# Big Bang

The Big Bang theory is the prevailing cosmological model of the observable universe from the earliest known periods through its subsequent large-scale evolution.[1][2][3] The model describes how the universe expanded from an initial state of high density and temperature,[4] and offers a comprehensive explanation for a broad range of observed phenomena, including the abundance of light elements, the cosmic microwave background (CMB) radiation, and large-scale structure.

Timeline of the metric expansion of space, where space, including hypothetical non-observable portions of the universe, is represented at each time by the circular sections. On the left, the dramatic expansion occurs in the inflationary epoch; and at the center, the expansion accelerates (artist's concept; not to scale).

Crucially, the theory is compatible with Hubble–Lemaître law — the observation that the farther away galaxies are, the faster they are moving away from Earth. Extrapolating this cosmic expansion backwards in time using the known laws of physics, the theory describes an increasingly concentrated cosmos preceded by a singularity in which space and time lose meaning (typically named "the Big Bang singularity").[5] Detailed measurements of the expansion rate of the universe place the Big Bang singularity at around 13.8 billion years ago, which is thus considered the age of the universe.[6]

After its initial expansion, an event that is by itself often called "the Big Bang", the universe cooled sufficiently to allow the formation of subatomic particles, and later atoms. Giant clouds of these primordial elements – mostly hydrogen, with some helium and lithium – later coalesced through gravity, forming early stars and galaxies, the descendants of which are visible today. Besides these primordial building materials, astronomers observe the gravitational effects of an unknown dark matter surrounding galaxies. Most of the gravitational potential in the universe seems to be in this form, and the Big Bang theory and various observations indicate that this excess gravitational potential is not created by baryonic matter, such as normal atoms. Measurements of the redshifts of supernovae indicate that the expansion of the universe is accelerating, an observation attributed to dark energy's existence.[7]

Georges Lemaître first noted in 1927 that an expanding universe could be traced back in time to an originating single point, which he called the "primeval atom". Edwin Hubble confirmed through analysis of galactic redshifts in 1929 that galaxies are indeed drifting apart; this is important observational evidence for an expanding universe. For several decades, the scientific community was divided between supporters of the Big Bang and the rival steady-state model which both offered explanations for the observed expansion, but the steady-state model stipulated an eternal universe in contrast to the Big Bang's finite age. In 1964, the CMB was discovered, which convinced many cosmologists that the steady-state theory was falsified,[8] since, unlike the steady-state theory, the hot Big Bang predicted a uniform background radiation throughout the universe caused by the high temperatures and densities in the distant past. A wide range of empirical evidence strongly favors the Big Bang, which is now essentially universally accepted.[9]

## Features of the model

The Big Bang theory offers a comprehensive explanation for a broad range of observed phenomena, including the abundances of the light elements, the CMB, large-scale structure, and Hubble's law.[10] The theory depends on two major assumptions: the universality of physical laws and the cosmological principle. The universality of physical laws is one of the underlying principles of the theory of relativity. The cosmological principle states that on large scales the universe is homogeneous and isotropic – appearing the same in all directions regardless of location.[11]

These ideas were initially taken as postulates, but later efforts were made to test each of them. For example, the first assumption has been tested by observations showing that largest possible deviation of the fine-structure constant over much of the age of the universe is of order 10−5.[12] Also, general relativity has passed stringent tests on the scale of the Solar System and binary stars.[13][14][notes 1]

The large-scale universe appears isotropic as viewed from Earth. If it is indeed isotropic, the cosmological principle can be derived from the simpler Copernican principle, which states that there is no preferred (or special) observer or vantage point. To this end, the cosmological principle has been confirmed to a level of 10−5 via observations of the temperature of the CMB. At the scale of the CMB horizon, the universe has been measured to be homogeneous with an upper bound on the order of 10% inhomogeneity, as of 1995.[15]

### Expansion of space

The expansion of the Universe was inferred from early twentieth century astronomical observations and is an essential ingredient of the Big Bang theory. Mathematically, general relativity describes spacetime by a metric, which determines the distances that separate nearby points. The points, which can be galaxies, stars, or other objects, are specified using a coordinate chart or "grid" that is laid down over all spacetime. The cosmological principle implies that the metric should be homogeneous and isotropic on large scales, which uniquely singles out the Friedmann–Lemaître–Robertson–Walker (FLRW) metric. This metric contains a scale factor, which describes how the size of the universe changes with time. This enables a convenient choice of a coordinate system to be made, called comoving coordinates. In this coordinate system, the grid expands along with the universe, and objects that are moving only because of the expansion of the universe, remain at fixed points on the grid. While their coordinate distance (comoving distance) remains constant, the physical distance between two such co-moving points expands proportionally with the scale factor of the universe.[16]

The Big Bang is not an explosion of matter moving outward to fill an empty universe. Instead, space itself expands with time everywhere and increases the physical distances between comoving points. In other words, the Big Bang is not an explosion in space, but rather an expansion of space.[4] Because the FLRW metric assumes a uniform distribution of mass and energy, it applies to our universe only on large scales—local concentrations of matter such as our galaxy do not necessarily expand with the same speed as the whole Universe.[17]

### Horizons

An important feature of the Big Bang spacetime is the presence of particle horizons. Since the universe has a finite age, and light travels at a finite speed, there may be events in the past whose light has not yet had time to reach us. This places a limit or a past horizon on the most distant objects that can be observed. Conversely, because space is expanding, and more distant objects are receding ever more quickly, light emitted by us today may never "catch up" to very distant objects. This defines a future horizon, which limits the events in the future that we will be able to influence. The presence of either type of horizon depends on the details of the FLRW model that describes our universe.[18]

Our understanding of the universe back to very early times suggests that there is a past horizon, though in practice our view is also limited by the opacity of the universe at early times. So our view cannot extend further backward in time, though the horizon recedes in space. If the expansion of the universe continues to accelerate, there is a future horizon as well.[18]

### Thermalisation

Some processes in the early universe occurred too slowly, compared to the expansion rate of the universe, to reach approximate thermodynamic equilibrium. Others were fast enough to reach thermalisation. The parameter usually used to find out whether a process in the very early universe has reached thermal equilibrium is the ratio between the rate of the process (usually rate of collisions between particles) and the Hubble parameter. The larger the ratio, the more time particles had to thermalise before they were too far away from each other.[19]

## Timeline

 A graphical timeline is available atGraphical timeline of the Big Bang

According to the Big Bang theory, the universe at the beginning was very hot and very compact, and since then it has been expanding and cooling down.

### Singularity

Extrapolation of the expansion of the universe backwards in time using general relativity yields an infinite density and temperature at a finite time in the past.[20] This irregular behavior, known as the gravitational singularity, indicates that general relativity is not an adequate description of the laws of physics in this regime. Models based on general relativity alone can not extrapolate toward the singularity—before the end of the so-called Planck epoch.[5]

This primordial singularity is itself sometimes called "the Big Bang",[21] but the term can also refer to a more generic early hot, dense phase[22][notes 2] of the universe. In either case, "the Big Bang" as an event is also colloquially referred to as the "birth" of our universe since it represents the point in history where the universe can be verified to have entered into a regime where the laws of physics as we understand them (specifically general relativity and the Standard Model of particle physics) work. Based on measurements of the expansion using Type Ia supernovae and measurements of temperature fluctuations in the cosmic microwave background, the time that has passed since that event—known as the "age of the universe"—is 13.799 ± 0.021 billion years.[23]

Despite being extremely dense at this time—far denser than is usually required to form a black hole—the universe did not re-collapse into a singularity. Commonly used calculations and limits for explaining gravitational collapse are usually based upon objects of relatively constant size, such as stars, and do not apply to rapidly expanding space such as the Big Bang. Since the early universe did not immediately collapse into a multitude of black holes, matter at that time must have been very evenly distributed with a negligible density gradient.[24]

### Inflation and baryogenesis

The earliest phases of the Big Bang are subject to much speculation, since astronomical data about them are not available. In the most common models the universe was filled homogeneously and isotropically with a very high energy density and huge temperatures and pressures, and was very rapidly expanding and cooling. The period from 0 to 10−43 seconds into the expansion, the Planck epoch, was a phase in which the four fundamental forces — the electromagnetic force, the strong nuclear force, the weak nuclear force, and the gravitational force, were unified as one.[25] In this stage, the characteristic scale length of the universe was the Planck length, 1.6×10−35 m, and consequently had a temperature of approximately 1032 degrees Celsius. Even the very concept of a particle breaks down in these conditions. A proper understanding of this period awaits the development of a theory of quantum gravity.[26][27] The Planck epoch was succeeded by the grand unification epoch beginning at 10−43 seconds, where gravitation separated from the other forces as the universe's temperature fell.[25]

At approximately 10−37 seconds into the expansion, a phase transition caused a cosmic inflation, during which the universe grew exponentially, unconstrained by the light speed invariance, and temperatures dropped by a factor of 100,000. Microscopic quantum fluctuations that occurred because of Heisenberg's uncertainty principle were amplified into the seeds that would later form the large-scale structure of the universe.[28] At a time around 10−36 seconds, the electroweak epoch begins when the strong nuclear force separates from the other forces, with only the electromagnetic force and weak nuclear force remaining unified.[29]

Inflation stopped at around the 10−33 to 10−32 seconds mark, with the universe's volume having increased by a factor of at least 1078. Reheating occurred until the universe obtained the temperatures required for the production of a quark–gluon plasma as well as all other elementary particles.[30][31] Temperatures were so high that the random motions of particles were at relativistic speeds, and particle–antiparticle pairs of all kinds were being continuously created and destroyed in collisions.[4] At some point, an unknown reaction called baryogenesis violated the conservation of baryon number, leading to a very small excess of quarks and leptons over antiquarks and antileptons—of the order of one part in 30 million. This resulted in the predominance of matter over antimatter in the present universe.[32]

### Cooling

Panoramic view of the entire near-infrared sky reveals the distribution of galaxies beyond the Milky Way. Galaxies are color-coded by redshift.

