# Lambda-CDM model

The ΛCDM (Lambda cold dark matter) or Lambda-CDM model is a parametrization of the Big Bang cosmological model in which the universe contains three major components: first, a cosmological constant denoted by Lambda (Greek Λ) and associated with dark energy; second, the postulated cold dark matter (abbreviated CDM); and third, ordinary matter. It is frequently referred to as the standard model of Big Bang cosmology because it is the simplest model that provides a reasonably good account of the following properties of the cosmos:

The model assumes that general relativity is the correct theory of gravity on cosmological scales. It emerged in the late 1990s as a concordance cosmology, after a period of time when disparate observed properties of the universe appeared mutually inconsistent, and there was no consensus on the makeup of the energy density of the universe.

The ΛCDM model can be extended by adding cosmological inflation, quintessence and other elements that are current areas of speculation and research in cosmology.

Some alternative models challenge the assumptions of the ΛCDM model. Examples of these are modified Newtonian dynamics, entropic gravity, modified gravity, theories of large-scale variations in the matter density of the universe, bimetric gravity, and scale invariance of empty space.[1][2][3][4]

## Overview

Lambda-CDM, accelerated expansion of the universe. The time-line in this schematic diagram extends from the Big Bang/inflation era 13.7 Byr ago to the present cosmological time.

Most modern cosmological models are based on the cosmological principle, which states that our observational location in the universe is not unusual or special; on a large-enough scale, the universe looks the same in all directions (isotropy) and from every location (homogeneity).[5]

The model includes an expansion of metric space that is well documented both as the red shift of prominent spectral absorption or emission lines in the light from distant galaxies and as the time dilation in the light decay of supernova luminosity curves. Both effects are attributed to a Doppler shift in electromagnetic radiation as it travels across expanding space. Although this expansion increases the distance between objects that are not under shared gravitational influence, it does not increase the size of the objects (e.g. galaxies) in space. It also allows for distant galaxies to recede from each other at speeds greater than the speed of light; local expansion is less than the speed of light, but expansion summed across great distances can collectively exceed the speed of light.

The letter ${\displaystyle \Lambda }$  (lambda) represents the cosmological constant, which is currently associated with a vacuum energy or dark energy in empty space that is used to explain the contemporary accelerating expansion of space against the attractive effects of gravity. A cosmological constant has negative pressure, ${\displaystyle p=-\rho c^{2}}$ , which contributes to the stress-energy tensor that, according to the general theory of relativity, causes accelerating expansion. The fraction of the total energy density of our (flat or almost flat) universe that is dark energy, ${\displaystyle \Omega _{\Lambda }}$ , is estimated to be 0.669 ± 0.038 based on the 2018 Dark Energy Survey results using Type Ia Supernovae[6] or 0.6847 ± 0.0073 based on the 2018 release of Planck satellite data, or more than 68.3% (2018 estimate) of the mass-energy density of the universe.[7]

Dark matter is postulated in order to account for gravitational effects observed in very large-scale structures (the "flat" rotation curves of galaxies; the gravitational lensing of light by galaxy clusters; and enhanced clustering of galaxies) that cannot be accounted for by the quantity of observed matter.

Cold dark matter as currently hypothesized is:

non-baryonic
It consists of matter other than protons and neutrons (and electrons, by convention, although electrons are not baryons).
cold
Its velocity is far less than the speed of light at the epoch of radiation-matter equality (thus neutrinos are excluded, being non-baryonic but not cold).
dissipationless
It cannot cool by radiating photons.
collisionless
The dark matter particles interact with each other and other particles only through gravity and possibly the weak force.

Dark matter constitutes about 26.8% (2013 estimate)[citation needed] of the mass-energy density of the universe. The remaining 4.8% (2013 estimate) comprises all ordinary matter observed as atoms, chemical elements, gas and plasma, the stuff of which visible planets, stars and galaxies are made. The great majority of ordinary matter in the universe is unseen, since visible stars and gas inside galaxies and clusters account for less than 10% of the ordinary matter contribution to the mass-energy density of the universe.[8]

Also, the energy density includes a very small fraction (~ 0.01%) in cosmic microwave background radiation, and not more than 0.5% in relic neutrinos. Although very small today, these were much more important in the distant past, dominating the matter at redshift > 3200.

