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In Big Bang cosmology the cosmic microwave background (CMB, CMBR) is electromagnetic radiation that is a remnant from an early stage of the universe, also known as "relic radiation". The CMB is faint cosmic background radiation
filling all space. It is an important source of data on the early
universe because it is the oldest electromagnetic radiation in the
universe, dating to the epoch of recombination when the first atoms were formed. With a traditional optical telescope, the space between stars and galaxies (the background) is completely dark. However, a sufficiently sensitive radio telescope shows a faint background noise, or glow, almost uniform, that is not associated with any star, galaxy, or other object. This glow is strongest in the microwave region of the radio spectrum. The accidental discovery of the CMB in 1965 by American radio astronomers Arno Penzias and Robert Wilson was the culmination of work initiated in the 1940s, and earned the discoverers the 1978 Nobel Prize in Physics.
CMB is landmark evidence of the Big Bang origin of the universe.
When the universe was young, before the formation of stars and planets,
it was denser, much hotter, and filled with an opaque fog of hydrogen plasma.
As the universe expanded the plasma grew cooler and the radiation
filling it expanded to longer wavelengths. When the temperature had
dropped enough, protons and electrons combined to form neutral hydrogen
atoms. Unlike the plasma, these newly conceived atoms could not scatter
the thermal radiation by Thomson scattering, and so the universe became transparent. Cosmologists refer to the time period when neutral atoms first formed as the recombination epoch, and the event shortly afterwards when photons started to travel freely through space is referred to as photon decoupling. The photons that existed at the time of photon decoupling have been propagating ever since, though growing less energetic, since the expansion of space causes their wavelength to increase over time (and wavelength is inversely proportional to energy according to Planck's relation). This is the source of the alternative term relic radiation. The surface of last scattering
refers to the set of points in space at the right distance from us so
that we are now receiving photons originally emitted from those points
at the time of photon decoupling.
According to the Theory of Quantum Fields in Curved Spacetimes the origin of these (thermal) microwave photons is related to redshifted particles created in the early Universe, when the production of particles by the expanding background played a significant role.
Importance of precise measurement
Precise
measurements of the CMB are critical to cosmology, since any proposed
model of the universe must explain this radiation. The CMB has a thermal
black body spectrum at a temperature of 2.72548±0.00057 K. The spectral radiance dEν/dν peaks at 160.23 GHz, in the microwave range of frequencies, corresponding to a photon energy of about 6.626 ⋅ 10−4 eV. Alternatively, if spectral radiance is defined as dEλ/dλ, then the peak wavelength is 1.063 mm (282 GHz, 1.168 ⋅ 10−3
eV photons). The glow is very nearly uniform in all directions, but the
tiny residual variations show a very specific pattern, the same as that
expected of a fairly uniformly distributed hot gas
that has expanded to the current size of the universe. In particular,
the spectral radiance at different angles of observation in the sky
contains small anisotropies,
or irregularities, which vary with the size of the region examined.
They have been measured in detail, and match what would be expected if
small thermal variations, generated by quantum fluctuations of matter in a very tiny space, had expanded to the size of the observable universe we see today. This is a very active field of study, with scientists seeking both better data (for example, the Planck spacecraft)
and better interpretations of the initial conditions of expansion.
Although many different processes might produce the general form of a
black body spectrum, no model other than the Big Bang has yet explained
the fluctuations. As a result, most cosmologists consider the Big Bang
model of the universe to be the best explanation for the CMB.
The high degree of uniformity throughout the observable universe and its faint but measured anisotropy lend strong support for the Big Bang model in general and the ΛCDM ("Lambda Cold Dark Matter") model in particular. Moreover, the fluctuations are coherent on angular scales that are larger than the apparent cosmological horizon at recombination. Either such coherence is acausally fine-tuned, or cosmic inflation occurred.
Other than the temperature and polarization anisotropy, the CMB
frequency spectrum is expected to feature tiny departures from the
black-body law known as spectral distortions.
These are also at the focus of an active research effort with the hope
of a first measurement within the forthcoming decades, as they contain a
wealth of information about the primordial universe and the formation
of structures at late time.
Features
Graph of cosmic microwave background spectrum measured by the FIRAS instrument on the
COBE, the most precisely measured
black body spectrum in nature. The
error bars
are too small to be seen even in an enlarged image, and it is
impossible to distinguish the observed data from the theoretical curve.
The cosmic microwave background radiation is an emission of uniform, black body thermal energy coming from all parts of the sky. The radiation is isotropic to roughly one part in 100,000: the root mean square variations are only 18 μK, after subtracting out a dipole anisotropy from the Doppler shift of the background radiation. The latter is caused by the peculiar velocity of the Sun relative to the comoving cosmic rest frame as it moves at some 369.82 ± 0.11 km/s towards the constellation Leo (galactic longitude 264.021 ± 0.011, galactic latitude 48.253 ± 0.005). The CMB dipole and aberration at higher multipoles have been measured, consistent with galactic motion.
In the Big Bang model for the formation of the universe, inflationary cosmology predicts that after about 10−37 seconds the nascent universe underwent exponential growth
that smoothed out nearly all irregularities. The remaining
irregularities were caused by quantum fluctuations in the inflation
field that caused the inflation event. Long before the formation of stars and planets, the early universe was smaller, much hotter and, starting 10−6 seconds after the Big Bang, filled with a uniform glow from its white-hot fog of interacting plasma of photons, electrons, and baryons.