The universe continued to decrease in density and fall in temperature, hence the typical energy of each particle was decreasing. Symmetry-breaking phase transitions put the fundamental forces of physics and the parameters of elementary particles into their present form, with the electromagnetic force and weak nuclear force separating at about 10−12 seconds.[29][33] After about 10−11 seconds, the picture becomes less speculative, since particle energies drop to values that can be attained in particle accelerators. At about 10−6 seconds, quarks and gluons combined to form baryons such as protons and neutrons. The small excess of quarks over antiquarks led to a small excess of baryons over antibaryons. The temperature was now no longer high enough to create new proton–antiproton pairs (similarly for neutrons–antineutrons), so a mass annihilation immediately followed, leaving just one in 108 of the original matter particles and none of their antiparticles.[34] A similar process happened at about 1 second for electrons and positrons. After these annihilations, the remaining protons, neutrons and electrons were no longer moving relativistically and the energy density of the universe was dominated by photons (with a minor contribution from neutrinos).

A few minutes into the expansion, when the temperature was about a billion kelvin and the density of matter in the universe was comparable to the current density of Earth's atmosphere, neutrons combined with protons to form the universe's deuterium and helium nuclei in a process called Big Bang nucleosynthesis (BBN).[35] Most protons remained uncombined as hydrogen nuclei.[36]

As the universe cooled, the rest energy density of matter came to gravitationally dominate that of the photon radiation. After about 379,000 years, the electrons and nuclei combined into atoms (mostly hydrogen), which were able to emit radiation. This relic radiation, which continued through space largely unimpeded, is known as the cosmic microwave background.[36]

### Structure formation

Artist's depiction of the WMAP satellite gathering data to help scientists understand the Big Bang

Over a long period of time, the slightly denser regions of the uniformly distributed matter gravitationally attracted nearby matter and thus grew even denser, forming gas clouds, stars, galaxies, and the other astronomical structures observable today.[4] The details of this process depend on the amount and type of matter in the universe. The four possible types of matter are known as cold dark matter, warm dark matter, hot dark matter, and baryonic matter. The best measurements available, from the Wilkinson Microwave Anisotropy Probe (WMAP), show that the data is well-fit by a Lambda-CDM model in which dark matter is assumed to be cold (warm dark matter is ruled out by early reionization),[38] and is estimated to make up about 23% of the matter/energy of the universe, while baryonic matter makes up about 4.6%.[39] In an "extended model" which includes hot dark matter in the form of neutrinos,[40] then if the "physical baryon density" ${\displaystyle \Omega _{\text{b}}h^{2}}$ is estimated at about 0.023 (this is different from the 'baryon density' ${\displaystyle \Omega _{\text{b}}}$ expressed as a fraction of the total matter/energy density, which is about 0.046), and the corresponding cold dark matter density ${\displaystyle \Omega _{\text{c}}h^{2}}$ is about 0.11, the corresponding neutrino density ${\displaystyle \Omega _{\text{v}}h^{2}}$ is estimated to be less than 0.0062.[39]

### Cosmic acceleration

Independent lines of evidence from Type Ia supernovae and the CMB imply that the universe today is dominated by a mysterious form of energy known as dark energy, which apparently permeates all of space. The observations suggest 73% of the total energy density of today's universe is in this form. When the universe was very young, it was likely infused with dark energy, but with less space and everything closer together, gravity predominated, and it was slowly braking the expansion. But eventually, after numerous billion years of expansion, the declining density of matter relative to the density of dark energy caused the expansion of the universe to slowly begin to accelerate.[7]

Dark energy in its simplest formulation takes the form of the cosmological constant term in Einstein field equations of general relativity, but its composition and mechanism are unknown and, more generally, the details of its equation of state and relationship with the Standard Model of particle physics continue to be investigated both through observation and theoretically.[7]

All of this cosmic evolution after the inflationary epoch can be rigorously described and modeled by the ΛCDM model of cosmology, which uses the independent frameworks of quantum mechanics and general relativity. There are no easily testable models that would describe the situation prior to approximately 10−15 seconds.[41] Understanding this earliest of eras in the history of the universe is currently one of the greatest unsolved problems in physics.

## History

### Etymology

English astronomer Fred Hoyle is credited with coining the term "Big Bang" during a talk for a March 1949 BBC Radio broadcast,[42] saying: "These theories were based on the hypothesis that all the matter in the universe was created in one big bang at a particular time in the remote past."[43][44]

It is popularly reported that Hoyle, who favored an alternative "steady-state" cosmological model, intended this to be pejorative,[45] but Hoyle explicitly denied this and said it was just a striking image meant to highlight the difference between the two models.[46][47]

### Development

Hubble eXtreme Deep Field (XDF)
XDF size compared to the size of the Moon (XDF is the small box to the left of, and nearly below, the Moon) – several thousand galaxies, each consisting of billions of stars, are in this small view.
XDF (2012) view – each light speck is a galaxy – some of these are as old as 13.2 billion years[48] – the universe is estimated to contain 200 billion galaxies.
XDF image shows fully mature galaxies in the foreground plane – nearly mature galaxies from 5 to 9 billion years ago – protogalaxies, blazing with young stars, beyond 9 billion years.

The Big Bang theory developed from observations of the structure of the universe and from theoretical considerations. In 1912, Vesto Slipher measured the first Doppler shift of a "spiral nebula" (spiral nebula is the obsolete term for spiral galaxies), and soon discovered that almost all such nebulae were receding from Earth. He did not grasp the cosmological implications of this fact, and indeed at the time it was highly controversial whether or not these nebulae were "island universes" outside our Milky Way.[49][50] Ten years later, Alexander Friedmann, a Russian cosmologist and mathematician, derived the Friedmann equations from Einstein field equations, showing that the universe might be expanding in contrast to the static universe model advocated by Albert Einstein at that time.[51]

In 1924, American astronomer Edwin Hubble's measurement of the great distance to the nearest spiral nebulae showed that these systems were indeed other galaxies. Starting that same year, Hubble painstakingly developed a series of distance indicators, the forerunner of the cosmic distance ladder, using the 100-inch (2.5 m) Hooker telescope at Mount Wilson Observatory. This allowed him to estimate distances to galaxies whose redshifts had already been measured, mostly by Slipher. In 1929, Hubble discovered a correlation between distance and recessional velocity—now known as Hubble's law.[52][53] By that time, Lemaître had already shown that this was expected, given the cosmological principle.[7]

Independently deriving Friedmann's equations in 1927, Georges Lemaître, a Belgian physicist and Roman Catholic priest, proposed that the inferred recession of the nebulae was due to the expansion of the universe.[54] In 1931, Lemaître went further and suggested that the evident expansion of the universe, if projected back in time, meant that the further in the past the smaller the universe was, until at some finite time in the past all the mass of the universe was concentrated into a single point, a "primeval atom" where and when the fabric of time and space came into existence.[55]

In the 1920s and 1930s, almost every major cosmologist preferred an eternal steady-state universe, and several complained that the beginning of time implied by the Big Bang imported religious concepts into physics; this objection was later repeated by supporters of the steady-state theory.[56] This perception was enhanced by the fact that the originator of the Big Bang theory, Lemaître, was a Roman Catholic priest.[57] Arthur Eddington agreed with Aristotle that the universe did not have a beginning in time, viz., that matter is eternal. A beginning in time was "repugnant" to him.[58][59] Lemaître, however, disagreed:

If the world has begun with a single quantum, the notions of space and time would altogether fail to have any meaning at the beginning; they would only begin to have a sensible meaning when the original quantum had been divided into a sufficient number of quanta. If this suggestion is correct, the beginning of the world happened a little before the beginning of space and time.[60]

During the 1930s, other ideas were proposed as non-standard cosmologies to explain Hubble's observations, including the Milne model,[61] the oscillatory universe (originally suggested by Friedmann, but advocated by Albert Einstein and Richard C. Tolman)[62] and Fritz Zwicky's tired light hypothesis.[63]

After World War II, two distinct possibilities emerged. One was Fred Hoyle's steady-state model, whereby new matter would be created as the universe seemed to expand. In this model the universe is roughly the same at any point in time.[64] The other was Lemaître's Big Bang theory, advocated and developed by George Gamow, who introduced BBN[65] and whose associates, Ralph Alpher and Robert Herman, predicted the CMB.[66] Ironically, it was Hoyle who coined the phrase that came to be applied to Lemaître's theory, referring to it as "this big bang idea" during a BBC Radio broadcast in March 1949.[47][44][notes 3] For a while, support was split between these two theories. Eventually, the observational evidence, most notably from radio source counts, began to favor Big Bang over steady state. The discovery and confirmation of the CMB in 1964 secured the Big Bang as the best theory of the origin and evolution of the universe.[67] Much of the current work in cosmology includes understanding how galaxies form in the context of the Big Bang, understanding the physics of the universe at earlier and earlier times, and reconciling observations with the basic theory.

In 1968 and 1970, Roger Penrose, Stephen Hawking, and George F. R. Ellis published papers where they showed that mathematical singularities were an inevitable initial condition of relativistic models of the Big Bang.[68][69] Then, from the 1970s to the 1990s, cosmologists worked on characterizing the features of the Big Bang universe and resolving outstanding problems. In 1981, Alan Guth made a breakthrough in theoretical work on resolving certain outstanding theoretical problems in the Big Bang theory with the introduction of an epoch of rapid expansion in the early universe he called "inflation".[70] Meanwhile, during these decades, two questions in observational cosmology that generated much discussion and disagreement were over the precise values of the Hubble Constant[71] and the matter-density of the universe (before the discovery of dark energy, thought to be the key predictor for the eventual fate of the universe).[72]

In the mid-1990s, observations of certain globular clusters appeared to indicate that they were about 15 billion years old, which conflicted with most then-current estimates of the age of the universe (and indeed with the age measured today). This issue was later resolved when new computer simulations, which included the effects of mass loss due to stellar winds, indicated a much younger age for globular clusters.[73] While there still remain some questions as to how accurately the ages of the clusters are measured, globular clusters are of interest to cosmology as some of the oldest objects in the universe.

