In physics, redshift happens when light or other electromagnetic radiation from an object moving away from the observer is increased in wavelength, or shifted to the red end of the spectrum. In general, whether or not the radiation is within the visible spectrum, "redder" means an increase in wavelength – equivalent to a lower frequency and a lower photon energy, in accordance with, respectively, the wave and quantum theories of light.
Redshifts are an example of the Doppler effect, familiar in the change in the apparent pitches of sirens and frequency of the sound waves emitted by speeding vehicles. A redshift occurs whenever a light source moves away from an observer. Cosmological redshift is seen due to the expansion of the universe, and sufficiently distant light sources (generally more than a few million light years away) show redshift corresponding to the rate of increase in their distance from Earth. Finally, gravitational redshifts are a relativistic effect observed in electromagnetic radiation moving out of gravitational fields. Conversely, a decrease in wavelength is called blueshift and is generally seen when a lightemitting object moves toward an observer or when electromagnetic radiation moves into a gravitational field.
Although observing redshifts and blueshifts have several terrestrial applications (such as Doppler radar and radar guns),^{[1]} redshifts are most famously seen in the spectroscopic observations of astronomical objects.^{[2]}
A special relativistic redshift formula (and its classical approximation) can be used to calculate the redshift of a nearby object when spacetime is flat. However, many cases such as black holes and Big Bang cosmology require that redshifts be calculated using general relativity.^{[3]} Special relativistic, gravitational, and cosmological redshifts can be understood under the umbrella of frame transformation laws. There exist other physical processes that can lead to a shift in the frequency of electromagnetic radiation, including scattering and optical effects; however, the resulting changes are distinguishable from true redshift and not generally referred to as such (see section on physical optics and radiative transfer).
History
The history of the subject began with the development in the 19th century of wave mechanics and the exploration of phenomena associated with the Doppler effect. The effect is named after Christian Doppler, who offered the first known physical explanation for the phenomenon in 1842.^{[4]} The hypothesis was tested and confirmed for sound waves by the Dutch scientist Christophorus Buys Ballot in 1845.^{[5]} Doppler correctly predicted that the phenomenon should apply to all waves, and in particular suggested that the varying colors of stars could be attributed to their motion with respect to the Earth.^{[6]} Before this was verified, however, it was found that stellar colors were primarily due to a star's temperature, not motion. Only later was Doppler vindicated by verified redshift observations.
The first Doppler redshift was described by French physicist Hippolyte Fizeau in 1848, who pointed to the shift in spectral lines seen in stars as being due to the Doppler effect. The effect is sometimes called the "Doppler–Fizeau effect". In 1868, British astronomer William Huggins was the first to determine the velocity of a star moving away from the Earth by this method.^{[7]} In 1871, optical redshift was confirmed when the phenomenon was observed in Fraunhofer lines using solar rotation, about 0.1 Å in the red.^{[8]}
In 1887, Vogel and Scheiner discovered the annual Doppler effect, the yearly change in the Doppler shift of stars located near the ecliptic due to the orbital velocity of the Earth.^{[9]} In 1901, Aristarkh Belopolsky verified optical redshift in the laboratory using a system of rotating mirrors.^{[10]}
The earliest occurrence of the term "redshift" in print (in this hyphenated form), appears to be by American astronomer Walter S. Adams in 1908, where he mentions "Two methods of investigating that nature of the nebular redshift".^{[11]} The word doesn't appear unhyphenated until about 1934 by Willem de Sitter, perhaps indicating that up to that point its German equivalent, Rotverschiebung, was more commonly used.^{[12]}
Beginning with observations in 1912, Vesto Slipher discovered that most spiral nebulae had considerable redshifts. Slipher first reports on his measurement in the inaugural volume of the Lowell Observatory Bulletin.^{[13]} Three years later, he wrote a review in the journal Popular Astronomy.^{[14]} In it he states, "[...] the early discovery that the great Andromeda spiral had the quite exceptional velocity of –300 km(/s) showed the means then available, capable of investigating not only the spectra of the spirals but their velocities as well."^{[15]} Slipher reported the velocities for 15 spiral nebulae spread across the entire celestial sphere, all but three having observable "positive" (that is recessional) velocities. Subsequently, Edwin Hubble discovered an approximate relationship between the redshifts of such "nebulae" (now known to be galaxies in their own right) and the distances to them with the formulation of his eponymous Hubble's law.^{[16]} These observations corroborated Alexander Friedmann's 1922 work, in which he derived the famous Friedmann equations.^{[17]} They are today considered strong evidence for an expanding universe and the Big Bang theory.^{[18]}