As the universe expanded, adiabatic cooling caused the energy density of the plasma to decrease until it became favorable for electrons to combine with protons, forming hydrogen atoms. This recombination event happened when the temperature was around 3000 K or when the universe was approximately 379,000 years old. As photons did not interact with these electrically neutral atoms, the former began to travel freely through space, resulting in the decoupling of matter and radiation.
The color temperature of the ensemble of decoupled photons has continued to diminish ever since; now down to 2.7260±0.0013 K,
it will continue to drop as the universe expands. The intensity of the
radiation corresponds to black-body radiation at 2.726 K because
red-shifted black-body radiation is just like black-body radiation at a
lower temperature. According to the Big Bang model, the radiation from
the sky we measure today comes from a spherical surface called the surface of last scattering. This represents the set of locations in space at which the decoupling event is estimated to have occurred
and at a point in time such that the photons from that distance have
just reached observers. Most of the radiation energy in the universe is
in the cosmic microwave background, making up a fraction of roughly 6×10−5 of the total density of the universe.
Two of the greatest successes of the Big Bang theory are its
prediction of the almost perfect black body spectrum and its detailed
prediction of the anisotropies in the cosmic microwave background. The
CMB spectrum has become the most precisely measured black body spectrum
in nature.
The energy density of the CMB is 0.260 eV/cm3 (4.17×10−14 J/m3) which yields about 411 photons/cm3.
History
The cosmic microwave background was first predicted in 1948 by Ralph Alpher and Robert Herman, in close relation to work performed by Alpher's PhD advisor George Gamow.
Alpher and Herman were able to estimate the temperature of the cosmic
microwave background to be 5 K, though two years later they re-estimated
it at 28 K. This high estimate was due to a misestimate of the Hubble constant
by Alfred Behr, which could not be replicated and was later abandoned
for the earlier estimate. Although there were several previous estimates
of the temperature of space, these suffered from two flaws. First, they
were measurements of the effective temperature of space and did not suggest that space was filled with a thermal Planck spectrum. Next, they depend on our being at a special spot at the edge of the Milky Way
galaxy and they did not suggest the radiation is isotropic. The
estimates would yield very different predictions if Earth happened to be
located elsewhere in the universe.
The
Holmdel Horn Antenna on which Penzias and Wilson discovered the cosmic microwave background. The antenna was constructed in 1959 to support
Project Echo—the
National Aeronautics and Space Administration's passive communications
satellites, which used large earth orbiting aluminized plastic balloons
as reflectors to bounce radio signals from one point on the Earth to
another.
The 1948 results of Alpher and Herman were discussed in many physics
settings through about 1955, when both left the Applied Physics
Laboratory at Johns Hopkins University.
The mainstream astronomical community, however, was not intrigued at
the time by cosmology. Alpher and Herman's prediction was rediscovered
by Yakov Zel'dovich in the early 1960s, and independently predicted by Robert Dicke at the same time. The first published recognition of the CMB radiation as a detectable phenomenon appeared in a brief paper by Soviet astrophysicists A. G. Doroshkevich and Igor Novikov, in the spring of 1964. In 1964, David Todd Wilkinson and Peter Roll, Dicke's colleagues at Princeton University, began constructing a Dicke radiometer to measure the cosmic microwave background. In 1964, Arno Penzias and Robert Woodrow Wilson at the Crawford Hill location of Bell Telephone Laboratories in nearby Holmdel Township, New Jersey
had built a Dicke radiometer that they intended to use for radio
astronomy and satellite communication experiments. On 20 May 1964 they
made their first measurement clearly showing the presence of the
microwave background, with their instrument having an excess 4.2K antenna temperature which they could not account for. After receiving a telephone call from Crawford Hill, Dicke said "Boys, we've been scooped."
A meeting between the Princeton and Crawford Hill groups determined
that the antenna temperature was indeed due to the microwave background.
Penzias and Wilson received the 1978 Nobel Prize in Physics for their discovery.
The interpretation of the cosmic microwave background was a controversial issue in the 1960s with some proponents of the steady state theory arguing that the microwave background was the result of scattered starlight from distant galaxies. Using this model, and based on the study of narrow absorption line features in the spectra of stars, the astronomer Andrew McKellar wrote in 1941: "It can be calculated that the 'rotational temperature' of interstellar space is 2 K."
However, during the 1970s the consensus was established that the cosmic
microwave background is a remnant of the big bang. This was largely
because new measurements at a range of frequencies showed that the
spectrum was a thermal, black body spectrum, a result that the steady state model was unable to reproduce.
Harrison, Peebles, Yu and Zel'dovich realized that the early universe would require inhomogeneities at the level of 10−4 or 10−5. Rashid Sunyaev later calculated the observable imprint that these inhomogeneities would have on the cosmic microwave background.
Increasingly stringent limits on the anisotropy of the cosmic microwave
background were set by ground-based experiments during the 1980s. RELIKT-1,
a Soviet cosmic microwave background anisotropy experiment on board the
Prognoz 9 satellite (launched 1 July 1983) gave upper limits on the
large-scale anisotropy. The NASA COBE
mission clearly confirmed the primary anisotropy with the Differential
Microwave Radiometer instrument, publishing their findings in 1992. The team received the Nobel Prize in physics for 2006 for this discovery.