Significant progress in Big Bang cosmology has been made since the late 1990s as a result of advances in telescope technology as well as the analysis of data from satellites such as the Cosmic Background Explorer (COBE),[74] the Hubble Space Telescope and WMAP.[75] Cosmologists now have fairly precise and accurate measurements of many of the parameters of the Big Bang model, and have made the unexpected discovery that the expansion of the universe appears to be accelerating.[76][77]

## Observational evidence

"[The] big bang picture is too firmly grounded in data from every area to be proved invalid in its general features."

Lawrence Krauss[78]

The earliest and most direct observational evidence of the validity of the theory are the expansion of the universe according to Hubble's law (as indicated by the redshifts of galaxies), discovery and measurement of the cosmic microwave background and the relative abundances of light elements produced by Big Bang nucleosynthesis (BBN). More recent evidence includes observations of galaxy formation and evolution, and the distribution of large-scale cosmic structures,[79] These are sometimes called the "four pillars" of the Big Bang theory.[80]

Precise modern models of the Big Bang appeal to various exotic physical phenomena that have not been observed in terrestrial laboratory experiments or incorporated into the Standard Model of particle physics. Of these features, dark matter is currently the subject of most active laboratory investigations.[81] Remaining issues include the cuspy halo problem[82] and the dwarf galaxy problem[83] of cold dark matter. Dark energy is also an area of intense interest for scientists, but it is not clear whether direct detection of dark energy will be possible.[84] Inflation and baryogenesis remain more speculative features of current Big Bang models. Viable, quantitative explanations for such phenomena are still being sought. These are currently unsolved problems in physics.

### Hubble's law and the expansion of space

Observations of distant galaxies and quasars show that these objects are redshifted: the light emitted from them has been shifted to longer wavelengths. This can be seen by taking a frequency spectrum of an object and matching the spectroscopic pattern of emission or absorption lines corresponding to atoms of the chemical elements interacting with the light. These redshifts are uniformly isotropic, distributed evenly among the observed objects in all directions. If the redshift is interpreted as a Doppler shift, the recessional velocity of the object can be calculated. For some galaxies, it is possible to estimate distances via the cosmic distance ladder. When the recessional velocities are plotted against these distances, a linear relationship known as Hubble's law is observed:[52] ${\displaystyle v=H_{0}D}$ where

• ${\displaystyle v}$ is the recessional velocity of the galaxy or other distant object,
• ${\displaystyle D}$ is the comoving distance to the object, and
• ${\displaystyle H_{0}}$ is Hubble's constant, measured to be 70.4+1.3
−1.4
km/s/Mpc by the WMAP.[39]

Hubble's law has two possible explanations. Either we are at the center of an explosion of galaxies—which is untenable under the assumption of the Copernican principle—or the universe is uniformly expanding everywhere. This universal expansion was predicted from general relativity by Friedmann in 1922[51] and Lemaître in 1927,[54] well before Hubble made his 1929 analysis and observations, and it remains the cornerstone of the Big Bang theory as developed by Friedmann, Lemaître, Robertson, and Walker.

The theory requires the relation ${\displaystyle v=HD}$ to hold at all times, where ${\displaystyle D}$ is the comoving distance, v is the recessional velocity, and ${\displaystyle v}$, ${\displaystyle H}$, and ${\displaystyle D}$ vary as the universe expands (hence we write ${\displaystyle H_{0}}$ to denote the present-day Hubble "constant"). For distances much smaller than the size of the observable universe, the Hubble redshift can be thought of as the Doppler shift corresponding to the recession velocity ${\displaystyle v}$. However, the redshift is not a true Doppler shift, but rather the result of the expansion of the universe between the time the light was emitted and the time that it was detected.[85]

That space is undergoing metric expansion is shown by direct observational evidence of the cosmological principle and the Copernican principle, which together with Hubble's law have no other explanation. Astronomical redshifts are extremely isotropic and homogeneous,[52] supporting the cosmological principle that the universe looks the same in all directions, along with much other evidence. If the redshifts were the result of an explosion from a center distant from us, they would not be so similar in different directions.

Measurements of the effects of the cosmic microwave background radiation on the dynamics of distant astrophysical systems in 2000 proved the Copernican principle, that, on a cosmological scale, the Earth is not in a central position.[86] Radiation from the Big Bang was demonstrably warmer at earlier times throughout the universe. Uniform cooling of the CMB over billions of years is explainable only if the universe is experiencing a metric expansion, and excludes the possibility that we are near the unique center of an explosion.

The cosmic microwave background spectrum measured by the FIRAS instrument on the COBE satellite is the most-precisely measured blackbody spectrum in nature.[87] The data points and error bars on this graph are obscured by the theoretical curve.

In 1964, Arno Penzias and Robert Wilson serendipitously discovered the cosmic background radiation, an omnidirectional signal in the microwave band.[67] Their discovery provided substantial confirmation of the big-bang predictions by Alpher, Herman and Gamow around 1950. Through the 1970s, the radiation was found to be approximately consistent with a blackbody spectrum in all directions; this spectrum has been redshifted by the expansion of the universe, and today corresponds to approximately 2.725 K. This tipped the balance of evidence in favor of the Big Bang model, and Penzias and Wilson were awarded the 1978 Nobel Prize in Physics.

The surface of last scattering corresponding to emission of the CMB occurs shortly after recombination, the epoch when neutral hydrogen becomes stable. Prior to this, the universe comprised a hot dense photon-baryon plasma sea where photons were quickly scattered from free charged particles. Peaking at around 372±14 kyr,[38] the mean free path for a photon becomes long enough to reach the present day and the universe becomes transparent.

9 year WMAP image of the cosmic microwave background radiation (2012).[88][89] The radiation is isotropic to roughly one part in 100,000.[90]

In 1989, NASA launched COBE, which made two major advances: in 1990, high-precision spectrum measurements showed that the CMB frequency spectrum is an almost perfect blackbody with no deviations at a level of 1 part in 104, and measured a residual temperature of 2.726 K (more recent measurements have revised this figure down slightly to 2.7255 K); then in 1992, further COBE measurements discovered tiny fluctuations (anisotropies) in the CMB temperature across the sky, at a level of about one part in 105.[74] John C. Mather and George Smoot were awarded the 2006 Nobel Prize in Physics for their leadership in these results.

During the following decade, CMB anisotropies were further investigated by a large number of ground-based and balloon experiments. In 2000–2001, several experiments, most notably BOOMERanG, found the shape of the universe to be spatially almost flat by measuring the typical angular size (the size on the sky) of the anisotropies.[91][92][93]

In early 2003, the first results of the Wilkinson Microwave Anisotropy Probe were released, yielding what were at the time the most accurate values for some of the cosmological parameters. The results disproved several specific cosmic inflation models, but are consistent with the inflation theory in general.[75] The Planck space probe was launched in May 2009. Other ground and balloon-based cosmic microwave background experiments are ongoing.

### Abundance of primordial elements

Using the Big Bang model, it is possible to calculate the concentration of helium-4, helium-3, deuterium, and lithium-7 in the universe as ratios to the amount of ordinary hydrogen.[35] The relative abundances depend on a single parameter, the ratio of photons to baryons. This value can be calculated independently from the detailed structure of CMB fluctuations. The ratios predicted (by mass, not by number) are about 0.25 for ${\displaystyle {\ce {^4He/H}}}$, about 10−3 for ${\displaystyle {\ce {^2H/H}}}$, about 10−4 for ${\displaystyle {\ce {^3He/H}}}$ and about 10−9 for ${\displaystyle {\ce {^7Li/H}}}$.[35]

The measured abundances all agree at least roughly with those predicted from a single value of the baryon-to-photon ratio. The agreement is excellent for deuterium, close but formally discrepant for ${\displaystyle {\ce {^4He}}}$, and off by a factor of two for ${\displaystyle {\ce {^7Li}}}$ (this anomaly is known as the cosmological lithium problem); in the latter two cases, there are substantial systematic uncertainties. Nonetheless, the general consistency with abundances predicted by BBN is strong evidence for the Big Bang, as the theory is the only known explanation for the relative abundances of light elements, and it is virtually impossible to "tune" the Big Bang to produce much more or less than 20–30% helium.[94] Indeed, there is no obvious reason outside of the Big Bang that, for example, the young universe (i.e., before star formation, as determined by studying matter supposedly free of stellar nucleosynthesis products) should have more helium than deuterium or more deuterium than ${\displaystyle {\ce {^3He}}}$, and in constant ratios, too.[95]:182–185

### Galactic evolution and distribution

Detailed observations of the morphology and distribution of galaxies and quasars are in agreement with the current state of the Big Bang theory. A combination of observations and theory suggest that the first quasars and galaxies formed about a billion years after the Big Bang, and since then, larger structures have been forming, such as galaxy clusters and superclusters.[96]

Populations of stars have been aging and evolving, so that distant galaxies (which are observed as they were in the early universe) appear very different from nearby galaxies (observed in a more recent state). Moreover, galaxies that formed relatively recently, appear markedly different from galaxies formed at similar distances but shortly after the Big Bang. These observations are strong arguments against the steady-state model. Observations of star formation, galaxy and quasar distributions and larger structures, agree well with Big Bang simulations of the formation of structure in the universe, and are helping to complete details of the theory.[96][97]

### Primordial gas clouds

Focal plane of BICEP2 telescope under a microscope - used to search for polarization in the CMB.[98][99][100][101]

In 2011, astronomers found what they believe to be pristine clouds of primordial gas by analyzing absorption lines in the spectra of distant quasars. Before this discovery, all other astronomical objects have been observed to contain heavy elements that are formed in stars. These two clouds of gas contain no elements heavier than hydrogen and deuterium.[102][103] Since the clouds of gas have no heavy elements, they likely formed in the first few minutes after the Big Bang, during BBN.