Measurement, characterization, and interpretation
The spectrum of light that comes from a single source (see idealized spectrum illustration topright) can be measured. To determine the redshift, one searches for features in the spectrum such as absorption lines, emission lines, or other variations in light intensity. If found, these features can be compared with known features in the spectrum of various chemical compounds found in experiments where that compound is located on earth. A very common atomic element in space is hydrogen. The spectrum of originally featureless light shone through hydrogen will show a signature spectrum specific to hydrogen that has features at regular intervals. If restricted to absorption lines it would look similar to the illustration (top right). If the same pattern of intervals is seen in an observed spectrum from a distant source but occurring at shifted wavelengths, it can be identified as hydrogen too. If the same spectral line is identified in both spectra but at different wavelengths then the redshift can be calculated using the table below. Determining the redshift of an object in this way requires a frequency or wavelengthrange. In order to calculate the redshift one has to know the wavelength of the emitted light in the rest frame of the source, in other words, the wavelength that would be measured by an observer located adjacent to and comoving with the source. Since in astronomical applications this measurement cannot be done directly, because that would require travelling to the distant star of interest, the method using spectral lines described here is used instead. Redshifts cannot be calculated by looking at unidentified features whose restframe frequency is unknown, or with a spectrum that is featureless or white noise (random fluctuations in a spectrum).^{[20]}
Redshift (and blueshift) may be characterized by the relative difference between the observed and emitted wavelengths (or frequency) of an object. In astronomy, it is customary to refer to this change using a dimensionless quantity called z. If λ represents wavelength and f represents frequency (note, λf = c where c is the speed of light), then z is defined by the equations:^{[21]}
Calculation of redshift, $z$
Based on wavelength 
Based on frequency

$z\; =\; \backslash frac\{\backslash lambda\_\{\backslash mathrm\{obsv\}\}\; \; \backslash lambda\_\{\backslash mathrm\{emit\}\}\}\{\backslash lambda\_\{\backslash mathrm\{emit\}\}\}$

$z\; =\; \backslash frac\{f\_\{\backslash mathrm\{emit\}\}\; \; f\_\{\backslash mathrm\{obsv\}\}\}\{f\_\{\backslash mathrm\{obsv\}\}\}$

$1+z\; =\; \backslash frac\{\backslash lambda\_\{\backslash mathrm\{obsv\}\}\}\{\backslash lambda\_\{\backslash mathrm\{emit\}\}\}$

$1+z\; =\; \backslash frac\{f\_\{\backslash mathrm\{emit\}\}\}\{f\_\{\backslash mathrm\{obsv\}\}\}$

After z is measured, the distinction between redshift and blueshift is simply a matter of whether z is positive or negative. See the formula section below for some basic interpretations that follow when either a redshift or blueshift is observed. For example, Doppler effect blueshifts (z < 0) are associated with objects approaching (moving closer to) the observer with the light shifting to greater energies. Conversely, Doppler effect redshifts (z > 0) are associated with objects receding (moving away) from the observer with the light shifting to lower energies. Likewise, gravitational blueshifts are associated with light emitted from a source residing within a weaker gravitational field as observed from within a stronger gravitational field, while gravitational redshifting implies the opposite conditions.
Redshift formulae
In general relativity one can derive several important specialcase formulae for redshift in certain special spacetime geometries, as summarized in the following table. In all cases the magnitude of the shift (the value of z) is independent of the wavelength.^{[2]}
Redshift Summary
Redshift type 
Geometry 
Formula^{[22]}

Relativistic Doppler 
Minkowski space (flat spacetime) 
$1\; +\; z\; =\; \backslash gamma\; \backslash left(1\; +\; \backslash frac\{v\_\{\backslash parallel\}\}\{c\}\backslash right)$ $z\; \backslash approx\; \backslash frac\{v\_\{\backslash parallel\}\}\{c\}$ for small $v$
$1\; +\; z\; =\; \backslash sqrt\{\backslash frac\{1+\backslash frac\{v\}\{c\}\}\{1\backslash frac\{v\}\{c\}\}\}$ for motion completely in the radial direction.