Inspired by the COBE results, a series of ground and
balloon-based experiments measured cosmic microwave background
anisotropies on smaller angular scales over the next decade. The primary
goal of these experiments was to measure the scale of the first
acoustic peak, which COBE did not have sufficient resolution to resolve.
This peak corresponds to large scale density variations in the early
universe that are created by gravitational instabilities, resulting in
acoustical oscillations in the plasma. The first peak in the anisotropy was tentatively detected by the Toco experiment and the result was confirmed by the BOOMERanG and MAXIMA experiments. These measurements demonstrated that the geometry of the universe is approximately flat, rather than curved. They ruled out cosmic strings as a major component of cosmic structure formation and suggested cosmic inflation was the right theory of structure formation.
The second peak was tentatively detected by several experiments before being definitively detected by WMAP, which has tentatively detected the third peak.
As of 2010, several experiments to improve measurements of the
polarization and the microwave background on small angular scales are
ongoing. These include DASI, WMAP, BOOMERanG, QUaD, Planck spacecraft, Atacama Cosmology Telescope, South Pole Telescope and the QUIET telescope.
Relationship to the Big Bang
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The cosmic microwave background radiation and the cosmological redshift-distance relation are together regarded as the best available evidence for the Big Bang theory. Measurements of the CMB have made the inflationary Big Bang theory the Standard Cosmological Model. The discovery of the CMB in the mid-1960s curtailed interest in alternatives such as the steady state theory.
In the late 1940s Alpher and Herman reasoned that if there was a
big bang, the expansion of the universe would have stretched the
high-energy radiation of the very early universe into the microwave
region of the electromagnetic spectrum,
and down to a temperature of about 5 K. They were slightly off with
their estimate, but they had the right idea. They predicted the CMB. It
took another 15 years for Penzias and Wilson to stumble into discovering
that the microwave background was actually there.
The CMB gives a snapshot of the universe when, according to standard cosmology, the temperature dropped enough to allow electrons and protons to form hydrogen atoms, thereby making the universe nearly transparent to radiation because light was no longer being scattered
off free electrons. When it originated some 380,000 years after the Big
Bang—this time is generally known as the "time of last scattering" or
the period of recombination or decoupling—the temperature of the universe was about 3000 K. This corresponds to an energy of about 0.26 eV, which is much less than the 13.6 eV ionization energy of hydrogen.
Since decoupling, the color temperature of the background radiation has dropped by an average factor of 1090 due to the expansion of the universe. As the universe expands, the CMB photons are redshifted, causing them to decrease in energy. The color temperature of this radiation stays inversely proportional to a parameter that describes the relative expansion of the universe over time, known as the scale length. The color temperature Tr of the CMB as a function of redshift, z, can be shown to be proportional to the color temperature of the CMB as observed in the present day (2.725 K or 0.2348 meV):
- Tr = 2.725 ⋅ (1 + z)
For details about the reasoning that the radiation is evidence for the Big Bang, see Cosmic background radiation of the Big Bang.
Primary anisotropy
The power spectrum of the cosmic microwave background radiation temperature anisotropy in terms of the angular scale (or
multipole moment). The data shown comes from the
WMAP (2006),
Acbar (2004)
Boomerang (2005),
CBI (2004), and
VSA (2004) instruments. Also shown is a theoretical model (solid line).
The anisotropy,
or directional dependency, of the cosmic microwave background is
divided into two types: primary anisotropy, due to effects that occur at
the surface of last scattering and before; and secondary anisotropy,
due to effects such as interactions of the background radiation with
intervening hot gas or gravitational potentials, which occur between the
last scattering surface and the observer.
The structure of the cosmic microwave background anisotropies is
principally determined by two effects: acoustic oscillations and diffusion damping (also called collisionless damping or Silk damping). The acoustic oscillations arise because of a conflict in the photon–baryon
plasma in the early universe. The pressure of the photons tends to
erase anisotropies, whereas the gravitational attraction of the baryons,
moving at speeds much slower than light, makes them tend to collapse to
form overdensities. These two effects compete to create acoustic
oscillations, which give the microwave background its characteristic
peak structure. The peaks correspond, roughly, to resonances in which
the photons decouple when a particular mode is at its peak amplitude.
The peaks contain interesting physical signatures. The angular scale of the first peak determines the curvature of the universe (but not the topology of the universe). The next peak—ratio of the odd peaks to the even peaks—determines the reduced baryon density. The third peak can be used to get information about the dark-matter density.
The locations of the peaks give important information about the
nature of the primordial density perturbations. There are two
fundamental types of density perturbations called adiabatic and isocurvature.
A general density perturbation is a mixture of both, and different
theories that purport to explain the primordial density perturbation
spectrum predict different mixtures.
- Adiabatic density perturbations
- In an adiabatic density perturbation, the fractional additional number density of each type of particle (baryons, photons
...) is the same. That is, if at one place there is a 1% higher number
density of baryons than average, then at that place there is a 1% higher
number density of photons (and a 1% higher number density in neutrinos)
than average. Cosmic inflation predicts that the primordial perturbations are adiabatic.