### Other lines of evidence

The age of the universe as estimated from the Hubble expansion and the CMB is now in good agreement with other estimates using the ages of the oldest stars, both as measured by applying the theory of stellar evolution to globular clusters and through radiometric dating of individual Population II stars.[104] It is also in good agreement with age estimates based on measurements of the expansion using Type Ia supernovae and measurements of temperature fluctuations in the cosmic microwave background.[23] The agreement of independent measurements of this age supports the Lambda-CDM (ΛCDM) model, since the model is used to relate some of the measurements to an age estimate, and all estimates turn out to agree. Still, some observations of objects from the relatively early universe (in particular quasar APM 08279+5255) raise concern as to whether these objects had enough time to form so early in the ΛCDM model.[105][106]

The prediction that the CMB temperature was higher in the past has been experimentally supported by observations of very low temperature absorption lines in gas clouds at high redshift.[107] This prediction also implies that the amplitude of the Sunyaev–Zel'dovich effect in clusters of galaxies does not depend directly on redshift. Observations have found this to be roughly true, but this effect depends on cluster properties that do change with cosmic time, making precise measurements difficult.[108][109]

### Future observations

Future gravitational-wave observatories might be able to detect primordial gravitational waves, relics of the early universe, up to less than a second after the Big Bang.[110][111]

As with any theory, a number of mysteries and problems have arisen as a result of the development of the Big Bang theory. Some of these mysteries and problems have been resolved while others are still outstanding. Proposed solutions to some of the problems in the Big Bang model have revealed new mysteries of their own. For example, the horizon problem, the magnetic monopole problem, and the flatness problem are most commonly resolved with inflationary theory, but the details of the inflationary universe are still left unresolved and many, including some founders of the theory, say it has been disproven.[112][113][114][115] What follows are a list of the mysterious aspects of the Big Bang theory still under intense investigation by cosmologists and astrophysicists.

### Baryon asymmetry

It is not yet understood why the universe has more matter than antimatter.[32] It is generally assumed that when the universe was young and very hot it was in statistical equilibrium and contained equal numbers of baryons and antibaryons. However, observations suggest that the universe, including its most distant parts, is made almost entirely of matter. A process called baryogenesis was hypothesized to account for the asymmetry. For baryogenesis to occur, the Sakharov conditions must be satisfied. These require that baryon number is not conserved, that C-symmetry and CP-symmetry are violated and that the universe depart from thermodynamic equilibrium.[116] All these conditions occur in the Standard Model, but the effects are not strong enough to explain the present baryon asymmetry.

### Dark energy

Measurements of the redshift–magnitude relation for type Ia supernovae indicate that the expansion of the universe has been accelerating since the universe was about half its present age. To explain this acceleration, general relativity requires that much of the energy in the universe consists of a component with large negative pressure, dubbed "dark energy".[7]

Dark energy, though speculative, solves numerous problems. Measurements of the cosmic microwave background indicate that the universe is very nearly spatially flat, and therefore according to general relativity the universe must have almost exactly the critical density of mass/energy. But the mass density of the universe can be measured from its gravitational clustering, and is found to have only about 30% of the critical density.[7] Since theory suggests that dark energy does not cluster in the usual way it is the best explanation for the "missing" energy density. Dark energy also helps to explain two geometrical measures of the overall curvature of the universe, one using the frequency of gravitational lenses,[117] and the other using the characteristic pattern of the large-scale structure as a cosmic ruler.

Negative pressure is believed to be a property of vacuum energy, but the exact nature and existence of dark energy remains one of the great mysteries of the Big Bang. Results from the WMAP team in 2008 are in accordance with a universe that consists of 73% dark energy, 23% dark matter, 4.6% regular matter and less than 1% neutrinos.[39] According to theory, the energy density in matter decreases with the expansion of the universe, but the dark energy density remains constant (or nearly so) as the universe expands. Therefore, matter made up a larger fraction of the total energy of the universe in the past than it does today, but its fractional contribution will fall in the far future as dark energy becomes even more dominant.

The dark energy component of the universe has been explained by theorists using a variety of competing theories including Einstein's cosmological constant but also extending to more exotic forms of quintessence or other modified gravity schemes.[118] A cosmological constant problem, sometimes called the "most embarrassing problem in physics", results from the apparent discrepancy between the measured energy density of dark energy, and the one naively predicted from Planck units.[119]

### Dark matter

Chart shows the proportion of different components of the universe   about 95% is dark matter and dark energy.

During the 1970s and the 1980s, various observations showed that there is not sufficient visible matter in the universe to account for the apparent strength of gravitational forces within and between galaxies. This led to the idea that up to 90% of the matter in the universe is dark matter that does not emit light or interact with normal baryonic matter. In addition, the assumption that the universe is mostly normal matter led to predictions that were strongly inconsistent with observations. In particular, the universe today is far more lumpy and contains far less deuterium than can be accounted for without dark matter. While dark matter has always been controversial, it is inferred by various observations: the anisotropies in the CMB, galaxy cluster velocity dispersions, large-scale structure distributions, gravitational lensing studies, and X-ray measurements of galaxy clusters.[120]

Indirect evidence for dark matter comes from its gravitational influence on other matter, as no dark matter particles have been observed in laboratories. Many particle physics candidates for dark matter have been proposed, and several projects to detect them directly are underway.[121]

Additionally, there are outstanding problems associated with the currently favored cold dark matter model which include the dwarf galaxy problem[83] and the cuspy halo problem.[82] Alternative theories have been proposed that do not require a large amount of undetected matter, but instead modify the laws of gravity established by Newton and Einstein; yet no alternative theory has been as successful as the cold dark matter proposal in explaining all extant observations.[122]

### Horizon problem

The horizon problem results from the premise that information cannot travel faster than light. In a universe of finite age this sets a limit—the particle horizon—on the separation of any two regions of space that are in causal contact.[123] The observed isotropy of the CMB is problematic in this regard: if the universe had been dominated by radiation or matter at all times up to the epoch of last scattering, the particle horizon at that time would correspond to about 2 degrees on the sky. There would then be no mechanism to cause wider regions to have the same temperature.[95]:191–202

A resolution to this apparent inconsistency is offered by inflationary theory in which a homogeneous and isotropic scalar energy field dominates the universe at some very early period (before baryogenesis). During inflation, the universe undergoes exponential expansion, and the particle horizon expands much more rapidly than previously assumed, so that regions presently on opposite sides of the observable universe are well inside each other's particle horizon. The observed isotropy of the CMB then follows from the fact that this larger region was in causal contact before the beginning of inflation.[28]:180–186

Heisenberg's uncertainty principle predicts that during the inflationary phase there would be quantum thermal fluctuations, which would be magnified to a cosmic scale. These fluctuations served as the seeds for all the current structures in the universe.[95]:207 Inflation predicts that the primordial fluctuations are nearly scale invariant and Gaussian, which has been accurately confirmed by measurements of the CMB.[75]:sec 6

If inflation occurred, exponential expansion would push large regions of space well beyond our observable horizon.[28]:180–186

A related issue to the classic horizon problem arises because in most standard cosmological inflation models, inflation ceases well before electroweak symmetry breaking occurs, so inflation should not be able to prevent large-scale discontinuities in the electroweak vacuum since distant parts of the observable universe were causally separate when the electroweak epoch ended.[124]

### Magnetic monopoles

The magnetic monopole objection was raised in the late 1970s. Grand Unified theories (GUTs) predicted topological defects in space that would manifest as magnetic monopoles. These objects would be produced efficiently in the hot early universe, resulting in a density much higher than is consistent with observations, given that no monopoles have been found. This problem is resolved by cosmic inflation, which removes all point defects from the observable universe, in the same way that it drives the geometry to flatness.[123]

### Flatness problem

The overall geometry of the universe is determined by whether the Omega cosmological parameter is less than, equal to or greater than 1. Shown from top to bottom are a closed universe with positive curvature, a hyperbolic universe with negative curvature and a flat universe with zero curvature.

The flatness problem (also known as the oldness problem) is an observational problem associated with a FLRW.[123] The universe may have positive, negative, or zero spatial curvature depending on its total energy density. Curvature is negative if its density is less than the critical density; positive if greater; and zero at the critical density, in which case space is said to be flat. Observations indicate the universe is consistent with being flat.[125][126]

The problem is that any small departure from the critical density grows with time, and yet the universe today remains very close to flat.[notes 4] Given that a natural timescale for departure from flatness might be the Planck time, 10−43 seconds,[4] the fact that the universe has reached neither a heat death nor a Big Crunch after billions of years requires an explanation. For instance, even at the relatively late age of a few minutes (the time of nucleosynthesis), the density of the universe must have been within one part in 1014 of its critical value, or it would not exist as it does today.[127]

## Ultimate fate of the universe

Before observations of dark energy, cosmologists considered two scenarios for the future of the universe. If the mass density of the universe were greater than the critical density, then the universe would reach a maximum size and then begin to collapse. It would become denser and hotter again, ending with a state similar to that in which it started—a Big Crunch.[18]

Alternatively, if the density in the universe were equal to or below the critical density, the expansion would slow down but never stop. Star formation would cease with the consumption of interstellar gas in each galaxy; stars would burn out, leaving white dwarfs, neutron stars, and black holes. Collisions between these would result in mass accumulating into larger and larger black holes. The average temperature of the universe would very gradually asymptotically approach absolute zero—a Big Freeze.[128] Moreover, if protons are unstable, then baryonic matter would disappear, leaving only radiation and black holes. Eventually, black holes would evaporate by emitting Hawking radiation. The entropy of the universe would increase to the point where no organized form of energy could be extracted from it, a scenario known as heat death.[129]

Modern observations of accelerating expansion imply that more and more of the currently visible universe will pass beyond our event horizon and out of contact with us. The eventual result is not known. The ΛCDM model of the universe contains dark energy in the form of a cosmological constant. This theory suggests that only gravitationally bound systems, such as galaxies, will remain together, and they too will be subject to heat death as the universe expands and cools. Other explanations of dark energy, called phantom energy theories, suggest that ultimately galaxy clusters, stars, planets, atoms, nuclei, and matter itself will be torn apart by the ever-increasing expansion in a so-called Big Rip.[130]

