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Distance measure

In cosmology, distance measures quantify the separation between astronomical objects, accounting for the expansion of the universe, which complicates direct application of Euclidean geometry. Unlike static spaces, the universe's expansion—described by the Friedmann–Lemaître–Robertson–Walker (FLRW) metric—means that light from distant objects travels through an evolving geometry, leading to multiple specialized distance definitions based on observables like redshift, angular size, and flux.^[1] These measures arose historically from efforts to interpret observations of galaxies and supernovae. Early work by Edwin Hubble in the 1920s established the linear velocity-distance relation (Hubble's law), but as cosmology developed in the mid-20th century with general relativity and the Big Bang model, theorists like Weinberg (1972) and Peebles (1993) formalized distances incorporating curvature and dark energy. Today, they are crucial for mapping cosmic structure, testing models like ΛCDM, and measuring parameters such as the Hubble constant.^[1] Key line-of-sight measures include the comoving distance (invariant for expanding objects) and proper distance (at a given epoch), while transverse measures encompass angular diameter distance (relating physical to observed angular size) and luminosity distance (relating intrinsic luminosity to observed brightness). These are interconnected via the scale factor and redshift z, where $1 + z = 1/a(t) with a(t) the scale factor, and obey Etherington's reciprocity relation in smooth spacetimes. Later sections detail these in the FLRW framework, corrections for peculiar velocities, and their observational applications.^[1]

Introduction

Definition and context

In cosmology, the conventional Euclidean distance, which assumes a static, flat geometry, fails to accurately describe separations between objects in a curved and expanding spacetime governed by general relativity, as the distances between comoving objects continuously evolve due to cosmic expansion.^[2] This necessitates multiple specialized distance measures, each derived from distinct observables such as the observed flux of radiation, the angular diameter of celestial objects, and time delays in propagating signals, to infer physical separations in an evolving universe.^[2] A distance measure is formally defined as a function that connects the redshift z—a key indicator of cosmic expansion—to the effective physical distance between sources in Friedmann-Lemaître-Robertson-Walker (FLRW) models, which parameterize the universe's large-scale geometry.^[2] These models assume the universe is homogeneous, meaning any measurable property remains uniform when averaged over sufficiently large scales, and isotropic, appearing the same in all directions from any vantage point, collectively known as the cosmological principle.^[3] Underpinning this framework is general relativity, which provides the gravitational dynamics for the expansion.^[2] Redshift z acts as a primary proxy for distance, encoding the cumulative expansion along the line of sight.^[2] For example, in a flat, non-expanding Euclidean space, all distance measures reduce to a single invariant quantity, but in cosmology, expansion causes them to diverge, reflecting the dynamic interplay of geometry and evolution.^[2]