- Isocurvature density perturbations
- In an isocurvature density perturbation, the sum (over different
types of particle) of the fractional additional densities is zero. That
is, a perturbation where at some spot there is 1% more energy in baryons
than average, 1% more energy in photons than average, and 2% less energy in neutrinos than average, would be a pure isocurvature perturbation. Hypothetical cosmic strings would produce mostly isocurvature primordial perturbations.
The CMB spectrum can distinguish between these two because these two
types of perturbations produce different peak locations. Isocurvature
density perturbations produce a series of peaks whose angular scales (ℓ
values of the peaks) are roughly in the ratio 1 : 3 : 5 : ..., while
adiabatic density perturbations produce peaks whose locations are in the
ratio 1 : 2 : 3 : ...
Observations are consistent with the primordial density perturbations
being entirely adiabatic, providing key support for inflation, and
ruling out many models of structure formation involving, for example,
cosmic strings.
Collisionless damping is caused by two effects, when the treatment of the primordial plasma as fluid begins to break down:
- the increasing mean free path of the photons as the primordial plasma becomes increasingly rarefied in an expanding universe,
- the finite depth of the last scattering surface (LSS), which causes
the mean free path to increase rapidly during decoupling, even while
some Compton scattering is still occurring.
These effects contribute about equally to the suppression of
anisotropies at small scales and give rise to the characteristic
exponential damping tail seen in the very small angular scale
anisotropies.
The depth of the LSS refers to the fact that the decoupling of
the photons and baryons does not happen instantaneously, but instead
requires an appreciable fraction of the age of the universe up to that
era. One method of quantifying how long this process took uses the photon visibility function (PVF). This function is defined so that, denoting the PVF by P(t), the probability that a CMB photon last scattered between time t and t + dt is given by P(t) dt.
The maximum of the PVF (the time when it is most likely that a
given CMB photon last scattered) is known quite precisely. The
first-year WMAP results put the time at which P(t) has a maximum as 372,000 years. This is often taken as the "time" at which the CMB formed. However, to figure out how long
it took the photons and baryons to decouple, we need a measure of the
width of the PVF. The WMAP team finds that the PVF is greater than half
of its maximal value (the "full width at half maximum", or FWHM) over an
interval of 115,000 years. By this measure, decoupling took place over
roughly 115,000 years, and when it was complete, the universe was
roughly 487,000 years old.
Late time anisotropy
Since
the CMB came into existence, it has apparently been modified by several
subsequent physical processes, which are collectively referred to as
late-time anisotropy, or secondary anisotropy. When the CMB photons
became free to travel unimpeded, ordinary matter in the universe was
mostly in the form of neutral hydrogen and helium atoms. However,
observations of galaxies today seem to indicate that most of the volume
of the intergalactic medium (IGM) consists of ionized material (since there are few absorption lines due to hydrogen atoms). This implies a period of reionization during which some of the material of the universe was broken into hydrogen ions.
The CMB photons are scattered by free charges such as electrons
that are not bound in atoms. In an ionized universe, such charged
particles have been liberated from neutral atoms by ionizing
(ultraviolet) radiation. Today these free charges are at sufficiently
low density in most of the volume of the universe that they do not
measurably affect the CMB. However, if the IGM was ionized at very early
times when the universe was still denser, then there are two main
effects on the CMB:
- Small scale anisotropies are erased. (Just as when looking at an object through fog, details of the object appear fuzzy.)
- The physics of how photons are scattered by free electrons (Thomson scattering)
induces polarization anisotropies on large angular scales. This broad
angle polarization is correlated with the broad angle temperature
perturbation.
Both of these effects have been observed by the WMAP spacecraft,
providing evidence that the universe was ionized at very early times, at
a redshift more than 17.
The detailed provenance of this early ionizing radiation is still a
matter of scientific debate. It may have included starlight from the
very first population of stars (population III
stars), supernovae when these first stars reached the end of their
lives, or the ionizing radiation produced by the accretion disks of
massive black holes.
The time following the emission of the cosmic microwave
background—and before the observation of the first stars—is
semi-humorously referred to by cosmologists as the Dark Age, and is a period which is under intense study by astronomers (see 21 centimeter radiation).
Two other effects which occurred between reionization and our
observations of the cosmic microwave background, and which appear to
cause anisotropies, are the Sunyaev–Zel'dovich effect, where a cloud of high-energy electrons scatters the radiation, transferring some of its energy to the CMB photons, and the Sachs–Wolfe effect,
which causes photons from the Cosmic Microwave Background to be
gravitationally redshifted or blueshifted due to changing gravitational
fields.
Polarization
This
artist's impression shows how light from the early universe is
deflected by the gravitational lensing effect of massive cosmic
structures forming B-modes as it travels across the universe.
The cosmic microwave background is polarized at the level of a few microkelvin. There are two types of polarization, called E-modes and B-modes. This is in analogy to electrostatics, in which the electric field (E-field) has a vanishing curl and the magnetic field (B-field) has a vanishing divergence. The E-modes arise naturally from Thomson scattering
in a heterogeneous plasma. The B-modes are not produced by standard
scalar type perturbations. Instead they can be created by two
mechanisms: the first one is by gravitational lensing of E-modes, which
has been measured by the South Pole Telescope in 2013; the second one is from gravitational waves arising from cosmic inflation. Detecting the B-modes is extremely difficult, particularly as the degree of foreground contamination is unknown, and the weak gravitational lensing signal mixes the relatively strong E-mode signal with the B-mode signal.