## Misconceptions

One of the common misconceptions about the Big Bang model is that it fully explains the origin of the universe. However, the Big Bang model does not describe how energy, time, and space were caused, but rather it describes the emergence of the present universe from an ultra-dense and high-temperature initial state.[131] It is misleading to visualize the Big Bang by comparing its size to everyday objects. When the size of the universe at Big Bang is described, it refers to the size of the observable universe, and not the entire universe.[17]

Hubble's law predicts that galaxies that are beyond Hubble distance recede faster than the speed of light. However, special relativity does not apply beyond motion through space. Hubble's law describes velocity that results from expansion of space, rather than through space.[17]

Astronomers often refer to the cosmological redshift as a Doppler shift which can lead to a misconception.[17] Although similar, the cosmological redshift is not identical to the classically derived Doppler redshift because most elementary derivations of the Doppler redshift do not accommodate the expansion of space. Accurate derivation of the cosmological redshift requires the use of general relativity, and while a treatment using simpler Doppler effect arguments gives nearly identical results for nearby galaxies, interpreting the redshift of more distant galaxies as due to the simplest Doppler redshift treatments can cause confusion.[17]

## Pre–Big Bang cosmology

The Big Bang explains the evolution of the universe from a starting density and temperature that is well beyond humanity's capability to replicate, so extrapolations to the most extreme conditions and earliest times are necessarily more speculative. Lemaître called this initial state the "primeval atom" while Gamow called the material "ylem". How the initial state of the universe originated is still an open question, but the Big Bang model does constrain some of its characteristics. For example, specific laws of nature most likely came to existence in a random way, but as inflation models show, some combinations of these are far more probable.[132] A topologically flat universe implies a balance between gravitational potential energy and other energy forms, requiring no additional energy to be created.[125][126]

The Big Bang theory, built upon the equations of classical general relativity, indicates a singularity at the origin of cosmic time, and such an infinite energy density may be a physical impossibility. However, the physical theories of general relativity and quantum mechanics as currently realized are not applicable before the Planck epoch, and correcting this will require the development of a correct treatment of quantum gravity.[20] Certain quantum gravity treatments, such as the Wheeler–DeWitt equation, imply that time itself could be an emergent property.[133] As such, physics may conclude that time did not exist before the Big Bang.[134][135]

While it is not known what could have preceded the hot dense state of the early universe or how and why it originated, or even whether such questions are sensible, speculation abounds on the subject of "cosmogony".

Some speculative proposals in this regard, each of which entails untested hypotheses, are:

• The simplest models, in which the Big Bang was caused by quantum fluctuations. That scenario had very little chance of happening, but, according to the totalitarian principle, even the most improbable event will eventually happen. It took place instantly, in our perspective, due to the absence of perceived time before the Big Bang.[136][137][138][139]
• Models including the Hartle–Hawking no-boundary condition, in which the whole of spacetime is finite; the Big Bang does represent the limit of time but without any singularity.[140] In such case, the universe is self-sufficient.[141]
• Brane cosmology models, in which inflation is due to the movement of branes in string theory; the pre-Big Bang model; the ekpyrotic model, in which the Big Bang is the result of a collision between branes; and the cyclic model, a variant of the ekpyrotic model in which collisions occur periodically. In the latter model the Big Bang was preceded by a Big Crunch and the universe cycles from one process to the other.[142][143][144][145]
• Eternal inflation, in which universal inflation ends locally here and there in a random fashion, each end-point leading to a bubble universe, expanding from its own big bang.[146][147]

Proposals in the last two categories see the Big Bang as an event in either a much larger and older universe or in a multiverse.

## Religious and philosophical interpretations

As a description of the origin of the universe, the Big Bang has significant bearing on religion and philosophy.[148][149] As a result, it has become one of the liveliest areas in the discourse between science and religion.[150] Some believe the Big Bang implies a creator,[151][152] while others argue that Big Bang cosmology makes the notion of a creator superfluous.[149][153]

• Anthropic principle  Philosophical premise that all scientific observations presuppose a universe compatible with the emergence of sentient organisms that make those observations
• Big Bounce  Hypothetical cosmological model for the origin of the known universe
• Big Crunch  Theoretical scenario for the ultimate fate of the universe
• Cold Big Bang  A designation of an absolute zero temperature at the beginning of the Universe
• Cosmic Calendar
• Cosmogony  Branch of science or a theory concerning the origin of the universe.
• Eureka: A Prose Poem  A lengthy non-fiction work by American author Edgar Allan Poe, a Big Bang speculation
• Future of an expanding universe  Future scenario assuming that the expansion of the universe will continue forever
• Heat death of the universe  Possible fate of the universe. Also known as the Big Chill and the Big Freeze
• Shape of the universe  The local and global geometry of the universe
• Steady-state model  Model of the evolution of the universe, a discredited theory that denied the Big Bang and posited that the universe always existed.

## Notes

1. Further information of, and references for, tests of general relativity are given in the article tests of general relativity.
2. There is no consensus about how long the Big Bang phase lasted. For some writers, this denotes only the initial singularity, for others the whole history of the universe. Usually, at least the first few minutes (during which helium is synthesized) are said to occur "during the Big Bang".
3. It is commonly reported that Hoyle intended this to be pejorative. However, Hoyle later denied that, saying that it was just a striking image meant to emphasize the difference between the two theories for radio listeners.[46]
4. Strictly, dark energy in the form of a cosmological constant drives the universe towards a flat state; however, our universe remained close to flat for several billion years before the dark energy density became significant.