Historical development

The concept of distance measures in cosmology emerged in the early 20th century alongside the recognition of the universe's expansion. In 1929, Edwin Hubble published observations demonstrating a linear relationship between the radial velocities of galaxies and their distances, establishing the foundation for initial distance estimates based on recession velocities. This discovery, derived from spectroscopic data of 24 extra-galactic nebulae, implied an expanding universe and provided the first empirical framework for scaling cosmic distances beyond the Milky Way. During the 1930s, the theoretical underpinnings advanced with the independent work of Howard Robertson and Arthur Walker, who formalized the Friedmann-Lemaître-Robertson-Walker (FLRW) metric, introducing comoving coordinates to describe distances in an expanding, homogeneous, and isotropic universe. These coordinates, which remain fixed relative to the cosmic rest frame while physical distances scale with the universe's expansion, enabled consistent distance calculations across different epochs. Concurrently, concepts like angular diameter distance were formalized in early relativistic cosmological models, initially explored in kinematic frameworks of the era, and later adapted to the Big Bang paradigm following its acceptance in the 1940s and 1950s. In the 1940s, Walter Baade and Rudolf Minkowski advanced practical distance measurements by classifying supernovae into Type I and II based on spectral observations, leveraging their luminosities as standard candles to introduce luminosity distance estimates for distant galaxies. In 1998, observations of Type Ia supernovae by the High-Z Supernova Search Team and Supernova Cosmology Project revealed that the universe's expansion is accelerating, using luminosity distances to provide evidence for dark energy and refining cosmological parameters.^[4] The late 20th century saw distance measures integrated with cosmic microwave background (CMB) observations, providing geometric constraints on cosmology. The Cosmic Background Explorer (COBE) mission in 1992 detected CMB temperature anisotropies, providing initial constraints on cosmic geometry. Subsequent ground-based and satellite experiments in the late 1990s and 2000s offered the first precise measurements of the angular diameter distance to the last scattering surface at redshift z ≈ 1100, which refined models of cosmic expansion. Subsequent Planck satellite data from 2013 to 2018 further tightened these constraints, yielding a Hubble constant of 67.4 ± 0.5 km/s/Mpc and highlighting the Hubble tension—a discrepancy between CMB-inferred values and local measurements around 73 km/s/Mpc.^[5] By the 2020s, James Webb Space Telescope (JWST) observations of high-redshift (high-z) galaxies and supernovae have refined distance measures at z > 10, revealing unexpectedly luminous early galaxies that challenge pre-2020 dark energy models and suggest possible modifications to the cosmological constant or equation of state. These data, including detections up to z ≈ 14, have addressed gaps in high-z distance ladders, enhancing precision in luminosity and angular diameter distances while probing dark energy dynamics.^[6]

Cosmological Foundations

FLRW metric and expansion

The Friedmann–Lemaître–Robertson–Walker (FLRW) metric provides the mathematical framework for describing a homogeneous and isotropic universe in general relativity, serving as the foundation for modern cosmological distance measures. This metric arises from the cosmological principle, which posits that the universe is homogeneous (uniform on large scales) and isotropic (appearing the same in all directions from any point), implying a spacetime symmetry that constrains the possible forms of the metric tensor. To derive it, consider a coordinate system adapted to comoving observers—those at rest relative to the expanding cosmic background—where the spatial coordinates remain fixed while the proper distances between them evolve with time. The line element in such a spacetime takes the general form ds^2 = -c^2 dt^2 + g_{ij} dx^i dx^j, with the spatial part g_{ij} reflecting isotropy and homogeneity. For isotropy around a point, the spatial metric must be that of a three-dimensional hypersurface of constant curvature, leading to the form dl^2 = \frac{dr^2}{1 - k r^2} + r^2 (d\theta^2 + \sin^2\theta d\phi^2), where r is a comoving radial coordinate, d\Omega^2 = d\theta^2 + \sin^2\theta d\phi^2 is the metric on the unit sphere, and k is the curvature parameter (with k = +1, 0, -1 corresponding to closed, flat, and open geometries, respectively, up to a normalization of the curvature radius). Allowing for time-dependent expansion, the full metric becomes ds^2 = -c^2 dt^2 + a(t)^2 \left[ \frac{dr^2}{1 - k r^2} + r^2 d\Omega^2 \right], where a(t) is the dimensionless scale factor that encodes the universe's expansion history, normalized such that a(t_0) = 1 today.^[7] The scale factor a(t) drives the expansion of the universe, quantified by the Hubble parameter H(t) = \frac{\dot{a}(t)}{a(t)}, which measures the fractional rate of change of distances at time t. This parameter relates the dynamics of the universe to its energy content through the Friedmann equations, derived by applying Einstein's field equations to the FLRW metric. The first Friedmann equation is 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 \rho is the total energy density (including matter, radiation, and dark energy), G is Newton's constant, \Lambda is the cosmological constant, and the curvature term -\frac{k c^2}{a^2} reflects the geometry's influence on expansion. The second Friedmann equation, \frac{\ddot{a}}{a} = -\frac{4\pi G}{3} \left( \rho + \frac{3p}{c^2} \right) + \frac{\Lambda c^2}{3}, governs acceleration, with p as pressure; for matter-dominated eras (p = 0), expansion decelerates, while dark energy (p = -\rho c^2) drives late-time acceleration. These equations link H(t) directly to the densities of components: matter \rho_m \propto a^{-3}, radiation \rho_r \propto a^{-4}, and dark energy \rho_\Lambda constant in the standard model.^[7]^[8] The curvature parameter k plays a crucial role in distance calculations by determining the global geometry: positive k = +1 implies a closed, finite universe; k = 0 a flat, infinite one; and k = -1 an open, hyperbolic space. In the standard \LambdaCDM model, observations favor a spatially flat universe (k = 0), where the curvature density parameter \Omega_k = -\frac{k c^2}{H_0^2 a^2} \approx 0, as evidenced by cosmic microwave background anisotropies and large-scale structure data. This flatness simplifies distance measures, assuming Euclidean geometry on large scales, though non-zero k would introduce corrections scaling with redshift.^[7] For light propagation, which underlies astronomical distance measures, photons follow null geodesics (ds = 0) in the FLRW metric. Setting ds = 0 and assuming radial motion (d\Omega = 0), the geodesic equation simplifies to c dt = \pm a(t) \frac{dr}{\sqrt{1 - k r^2}}. Integrating along the past light cone from emission at t_e to observation at t_0, this yields the comoving distance in terms of conformal time \eta, defined as d\eta = \frac{c dt}{a(t)} or \eta = \int_{t_e}^{t_0} \frac{c dt}{a(t)}, which rescales the metric to a conformally static form ds^2 = a(\eta)^2 (-c^2 d\eta^2 + d\chi^2 + \sinh^2(\sqrt{|k|} \chi) d\Omega^2 ) (adjusted for curvature), facilitating solutions for photon paths.^[7]