The model includes a single originating event, the "Big Bang", which was not an explosion but the abrupt appearance of expanding space-time containing radiation at temperatures of around 1015 K. This was immediately (within 10−29 seconds) followed by an exponential expansion of space by a scale multiplier of 1027 or more, known as cosmic inflation. The early universe remained hot (above 10,000 K) for several hundred thousand years, a state that is detectable as a residual cosmic microwave background, or CMB, a very low energy radiation emanating from all parts of the sky. The "Big Bang" scenario, with cosmic inflation and standard particle physics, is the only current cosmological model consistent with the observed continuing expansion of space, the observed distribution of lighter elements in the universe (hydrogen, helium, and lithium), and the spatial texture of minute irregularities (anisotropies) in the CMB radiation. Cosmic inflation also addresses the "horizon problem" in the CMB; indeed, it seems likely that the universe is larger than the observable particle horizon.

The model uses the Friedmann–Lemaître–Robertson–Walker metric, the Friedmann equations and the cosmological equations of state to describe the observable universe from right after the inflationary epoch to present and future.

## Cosmic expansion history

The expansion of the universe is parameterized by a dimensionless scale factor ${\displaystyle a=a(t)}$  (with time ${\displaystyle t}$  counted from the birth of the universe), defined relative to the present day, so ${\displaystyle a_{0}=a(t_{0})=1}$ ; the usual convention in cosmology is that subscript 0 denotes present-day values, so ${\displaystyle t_{0}}$  is the current age of the universe. The scale factor is related to the observed redshift[9] ${\displaystyle z}$  of the light emitted at time ${\displaystyle t_{\mathrm {em} }}$  by

${\displaystyle a(t_{\text{em}})={\frac {1}{1+z}}\,.}$

The expansion rate is described by the time-dependent Hubble parameter, ${\displaystyle H(t)}$ , defined as

${\displaystyle H(t)\equiv {\frac {\dot {a}}{a}},}$

where ${\displaystyle {\dot {a}}}$  is the time-derivative of the scale factor. The first Friedmann equation gives the expansion rate in terms of the matter+radiation density ${\displaystyle \rho }$ , the curvature ${\displaystyle k}$ , and the cosmological constant ${\displaystyle \Lambda }$ ,[9]

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

where as usual ${\displaystyle c}$  is the speed of light and ${\displaystyle G}$  is the gravitational constant. A critical density ${\displaystyle \rho _{\mathrm {crit} }}$  is the present-day density, which gives zero curvature ${\displaystyle k}$ , assuming the cosmological constant ${\displaystyle \Lambda }$  is zero, regardless of its actual value. Substituting these conditions to the Friedmann equation gives

${\displaystyle \rho _{\mathrm {crit} }={\frac {3H_{0}^{2}}{8\pi G}}=1.878\;47(23)\times 10^{-26}\;h^{2}\;{\text{kg}}\;{\text{m}}^{-3},}$ [10]

where ${\displaystyle h\equiv H_{0}/(100\;\mathrm {km\;s^{-1}\;Mpc^{-1}} )}$  is the reduced Hubble constant. If the cosmological constant were actually zero, the critical density would also mark the dividing line between eventual recollapse of the universe to a Big Crunch, or unlimited expansion. For the Lambda-CDM model with a positive cosmological constant (as observed), the universe is predicted to expand forever regardless of whether the total density is slightly above or below the critical density; though other outcomes are possible in extended models where the dark energy is not constant but actually time-dependent.

It is standard to define the present-day density parameter ${\displaystyle \Omega _{x}}$  for various species as the dimensionless ratio

${\displaystyle \Omega _{x}\equiv {\frac {\rho _{x}(t=t_{0})}{\rho _{\mathrm {crit} }}}={\frac {8\pi G\rho _{x}(t=t_{0})}{3H_{0}^{2}}}}$

where the subscript ${\displaystyle x}$  is one of ${\displaystyle b}$  for baryons, ${\displaystyle c}$  for cold dark matter, ${\displaystyle rad}$  for radiation (photons plus relativistic neutrinos), and ${\displaystyle DE}$  or ${\displaystyle \Lambda }$  for dark energy.

Since the densities of various species scale as different powers of ${\displaystyle a}$ , e.g. ${\displaystyle a^{-3}}$  for matter etc., the Friedmann equation can be conveniently rewritten in terms of the various density parameters as

${\displaystyle H(a)\equiv {\frac {\dot {a}}{a}}=H_{0}{\sqrt {(\Omega _{c}+\Omega _{b})a^{-3}+\Omega _{\text{rad}}a^{-4}+\Omega _{k}a^{-2}+\Omega _{DE}a^{-3(1+w)}}}}$

where w is the equation of state of dark energy, and assuming negligible neutrino mass (significant neutrino mass requires a more complex equation). The various ${\displaystyle \Omega }$  parameters add up to ${\displaystyle 1}$  by construction. In the general case this is integrated by computer to give the expansion history ${\displaystyle a(t)}$  and also observable distance-redshift relations for any chosen values of the cosmological parameters, which can then be compared with observations such as supernovae and baryon acoustic oscillations.

