB), combined with the Copernican principle, is not sufficient to prove homogeneity ...
[20]
[astro-ph/9804062] The Large-Scale Smoothness of the Universe
New measurements of galaxy clustering and background radiations provide improved constraints on the isotropy and homogeneity of the Universe on large scales.<|control11|><|separator|>
[21]
Testing cosmic homogeneity and isotropy using galaxy correlations
May 29, 2014 · Unlike previous tests, the tests described here compare galaxy distributions in equal volumes at the same redshift z.
[22]
[PDF] 4. The Einstein Equations - DAMTP
The force of gravity is mediated by a gravitational field. The glory of general relativity is that this field is identified with a metric gµν(x) on a 4d ...
[23]
TASI Lectures: Introduction to Cosmology - M. Trodden & S.M. Carroll
The universe is spatially homogeneous and isotropic on the largest scales. "Isotropy" is the claim that the universe looks the same in all direction.
[24]
[PDF] 22. Big-Bang Cosmology - Particle Data Group
Dec 1, 2023 · Together, homogeneity and isotropy allow us to extend the Copernican Principle to the Cosmological Principle, stating that all spatial positions ...
[25]
The Cosmological Constant - Sean M. Carroll
Einstein therefore proposed a modification of his equations, to Equation 7 (7) where Lambda is a new free parameter, the cosmological constant.
[26]
100 years of mathematical cosmology: Models, theories, and ...
On 8 February 1917, Einstein announced the first application of general relativity to the universe considered as a whole, the Einstein static universe [8]. It ...
[27]
[PDF] 1935Ap J 82. . 2 8 4R KINEMATICS AND WORLD-STRUCTURE
KINEMATICS AND WORLD-STRUCTURE. By H. P. ROBERTSON. ABSTRACT. The idealized cosmological problem, in which the nebulae are considered as particles in.
[28]
[PDF] 1935MNRAS..95..263W I935 Jan- Milne's Kinematical System and ...
cates that each fundamental particle is a centre of spherical symmetry, whence the 4-space must exhibit spherical symmetry about each world-line. We are ...
[29]
Über die Krümmung des Raumes | Zeitschrift für Physik A Hadrons ...
Über die Krümmung des Raumes. Published: December 1922. Volume 10, pages 377–386, (1922); Cite this article. Download PDF · Zeitschrift für Physik. Über die ...
[30]
[PDF] A homogeneous universe of constant mass and increasing radius ...
Jun 13, 2013 · Original paper: Georges Lemaître, Un univers homogène de masse constante et de rayon croissant, rendant compte de la vitesse radiale des ...
[31]
[1807.06209] Planck 2018 results. VI. Cosmological parameters - arXiv
Jul 17, 2018 · Abstract:We present cosmological parameter results from the final full-mission Planck measurements of the CMB anisotropies.
[32]
[PDF] 10 Homogeneous, Isotropic Cosmology - JILA
Universes satisfying the cosmological principle are described by the Friedmann-Lemaıtre-Robertson-Walker. (FLRW) metric, equation (10.26) below, discovered ...Missing: continuity | Show results with:continuity
[33]
Hubble Constant - Nasa Lambda
Current values in the literature hover near 70 km/s/Mpc. However, a concordance value with associated uncertainty 1% or less has yet to be reached, and ...
[34]
[PDF] 1 Robertson-Walker metric 2 Kinematics of RW metric
simple conservation law leads to a straightforward derivation of ρ(t) once the equation of state p(ρ) ... expansion rate, or speed, measure by the Hubble constant ...<|control11|><|separator|>
[35]
[PDF] 1 Cosmological principle 2 FRW metric - Caltech (Tapir)
The function H(t) is called the Hubble parameter or Hubble rate or Hubble. “constant.” (Describes rate of expansion.) • The function a(t) is called the scale ...
[36]
Cosmic History - NASA Science
Oct 22, 2024 · Around 13.8 billion years ago, the universe expanded faster than the speed of light for a fraction of a second, a period called cosmic inflation.Missing: principle CMB<|separator|>
[37]
[1411.0172] Ralph A. Alpher, George Antonovich Gamow, and the ...
Nov 1, 2014 · Abstract:The first prediction of the existence of "relict radiation" or radiation remaining from the "Big Bang" was made in 1948.
[38]
Big Bang Nucleosynthesis and the Observed Abundances of Light ...
Sep 19, 1996 · The predictions of Standard Big Bang Nucleosynthesis are summarized and compared with observations of abundances of helium in HII regions.
[39]
The Cosmic Microwave Background Radiation - E. Gawiser & J. Silk
The Cosmic Microwave Background (CMB) is radiation released during the decoupling era, observed today as microwave radiation from 15 billion light years away.
[40]
[astro-ph/9609105] The Sachs-Wolfe Effect - arXiv
Sep 16, 1996 · We present a pedagogical derivation of the Sachs-Wolfe effect, specifically the factor 1/3 relating the temperature fluctuations to gravitational potentials.
[41]
[PDF] Probing the Large-Scale Homogeneity of the Universe with Galaxy ...
Mar 19, 2007 · First results from the 2dF Galaxy Redshift Survey. In G. Efstathiou, editor, Large-Scale Structure in the Universe, 1999. 84. Page 85 ...
[42]
Testing homogeneity on large scales in the Sloan Digital Sky Survey ...
Our finding that the galaxy distribution is homogeneous on scales larger than 60–70 h−1 Mpc is consistent with the size of the largest statistically significant ...
[43]
Testing homogeneity in the Sloan Digital Sky Survey Data Release ...
Homogeneity and isotropy on sufficiently large scales is an assumption which is fundamental to our current understanding of the Universe. This assumption which ...Abstract · INTRODUCTION · METHOD OF ANALYSIS · DATA
[44]
COSMOLOGICAL DENSITY FLUCTUATIONS ON 100 Mpc SCALES ...