Redshift and scale factor

In cosmology, the redshift z quantifies the stretching of photon wavelengths due to the universe's expansion, defined as $1 + z = \frac{\lambda_\mathrm{obs}}{\lambda_\mathrm{emit}}, where \lambda_\mathrm{obs} is the observed wavelength and \lambda_\mathrm{emit} is the emitted wavelength.^[9] This cosmological redshift relates directly to the cosmic scale factor a(t), normalized such that a(t_0) = 1 today, via $1 + z = \frac{a(t_0)}{a(t_e)} = \frac{1}{a(t_e)}, where t_e is the emission time.^[9] This relation arises because the expansion stretches the wavelength proportionally to the increase in the scale factor between emission and observation.^[10] Redshift phenomena include three main types: Doppler redshift from relative peculiar motions of objects, gravitational redshift from differences in gravitational potential, and cosmological redshift from the overall expansion of space.^[11] In the context of large-scale cosmology, gravitational effects are typically negligible compared to expansion, and peculiar velocities contribute only small corrections at low redshifts, making cosmological redshift the primary mechanism for observed shifts in distant galaxies and quasars.^[11] The Doppler component, while important for local motions, diminishes in significance over cosmological distances where expansion dominates.^[12] The connection between redshift and recession velocity is approximated at low z (z \ll [1](/page/1)) by v \approx c z, forming the basis of Hubble's law, which links velocity to distance via the Hubble parameter.^[13] For higher redshifts, this non-relativistic approximation fails as recession speeds can exceed c without violating special relativity, since the expansion is a coordinate effect in the Friedmann-Lemaître-Robertson-Walker (FLRW) framework; the full relation requires integrating the scale factor's evolution over the expansion history.^[14] This integral form accounts for the cumulative stretching along the photon's path, providing a more accurate velocity interpretation for distant objects.^[14] Cosmological redshifts are measured primarily through spectroscopy, identifying shifts in atomic emission or absorption lines such as the Lyman-\alpha line at rest wavelength 121.6 nm, which appears at observed wavelengths \lambda_\mathrm{obs} = 121.6 (1 + [z](/page/Z)) nm.^[15] High-resolution spectra from quasars and galaxies allow precise z determination, enabling mapping of the large-scale structure.^[15] For the cosmic microwave background (CMB), the blackbody temperature scales inversely with the scale factor as T(z) = T_0 (1 + [z](/page/Z)), where T_0 \approx 2.725 K today, providing an independent redshift probe at z \approx 1100.^[16] The observed redshift z is essential for distance measures, as it fixes the lookback time—the elapsed time since emission—through integration over the expansion rate H(z), and encodes the cumulative expansion history needed to compute distances in the FLRW model.^[9] Without knowledge of z, the scale factor at emission cannot be inferred, rendering subsequent distance calculations impossible.^[10]