E-modes
E-modes were first seen in 2002 by the Degree Angular Scale Interferometer (DASI).
B-modes
Cosmologists predict two types of B-modes, the first generated during cosmic inflation shortly after the big bang, and the second generated by gravitational lensing at later times.
Primordial gravitational waves
Primordial gravitational waves are gravitational waves that could be observed in the polarisation of the cosmic microwave background and having their origin in the early universe. Models of cosmic inflation
predict that such gravitational waves should appear; thus, their
detection supports the theory of inflation, and their strength can
confirm and exclude different models of inflation. It is the result of
three things: inflationary expansion of space itself, reheating after
inflation, and turbulent fluid mixing of matter and radiation.
On 17 March 2014 it was announced that the BICEP2 instrument had detected the first type of B-modes, consistent with inflation and gravitational waves in the early universe at the level of r = 0.20+0.07
−0.05, which is the amount of power present in gravitational waves
compared to the amount of power present in other scalar density
perturbations in the very early universe. Had this been confirmed it
would have provided strong evidence for cosmic inflation and the Big
Bang and against the ekpyrotic model of Paul Steinhardt and Neil Turok. However, on 19 June 2014, considerably lowered confidence in confirming the findings was reported
and on 19 September 2014 new results of the Planck experiment reported that the results of BICEP2 can be fully attributed to cosmic dust.
Gravitational lensing
The second type of B-modes was discovered in 2013 using the South Pole Telescope with help from the Herschel Space Observatory. In October 2014, a measurement of the B-mode polarization at 150 GHz was published by the POLARBEAR experiment.
Compared to BICEP2, POLARBEAR focuses on a smaller patch of the sky and
is less susceptible to dust effects. The team reported that POLARBEAR's
measured B-mode polarization was of cosmological origin (and not just
due to dust) at a 97.2% confidence level.
Microwave background observations
Subsequent to the discovery of the CMB, hundreds of cosmic microwave
background experiments have been conducted to measure and characterize
the signatures of the radiation. The most famous experiment is probably
the NASA Cosmic Background Explorer (COBE)
satellite that orbited in 1989–1996 and which detected and quantified
the large scale anisotropies at the limit of its detection capabilities.
Inspired by the initial COBE results of an extremely isotropic and
homogeneous background, a series of ground- and balloon-based
experiments quantified CMB anisotropies on smaller angular scales over
the next decade. The primary goal of these experiments was to measure
the angular scale of the first acoustic peak, for which COBE did not
have sufficient resolution. These measurements were able to rule out cosmic strings as the leading theory of cosmic structure formation, and suggested cosmic inflation was the right theory. During the 1990s, the first peak was measured with increasing sensitivity and by 2000 the BOOMERanG experiment
reported that the highest power fluctuations occur at scales of
approximately one degree. Together with other cosmological data, these
results implied that the geometry of the universe is flat. A number of ground-based interferometers provided measurements of the fluctuations with higher accuracy over the next three years, including the Very Small Array, Degree Angular Scale Interferometer (DASI), and the Cosmic Background Imager
(CBI). DASI made the first detection of the polarization of the CMB and
the CBI provided the first E-mode polarization spectrum with compelling
evidence that it is out of phase with the T-mode spectrum.
In June 2001, NASA launched a second CMB space mission, WMAP, to make much more precise measurements of the large scale anisotropies over the full sky. WMAP used symmetric, rapid-multi-modulated scanning, rapid switching radiometers to minimize non-sky signal noise.
The first results from this mission, disclosed in 2003, were detailed
measurements of the angular power spectrum at a scale of less than one
degree, tightly constraining various cosmological parameters. The
results are broadly consistent with those expected from cosmic inflation
as well as various other competing theories, and are available in
detail at NASA's data bank for Cosmic Microwave Background (CMB) (see
links below). Although WMAP provided very accurate measurements of the
large scale angular fluctuations in the CMB (structures about as broad
in the sky as the moon), it did not have the angular resolution to
measure the smaller scale fluctuations which had been observed by former
ground-based interferometers.
A third space mission, the ESA (European Space Agency) Planck Surveyor,
was launched in May 2009 and performed an even more detailed
investigation until it was shut down in October 2013. Planck employed
both HEMT radiometers and bolometer technology and measured the CMB at a smaller scale than WMAP. Its detectors were trialled in the Antarctic Viper telescope as ACBAR (Arcminute Cosmology Bolometer Array Receiver) experiment—which has produced the most precise measurements at small angular scales to date—and in the Archeops balloon telescope.
On 21 March 2013, the European-led research team behind the Planck cosmology probe released the mission's all-sky map (565x318 jpeg, 3600x1800 jpeg) of the cosmic microwave background. The map suggests the universe is slightly older than researchers
expected. According to the map, subtle fluctuations in temperature were
imprinted on the deep sky when the cosmos was about 370000
years old. The imprint reflects ripples that arose as early, in the
existence of the universe, as the first nonillionth of a second.