In the minimal 6-parameter Lambda-CDM model, it is assumed that curvature ${\displaystyle \Omega _{k}}$  is zero and ${\displaystyle w=-1}$ , so this simplifies to

${\displaystyle H(a)=H_{0}{\sqrt {\Omega _{m}a^{-3}+\Omega _{\text{rad}}a^{-4}+\Omega _{\Lambda }}}}$

Observations show that the radiation density is very small today, ${\displaystyle \Omega _{\text{rad}}\sim 10^{-4}}$ ; if this term is neglected the above has an analytic solution[11]

${\displaystyle a(t)=(\Omega _{m}/\Omega _{\Lambda })^{1/3}\,\sinh ^{2/3}(t/t_{\Lambda })}$

where ${\displaystyle t_{\Lambda }\equiv 2/(3H_{0}{\sqrt {\Omega _{\Lambda }}})\ ;}$  this is fairly accurate for ${\displaystyle a>0.01}$  or ${\displaystyle t>10}$ million years. Solving for ${\displaystyle a(t)=1}$  gives the present age of the universe ${\displaystyle t_{0}}$  in terms of the other parameters.

It follows that the transition from decelerating to accelerating expansion (the second derivative ${\displaystyle {\ddot {a}}}$  crossing zero) occurred when

${\displaystyle a=(\Omega _{m}/2\Omega _{\Lambda })^{1/3}}$

which evaluates to ${\displaystyle a\sim 0.6}$  or ${\displaystyle z\sim 0.66}$  for the best-fit parameters estimated from the Planck spacecraft.

## Historical development

The discovery of the Cosmic Microwave Background (CMB) in 1964 confirmed a key prediction of the Big Bang cosmology. From that point on, it was generally accepted that the universe started in a hot, dense state and has been expanding over time. The rate of expansion depends on the types of matter and energy present in the universe, and in particular, whether the total density is above or below the so-called critical density.

During the 1970s, most attention focused on pure-baryonic models, but there were serious challenges explaining the formation of galaxies, given the small anisotropies in the CMB (upper limits at that time). In the early 1980s, it was realized that this could be resolved if cold dark matter dominated over the baryons, and the theory of cosmic inflation motivated models with critical density.

During the 1980s, most research focused on cold dark matter with critical density in matter, around 95% CDM and 5% baryons: these showed success at forming galaxies and clusters of galaxies, but problems remained; notably, the model required a Hubble constant lower than preferred by observations, and observations around 1988–1990 showed more large-scale galaxy clustering than predicted.

These difficulties sharpened with the discovery of CMB anisotropy by COBE in 1992, and several modified CDM models, including Λ-CDM and mixed cold and hot dark matter, came under active consideration through the mid-1990s. The Λ-CDM model then became the leading model following the observations of accelerating expansion in 1998, and was quickly supported by other observations: in 2000, the BOOMERanG microwave background experiment measured the total (matter–energy) density to be close to 100% of critical, whereas in 2001 the 2dFGRS galaxy redshift survey measured the matter density to be near 25%; the large difference between these values supports a positive Λ or dark energy. Much more precise spacecraft measurements of the microwave background from WMAP in 2003–2010 and Planck in 2013–2015 have continued to support the model and pin down the parameter values, most of which are now constrained below 1 percent uncertainty.

There is currently active research into many aspects of the Λ-CDM model, both to refine the parameters and possibly detect deviations. In addition, Λ-CDM has no explicit physical theory for the origin or physical nature of dark matter or dark energy; the nearly scale-invariant spectrum of the CMB perturbations, and their image across the celestial sphere, are believed to result from very small thermal and acoustic irregularities at the point of recombination.

A large majority of astronomers and astrophysicists support the ΛCDM model or close relatives of it, but Milgrom, McGaugh, and Kroupa are leading critics, attacking the dark matter portions of the theory from the perspective of galaxy formation models and supporting the alternative MOND theory, which requires a modification of the Einstein field equations and the Friedmann equations as seen in proposals such as MOG theory or TeVeS theory. Other proposals by theoretical astrophysicists of cosmological alternatives to Einstein's general relativity that attempt to account for dark energy or dark matter include f(R) gravity, scalar–tensor theories such as galileon theories, brane cosmologies, the DGP model, and massive gravity and its extensions such as bimetric gravity.