$1\; +\; z=\backslash frac\{1\}\{\backslash sqrt\{1\backslash frac\{v^2\}\{c^2\}\}\}$ for motion completely in the transverse direction.

Cosmological redshift 
FLRW spacetime (expanding Big Bang universe) 
$1\; +\; z\; =\; \backslash frac\{a\_\{\backslash mathrm\{now\}\}\}\{a\_\{\backslash mathrm\{then\}\}\}$

Gravitational redshift 
any stationary spacetime (e.g. the Schwarzschild geometry) 
$1\; +\; z\; =\; \backslash sqrt\{\backslash frac\{g\_\{tt\}(\backslash text\{receiver\})\}\{g\_\{tt\}(\backslash text\{source\})\}\}$ (for the Schwarzschild geometry, $1\; +\; z\; =\; \backslash sqrt\{\backslash frac\{1\; \; \backslash frac\{2GM\}\{\; c^2\; r\_\{\backslash text\{receiver\}\}\}\}\{1\; \; \backslash frac\{2GM\}\{\; c^2\; r\_\{\backslash text\{source\}\; \}\}\}\}$

Doppler effect
If a source of the light is moving away from an observer, then redshift (z > 0) occurs; if the source moves towards the observer, then blueshift (z < 0) occurs. This is true for all electromagnetic waves and is explained by the Doppler effect. Consequently, this type of redshift is called the Doppler redshift. If the source moves away from the observer with velocity v, which is much less than the speed of light ($v\; \backslash ll\; c$), the redshift is given by
 $z\; \backslash approx\; \backslash frac\{v\}\{c\}$ (since $\backslash gamma\; \backslash approx\; 1$)
where c is the speed of light. In the classical Doppler effect, the frequency of the source is not modified, but the recessional motion causes the illusion of a lower frequency.
A more complete treatment of the Doppler redshift requires considering relativistic effects associated with motion of sources close to the speed of light. A complete derivation of the effect can be found in the article on the relativistic Doppler effect. In brief, objects moving close to the speed of light will experience deviations from the above formula due to the time dilation of special relativity which can be corrected for by introducing the Lorentz factor γ into the classical Doppler formula as follows:
 $1\; +\; z\; =\; \backslash left(1\; +\; \backslash frac\{v\}\{c\}\backslash right)\; \backslash gamma.$
This phenomenon was first observed in a 1938 experiment performed by Herbert E. Ives and G.R. Stilwell, called the Ives–Stilwell experiment.^{[23]}
Since the Lorentz factor is dependent only on the magnitude of the velocity, this causes the redshift associated with the relativistic correction to be independent of the orientation of the source movement. In contrast, the classical part of the formula is dependent on the projection of the movement of the source into the lineofsight which yields different results for different orientations. If θ is the angle between the direction of relative motion and the direction of emission in the observer's frame^{[24]} (zero angle is directly away from the observer), the full form for the relativistic Doppler effect becomes:
 $1+\; z\; =\; \backslash frac\{1\; +\; v\; \backslash cos\; (\backslash theta)/c\}\{\backslash sqrt\{1v^2/c^2\}\}$
and for motion solely in the line of sight (θ = 0°), this equation reduces to:
 $1\; +\; z\; =\; \backslash sqrt\{\backslash frac\{1\; +\; \backslash frac\{v\}\{c\}\}\{1\; \; \backslash frac\{v\}\{c\}\}\}.$
For the special case that the light is approaching at right angles (θ = 90°) to the direction of relative motion in the observer's frame,^{[25]} the relativistic redshift is known as the transverse redshift, and a redshift:
 $1\; +\; z\; =\; \backslash frac\{1\}\{\backslash sqrt\{1v^2/c^2\}\}$
is measured, even though the object is not moving away from the observer. Even when the source is moving towards the observer, if there is a transverse component to the motion then there is some speed at which the dilation just cancels the expected blueshift and at higher speed the approaching source will be redshifted.^{[26]}
Expansion of space
In the early part of the twentieth century, Slipher, Hubble and others made the first measurements of the redshifts and blueshifts of galaxies beyond the Milky Way. They initially interpreted these redshifts and blueshifts as due solely to the Doppler effect, but later Hubble discovered a rough correlation between the increasing redshifts and the increasing distance of galaxies. Theorists almost immediately realized that these observations could be explained by a different mechanism for producing redshifts. Hubble's law of the correlation between redshifts and distances is required by models of cosmology derived from general relativity that have a metric expansion of space.^{[18]} As a result, photons propagating through the expanding space are stretched, creating the cosmological redshift.