Line-of-Sight Distance Measures

Comoving distance

The comoving distance, often denoted as \chi(z), represents the line-of-sight separation between two events in comoving coordinates, which remains invariant under the cosmic expansion. It is defined as the integral along the photon's path in an expanding universe, given by

\chi(z) = \int_0^z \frac{c \, dz'}{H(z')},

where c is the speed of light and H(z) is the Hubble parameter at redshift z'. This distance corresponds to the proper distance that two comoving objects (those moving solely with the Hubble flow) would have today if extrapolated backward without accounting for expansion effects. In a flat \LambdaCDM universe, the Hubble parameter takes the form

H(z) = H_0 \sqrt{\Omega_m (1+z)^3 + \Omega_\Lambda},

where H_0 is the present-day Hubble constant, \Omega_m is the present-day matter density parameter, and \Omega_\Lambda is the present-day dark energy density parameter (with \Omega_m + \Omega_\Lambda = 1 for flatness). Substituting this into the integral yields the specific expression for \chi(z) in this model. Galaxies or other structures at fixed comoving distance \chi maintain constant separation in these coordinates over cosmic time, providing a fixed "grid" for mapping the large-scale structure of the universe. For universes with nonzero spatial curvature (k \neq 0), the comoving distance \chi(z) is still computed via the same integral form, but H(z) now includes a curvature term:

H(z) = H_0 \sqrt{\Omega_m (1+z)^3 + \Omega_k (1+z)^2 + \Omega_\Lambda},

where \Omega_k = -k c^2 / (H_0^2 a_0^2) measures the curvature (k > 0 for closed, k < 0 for open, and a_0 = 1 today). In the general Friedmann-Lemaître-Robertson-Walker (FLRW) metric, the line-of-sight proper distance at any epoch is a(t) \chi, but the comoving \chi itself absorbs the expansion history. While the radial \chi remains the integral, the full spatial separation in curved geometries involves curvature-dependent functions applied to \chi, such as the sk(\chi) term in the metric (sinh for open and sin for closed universes). This measure serves as the foundation for computing comoving volume elements in cosmological surveys, where the differential volume is dV_c = \chi^2 \, d\chi \, d\Omega in flat space, enabling the estimation of galaxy number densities and clustering statistics. It is particularly crucial in baryon acoustic oscillation (BAO) analyses, where the comoving sound horizon scale at recombination (\sim 150 \, \mathrm{Mpc}) acts as a standard ruler; by measuring the observed angular or redshift separation of this feature, surveys infer \chi(z) and constrain cosmological parameters like H_0 and \Omega_m.^[17]