## References

1. Silk 2009, p. 208.
2. Singh 2004, p. 560. Book limited to 532 pages. Correct source page requested.
3. NASA/WMAP Science Team (6 June 2011). "Cosmology: The Study of the Universe". Universe 101: Big Bang Theory. Washington, D.C.: NASA. Archived from the original on 29 June 2011. Retrieved 18 December 2019. The second section discusses the classic tests of the Big Bang theory that make it so compelling as the most likely valid and accurate description of our universe.
4. Bridge, Mark (Director) (30 July 2014). First Second of the Big Bang. How The Universe Works. Silver Spring, MD. Science Channel.
5. Chow 2008, p. 211
6. "Planck reveals an almost perfect universe". Max-Planck-Gesellschaft. 21 March 2013. Retrieved 17 November 2020.
7. Peebles, P. J. E.; Ratra, Bharat (22 April 2003). "The cosmological constant and dark energy". Reviews of Modern Physics. 75 (2): 559–606. arXiv:astro-ph/0207347. Bibcode:2003RvMP...75..559P. doi:10.1103/RevModPhys.75.559. S2CID 118961123.
8. Kragh 1996, p. 319: "At the same time that observations tipped the balance definitely in favor of relativistic big-bang theory, ..."
9. Wright, Edward L. (24 May 2013). "Frequently Asked Questions in Cosmology: What is the evidence for the Big Bang?". Ned Wright's Cosmology Tutorial. Los Angeles: Division of Astronomy & Astrophysics, University of California, Los Angeles. Archived from the original on 20 June 2013. Retrieved 25 November 2019.
10. Francis, Charles (2018). Light after Dark I: Structures of the Sky. Troubador Publishing Ltd. p. 199. ISBN 9781785897122.
11. Ivanchik, Alexandre V.; Potekhin, Alexander Y.; Varshalovich, Dmitry A. (March 1999). "The fine-structure constant: a new observational limit on its cosmological variation and some theoretical consequences". Astronomy & Astrophysics. 343 (2): 439–445. arXiv:astro-ph/9810166. Bibcode:1999A&A...343..439I.
12. Turyshev, Slava G. (November 2008). "Experimental Tests of General Relativity". Annual Review of Nuclear and Particle Science. 58 (1): 207–248. arXiv:0806.1731. Bibcode:2008ARNPS..58..207T. doi:10.1146/annurev.nucl.58.020807.111839. S2CID 119199160.
13. Ishak, Mustapha (December 2019). "Testing general relativity in cosmology". Living Reviews in Relativity. 22 (1): 204. arXiv:1806.10122. Bibcode:2019LRR....22....1I. doi:10.1007/s41114-018-0017-4. PMC 6299071. PMID 30613193. 1.
14. Goodman, Jeremy (15 August 1995). "Geocentrism reexamined" (PDF). Physical Review D. 52 (4): 1821–1827. arXiv:astro-ph/9506068. Bibcode:1995PhRvD..52.1821G. doi:10.1103/PhysRevD.52.1821. PMID 10019408. S2CID 37979862. Archived (PDF) from the original on 2 May 2019. Retrieved 2 December 2019.
15. d'Inverno 1992, chpt. 23
16. Davis, Tamara M.; Lineweaver, Charles H. (31 March 2004). "Expanding Confusion: Common Misconceptions of Cosmological Horizons and the Superluminal Expansion of the Universe". Publications of the Astronomical Society of Australia. 21 (1): 97–109. arXiv:astro-ph/0310808. Bibcode:2004PASA...21...97D. doi:10.1071/as03040. S2CID 13068122.
17. Kolb & Turner 1988, chpt. 3
18. Enqvist, K.; Sirkka, J. (September 1993). "Chemical equilibrium in QCD gas in the early universe". Physics Letters B. 314 (3–4): 298–302. arXiv:hep-ph/9304273. Bibcode:1993PhLB..314..298E. doi:10.1016/0370-2693(93)91239-J. S2CID 119406262.
19. Hawking & Ellis 1973
20. Roos 2012, p. 216: "This singularity is termed the Big Bang."
21. Drees 1990, pp. 223–224
22. Planck Collaboration (October 2016). "Planck 2015 results. XIII. Cosmological parameters". Astronomy & Astrophysics. 594: Article A13. arXiv:1502.01589. Bibcode:2016A&A...594A..13P. doi:10.1051/0004-6361/201525830. S2CID 119262962. (See Table 4, Age/Gyr, last column.)
23. Musser, George (22 September 2003). "Why didn't all this matter immediately collapse into a black hole?". Scientific American. Retrieved 22 March 2020.
24. Unruh, W.G.; Semenoff, G.W., eds. (1988). The early universe. Reidel. ISBN 90-277-2619-1. OCLC 905464231.
25. Hawley, John F.; Holcomb, Katherine A. (7 July 2005). Foundations of Modern Cosmology. OUP Oxford. p. 355. ISBN 9780198530961.
26. "Brief History of the Universe". www.astro.ucla.edu. Retrieved 28 April 2020.
27. Guth 1998
28. "Big Bang models back to Planck time". hyperphysics.phy-astr.gsu.edu. Retrieved 28 April 2020.
29. Schewe, Phillip F.; Stein, Ben P. (20 April 2005). "An Ocean of Quarks". Physics News Update. Vol. 728 no. 1. Archived from the original on 23 April 2005. Retrieved 30 November 2019.
30. Høg, Erik (2014). "Astrosociology: Interviews about an infinite universe". Asian Journal of Physics. arXiv:1408.4795. Bibcode:2014arXiv1408.4795H.
31. Kolb & Turner 1988, chpt. 6
32. Kolb & Turner 1988, chpt. 7
33. Weenink, Jan (26 February 2009). "Baryogenesis" (PDF). Tomislav Prokopec.
34. Kolb & Turner 1988, chpt. 4
35. Peacock 1999, chpt. 9
36. Clavin, Whitney; Jenkins, Ann; Villard, Ray (7 January 2014). "NASA's Hubble and Spitzer Team up to Probe Faraway Galaxies". Jet Propulsion Laboratory. Washington, D.C.: NASA. Archived from the original on 3 September 2019. Retrieved 8 January 2014.
37. Spergel, David N.; Verde, Licia; Peiris, Hiranya V.; et al. (September 2003). "First-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Determination of Cosmological Parameters". The Astrophysical Journal Supplement Series. 148 (1): 175–194. arXiv:astro-ph/0302209. Bibcode:2003ApJS..148..175S. doi:10.1086/377226. S2CID 10794058.
38. Jarosik, Norman; Bennett, Charles L.; Dunkley, Jo; et al. (February 2011). "Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Sky Maps, Systematic Errors, and Basic Results" (PDF). The Astrophysical Journal Supplement Series. 192 (2): Article 14. arXiv:1001.4744. Bibcode:2011ApJS..192...14J. doi:10.1088/0067-0049/192/2/14. hdl:2152/43001. S2CID 46171526. Archived (PDF) from the original on 14 September 2019. Retrieved 2 December 2019. (See Table 8.)
39. Overbye, Dennis (15 April 2020). "Why The Big Bang Produced Something Rather Than Nothing - How did matter gain the edge over antimatter in the early universe? Maybe, just maybe, neutrinos". The New York Times. Retrieved 16 April 2020.
40. Manly 2011, chpt. 7: "The Ultimate Free Lunch".
41. "'Big bang' astronomer dies". Sci/Tech. BBC News. London: BBC. 22 August 2001. Archived from the original on 3 September 2019. Retrieved 2 December 2019.
42. "Hoyle on the Radio: Creating the 'Big Bang'". Fred Hoyle: An Online Exhibition. Cambridge, UK: St John's College. Archived from the original on 26 May 2014. Retrieved 2 December 2019.
43. Kragh, Helge (April 2013). "Big Bang: the etymology of a name". Astronomy & Geophysics. 54 (2): 2.28–2.30. Bibcode:2013A&G....54b2.28K. doi:10.1093/astrogeo/att035.
44. Mattson, Barbara (Project Leader) (8 December 2017). "Hoyle Scoffs at 'Big Bang' Universe Theory". Cosmic Times (hosted by Imagine the Universe!). Greenbelt, MD: NASA: High Energy Astrophysics Science Archive Research Center. OCLC 227004453. Archived from the original on 10 March 2018. Retrieved 2 December 2019.
45. Croswell 1995, chapter 9, page 113
46. Mitton 2011, p. 129: "To create a picture in the mind of the listener, Hoyle had likened the explosive theory of the universe's origin to a 'big bang'."
47. Moskowitz, Clara (25 September 2012). "Hubble Telescope Reveals Farthest View Into Universe Ever". Space.com. New York: Future plc. Archived from the original on 12 October 2019. Retrieved 3 December 2019.
48. Slipher, Vesto M. (1913). "The Radial Velocity of the Andromeda Nebula". Lowell Observatory Bulletin. 1: 56–57. Bibcode:1913LowOB...2...56S.
49. Slipher, Vesto M. (January 1915). "Spectrographic Observations of Nebulae". Popular Astronomy. 23: 21–24. Bibcode:1915PA.....23...21S.
50. Friedman, Alexander (December 1922). "Über die Krümmung des Raumes". Zeitschrift für Physik (in German). 10 (1): 377–386. Bibcode:1922ZPhy...10..377F. doi:10.1007/BF01332580. S2CID 125190902.
51. Hubble, Edwin (15 March 1929). "A Relation Between Distance and Radial Velocity Among Extra-Galactic Nebulae". Proceedings of the National Academy of Sciences. 15 (3): 168–173. Bibcode:1929PNAS...15..168H. doi:10.1073/pnas.15.3.168. PMC 522427. PMID 16577160. Archived from the original on 1 October 2006. Retrieved 28 November 2019.
52. Christianson 1995
53. Lemaître, Georges (April 1927). "Un Univers homogène de masse constante et de rayon croissant rendant compte de la vitesse radiale des nébuleuses extra-galactiques". Annales de la Société scientifique de Bruxelles (in French). 47: 49–59. Bibcode:1927ASSB...47...49L.
54. Lemaître, Abbé Georges (24 October 1931). "Contributions to a British Association Discussion on the Evolution of the Universe". Nature. 128 (3234): 704–706. Bibcode:1931Natur.128..704L. doi:10.1038/128704a0. S2CID 4028196.
55. Kragh 1996
56. "Big bang theory is introduced – 1927". A Science Odyssey. Boston, MA: WGBH Boston. 1998. Archived from the original on 23 April 1999. Retrieved 31 July 2014.
57. Eddington, Arthur S. (21 March 1931). "The End of the World: from the Standpoint of Mathematical Physics". Nature. 127 (3203): 447–453. Bibcode:1931Natur.127..447E. doi:10.1038/127447a0. S2CID 4140648.
58. Appolloni, Simon (17 June 2011). "'Repugnant', 'Not Repugnant at All': How the Respective Epistemic Attitudes of Georges Lemaitre and Sir Arthur Eddington Influenced How Each Approached the Idea of a Beginning of the Universe". IBSU Scientific Journal. 5 (1): 19–44.
59. Lemaître, Georges (9 May 1931). "The Beginning of the World from the Point of View of Quantum Theory". Nature. 127 (3210): 706. Bibcode:1931Natur.127..706L. doi:10.1038/127706b0. ISSN 0028-0836. S2CID 4089233.
60. Milne 1935
61. Tolman 1934