There is a distinction between a redshift in cosmological context as compared to that witnessed when nearby objects exhibit a local Dopplereffect redshift. Rather than cosmological redshifts being a consequence of relative velocities, the photons instead increase in wavelength and redshift because of a feature of the spacetime through which they are traveling that causes space to expand.^{[27]} Due to the expansion increasing as distances increase, the distance between two remote galaxies can increase at more than 3×10^{8} m/s, but this does not imply that the galaxies move faster than the speed of light at their present location (which is forbidden by Lorentz covariance).
Mathematical derivation
The observational consequences of this effect can be derived using the equations from general relativity that describe a homogeneous and isotropic universe.
To derive the redshift effect, use the geodesic equation for a light wave, which is
 $ds^2=0=c^2dt^2+\backslash frac\{a^2\; dr^2\}\{1kr^2\}$
where
 $ds^2$ is the spacetime interval
 $dt^2$ is the time interval
 $dr^2$ is the spatial interval
 $c$ is the speed of light
 $a$ is the timedependent cosmic scale factor
 $k$ is the curvature per unit area.
For an observer observing the crest of a light wave at a position $r=0$ and time $t=t\_\backslash mathrm\{now\}$, the crest of the light wave was emitted at a time $t=t\_\backslash mathrm\{then\}$ in the past and a distant position $r=R$. Integrating over the path in both space and time that the light wave travels yields:
 $$
c \int_{t_\mathrm{then}}^{t_\mathrm{now}} \frac{dt}{a}\; =
\int_{R}^{0} \frac{dr}{\sqrt{1kr^2}}\,.
In general, the wavelength of light is not the same for the two positions and times considered due to the changing properties of the metric. When the wave was emitted, it had a wavelength $\backslash lambda\_\backslash mathrm\{then\}$. The next crest of the light wave was emitted at a time
 $t=t\_\backslash mathrm\{then\}+\backslash lambda\_\backslash mathrm\{then\}/c\backslash ,.$
The observer sees the next crest of the observed light wave with a wavelength $\backslash lambda\_\backslash mathrm\{now\}$ to arrive at a time
 $t=t\_\backslash mathrm\{now\}+\backslash lambda\_\backslash mathrm\{now\}/c\backslash ,.$
Since the subsequent crest is again emitted from $r=R$ and is observed at $r=0$, the following equation can be written:
 $$
c \int_{t_\mathrm{then}+\lambda_\mathrm{then}/c}^{t_\mathrm{now}+\lambda_\mathrm{now}/c} \frac{dt}{a}\; =
\int_{R}^{0} \frac{dr}{\sqrt{1kr^2}}\,.
The righthand side of the two integral equations above are identical which means
 $$
c \int_{t_\mathrm{then}+\lambda_\mathrm{then}/c}^{t_\mathrm{now}+\lambda_\mathrm{now}/c} \frac{dt}{a}\; =
c \int_{t_\mathrm{then}}^{t_\mathrm{now}} \frac{dt}{a}\,
or, alternatively,
 $$
\int_{t_\mathrm{now}}^{t_\mathrm{now}+\lambda_\mathrm{now}/c} \frac{dt}{a}\; =
\int_{t_\mathrm{then}}^{t_\mathrm{then}+\lambda_\mathrm{then}/c} \frac{dt}{a}\,.
For very small variations in time (over the period of one cycle of a light wave) the scale factor is essentially a constant ($a=a\_\backslash mathrm\{now\}$ today and $a=a\_\backslash mathrm\{then\}$ previously). This yields
 $\backslash frac\{t\_\backslash mathrm\{now\}+\backslash lambda\_\backslash mathrm\{now\}/c\}\{a\_\backslash mathrm\{now\}\}\backslash frac\{t\_\backslash mathrm\{now\}\}\{a\_\backslash mathrm\{now\}\}\backslash ;\; =\; \backslash frac\{t\_\backslash mathrm\{then\}+\backslash lambda\_\backslash mathrm\{then\}/c\}\{a\_\backslash mathrm\{then\}\}\backslash frac\{t\_\backslash mathrm\{then\}\}\{a\_\backslash mathrm\{then\}\}$
which can be rewritten as
 $\backslash frac\{\backslash lambda\_\backslash mathrm\{now\}\}\{\backslash lambda\_\backslash mathrm\{then\}\}=\backslash frac\{a\_\backslash mathrm\{now\}\}\{a\_\backslash mathrm\{then\}\}\backslash ,.$
Using the definition of redshift provided above, the equation
 $1+z\; =\; \backslash frac\{a\_\backslash mathrm\{now\}\}\{a\_\backslash mathrm\{then\}\}$
is obtained. In an expanding universe such as the one we inhabit, the scale factor is monotonically increasing as time passes, thus, z is positive and distant galaxies appear redshifted.