Apparently, these ripples gave rise to the present vast cosmic web of galaxy clusters and dark matter. Based on the 2013 data, the universe contains 4.9% ordinary matter, 26.8% dark matter and 68.3% dark energy. On 5 February 2015, new data was released by the Planck mission, according to which the age of the universe is 13.799±0.021 billion years old and the Hubble constant was measured to be 67.74±0.46 (km/s)/Mpc.
Additional ground-based instruments such as the South Pole Telescope in Antarctica and the proposed Clover Project, Atacama Cosmology Telescope and the QUIET telescope in Chile will provide additional data not available from satellite observations, possibly including the B-mode polarization.
Data reduction and analysis
Raw
CMBR data, even from space vehicles such as WMAP or Planck, contain
foreground effects that completely obscure the fine-scale structure of
the cosmic microwave background. The fine-scale structure is
superimposed on the raw CMBR data but is too small to be seen at the
scale of the raw data. The most prominent of the foreground effects is
the dipole anisotropy caused by the Sun's motion relative to the CMBR
background. The dipole anisotropy and others due to Earth's annual
motion relative to the Sun and numerous microwave sources in the
galactic plane and elsewhere must be subtracted out to reveal the
extremely tiny variations characterizing the fine-scale structure of the
CMBR background.
The detailed analysis of CMBR data to produce maps, an angular
power spectrum, and ultimately cosmological parameters is a complicated,
computationally difficult problem. Although computing a power spectrum
from a map is in principle a simple Fourier transform, decomposing the map of the sky into spherical harmonics,
where the
term measures the mean temperature and
term accounts for the fluctuation, where the
refers to a
spherical harmonic, and
ℓ is the multipole number while
m is the azimuthal number.
By applying the angular correlation function, the sum can be reduced to an expression that only involves ℓ and power spectrum term 
The angled brackets indicate the average with respect to all observers
in the universe; since the universe is homogeneous and isotropic,
therefore there is an absence of preferred observing direction. Thus, C is independent of m. Different choices of ℓ correspond to multipole moments of CMB.
In practice it is hard to take the effects of noise and
foreground sources into account. In particular, these foregrounds are
dominated by galactic emissions such as Bremsstrahlung, synchrotron, and dust
that emit in the microwave band; in practice, the galaxy has to be
removed, resulting in a CMB map that is not a full-sky map. In addition,
point sources like galaxies and clusters represent another source of
foreground which must be removed so as not to distort the short scale
structure of the CMB power spectrum.
Constraints on many cosmological parameters can be obtained from
their effects on the power spectrum, and results are often calculated
using Markov chain Monte Carlo sampling techniques.
CMBR monopole term (ℓ = 0)
When ℓ = 0, the
term reduced to 1, and what we have left here is just the mean
temperature of the CMB. This "mean" is called CMB monopole, and it is
observed to have an average temperature of about Tγ = 2.7255 ± 0.0006K
with one standard deviation confidence. The accuracy of this mean
temperature may be impaired by the diverse measurements done by
different mapping measurements. Such measurements demand absolute
temperature devices, such as the FIRAS instrument on the COBE satellite. The measured kTγ is equivalent to 0.234 meV or 4.6 × 10−10 mec2. The photon number density of a blackbody having such temperature is 
. Its energy density is 
, and the ratio to the critical density is Ωγ = 5.38 × 10−5.
CMBR dipole anisotropy (ℓ = 1)
CMB dipole represents the largest anisotropy, which is in the first spherical harmonic (ℓ = 1). When ℓ = 1, the
term reduces to one cosine function and thus encodes amplitude
fluctuation. The amplitude of CMB dipole is around 3.3621 ± 0.0010 mK. Since the universe is presumed to be homogeneous and isotropic, an observer should see the blackbody spectrum with temperature T at every point in the sky. The spectrum of the dipole has been confirmed to be the differential of a blackbody spectrum.
CMB dipole is frame-dependent. The CMB dipole moment could also
be interpreted as the peculiar motion of the Earth toward the CMB. Its
amplitude depends on the time due to the Earth's orbit about the
barycenter of the solar system. This enables us to add a time-dependent
term to the dipole expression. The modulation of this term is 1 year, which fits the observation done by COBE FIRAS. The dipole moment does not encode any primordial information.
From the CMB data, it is seen that the Sun appears to be moving at 368±2 km/s
relative to the reference frame of the CMB (also called the CMB rest
frame, or the frame of reference in which there is no motion through the
CMB). The Local Group — the galaxy group that includes our own Milky Way galaxy — appears to be moving at 627±22 km/s in the direction of galactic longitude ℓ = 276°±3°, b = 30°±3°.
This motion results in an anisotropy of the data (CMB appearing
slightly warmer in the direction of movement than in the opposite
direction).
The standard interpretation of this temperature variation is a simple
velocity redshift and blueshift due to motion relative to the CMB, but
alternative cosmological models can explain some fraction of the
observed dipole temperature distribution in the CMB.
A 2021 study of Wide-field Infrared Survey Explorer questions the kinematic interpretation of CMB anisotropy with high statistical confidence.