Proper distance

The proper distance, denoted d_p(z), is the physical distance between an observer and an object at redshift z, measured at a fixed cosmic time—specifically, the present epoch—along a radial line in the Friedmann-Lemaître-Robertson-Walker (FLRW) metric.^[2] It corresponds to the length that would be measured by a set of rigidly held rods at the current scale factor a(t_0) = 1.^[18] In a flat universe, the formula is d_p(z) = \chi(z), where \chi(z) is the comoving distance given by the integral \chi(z) = \int_0^z \frac{c \, dz'}{H(z')}, with H(z) = H_0 \sqrt{\Omega_m (1+z')^3 + \Omega_\Lambda} for a flat \LambdaCDM model (assuming \Omega_k = 0).^[2] This measure distinguishes itself from the comoving distance by incorporating the expansion up to the present day, yielding the current physical separation rather than a time-independent coordinate.^[18] At the object's emission time t_e, the proper distance scales as d_p(t_e) = a(t_e) \chi(z) = \frac{\chi(z)}{1+z}, highlighting how physical rulers were shorter in the past due to the smaller scale factor.^[2] The comoving distance \chi(z) forms the foundational integral, equivalent to \int_{t_e}^{t_0} \frac{c \, dt}{a(t)}, which proper distance at present directly adopts since a(t_0) = 1.^[18] Proper distance finds key applications in galaxy clustering analyses, where it quantifies the present-day physical scales of overdensities and voids, enabling tests of structure growth models against observations like the two-point correlation function in proper coordinates. For nearby objects (z \ll 1), it supports proper motion distance estimates, linking observed angular displacements to transverse peculiar velocities, as in kinematic studies of extragalactic jets.^[2]

Light-travel distance

The light-travel distance d_{LT}(z) to a source at redshift z is defined as d_{LT}(z) = \int_0^z \frac{c \, dz'}{H(z') (1 + z')}, where c is the speed of light and H(z) is the Hubble parameter as a function of redshift.^[2] This distance measure represents the path length traversed by the light ray from the source to the observer, accounting for the cosmic expansion during transit; it is equal to c times the lookback time, the coordinate time interval between emission and observation.^[2] Unlike the proper distance d_p(z), which is the physical separation at the current epoch and given by d_p(z) = \int_0^z \frac{c \, dz'}{H(z')}, the light-travel distance incorporates the varying scale factor along the light's path, resulting in d_{LT}(z) < d_p(z) for z > 0 in an expanding universe.^[2] The light-travel distance finds applications in estimating the age of the universe, obtained as the limit d_{LT}(\infty)/c, which integrates the cosmic history from the Big Bang to the present.^[2] It also informs the timing of supernova light curves, where the observed duration is stretched by a factor of (1 + z) due to time dilation, allowing models to align emission events with the lookback time derived from d_{LT}(z).

Transverse Distance Measures

Transverse comoving distance

The transverse comoving distance, denoted d_M(z), measures the proper distance between two points at redshift z that are separated by a small angular displacement perpendicular to the line of sight, in a coordinate system that expands with the universe's Hubble flow.^[2] It generalizes the line-of-sight comoving distance to transverse directions, remaining fixed over cosmic time for objects comoving with the expansion.^[2] In a flat universe, d_M(z) equals the line-of-sight comoving distance \chi(z) = \int_0^z \frac{c \, dz'}{H(z')}, where c is the speed of light and H(z) is the Hubble parameter at redshift z'.^[2] For curved universes, curvature modifies this relation to account for the geometry of space. The general expression is

d_M(z) = \frac{c}{H_0 \sqrt{|\Omega_k|}} \sinh\left( \sqrt{|\Omega_k|} \int_0^z \frac{H_0 \, dz'}{H(z')} \right)

for an open universe (\Omega_k > 0), where H_0 is the present-day Hubble constant and \Omega_k is the curvature density parameter; the hyperbolic sine is replaced by the sine function for a closed universe (\Omega_k < 0).^[2] In the flat-space limit (\Omega_k = [0](/page/0)), this reduces to \chi(z).^[2] This distance plays a crucial role in interpreting observations of angular scales in the large-scale structure of the universe, such as the angular size of baryon acoustic oscillations (BAO) in galaxy surveys, where it relates observed angular separations to comoving scales.^[2] It is also essential for gravitational lensing calculations, providing the transverse separation needed to compute deflection angles and magnification effects between lens and source.^[2] At high redshifts, the effects of spatial curvature become pronounced, altering the transverse separation: in hyperbolic (open) geometries, distances grow more rapidly than in flat space, while in spherical (closed) geometries, they are compressed due to the positive curvature.^[2] These deviations allow constraints on \Omega_k from transverse measurements, complementing radial probes.^[2]