Using a model of the expansion of the universe, redshift can be related to the age of an observed object, the socalled cosmic time–redshift relation. Denote a density ratio as Ω_{0}:
 $\backslash Omega\_0\; =\; \backslash frac\; \{\backslash rho\}\{\; \backslash rho\_\{crit\}\}\; \backslash \; ,$
with ρ_{crit} the critical density demarcating a universe that eventually crunches from one that simply expands. This density is about three hydrogen atoms per thousand liters of space.^{[28]} At large redshifts one finds:
 $t(z)\; =\; \backslash frac\; \{2\}\{3\; H\_0\; \{\backslash Omega\_0\}^\{1/2\}\; (1+\; z\; )^\{3/2\}\}\; \backslash \; ,$
where H_{0} is the presentday Hubble constant, and z is the redshift.^{[29]}^{[30]}^{[31]}
Distinguishing between cosmological and local effects
For cosmological redshifts of z < 0.01 additional Doppler redshifts and blueshifts due to the peculiar motions of the galaxies relative to one another cause a wide scatter from the standard Hubble Law.^{[32]} The resulting situation can be illustrated by the Expanding Rubber Sheet Universe, a common cosmological analogy used to describe the expansion of space. If two objects are represented by ball bearings and spacetime by a stretching rubber sheet, the Doppler effect is caused by rolling the balls across the sheet to create peculiar motion. The cosmological redshift occurs when the ball bearings are stuck to the sheet and the sheet is stretched.^{[33]}^{[34]}^{[35]}
The redshifts of galaxies include both a component related to recessional velocity from expansion of the universe, and a component related to peculiar motion (Doppler shift).^{[36]} The redshift due to expansion of the universe depends upon the recessional velocity in a fashion determined by the cosmological model chosen to describe the expansion of the universe, which is very different from how Doppler redshift depends upon local velocity.^{[37]} Describing the cosmological expansion origin of redshift, cosmologist Edward Robert Harrison said, "Light leaves a galaxy, which is stationary in its local region of space, and is eventually received by observers who are stationary in their own local region of space. Between the galaxy and the observer, light travels through vast regions of expanding space. As a result, all wavelengths of the light are stretched by the expansion of space. It is as simple as that....^{[38]} Steven Weinberg clarified, "The increase of wavelength from emission to absorption of light does not depend on the rate of change of a(t) [here a(t) is the RobertsonWalker scale factor] at the times of emission or absorption, but on the increase of a(t) in the whole period from emission to absorption."^{[39]}
Popular literature often uses the expression "Doppler redshift" instead of "cosmological redshift" to describe the redshift of galaxies dominated by the expansion of spacetime, but the cosmological redshift is not found using the relativistic Doppler equation^{[40]} which is instead characterized by special relativity; thus v > c is impossible while, in contrast, v > c is possible for cosmological redshifts because the space which separates the objects (for example, a quasar from the Earth) can expand faster than the speed of light.^{[41]} More mathematically, the viewpoint that "distant galaxies are receding" and the viewpoint that "the space between galaxies is expanding" are related by changing coordinate systems. Expressing this precisely requires working with the mathematics of the FriedmannRobertsonWalker metric.^{[42]}
If the universe were contracting instead of expanding, we would see distant galaxies blueshifted by an amount proportional to their distance instead of redshifted.^{[43]}
Gravitational redshift
In the theory of general relativity, there is time dilation within a gravitational well. This is known as the gravitational redshift or Einstein Shift.^{[44]} The theoretical derivation of this effect follows from the Schwarzschild solution of the Einstein equations which yields the following formula for redshift associated with a photon traveling in the gravitational field of an uncharged, nonrotating, spherically symmetric mass:
 $1+z=\backslash frac\{1\}\{\backslash sqrt\{1\backslash frac\{2GM\}\{rc^2\}\}\},$
where
 $G\backslash ,$ is the gravitational constant,
 $M\backslash ,$ is the mass of the object creating the gravitational field,
 $r\backslash ,$ is the radial coordinate of the source (which is analogous to the classical distance from the center of the object, but is actually a Schwarzschild coordinate), and
 $c\backslash ,$ is the speed of light.