Multipole (ℓ ≥ 2)
The temperature variation in the CMB temperature maps at higher multipoles, or ℓ
≥ 2, is considered to be the result of perturbations of the density in
the early Universe, before the recombination epoch. Before
recombination, the Universe consisted of a hot, dense plasma of
electrons and baryons. In such a hot dense environment, electrons and
protons could not form any neutral atoms. The baryons in such early
Universe remained highly ionized and so were tightly coupled with
photons through the effect of Thompson scattering. These phenomena
caused the pressure and gravitational effects to act against each other,
and triggered fluctuations in the photon-baryon plasma. Quickly after
the recombination epoch, the rapid expansion of the universe caused the
plasma to cool down and these fluctuations are "frozen into" the CMB
maps we observe today. The said procedure happened at a redshift of
around z ⋍ 1100.
Other anomalies
With the increasingly precise data provided by WMAP, there have been a
number of claims that the CMB exhibits anomalies, such as very large
scale anisotropies, anomalous alignments, and non-Gaussian
distributions. The most longstanding of these is the low-ℓ multipole controversy. Even in the COBE map, it was observed that the quadrupole (ℓ
= 2, spherical harmonic) has a low amplitude compared to the
predictions of the Big Bang. In particular, the quadrupole and octupole (ℓ = 3) modes appear to have an unexplained alignment with each other and with both the ecliptic plane and equinoxes.
A number of groups have suggested that this could be the signature of
new physics at the greatest observable scales; other groups suspect
systematic errors in the data.
Ultimately, due to the foregrounds and the cosmic variance
problem, the greatest modes will never be as well measured as the small
angular scale modes. The analyses were performed on two maps that have
had the foregrounds removed as far as possible: the "internal linear
combination" map of the WMAP collaboration and a similar map prepared by
Max Tegmark and others. Later analyses have pointed out that these are the modes most susceptible to foreground contamination from synchrotron, dust, and Bremsstrahlung emission, and from experimental uncertainty in the monopole and dipole.
A full Bayesian analysis of the WMAP power spectrum demonstrates that the quadrupole prediction of Lambda-CDM cosmology is consistent with the data at the 10% level and that the observed octupole is not remarkable.[102]
Carefully accounting for the procedure used to remove the foregrounds
from the full sky map further reduces the significance of the alignment
by ~5%.
Recent observations with the Planck telescope,
which is very much more sensitive than WMAP and has a larger angular
resolution, record the same anomaly, and so instrumental error (but not
foreground contamination) appears to be ruled out. Coincidence is a possible explanation, chief scientist from WMAP, Charles L. Bennett
suggested coincidence and human psychology were involved, "I do think
there is a bit of a psychological effect; people want to find unusual
things."
Future evolution
Assuming the universe keeps expanding and it does not suffer a Big Crunch, a Big Rip, or another similar fate, the cosmic microwave background will continue redshifting until it will no longer be detectable, and will be superseded first by the one produced by starlight,
and perhaps, later by the background radiation fields of processes that
may take place in the far future of the universe such as proton decay, evaporation of black holes, and positronium decay.
Timeline of prediction, discovery and interpretation
Thermal (non-microwave background) temperature predictions
- 1896 – Charles Édouard Guillaume estimates the "radiation of the stars" to be 5–6K.
- 1926 – Sir Arthur Eddington estimates the non-thermal radiation of starlight in the galaxy "... by the formula E = σT4 the effective temperature corresponding to this density is 3.18° absolute ... black body"
- 1930s – Cosmologist Erich Regener calculates that the non-thermal spectrum of cosmic rays in the galaxy has an effective temperature of 2.8 K
- 1931 – Term microwave first used in print: "When trials with
wavelengths as low as 18 cm. were made known, there was undisguised
surprise+that the problem of the micro-wave had been solved so soon." Telegraph & Telephone Journal XVII. 179/1
- 1934 – Richard Tolman shows that black-body radiation in an expanding universe cools but remains thermal
- 1938 – Nobel Prize winner (1920) Walther Nernst reestimates the cosmic ray temperature as 0.75K
- 1946 – Robert Dicke predicts "... radiation from cosmic matter" at <20 K, but did not refer to background radiation
- 1946 – George Gamow calculates a temperature of 50 K (assuming a 3-billion year old universe),
commenting it "... is in reasonable agreement with the actual
temperature of interstellar space", but does not mention background
radiation.
- 1953 – Erwin Finlay-Freundlich in support of his tired light theory, derives a blackbody temperature for intergalactic space of 2.3K with comment from Max Born suggesting radio astronomy as the arbitrator between expanding and infinite cosmologies.
Microwave background radiation predictions and measurements
- 1941 – Andrew McKellar
detected the cosmic microwave background as the coldest component of
the interstellar medium by using the excitation of CN doublet lines
measured by W. S. Adams in a B star, finding an "effective temperature
of space" (the average bolometric temperature) of 2.3 K
- 1946 – George Gamow calculates a temperature of 50 K (assuming a 3-billion year old universe),
commenting it "... is in reasonable agreement with the actual
temperature of interstellar space", but does not mention background
radiation.
- 1948 – Ralph Alpher and Robert Herman
estimate "the temperature in the universe" at 5 K. Although they do not
specifically mention microwave background radiation, it may be
inferred.
- 1949 – Ralph Alpher and Robert Herman re-re-estimate the temperature at 28 K.
- 1953 – George Gamow estimates 7 K.
- 1956 – George Gamow estimates 6 K.