## Successes

In addition to explaining pre-2000 observations, the model has made a number of successful predictions: notably the existence of the baryon acoustic oscillation feature, discovered in 2005 in the predicted location; and the statistics of weak gravitational lensing, first observed in 2000 by several teams. The polarization of the CMB, discovered in 2002 by DASI[12] is now a dramatic success: in the 2015 Planck data release,[13] there are seven observed peaks in the temperature (TT) power spectrum, six peaks in the temperature-polarization (TE) cross spectrum, and five peaks in the polarization (EE) spectrum. The six free parameters can be well constrained by the TT spectrum alone, and then the TE and EE spectra can be predicted theoretically to few-percent precision with no further adjustments allowed: comparison of theory and observations shows an excellent match.

## Challenges

Extensive searches for dark matter particles have so far shown no well-agreed detection; the dark energy may be almost impossible to detect in a laboratory, and its value is unnaturally small compared to naive theoretical predictions.

Comparison of the model with observations is very successful on large scales (larger than galaxies, up to the observable horizon), but may have some problems on sub-galaxy scales, possibly predicting too many dwarf galaxies and too much dark matter in the innermost regions of galaxies. This problem is called the "small scale crisis".[14] These small scales are harder to resolve in computer simulations, so it is not yet clear whether the problem is the simulations, non-standard properties of dark matter, or a more radical error in the model.

It has been argued that the ΛCDM model is built upon a foundation of conventionalist stratagems, rendering it unfalsifiable in the sense defined by Karl Popper.[15]

## Parameters

Planck Collaboration Cosmological parameters[17]
Description Symbol Value
Indepen-
dent
para-
meters
Physical baryon density parameter[a] Ωb h2 0.02230±0.00014
Physical dark matter density parameter[a] Ωc h2 0.1188±0.0010
Age of the universe t0 13.799±0.021 × 109 years
Scalar spectral index ns 0.9667±0.0040
Curvature fluctuation amplitude,
k0 = 0.002 Mpc−1
${\displaystyle \Delta _{R}^{2}}$  2.441+0.088
−0.092
×10−9
[20]
Reionization optical depth τ 0.066±0.012
Fixed
para-
meters
Total density parameter[b] Ωtot 1
Equation of state of dark energy w −1
Tensor/scalar ratio r 0
Running of spectral index ${\displaystyle dn_{\text{s}}/d\ln k}$  0
Sum of three neutrino masses ${\displaystyle \sum m_{\nu }}$  0.06 eV/c2[c][16]:40
Effective number of relativistic degrees
of freedom
Neff 3.046[d][16]:47
Calcu-
lated
values
Hubble constant H0 67.74±0.46 km s−1 Mpc−1
Baryon density parameter[b] Ωb 0.0486±0.0010[e]
Dark matter density parameter[b] Ωc 0.2589±0.0057[f]
Matter density parameter[b] Ωm 0.3089±0.0062
Dark energy density parameter[b] ΩΛ 0.6911±0.0062
Critical density ρcrit (8.62±0.12)×10−27 kg/m3[g]
The present root-mean-square matter fluctuation

averaged over a sphere of radius 8h1 Mpc

σ8 0.8159±0.0086
Redshift at decoupling z 1089.90±0.23
Age at decoupling t 377700±3200 years[20]
Redshift of reionization (with uniform prior) zre 8.5+1.0
−1.1
[21]

The simple ΛCDM model is based on six parameters: physical baryon density parameter; physical dark matter density parameter; the age of the universe; scalar spectral index; curvature fluctuation amplitude; and reionization optical depth.[22] In accordance with Occam's razor, six is the smallest number of parameters needed to give an acceptable fit to current observations; other possible parameters are fixed at "natural" values, e.g. total density parameter = 1.00, dark energy equation of state = −1. (See below for extended models that allow these to vary.)

The values of these six parameters are mostly not predicted by current theory (though, ideally, they may be related by a future "Theory of Everything"), except that most versions of cosmic inflation predict the scalar spectral index should be slightly smaller than 1, consistent with the estimated value 0.96. The parameter values, and uncertainties, are estimated using large computer searches to locate the region of parameter space providing an acceptable match to cosmological observations. From these six parameters, the other model values, such as the Hubble constant and the dark energy density, can be readily calculated.

Commonly, the set of observations fitted includes the cosmic microwave background anisotropy, the brightness/redshift relation for supernovae, and large-scale galaxy clustering including the baryon acoustic oscillation feature. Other observations, such as the Hubble constant, the abundance of galaxy clusters, weak gravitational lensing and globular cluster ages, are generally consistent with these, providing a check of the model, but are less precisely measured at present.