This gravitational redshift result can be derived from the assumptions of special relativity and the equivalence principle; the full theory of general relativity is not required.^{[45]}
The effect is very small but measurable on Earth using the Mössbauer effect and was first observed in the PoundRebka experiment.^{[46]} However, it is significant near a black hole, and as an object approaches the event horizon the red shift becomes infinite. It is also the dominant cause of large angularscale temperature fluctuations in the cosmic microwave background radiation (see SachsWolfe effect).^{[47]}^{[48]}
Observations in astronomy
The redshift observed in astronomy can be measured because the emission and absorption spectra for atoms are distinctive and well known, calibrated from spectroscopic experiments in laboratories on Earth. When the redshift of various absorption and emission lines from a single astronomical object is measured, z is found to be remarkably constant. Although distant objects may be slightly blurred and lines broadened, it is by no more than can be explained by thermal or mechanical motion of the source. For these reasons and others, the consensus among astronomers is that the redshifts they observe are due to some combination of the three established forms of Dopplerlike redshifts. Alternative hypotheses and explanations for redshift such as tired light are not generally considered plausible.^{[49]}
Spectroscopy, as a measurement, is considerably more difficult than simple photometry, which measures the brightness of astronomical objects through certain filters.^{[50]} When photometric data is all that is available (for example, the Hubble Deep Field and the Hubble Ultra Deep Field), astronomers rely on a technique for measuring photometric redshifts.^{[51]} Due to the broad wavelength ranges in photometric filters and the necessary assumptions about the nature of the spectrum at the lightsource, errors for these sorts of measurements can range up to δz = 0.5, and are much less reliable than spectroscopic determinations.^{[52]} However, photometry does at least allow a qualitative characterization of a redshift. For example, if a sunlike spectrum had a redshift of z = 1, it would be brightest in the infrared rather than at the yellowgreen color associated with the peak of its blackbody spectrum, and the light intensity will be reduced in the filter by a factor of four, $\{(1+z)^2\}$. Both the photon count rate and the photon energy are redshifted. (See K correction for more details on the photometric consequences of redshift.)^{[53]}
Local observations
In nearby objects (within our Milky Way galaxy) observed redshifts are almost always related to the lineofsight velocities associated with the objects being observed. Observations of such redshifts and blueshifts have enabled astronomers to measure velocities and parametrize the masses of the orbiting stars in spectroscopic binaries, a method first employed in 1868 by British astronomer William Huggins.^{[7]} Similarly, small redshifts and blueshifts detected in the spectroscopic measurements of individual stars are one way astronomers have been able to diagnose and measure the presence and characteristics of planetary systems around other stars and have even made very detailed differential measurements of redshifts during planetary transits to determine precise orbital parameters.^{[54]} Finely detailed measurements of redshifts are used in helioseismology to determine the precise movements of the photosphere of the Sun.^{[55]} Redshifts have also been used to make the first measurements of the rotation rates of planets,^{[56]} velocities of interstellar clouds,^{[57]} the rotation of galaxies,^{[2]} and the dynamics of accretion onto neutron stars and black holes which exhibit both Doppler and gravitational redshifts.^{[58]} Additionally, the temperatures of various emitting and absorbing objects can be obtained by measuring Doppler broadening – effectively redshifts and blueshifts over a single emission or absorption line.^{[59]} By measuring the broadening and shifts of the 21centimeter hydrogen line in different directions, astronomers have been able to measure the recessional velocities of interstellar gas, which in turn reveals the rotation curve of our Milky Way.^{[2]} Similar measurements have been performed on other galaxies, such as Andromeda.^{[2]} As a diagnostic tool, redshift measurements are one of the most important spectroscopic measurements made in astronomy.
The most distant objects exhibit larger redshifts corresponding to the Hubble flow of the universe. The largest observed redshift, corresponding to the greatest distance and furthest back in time, is that of the cosmic microwave background radiation; the numerical value of its redshift is about z = 1089 (z = 0 corresponds to present time), and it shows the state of the Universe about 13.8 billion years ago,^{[60]} and 379,000 years after the initial moments of the Big Bang.^{[61]}
The luminous pointlike cores of quasars were the first "highredshift" (z > 0.1) objects discovered before the improvement of telescopes allowed for the discovery of other highredshift galaxies.