- 1955 – Émile Le Roux of the Nançay Radio Observatory, in a sky survey at λ = 33 cm, reported a near-isotropic background radiation of 3 kelvins, plus or minus 2.
- 1957 – Tigran Shmaonov reports that "the absolute effective temperature of the radioemission background ... is 4±3 K".
It is noted that the "measurements showed that radiation intensity was
independent of either time or direction of observation ... it is now
clear that Shmaonov did observe the cosmic microwave background at a
wavelength of 3.2 cm"
- 1960s – Robert Dicke re-estimates a microwave background radiation temperature of 40 K
- 1964 – A. G. Doroshkevich and Igor Dmitrievich Novikov
publish a brief paper suggesting microwave searches for the black-body
radiation predicted by Gamow, Alpher, and Herman, where they name the
CMB radiation phenomenon as detectable.
- 1964–65 – Arno Penzias and Robert Woodrow Wilson measure the temperature to be approximately 3 K. Robert Dicke, James Peebles, P. G. Roll, and D. T. Wilkinson interpret this radiation as a signature of the big bang.
- 1966 – Rainer K. Sachs and Arthur M. Wolfe theoretically predict microwave background fluctuation amplitudes created by gravitational potential variations between observers and the last scattering surface (see Sachs-Wolfe effect)
- 1968 – Martin Rees and Dennis Sciama theoretically predict microwave background fluctuation amplitudes created by photons traversing time-dependent potential wells
- 1969 – R. A. Sunyaev and Yakov Zel'dovich study the inverse Compton scattering of microwave background photons by hot electrons (see Sunyaev–Zel'dovich effect)
- 1983 – Researchers from the Cambridge Radio Astronomy Group and the Owens Valley Radio Observatory first detect the Sunyaev–Zel'dovich effect from clusters of galaxies
- 1983 – RELIKT-1 Soviet CMB anisotropy experiment was launched.
- 1990 – FIRAS on the Cosmic Background Explorer
(COBE) satellite measures the black body form of the CMB spectrum with
exquisite precision, and shows that the microwave background has a
nearly perfect black-body spectrum and thereby strongly constrains the
density of the intergalactic medium.
- January 1992 – Scientists that analysed data from the RELIKT-1 report the discovery of anisotropy in the cosmic microwave background at the Moscow astrophysical seminar.
- 1992 – Scientists that analysed data from COBE DMR report the discovery of anisotropy in the cosmic microwave background.
- 1995 – The Cosmic Anisotropy Telescope performs the first high resolution observations of the cosmic microwave background.
- 1999 – First measurements of acoustic oscillations in the CMB
anisotropy angular power spectrum from the TOCO, BOOMERANG, and Maxima
Experiments. The BOOMERanG experiment makes higher quality maps at intermediate resolution, and confirms that the universe is "flat".
- 2002 – Polarization discovered by DASI.
- 2003 – E-mode polarization spectrum obtained by the CBI. The CBI and the Very Small Array produces yet higher quality maps at high resolution (covering small areas of the sky).
- 2003 – The Wilkinson Microwave Anisotropy Probe spacecraft produces an even higher quality map at low and intermediate resolution of the whole sky (WMAP provides no high-resolution data, but improves on the intermediate resolution maps from BOOMERanG).
- 2004 – E-mode polarization spectrum obtained by the CBI.
- 2004 – The Arcminute Cosmology Bolometer Array Receiver produces a higher quality map of the high resolution structure not mapped by WMAP.
- 2005 – The Arcminute Microkelvin Imager and the Sunyaev–Zel'dovich Array begin the first surveys for very high redshift clusters of galaxies using the Sunyaev–Zel'dovich effect.
- 2005 – Ralph A. Alpher is awarded the National Medal of Science
for his groundbreaking work in nucleosynthesis and prediction that the
universe expansion leaves behind background radiation, thus providing a
model for the Big Bang theory.
- 2006 – The long-awaited three-year WMAP results are released, confirming previous analysis, correcting several points, and including polarization data.
- 2006 – Two of COBE's principal investigators, George Smoot and John Mather, received the Nobel Prize in Physics in 2006 for their work on precision measurement of the CMBR.
- 2006–2011 – Improved measurements from WMAP, new supernova surveys ESSENCE and SNLS, and baryon acoustic oscillations from SDSS and WiggleZ, continue to be consistent with the standard Lambda-CDM model.
- 2010 – The first all-sky map from the Planck telescope is released.
- 2013 – An improved all-sky map from the Planck telescope is released, improving the measurements of WMAP and extending them to much smaller scales.
- 2014 – On March 17, 2014, astrophysicists of the BICEP2 collaboration announced the detection of inflationary gravitational waves in the B-mode power spectrum, which if confirmed, would provide clear experimental evidence for the theory of inflation. However, on 19 June 2014, lowered confidence in confirming the cosmic inflation findings was reported.
- 2015 – On January 30, 2015, the same team of astronomers from BICEP2
withdrew the claim made on the previous year. Based on the combined
data of BICEP2 and Planck, the European Space Agency announced that the signal can be entirely attributed to dust in the Milky Way.
- 2018 – The final data and maps from the Planck telescope is released, with improved measurements of the polarization on large scales.
- 2019 – Planck telescope analyses of their final 2018 data continue to be released.