Angular diameter distance

The angular diameter distance, denoted d_A(z), relates the physical transverse size l of an object at redshift z to its observed angular size \theta (in radians) via the relation \theta = l / d_A(z) for small angles.^[19] This measure is essential for interpreting the apparent sizes of cosmological objects as affected by the universe's expansion.^[19] In the Friedmann–Lemaître–Robertson–Walker (FLRW) metric, the line element for transverse separations is ds^2 = a^2(t_e) \left[ d\chi^2 + f_K(\chi)^2 d\Omega^2 \right], where a(t_e) = 1/(1+[z](/page/Z)) is the scale factor at emission time t_e, \chi is the radial comoving coordinate, and f_K(\chi) accounts for spatial curvature (with f_K(\chi) = \chi in a flat universe). For a small angular separation d\theta, the proper transverse size at emission is l = a(t_e) f_K(\chi) d\theta, leading to d_A(z) = l / d\theta = a(t_e) f_K(\chi). Since the transverse comoving distance is d_M(z) = f_K(\chi), the angular diameter distance follows as

d_A(z) = \frac{d_M(z)}{1 + [z](/page/Z)}.

^[19] The factor of (1+[z](/page/Z))^{-1} arises from the scale factor at emission, which diminishes the proper size relative to the comoving frame due to expansion.^[19] Physically, d_A(z) incorporates the effects of cosmic expansion on angular appearances, causing distant objects to subtend larger angles than in a static universe beyond a certain redshift. In decelerating models like Einstein–de Sitter, d_A(z) increases with z up to a maximum around z \approx 1.25, then decreases at higher redshifts; in accelerating \LambdaCDM universes dominated by dark energy, the maximum shifts to around z \approx 1.6, with a slower decrease thereafter.^[19]^[20]^[21] This shift in the maximum provides a geometric probe of acceleration.^[19] Applications of d_A(z) include measuring galaxy physical sizes from their angular extents, such as in surveys of disk galaxies to test expansion history.^[19] In the cosmic microwave background (CMB), d_A(z_\star) to the last scattering surface at z_\star \approx 1100 determines the angular scale of acoustic peaks in the power spectrum, with the first peak at \ell \approx 220 constraining curvature and dark energy.^[22] Gravitational lensing arcs also rely on d_A(z) ratios between lens and source redshifts to infer mass distributions and distances.^[19]

Luminosity distance

The luminosity distance d_L(z), denoted as a function of redshift z, quantifies the effective distance to a source based on its observed brightness in an expanding universe. It is defined such that the bolometric flux F received from a source with intrinsic bolometric luminosity L satisfies the relation

F = \frac{L}{4\pi d_L^2(z)},

where the flux is integrated over all frequencies.^[19] In the standard Friedmann-Lemaître-Robertson-Walker (FLRW) cosmology, for a flat universe, d_L(z) = (1 + z) d_M(z), with d_M(z) being the transverse comoving distance.^[19] This definition incorporates the effects of cosmic expansion on photon propagation. The additional factor of (1 + [z](/page/Z)) relative to d_M(z) stems from two redshift-dependent phenomena: the energy loss of each photon, which decreases its observed energy by a factor of $1/(1 + [z](/page/Z)) due to the stretching of wavelengths, and the time dilation of the source's emission, which dilutes the photon arrival rate by another factor of $1/(1 + [z](/page/Z)).^[23] Together, these yield an overall dimming effect of (1 + [z](/page/Z))^2 compared to a static-space inverse-square law, making d_L(z) larger than the angular diameter distance by precisely that factor, as per Etherington's distance duality relation.^[19] Type Ia supernovae (SNe Ia) are widely used as standard candles for luminosity distance measurements because their peak absolute magnitudes are empirically uniform after corrections for light-curve shape and host-galaxy properties, enabling reliable inference of d_L(z) from observed peak fluxes.^[24] These observations have mapped the universe's expansion history, revealing deviations from a decelerating model. In particular, analyses of high-redshift SNe Ia in 1998 by the Supernova Cosmology Project (led by Perlmutter et al.) and the High-Z Supernova Search Team (led by Riess et al.) demonstrated that luminosity distances at z \approx 0.5 were larger than expected in a matter-dominated universe, providing the first observational evidence for an accelerating expansion driven by dark energy.^[24] Contemporary applications of SNe Ia luminosity distances contribute to the Hubble tension, a discrepancy in the Hubble constant H_0. Local measurements, calibrated via Cepheid variables and extending to SNe Ia at low redshifts (z < 0.1), yield H_0 \approx 73 km/s/Mpc, while cosmic microwave background (CMB) inferences from high-redshift physics give H_0 \approx 67 km/s/Mpc, highlighting potential tensions in the standard cosmological model.^[25]