For galaxies more distant than the Local Group and the nearby Virgo Cluster, but within a thousand megaparsecs or so, the redshift is approximately proportional to the galaxy's distance. This correlation was first observed by Edwin Hubble and has come to be known as Hubble's law. Vesto Slipher was the first to discover galactic redshifts, in about the year 1912, while Hubble correlated Slipher's measurements with distances he measured by other means to formulate his Law. In the widely accepted cosmological model based on general relativity, redshift is mainly a result of the expansion of space: this means that the farther away a galaxy is from us, the more the space has expanded in the time since the light left that galaxy, so the more the light has been stretched, the more redshifted the light is, and so the faster it appears to be moving away from us. Hubble's law follows in part from the Copernican principle.^{[62]} Because it is usually not known how luminous objects are, measuring the redshift is easier than more direct distance measurements, so redshift is sometimes in practice converted to a crude distance measurement using Hubble's law.
Gravitational interactions of galaxies with each other and clusters cause a significant scatter in the normal plot of the Hubble diagram. The peculiar velocities associated with galaxies superimpose a rough trace of the mass of virialized objects in the universe. This effect leads to such phenomena as nearby galaxies (such as the Andromeda Galaxy) exhibiting blueshifts as we fall towards a common barycenter, and redshift maps of clusters showing a Fingers of God effect due to the scatter of peculiar velocities in a roughly spherical distribution.^{[62]} This added component gives cosmologists a chance to measure the masses of objects independent of the mass to light ratio (the ratio of a galaxy's mass in solar masses to its brightness in solar luminosities), an important tool for measuring dark matter.^{[63]}
The Hubble law's linear relationship between distance and redshift assumes that the rate of expansion of the universe is constant. However, when the universe was much younger, the expansion rate, and thus the Hubble "constant", was larger than it is today. For more distant galaxies, then, whose light has been travelling to us for much longer times, the approximation of constant expansion rate fails, and the Hubble law becomes a nonlinear integral relationship and dependent on the history of the expansion rate since the emission of the light from the galaxy in question. Observations of the redshiftdistance relationship can be used, then, to determine the expansion history of the universe and thus the matter and energy content.
While it was long believed that the expansion rate has been continuously decreasing since the Big Bang, recent observations of the redshiftdistance relationship using Type Ia supernovae have suggested that in comparatively recent times the expansion rate of the universe has begun to accelerate.
Highest redshifts
Currently, the objects with the highest known redshifts are galaxies and the objects producing gamma ray bursts. The most reliable redshifts are from spectroscopic data, and the highest confirmed spectroscopic redshift of a galaxy is that of
UDFy38135539
^{[64]}
at a redshift of $z=8.6$, corresponding to just 600 million years after the Big Bang.
The previous record was held by
IOK1,^{[65]} at a redshift $z\; =\; 6.96$, corresponding to just 750 million years after the Big Bang. Slightly less reliable are Lymanbreak redshifts, the highest of which is the lensed galaxy A1689zD1 at a redshift $z\; =\; 7.6$^{[66]} and the next highest being $z=7.0$.^{[67]} The most distant observed gamma ray burst was GRB 090423, which had a redshift of $z\; =\; 8.2$.^{[68]} The most distant known quasar, ULAS J1120+0641, is at $z\; =\; 7.1$.^{[69]}^{[70]} The highest known redshift radio galaxy (TN J09242201) is at a redshift $z\; =\; 5.2$^{[71]} and the highest known redshift molecular material is the detection of emission from the CO molecule from the quasar SDSS J1148+5251 at $z\; =\; 6.42$^{[72]}
Extremely red objects (EROs) are astronomical sources of radiation that radiate energy in the red and near infrared part of the electromagnetic spectrum. These may be starburst galaxies that have a high redshift accompanied by reddening from intervening dust, or they could be highly redshifted elliptical galaxies with an older (and therefore redder) stellar population.^{[73]} Objects that are even redder than EROs are termed hyper extremely red objects (HEROs).^{[74]}