62. Zwicky, Fritz (15 October 1929). "On the Red Shift of Spectral Lines through Interstellar Space". Proceedings of the National Academy of Sciences. 15 (10): 773–779. Bibcode:1929PNAS...15..773Z. doi:10.1073/pnas.15.10.773. PMC 522555. PMID 16577237.
63. Hoyle, Fred (October 1948). "A New Model for the Expanding Universe". Monthly Notices of the Royal Astronomical Society. 108 (5): 372–382. Bibcode:1948MNRAS.108..372H. doi:10.1093/mnras/108.5.372.
64. Alpher, Ralph A.; Bethe, Hans; Gamow, George (1 April 1948). "The Origin of Chemical Elements". Physical Review. 73 (7): 803–804. Bibcode:1948PhRv...73..803A. doi:10.1103/PhysRev.73.803. PMID 18877094.
65. Alpher, Ralph A.; Herman, Robert (13 November 1948). "Evolution of the Universe". Nature. 162 (4124): 774–775. Bibcode:1948Natur.162..774A. doi:10.1038/162774b0. S2CID 4113488.
66. Penzias, Arno A.; Wilson, R. W. (July 1965). "A Measurement of Excess Antenna Temperature at 4080 Mc/s". The Astrophysical Journal. 142: 419–421. Bibcode:1965ApJ...142..419P. doi:10.1086/148307. Archived from the original on 14 October 2019. Retrieved 5 December 2019.
67. Hawking, Stephen W.; Ellis, George F. R. (April 1968). "The Cosmic Black-Body Radiation and the Existence of Singularities in our Universe". The Astrophysical Journal. 152: 25. Bibcode:1968ApJ...152...25H. doi:10.1086/149520.
68. Hawking, Stephen W.; Penrose, Roger (27 January 1970). "The Singularities of Gravitational Collapse and Cosmology". Proceedings of the Royal Society A: Mathematical, Physical and Engineering Sciences. 314 (1519): 529–548. Bibcode:1970RSPSA.314..529H. doi:10.1098/rspa.1970.0021.
69. Guth, Alan (15 January 1981). "Inflationary universe: A possible solution to the horizon and flatness problems". Physical Review D. 23 (2): 347–356. Bibcode:1981PhRvD..23..347G. doi:10.1103/PhysRevD.23.347.
70. Huchra, John P. (2008). "The Hubble Constant". Science. 256 (5055): 321–5. doi:10.1126/science.256.5055.321. PMID 17743107. S2CID 206574821. Archived from the original on 30 September 2019. Retrieved 5 December 2019.
71. Livio 2000, p. 160
72. Navabi, Ali Akbar; Riazi, Nematollah (March 2003). "Is the Age Problem Resolved?". Journal of Astrophysics and Astronomy. 24 (1–2): 3–10. Bibcode:2003JApA...24....3N. doi:10.1007/BF03012187. S2CID 123471347.
73. Boggess, Nancy W.; Mather, John C.; Weiss, Rainer; et al. (1 October 1992). "The COBE Mission: Its Design and Performance Two Years after the launch". The Astrophysical Journal. 397: 420–429. Bibcode:1992ApJ...397..420B. doi:10.1086/171797.
74. Spergel, David N.; Bean, Rachel; Doré, Olivier; et al. (June 2007). "Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Implications for Cosmology". The Astrophysical Journal Supplement Series. 170 (2): 377–408. arXiv:astro-ph/0603449. Bibcode:2007ApJS..170..377S. doi:10.1086/513700. S2CID 1386346.
75. Reiss, Adam G.; Filippenko, Alexei V.; Challis, Peter; Clocchiatti, Alejandro; Diercks, Alan; Garnavich, Peter M.; Gilliland, Ron L.; Hogan, Craig J.; Jha, Saurabh; Kirshner, Robert P.; Leibundgut, B.; Phillips, M. M.; Reiss, David; Schmidt, Brian P.; Schommer, Robert A.; Smith, R. Chris; Spyromilio, J.; Stubbs, Christopher; Suntzeff, Nicholas B.; Tonry, John (1998). "Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant". The Astronomical Journal. 116 (3): 1009–1038. arXiv:astro-ph/9805201. doi:10.1086/300499.
76. Perlmutter, S.; Aldering, G.; Goldhaber, G.; Knop, R.A.; Nugent, P.; Castro, P.G.; Deustua, S.; Fabbro, S.; Goobar, A.; Groom, D.E.; Hook, I.M.; Kim, A.G.; Kim, M.Y.; Lee, J.C.; Nunes, N.J.; Pain, R.; Pennypacker, C.R.; Quimby, R.; Lidman, C.; Ellis, R.S.; Irwin, M.; McMahon, R.G.; Ruiz-Lapuente, P.; Walton, N.; Schaefer, B.; Boyle, B.J.; Filippenko, A.V.; Matheson, T.; Fruchter, A.S.; Panagia, N.; Newberg, H.J.M.; Couch, W.J. (1999). "Measurements of Omega and Lambda from 42 High-Redshift Supernovae". The Astrophysical Journal. 517 (2): 565586. arXiv:astro-ph/9812133. doi:10.1086/307221.
77. Krauss 2012, p. 118
78. Gladders, Michael D.; Yee, H. K. C.; Majumdar, Subhabrata; et al. (20 January 2007). "Cosmological Constraints from the Red-Sequence Cluster Survey". The Astrophysical Journal. 655 (1): 128–134. arXiv:astro-ph/0603588. Bibcode:2007ApJ...655..128G. doi:10.1086/509909. S2CID 10855653.
79. Shellard, Paul; et al., eds. (2012). "The Four Pillars of the Standard Cosmology". Outreach. Cambridge, UK: Centre for Theoretical Cosmology; University of Cambridge. Archived from the original on 2 November 2013. Retrieved 6 December 2019.
80. Sadoulet, Bernard; et al. "Direct Searches for Dark Matter" (PDF). Astro2010: The Astronomy and Astrophysics Decadal Survey (white paper). Washington, D.C.: National Academies Press on behalf of the National Research Council of the National Academy of Sciences. OCLC 850950122. Archived from the original on 13 April 2009. Retrieved 8 December 2019.
81. Diemand, Jürg; Zemp, Marcel; Moore, Ben; Stadel, Joachim; Carollo, C. Marcella (December 2005). "Cusps in cold dark matter haloes". Monthly Notices of the Royal Astronomical Society. 364 (2): 665–673. arXiv:astro-ph/0504215. Bibcode:2005MNRAS.364..665D. doi:10.1111/j.1365-2966.2005.09601.x.
82. Bullock, James S. (2010). "Notes on the Missing Satellites Problem". In Martinez-Delgado, David; Mediavilla, Evencio (eds.). Local Group Cosmology. pp. 95–122. arXiv:1009.4505. doi:10.1017/CBO9781139152303.004. ISBN 9781139152303. S2CID 119270708.
83. Cahn, Robert N.; et al. (2009). "Whitepaper: For a Comprehensive Space-Based Dark Energy Mission" (PDF). Astro2010: The Astronomy and Astrophysics Decadal Survey, Science White Papers, no. 35 (white paper). Washington, D.C.: National Academies Press on behalf of the National Research Council of the National Academy of Sciences. 2010: 35. Bibcode:2009astro2010S..35B. OCLC 850950122. Archived from the original on 7 August 2011. Retrieved 8 December 2019.
84. Peacock 1999, chpt. 3
85. Srianand, Raghunathan; Petitjean, Patrick; Ledoux, Cédric (21 December 2000). "The cosmic microwave background radiation temperature at a redshift of 2.34". Nature. 408 (6815): 931–935. arXiv:astro-ph/0012222. Bibcode:2000Natur.408..931S. doi:10.1038/35050020. PMID 11140672. S2CID 4313603. Lay summary European Southern Observatory (20 December 2000).
86. White, Martin (1999). "Anisotropies in the CMB" (PDF). In Arisaka, Katsushi; Bern, Zvi (eds.). DPF 99: Proceedings of the Los Angeles Meeting. Division of Particles and Fields Conference 1999 (DPF '99). Los Angeles: University of California, Los Angeles on behalf of the American Physical Society. arXiv:astro-ph/9903232. Bibcode:1999dpf..conf.....W. OCLC 43669022. Talk #9-10: The Cosmic Microwave Background. Archived (PDF) from the original on 4 February 2017. Retrieved 9 December 2019.
87. Bennett, Charles L.; Larson, Davin; Weiland, Janet L.; et al. (October 2013). "Nine-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Final Maps and Results". The Astrophysical Journal Supplement Series. 208 (2): Article 20. arXiv:1212.5225. Bibcode:2013ApJS..208...20B. doi:10.1088/0067-0049/208/2/20. S2CID 119271232.
88. Gannon, Megan (21 December 2012). "New 'Baby Picture' of Universe Unveiled". Space.com. New York: Future plc. Archived from the original on 29 October 2019. Retrieved 9 December 2019.
89. Wright 2004, p. 291
90. Melchiorri, Alessandro; Ade, Peter A.R.; de Bernardis, Paolo; et al. (20 June 2000). "A Measurement of Ω from the North American Test Flight of Boomerang". The Astrophysical Journal Letters. 536 (2): L63–L66. arXiv:astro-ph/9911445. Bibcode:2000ApJ...536L..63M. doi:10.1086/312744. PMID 10859119. S2CID 27518923.
91. de Bernardis, Paolo; Ade, Peter A.R.; Bock, James J.; et al. (27 April 2000). "A Flat Universe from High-Resolution Maps of the Cosmic Microwave Background Radiation" (PDF). Nature. 404 (6781): 955–959. arXiv:astro-ph/0004404. Bibcode:2000Natur.404..955D. doi:10.1038/35010035. hdl:10044/1/60851. PMID 10801117. S2CID 4412370. Archived (PDF) from the original on 2 May 2019. Retrieved 10 December 2019.
92. Miller, Andre D.; Caldwell, Robert H.; Devlin, Mark Joseph; et al. (10 October 1999). "A Measurement of the Angular Power Spectrum of the Cosmic Microwave Background from l = 100 to 400". The Astrophysical Journal Letters. 524 (1): L1–L4. arXiv:astro-ph/9906421. Bibcode:1999ApJ...524L...1M. doi:10.1086/312293. S2CID 1924091.
93. Steigman, Gary (February 2006). "Primordial Nucleosynthesis: Successes And Challenges". International Journal of Modern Physics E. 15 (1): 1–36. arXiv:astro-ph/0511534. Bibcode:2006IJMPE..15....1S. CiteSeerX 10.1.1.337.542. doi:10.1142/S0218301306004028. S2CID 12188807.
94. Ryden 2003
95. Bertschinger, Edmund (2000). "Cosmological Perturbation Theory and Structure Formation". arXiv:astro-ph/0101009.
96. Bertschinger, Edmund (September 1998). "Simulations of Structure Formation in the Universe" (PDF). Annual Review of Astronomy and Astrophysics. 36 (1): 599–654. Bibcode:1998ARA&A..36..599B. doi:10.1146/annurev.astro.36.1.599. S2CID 29015610. Archived from the original (PDF) on 9 March 2019.
97. "BICEP2 March 2014 Results and Data Products". The BICEP and Keck Array CMB Experiments. Cambridge, MA: FAS Research Computing, Harvard University. 16 December 2014 [Results originally released on 17 March 2014]. Archived from the original on 18 March 2014. Retrieved 10 December 2019.
98. Clavin, Whitney (17 March 2014). "NASA Technology Views Birth of the Universe". Jet Propulsion Laboratory. Washington, D.C.: NASA. Archived from the original on 10 October 2019. Retrieved 10 December 2019.
99. Overbye, Dennis (17 March 2014). "Space Ripples Reveal Big Bang's Smoking Gun". Space & Cosmos. The New York Times. New York. ISSN 0362-4331. Archived from the original on 17 March 2014. Retrieved 11 December 2019. "A version of this article appears in print on March 18, 2014, Section A, Page 1 of the New York edition with the headline: Space Ripples Reveal Big Bang's Smoking Gun." The online version of this article was originally titled "Detection of Waves in Space Buttresses Landmark Theory of Big Bang".