Parameter values listed below are from the Planck Collaboration Cosmological parameters 68% confidence limits for the base ΛCDM model from Planck CMB power spectra, in combination with lensing reconstruction and external data (BAO + JLA + H0).[16] See also Planck (spacecraft).

1. ^ a b The "physical baryon density parameter" Ωb h2 is the "baryon density parameter" Ωb multiplied by the square of the reduced Hubble constant h = H0 / (100 km s−1 Mpc−1).[18][19] Likewise for the difference between "physical dark matter density parameter" and "dark matter density parameter".
2. A density ρx = Ωxρcrit is expressed in terms of the critical density ρcrit, which is the total density of matter/energy needed for the universe to be spatially flat. Measurements indicate that the actual total density ρtot is very close if not equal to this value, see below.
3. ^ This is the minimal value allowed by solar and terrestrial neutrino oscillation experiments.
4. ^ from the Standard Model of particle physics
5. ^ Calculated from Ωbh2 and h = H0 / (100 km s−1 Mpc−1).
6. ^ Calculated from Ωch2 and h = H0 / (100 km s−1 Mpc−1).
7. ^ Calculated from h = H0 / (100 km s−1 Mpc−1) per ρcrit = 1.87847×10−26 h2 kg m−3.[10]

## Missing baryon problem

Massimo Persic and Paolo Salucci[23] firstly estimated the baryonic density today present in ellipticals, spirals, groups and clusters of galaxies. They performed an integration of the baryonic mass-to-light ratio over luminosity (in the following ${\textstyle M_{b}/L}$ ), weighted with the luminosity function ${\textstyle \phi (L)}$  over the previously mentioned classes of astrophysical objects:

${\displaystyle \rho _{b}=\sum \int L\phi (L){\frac {M_{b}}{L}}\,dL.}$

The result was:

${\displaystyle \Omega _{b}=\Omega _{*}+\Omega _{\text{gas}}=2.2\times 10^{-3}+1.5\times 10^{-3}h^{-1.3}\simeq 0.003}$

where ${\displaystyle h\simeq 0.72}$ .

Note that this value is much lower than the prediction of standard cosmic nucleosynthesis ${\displaystyle \Omega _{b}\simeq 0.0486}$ , so that stars and gas in galaxies and in galaxy groups and clusters account for less than 10% of the primordially synthesized baryons. This issue is known as the problem of the "missing baryons".

## Extended models

Extended model parameters
Description Symbol Value
Total density parameter ${\displaystyle \Omega _{\text{tot}}}$  1.0023+0.0056
−0.0054
Equation of state of dark energy ${\displaystyle w}$  −0.980±0.053
Tensor-to-scalar ratio ${\displaystyle r}$  < 0.11, k0 = 0.002 Mpc−1 (${\displaystyle 2\sigma }$ )
Running of the spectral index ${\displaystyle dn_{s}/d\ln k}$  −0.022±0.020, k0 = 0.002 Mpc−1
Sum of three neutrino masses ${\displaystyle \sum m_{\nu }}$  < 0.58 eV/c2 (${\displaystyle 2\sigma }$ )
Physical neutrino density parameter ${\displaystyle \Omega _{\nu }h^{2}}$  < 0.0062

Extended models allow one or more of the "fixed" parameters above to vary, in addition to the basic six; so these models join smoothly to the basic six-parameter model in the limit that the additional parameter(s) approach the default values. For example, possible extensions of the simplest ΛCDM model allow for spatial curvature (${\displaystyle \Omega _{tot}}$  may be different from 1); or quintessence rather than a cosmological constant where the equation of state of dark energy is allowed to differ from −1. Cosmic inflation predicts tensor fluctuations (gravitational waves). Their amplitude is parameterized by the tensor-to-scalar ratio (denoted ${\displaystyle r}$ ), which is determined by the unknown energy scale of inflation. Other modifications allow hot dark matter in the form of neutrinos more massive than the minimal value, or a running spectral index; the latter is generally not favoured by simple cosmic inflation models.

Allowing additional variable parameter(s) will generally increase the uncertainties in the standard six parameters quoted above, and may also shift the central values slightly. The Table below shows results for each of the possible "6+1" scenarios with one additional variable parameter; this indicates that, as of 2015, there is no convincing evidence that any additional parameter is different from its default value.

Some researchers have suggested that there is a running spectral index, but no statistically significant study has revealed one. Theoretical expectations suggest that the tensor-to-scalar ratio ${\displaystyle r}$  should be between 0 and 0.3, and the latest results are now within those limits.

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