The cosmic microwave background has a redshift of $z=1089$, corresponding to an age of approximately 379,000 years after the Big Bang and a comoving distance of more than 46 billion light years.^{[75]} The yettobeobserved first light from the oldest Population III stars, not long after atoms first formed and the CMB ceased to be absorbed almost completely, may have redshifts in the range of $20100\; math>.$[76] Other highredshift events predicted by physics but not presently observable are the cosmic neutrino background from about two seconds after the Big Bang (and a redshift in excess of $z>10^\{10\}$)^{[77]} and the cosmic gravitational wave background emitted directly from inflation at a redshift in excess of $z>10^\{25\}$.^{[78]}
Redshift surveys
With advent of automated telescopes and improvements in spectroscopes, a number of collaborations have been made to map the universe in redshift space. By combining redshift with angular position data, a redshift survey maps the 3D distribution of matter within a field of the sky. These observations are used to measure properties of the largescale structure of the universe. The Great Wall, a vast supercluster of galaxies over 500 million lightyears wide, provides a dramatic example of a largescale structure that redshift surveys can detect.^{[79]}
The first redshift survey was the CfA Redshift Survey, started in 1977 with the initial data collection completed in 1982.^{[80]} More recently, the 2dF Galaxy Redshift Survey determined the largescale structure of one section of the Universe, measuring redshifts for over 220,000 galaxies; data collection was completed in 2002, and the final data set was released 30 June 2003.^{[81]} The Sloan Digital Sky Survey (SDSS), is ongoing as of 2013 and aims to measure the redshifts of around 3 million objects.^{[82]} SDSS has recorded redshifts for galaxies as high as 0.8, and has been involved in the detection of quasars beyond z = 6. The DEEP2 Redshift Survey uses the Keck telescopes with the new "DEIMOS" spectrograph; a followup to the pilot program DEEP1, DEEP2 is designed to measure faint galaxies with redshifts 0.7 and above, and it is therefore planned to provide a high redshift complement to SDSS and 2dF.^{[83]}
Effects due to physical optics or radiative transfer
The interactions and phenomena summarized in the subjects of radiative transfer and physical optics can result in shifts in the wavelength and frequency of electromagnetic radiation. In such cases the shifts correspond to a physical energy transfer to matter or other photons rather than being due to a transformation between reference frames. These shifts can be due to such physical phenomena as coherence effects or the scattering of electromagnetic radiation whether from charged elementary particles, from particulates, or from fluctuations of the index of refraction in a dielectric medium as occurs in the radio phenomenon of radio whistlers.^{[2]} While such phenomena are sometimes referred to as "redshifts" and "blueshifts", in astrophysics lightmatter interactions that result in energy shifts in the radiation field are generally referred to as "reddening" rather than "redshifting" which, as a term, is normally reserved for the effects discussed above.^{[2]}
In many circumstances scattering causes radiation to redden because entropy results in the predominance of many lowenergy photons over few highenergy ones (while conserving total energy).^{[2]} Except possibly under carefully controlled conditions, scattering does not produce the same relative change in wavelength across the whole spectrum; that is, any calculated z is generally a function of wavelength. Furthermore, scattering from random media generally occurs at many angles, and z is a function of the scattering angle. If multiple scattering occurs, or the scattering particles have relative motion, then there is generally distortion of spectral lines as well.^{[2]}
In interstellar astronomy, visible spectra can appear redder due to scattering processes in a phenomenon referred to as interstellar reddening^{[2]} – similarly Rayleigh scattering causes the atmospheric reddening of the Sun seen in the sunrise or sunset and causes the rest of the sky to have a blue color. This phenomenon is distinct from redshifting because the spectroscopic lines are not shifted to other wavelengths in reddened objects and there is an additional dimming and distortion associated with the phenomenon due to photons being scattered in and out of the lineofsight.
For a list of scattering processes, see Scattering.
References
Notes
Articles
 Odenwald, S. & Fienberg, RT. 1993; "Galaxy Redshifts Reconsidered" in Sky & Telescope Feb. 2003; pp31–35 (This article is useful further reading in distinguishing between the 3 types of redshift and their causes.)
 Lineweaver, Charles H. and Tamara M. Davis, "Scientific American, March 2005. (This article is useful for explaining the cosmological redshift mechanism as well as clearing up misconceptions regarding the physics of the expansion of space.)
Book references
External links
 Ned Wright's Cosmology tutorial
 Cosmic reference guide entry on redshift
 Mike Luciuk's Astronomical Redshift tutorial
 Animated GIF of Cosmological Redshift by Wayne Hu

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