Relations and Corrections

Etherington's distance duality

Etherington's distance duality, also known as the reciprocity theorem, establishes a fundamental relation between the luminosity distance d_L(z) and the angular diameter distance d_A(z) at redshift z, given by

d_L(z) = d_A(z) (1 + z)^2.

This equation arises from the conservation of photon number and the geometry of light propagation in an expanding universe, as originally derived by Etherington in 1933 within the framework of general relativity applied to cosmology. The relation links the observed flux from a source, which defines d_L, to the apparent angular size of an object, which defines d_A, through the redshift factor accounting for cosmological expansion. The proof of this duality follows from the consistency of surface areas and photon fluxes in the spacetime metric. In a Friedmann-Lemaître-Robertson-Walker (FLRW) metric, the infinitesimal solid angle subtended by a source corresponds to a physical area at the source, while the bolometric flux received is diluted by the expansion-induced redshift in energy and time dilation. Equating these via the inverse square law for both area and flux yields the (1 + z)^2 factor, assuming null geodesics for photon paths and no absorption or scattering. This holds more generally in any metric theory of gravity where photons propagate without birefringence, meaning the speed of light is the same for all polarizations, independent of the specific dynamics like the Einstein field equations. Observational tests of the duality have utilized multiple probes to verify consistency. Type Ia supernovae provide d_L(z) measurements up to z \approx 2, while angular diameter distances from radio quasars or galaxy cluster Sunyaev-Zel'dovich effects extend to similar ranges; combined analyses confirm the relation to within 1-2% precision. Cosmic microwave background (CMB) anisotropies, which fix d_A(z) through acoustic peak positions at recombination (z \approx 1100), align with supernova-derived d_L when the duality is imposed, supporting standard \LambdaCDM cosmology. Any violation, parametrized as \eta(z) = d_L(z) / [d_A(z) (1 + z)^2] \neq 1, would signal new physics, such as theories with varying speed of light or non-metric gravity effects, though current data show no significant deviations at the percent level. The duality unifies transverse distance measures by enabling the interconversion of d_L and d_A, facilitating robust cosmological parameter estimation across datasets. It assumes a homogeneous and isotropic universe on large scales; in inhomogeneous models, such as those with significant local voids or structures, the relation can break down, leading to direction-dependent distances that require generalized frameworks beyond the standard FLRW approximation.