Density fluctuations on 100 h −1 Mpc scales produce hot and cold spots with ΔT ≈ 10 μK on the cosmic microwave background.
[45]
Euclid's first images: the dazzling edge of darkness - ESA
Nov 7, 2023 · These five images illustrate Euclid's full potential; they show that the telescope is ready to create the most extensive 3D map of the Universe yet.Missing: homogeneity | Show results with:homogeneity
[46]
First Results from DESI Make the Most Precise Measurement of Our ...
Apr 4, 2024 · Researchers have used the Dark Energy Spectroscopic Instrument to make the largest 3D map of our universe and world-leading measurements of dark energy.Missing: flat 2020s
[47]
The Challenge of the Largest Structures in the Universe to Cosmology
Sep 25, 2012 · Abstract:Large galaxy redshift surveys have long been used to constrain cosmological models and structure formation scenarios.
[48]
A structure in the early Universe at z ∼ 1.3 that exceeds the ...
Jan 7, 2013 · Note that the scale of ∼370 Mpc is much larger than the scales of ∼100–115 Mpc for homogeneity deduced by Scrimgeour et al. (2012), and, for our ...
[49]
[2402.07591] A Big Ring on the Sky - arXiv
Feb 12, 2024 · "A Big Ring on the Sky" (BR) is a circular, annulus-like, ultra-large structure of diameter ~400 Mpc, discovered in MgII-absorber catalogues.
[50]
[PDF] Super-Large-Scale Structures in the Sloan Digital Sky Survey ∗
The Sloan. Great Wall, located at a median redshift of z = 0.07804, has a total length of about. 433Mpc and a mean galaxy density of about six times that of the ...
[51]
Fractal dimension as a measure of the scale of homogeneity
The correlation dimension D2 of the distribution of points can be defined via the power-law scaling of the correlation integral, i.e. formula ⁠,. formula. 5.
[52]
Fractal Dimension as a measure of the scale of Homogeneity - arXiv
Jan 5, 2010 · In this paper we use the relation between the fractal dimensions and the correlation function to compute the dispersion for any given model in ...
[53]
CLUSTERING OF SLOAN DIGITAL SKY SURVEY III ...
In this paper, we measure the angular clustering using an optimal quadratic estimator at four redshift slices with an accuracy of ∼15%, with a bin size of δl = ...
[54]
An Independent Measure of the Kinematic Dipole from SDSS
Nov 8, 2024 · Currently, it suggests that the kinematic dipole appears consistent with the CMB, implying that any observed dipolar anisotropy in number ...
[55]
Searching for a preferred direction with Union2.1 data
Nov 28, 2013 · A cosmological preferred direction was reported from the Type Ia supernovae data in recent years. We use the Union2.1 data to give a simple ...
[56]
Cosmic radio dipole from NVSS and WENSS
We use linear estimators to determine the magnitude and direction of the cosmic radio dipole from the NRAO VLA Sky Survey (NVSS) and the Westerbork Northern ...Missing: axis | Show results with:axis
[57]
CMB low multipole alignments in the ΛCDM and dipolar models
Focusing on the low ℓ alignments and assuming ΛCDM, we confirm that the quadrupole/octupole and the dipole/quadrupole/octupole alignments are anomalous with a ...Missing: anomalously | Show results with:anomalously
[58]
Planck 2018 results - I. Overview and the cosmological legacy of ...
This paper presents the cosmological legacy of Planck, which currently provides our strongest constraints on the parameters of the standard ...Missing: Omega_m | Show results with:Omega_m
[59]
[PDF] Karl Popper and physical cosmology - PhilSci-Archive
“The most philosophically of all the sciences”: Karl Popper and physical cosmology. Helge Kragh. Centre for Science Studies, Institute of Physics and ...
[60]
Fine-Tuning - Stanford Encyclopedia of Philosophy
Aug 22, 2017 · Fine-tuning refers to sensitive dependences of facts on parameter values, like how the universe's laws and constants are fine-tuned for life.
[61]
Initial conditions problem in cosmological inflation revisited
Aug 10, 2023 · The results provide support for the argument that inflation does not solve the homogeneity and isotropy problem beginning from generic initial conditions ...
[62]
Measuring the homogeneity of the quantum universe | Phys. Rev. D
We illustrate the viability of the quantum homogeneity measures by a nontrivial application to two-dimensional Lorentzian quantum gravity formulated in terms of ...
[63]
Limitations of Big Bang cosmology and the Λ-CDM ... - UNLV Physics
The observed homogeneity and isotropy of the observable universe (as an axiom called the cosmological principle) shows that the universe beyond the ...<|control11|><|separator|>
[64]
Gravitational Energy as Dark Energy: the Timescape Cosmology
Dark energy is not the internal energy of a mysterious fluid, but a misidentification of those aspects of cosmological gravitational energy.<|control11|><|separator|>
[65]
Lemaitre-Tolman-Bondi model and accelerating expansion
**Summary of Key Points on LTB Models Explaining Accelerating Expansion Without Lambda:**
[66]
Testing LTB void models without the cosmic microwave background ...
Feb 27, 2013 · Abstract. We present new observational constraints on inhomogeneous models based on observables independent of the CMB and large-scale structure ...
[67]
Probing spatial homogeneity with LTB models: a detailed discussion
We show that current data provide no evidence for deviations from spatial homogeneity on large scales. More accurate constraints are required to ultimately ...
[68]
The quasi-steady-state cosmology - ScienceDirect.com
This paper outlines an alternative cosmology called the quasi-steady-state cosmology (QSSC) which was proposed in 1993 as a rival to the standard big bang ...