100. Overbye, Dennis (24 March 2014). "Ripples From the Big Bang". Out There. The New York Times. New York. ISSN 0362-4331. Archived from the original on 25 March 2014. Retrieved 24 March 2014. "A version of this article appears in print on March 25, 2014, Section D, Page 1 of the New York edition with the headline: Ripples From the Big Bang."
101. Fumagalli, Michele; O'Meara, John M.; Prochaska, J. Xavier (2 December 2011). "Detection of Pristine Gas Two Billion Years After the Big Bang". Science. 334 (6060): 1245–1249. arXiv:1111.2334. Bibcode:2011Sci...334.1245F. doi:10.1126/science.1213581. PMID 22075722. S2CID 2434386.
102. Stephens, Tim (10 November 2011). "Astronomers find clouds of primordial gas from the early universe". University News & Events. Santa Cruz, CA: University of California, Santa Cruz. Archived from the original on 14 November 2011. Retrieved 11 December 2019.
103. Perley, Daniel (21 February 2005). "Determination of the Universe's Age, to". Berkeley, CA: Department of Astronomy, University of California, Berkeley. Archived from the original on 11 September 2006. Retrieved 11 December 2019.
104. Yang, R. J., & Zhang, S. N. (2010). The age problem in the ΛCDM model. Monthly Notices of the Royal Astronomical Society, 407(3), 1835-1841.
105. Yu, H., & Wang, F. Y. (2014). Reconciling the cosmic age problem in the $$R_\mathrm {h}= ct$$ universe. The European Physical Journal C, 74(10), 3090.
106. Srianand, Raghunathan; Noterdaeme, Pasquier; Ledoux, Cédric; et al. (May 2008). "First detection of CO in a high-redshift damped Lyman-α system". Astronomy & Astrophysics. 482 (3): L39–L42. Bibcode:2008A&A...482L..39S. doi:10.1051/0004-6361:200809727.
107. Avgoustidis, Anastasios; Luzzi, Gemma; Martins, Carlos J.A.P.; et al. (14 February 2012). "Constraints on the CMB temperature-redshift dependence from SZ and distance measurements". Journal of Cosmology and Astroparticle Physics. 2012 (2): Article 013. arXiv:1112.1862. Bibcode:2012JCAP...02..013A. CiteSeerX 10.1.1.758.6956. doi:10.1088/1475-7516/2012/02/013. S2CID 119261969.
108. Belušević 2008, p. 16
109. Ghosh, Pallab (11 February 2016). "Einstein's gravitational waves 'seen' from black holes". Science & Environment. BBC News. London: BBC. Archived from the original on 11 February 2016. Retrieved 13 April 2017.
110. Billings, Lee (12 February 2016). "The Future of Gravitational Wave Astronomy". Scientific American. Archived from the original on 13 February 2016. Retrieved 13 April 2017.
111. Earman, John; Mosterín, Jesús (March 1999). "A Critical Look at Inflationary Cosmology". Philosophy of Science. 66 (1): 1–49. doi:10.1086/392675. JSTOR 188736. S2CID 120393154.
112. Hawking & Israel 2010, pp. 581–638, chpt. 12: "Singularities and time-asymmetry" by Roger Penrose.
113. Penrose 1989
114. Steinhardt, Paul J. (April 2011). "The Inflation Debate: Is the theory at the heart of modern cosmology deeply flawed?" (PDF). Scientific American. Vol. 304 no. 4. pp. 36–43. doi:10.1038/scientificamerican0411-36. Archived (PDF) from the original on 1 November 2019. Retrieved 23 December 2019.
115. Sakharov, Andrei D. (10 January 1967). "Нарушение СР-инвариантности, С-асимметрия и барионная асимметрия Вселенной" [Violation of CP-invariance, C-asymmetry and baryon asymmetry of the Universe] (PDF). Pis'ma v ZhETF (in Russian). 5 (1): 32–35. Archived (PDF) from the original on 28 July 2018.
116. Weinberg, Nevin N.; Kamionkowski, Marc (May 2003). "Constraining dark energy from the abundance of weak gravitational lenses". Monthly Notices of the Royal Astronomical Society. 341 (1): 251–262. arXiv:astro-ph/0210134. Bibcode:2003MNRAS.341..251W. doi:10.1046/j.1365-8711.2003.06421.x. S2CID 1193946.
117. Tanabashi, M. 2018, pp. 406–413, chpt. 27: "Dark Energy" (Revised September 2017) by David H. Weinberg and Martin White.
118. Rugh, Svend E.; Zinkernagel, Henrik (December 2002). "The quantum vacuum and the cosmological constant problem". Studies in History and Philosophy of Science Part B. 33 (4): 663–705. arXiv:hep-th/0012253. Bibcode:2002SHPMP..33..663R. doi:10.1016/S1355-2198(02)00033-3. S2CID 9007190.
119. Keel, William C. (October 2009) [Last changes: February 2015]. "Dark Matter". Bill Keel's Lecture Notes - Galaxies and the Universe. Archived from the original on 3 May 2019. Retrieved 15 December 2019.
120. Tanabashi, M. 2018, pp. 396–405, chpt. 26: "Dark Matter" (Revised September 2017) by Manuel Drees and Gilles Gerbier.
121. Dodelson, Scott (31 December 2011). "The Real Problem with MOND". International Journal of Modern Physics D. 20 (14): 2749–2753. arXiv:1112.1320. Bibcode:2011IJMPD..20.2749D. doi:10.1142/S0218271811020561. S2CID 119194106.
122. Kolb & Turner 1988, chpt. 8
123. Penrose 2007
124. Filippenko, Alexei V.; Pasachoff, Jay M. (March–April 2002). "A Universe from Nothing". Mercury. Vol. 31 no. 2. p. 15. Bibcode:2002Mercu..31b..15F. Archived from the original on 22 October 2013. Retrieved 10 March 2010.
125. Lawrence M. Krauss (Speaker); R. Elisabeth Cornwell (Producer) (21 October 2009). 'A Universe From Nothing' by Lawrence Krauss, AAI 2009 (Video). Washington, D.C.: Richard Dawkins Foundation for Reason and Science. Retrieved 17 October 2011.
126. Hawking & Israel 2010, pp. 504–517, chpt. 9: "The big bang cosmology — enigmas and nostrums" by Robert H. Dicke and Phillip J.E. Peebles.
127. NASA/WMAP Science Team (29 June 2015). "What is the Ultimate Fate of the Universe?". Universe 101: Big Bang Theory. Washington, D.C: NASA. Archived from the original on 15 October 2019. Retrieved 18 December 2019.
128. Adams, Fred C.; Laughlin, Gregory (April 1997). "A dying universe: the long-term fate and evolution of astrophysical objects". Reviews of Modern Physics. 69 (2): 337–372. arXiv:astro-ph/9701131. Bibcode:1997RvMP...69..337A. doi:10.1103/RevModPhys.69.337. S2CID 12173790..
129. Caldwell, Robert R.; Kamionkowski, Marc; Weinberg, Nevin N. (15 August 2003). "Phantom Energy: Dark Energy with w<−1 Causes a Cosmic Doomsday". Physical Review Letters. 91 (7): 071301. arXiv:astro-ph/0302506. Bibcode:2003PhRvL..91g1301C. doi:10.1103/PhysRevLett.91.071301. PMID 12935004.
130. "Brief Answers to Cosmic Questions". Universe Forum. Cambridge, MA: Harvard–Smithsonian Center for Astrophysics. Archived from the original on 13 April 2016. Retrieved 18 December 2019. Archival site: "The Universe Forum's role as part of NASA's Education Support Network concluded in September, 2009."
131. Hawking 1988, p. 69.
132. Carroll n.d.
133. Beckers, Mike (16 February 2015). "Quantentrick schafft Urknall-Singularität ab" [Quantum Trick Eliminates the Big Bang Singularity]. Cosmology. Spektrum der Wissenschaft (in German). Archived from the original on 21 July 2017. Retrieved 19 December 2019. Google translation
134. Hawking, Stephen W. (1996). "The Beginning of Time". Stephen Hawking (Lecture). London: The Stephen Hawking Foundation. Archived from the original on 6 November 2019. Retrieved 26 April 2017.
135. Wall, Mike (24 June 2012). "The Big Bang Didn't Need God to Start Universe, Researchers Say". Space.com.
136. Overbye, Dennis (22 May 2001). "Before the Big Bang, There Was . . . What?". The New York Times.
137. He, Dongshan; Gao, Dongfeng; Cai, Qing-yu (3 April 2014). "Spontaneous creation of the universe from nothing". Physical Review D. 89 (8): 083510. arXiv:1404.1207. Bibcode:2014PhRvD..89h3510H. doi:10.1103/PhysRevD.89.083510. S2CID 118371273.
138. Lincoln, Maya; Wasser, Avi (1 December 2013). "Spontaneous creation of the Universe Ex Nihilo". Physics of the Dark Universe. 2 (4): 195–199. Bibcode:2013PDU.....2..195L. doi:10.1016/j.dark.2013.11.004. ISSN 2212-6864.
139. Hartle, James H.; Hawking, Stephen W. (15 December 1983). "Wave function of the Universe". Physical Review D. 28 (12): 2960–2975. Bibcode:1983PhRvD..28.2960H. doi:10.1103/PhysRevD.28.2960.
140. Hawking 1988, p. 71.
141. Langlois, David (2003). "Brane Cosmology". Progress of Theoretical Physics Supplement. 148: 181–212. arXiv:hep-th/0209261. Bibcode:2002PThPS.148..181L. doi:10.1143/PTPS.148.181. S2CID 9751130.
142. Gibbons, Shellard & Rankin 2003, pp. 801–838, chpt. 43: "Inflationary theory versus the ekpyrotic/cyclic scenario" by Andrei Linde. Bibcode:2003ftpc.book..801L
143. Than, Ker (8 May 2006). "Recycled Universe: Theory Could Solve Cosmic Mystery". Space.com. New York: Future plc. Archived from the original on 6 September 2019. Retrieved 19 December 2019.
144. Kennedy, Barbara K. (1 July 2007). "What Happened Before the Big Bang?". News and Events. University Park, PA: Eberly College of Science, Pennsylvania State University. Archived from the original on 15 December 2019. Retrieved 19 December 2019.
145. Linde, Andrei D. (May 1986). "Eternal Chaotic Inflation". Modern Physics Letters A. 1 (2): 81–85. Bibcode:1986MPLA....1...81L. doi:10.1142/S0217732386000129. Archived from the original on 17 April 2019.
146. Linde, Andrei D. (14 August 1986). "Eternally Existing Self-Reproducing Chaotic Inflationary Universe". Physics Letters B. 175 (4): 395–400. Bibcode:1986PhLB..175..395L. doi:10.1016/0370-2693(86)90611-8.
147. Harris 2002, p. 128
148. Frame 2009, pp. 137–141
149. Harrison 2010, p. 9
150. Harris 2002, p. 129
151. Craig, William Lane (December 1999). "The Ultimate Question of Origins: God and the Beginning of the Universe". Astrophysics and Space Science (Lecture). 269–270 (1–4): 721–738. Bibcode:1999Ap&SS.269..721C. doi:10.1023/A:1017083700096. S2CID 117794135.
152. Hawking 1988, Introduction: "... a universe with no edge in space, no beginning or end in time, and nothing for a Creator to do." — Carl Sagan.