Peculiar velocity

In cosmology, peculiar velocity refers to the component of an object's velocity that deviates from the smooth Hubble flow, representing local deviations due to gravitational interactions within the large-scale structure of the universe. These velocities are typically measured relative to the cosmic microwave background (CMB) rest frame, which serves as the reference for the overall expansion. At low redshifts (z \ll 1), peculiar velocities induce a Doppler shift in the observed redshift, approximated as z_D \approx v_{\rm pec}/c, where v_{\rm pec} is the line-of-sight peculiar velocity and c is the speed of light. Peculiar velocities perturb standard distance measures by altering the inferred redshift, leading to errors in quantities like the luminosity distance d_L or angular diameter distance d_A. The relative perturbation is on the order of \delta d / d \sim v_{\rm pec} / [c (1+z)], which becomes significant for nearby objects where the cosmological redshift is small compared to the Doppler contribution.^[26] On larger scales, bulk flows—coherent peculiar motions of galaxy clusters and groups—amplify these effects, with velocities reaching hundreds of km/s in regions like the Local Supercluster or towards the Great Attractor. To mitigate these perturbations, corrections are applied using models of redshift-space distortions, such as the Kaiser effect, which describes the linear enhancement of structure along the line of sight in galaxy surveys due to coherent inflows. The CMB dipole provides a direct measure of our own peculiar velocity relative to the CMB rest frame, estimated at approximately 370 km/s towards galactic coordinates (l, b) \approx (264^\circ, 48^\circ). In the nearby universe (z < 0.1), where peculiar motions dominate over expansion, velocity field reconstructions from surveys like the 2MASS Redshift Survey and the ongoing Cosmicflows program enable precise mapping and correction of these effects up to distances of several hundred Mpc.^[27]^[28] These reconstructions, incorporating data from fundamental plane and Tully-Fisher relations, reveal bulk flows converging towards major structures and support tests of gravity on local scales. Redshift distortions from peculiar velocities, including nonlinear effects, are further analyzed in the context of cosmological foundations to refine distance inferences.^[29]

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[astro-ph/9810142] Cosmology with the Lyman-alpha Forest - arXiv
Oct 8, 1998 · Abstract: We outline the physical picture of the high-redshift Ly-alpha forest that has emerged from cosmological simulations, describe ...
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[PDF] measuring the redshift dependence of the cosmic microwave ...
1999). The adiabatic expansion of the universe and photon number conservation imply that the CMB temperature evolves with redshift as T (z) = T0(1 + z).
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[astro-ph/0501171] Detection of the Baryon Acoustic Peak in ... - arXiv
Jan 10, 2005 · Detection of the Baryon Acoustic Peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies. Authors:D. J. Eisenstein, I. Zehavi ...
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[PDF] Distances in Cosmology - MPA Garching
The reason lies in our definition of proper distance, as the distance between two events measured in a frame of reference where those two events happen at ...
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[PDF] Distance measures in cosmology - arXiv
The transverse comoving distance DM is not a proper distance—it is a proper distance divided by a ratio of scale factors. 5.
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Acoustic Peaks and the Cosmological Parameters
The distance to the surface of last scattering, corresponding to its angular size, is given by what is called the angular diameter distance. It has a simple ...Missing: applications | Show results with:applications
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[PDF] The need for accurate redshifts in supernova cosmology - arXiv
The CMB redshift is used to define a range of integration in equation (2.1), and hence a small change in this value can significantly change the luminosity ...
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[astro-ph/9805201] Observational Evidence from Supernovae for an ...
May 15, 1998 · Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant. Authors:Adam G. Riess, Alexei V. Filippenko, ...Missing: discovery | Show results with:discovery
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Hubble Constant and Tension - NASA Science
Aug 4, 2025 · But measurements derived from studying the CMB provide a Hubble Constant of about 67-68 kilometers per second per megaparsec. Scientists call ...
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On the perturbation of the luminosity distance by peculiar motions
We consider some aspects of the perturbation to the luminosity distance d(z) that are of relevance for SN1a cosmology and for future peculiar velocity surveys ...
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Reconstructed density and velocity fields from the 2MASS Redshift ...
Abstract. We present the reconstructed real-space density and the predicted velocity fields from the Two-Micron All-Sky Redshift Survey (2MRS). The 2MRS is.
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Density and velocity fields using CosmicFlows-4
This article publicly releases 3D reconstructions of the local Universe gravitational field below z = 0.8 that were computed using the CosmicFlows-4 (CF4) ...
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On the perturbation of the luminosity distance by peculiar motions
Nov 24, 2014 · We consider some aspects of the perturbation to the luminosity distance d(z) that are of relevance for SN1a cosmology and for future peculiar velocity surveys.