As the title states, in some older versions of Ubuntu/Linux (confirmed on 8 - 10, not know if still exists in 11, 12), the text censor focus sometimes just loses when auto-complete is up. The keyboard seems frozen and one has to click other places first and then click again to gain focus back. This bug is particularly annoying when working with IDEs with auto-complete features on, such as Eclipse. This issue is caused by SCIM (SCIM daemon is on, although one doesn't explicitly summon it.) As the SCIM development has been off for many years, this bug has not been fixed so far.
in System/Administration/Language Support, uncheck the "Enable support to enter complex characters".
There is no such an option at all in karmic koala.
3. use ibus/shut down SCIM when using Eclipse
4. delete ~/.xinput.d/en_US
This method works for me, but SCIM are not stable when working with Google-Chrome browser. Note that you may need to logout and login several times.
To explain the microscopic nature of dark matter requires physics beyond standard model. In fact, virtually all particle physicists believe that standard model is only an effective theory of some more fundamental theory. The following problems of standard model are the main motivation.
Gauge hierarchy problem. Gauge hierarchy problem asked why Higgs mass (∼100 GeV) is much smaller than Planck scale energy, the believed grand unification scale. A possible explanation is there is a TeV scale physics, which affects Higgs mass through quantum fluctuation.
Moreover, calculation shows if Higgs mass is smaller than 134 GeV, the quantum fluctuation will cause the collapse of Higgs field vacuum. The current preliminary Higgs mass from LHC (125.7 GeV) demands a mechanism to stabilize the Higgs field vacuum. All these problem can be solved by TeV physics including super-symmetric models and universal extra dimension models.
Neutrino mass, left-handed neutrino problem. In standard model, fermions acquire mass via Higgs mechanism. But fermion masses extend 14 orders of magnitude. This fact can hardly be viewed as a coincidence. Moreover, if neutrinos are massive, right-handed neutrinos must exist. One possibility is that there exist massive, non-interacting right-handed neutrinos, called sterile neutrinos. Sterile neutrino can solve the neutrino mass problem through see-saw mechanism.
Fig. 1: fermion masses.
Strong CP problem. In QCD, a term proportional to θϵμνρλFμνFρλ is allowed, which, if exists, will
break CP-symmetry and lead to phenomena like nonzero neutron electric dipole moment. The current
experimental observation constrains this term to be close to zero. Physicists do not believe this is a
coincidence. Introducing axions can solve this problem
There have been many well motivated extension of standard model. Each of them is designed to solve one or more problems listed above.
Supersymmetry
Supersymmetric standard models introduce an additional symmetry between fermions
and bosons called supersymmetry. Supersymmetry assigns each boson a fermionic supersymmetric partner. The lightest supersymmetric neutral particles (LSPs) are natural dark matter candidates, as protected by R-parity from decaying into lighter SM particles. If supersymmetry is broken at TeV scale, gauge hierarchy
and Higgs vacuum stability problem can be solved elegantly.
Another strong support of supersymmetry comes from attempt towards the grand unification. Physicists postulate all interactions have the same origin at Plank scale 1018∼1019 GeV. If this is true, strong weak and electromagnetism forces should be unified at around 1016 GeV. However, study of the evolution of three standard model couplings shows a discrepancy from unification at Planck scale. The discrepancy can be greatly reduced by introducing supersummetry (See Fig. 2).
Fig. 2: Left, evolution of couplings within standard model; Right, evolution of couplings by introducing a pair of vector like fermions carrying SM charges and masses of order 300 GeV-1 TeV.
For all these reasons, supersymmetric models are among the most favored standard model extensions.
But one common issue of these models is that they have a vast set of parameters. The Minimal Supersymmetric Standard Model (MSSM) for example already has 63 parameters. It is impossible to explore the
whole parameter space. By using theoretical arguments and/or current experimental data, majority of the
parameter can be fixed to certain reasonable values. The left parameter set, containing 5 - 10 parameters, can
be constrained by experiment from the upcoming particle physics experiments and astrophysics observation
if the model is designed for dark matter (See Fig 3).
Fig. 3: The parameter space of various MSSM models. The shaded area is excluded by measurement of
Bs→μ++μ− and Bd→μ+μ− branching ratios.
Extra Dimensions
Extra Dimension models (ED) assume there exist extra dimensions besides the usual
3+1 spacetime. The shape of the extra dimensions are usually curled, such as a small circle, to explain their
invisibility. In ED, each normal particle corresponds to a set of excitations in the extra dimension, known
as Kaluza-Klein (KK) tower. The mass of KK excitations in the tower, m2KK=m2SM+n2/R2,n=0,1,2,…
where R is the radius of the extra dimension, R−1≳ 300 GeV to explain why they have not been observed
in current colliders. Lightest KK particles (LKPs) are also natural dark matter candidates, as protected by
KK-parity. Meanwhile, if the radius of the extra dimension is about TeV−1 , ED extension of standard model
known as Universal Extra Dimension (UED) can replace Higgs mechanism to break the electroweak gauge
symmetry, hence solves the gauge hierarchy problem and Higgs vacuum stability problem.
Just like supersymmetry, ED may also modify gravity. In the large extra dimension model of Arkani-Hamed, Dimopoulos and Dvali (ADD), standard model is lived on TeV scale 4D surface (called brane), whereas gravity and only gravity can penetrate from Planck scale brane and the TeV scale brane by propa-
gating in the extra dimensions.
EDs are constrained by various collider experiments, gravity tests and dark matter relic density. In theminimal case (mUED), UED only has one free parameter, the radius R of the curled extra dimension (See Fig. 4).
Fig. 4: Combined collider constraints on mUED. MH is standard model Higgs mass. By Belanger et al.(2012)
Peccei-Quinn Theory
Peccei-Quinn theory is proposed to solve the strong CP problem in QCD. Peccei-
Quinn theory postulates the coupling constant θ of strong CP term is a dynamical field with a new global
symmetry Peiccei-Quinn symmetry. The new field is called axion. In some models, axion is also a dark matter candidate.
See-Saw Mechanism and Neutrino Masses
To explain neutrino mass, one may extend standard model
to include neutrino mass via Higgs mechanism as other fermions. So one need a right-handed neutrino.
Right-handed neutrino is a isospin singlet. It does not interaction with gauge bosons. Meanwhile, it can also
acquire a Majorana mass term. L=mDˉνRνL+mMˉνcLνR+h.c.
The mass matrix is,
(0mDmDmM)
mM∼MPl≫mD. there are two mass eigenstates, m1≃mM,m2≃−m2DmM. m2≪mD≪mM. This is the so-called see-saw mechanism. It explains why neutrino mass m2 is much smaller than fermion mass mD. The first mass eigenstate is a massive nearly non-interacting neutrino, called sterile neutrino. Sterile neutrino is a very good dark matter candidate.
It should be noted that these models may appear together, even producing new dark matter candidates.
For example, the supersymmetric partner of axion, called axino is also a dark matter candidate.
Weakly Interacting Massive Particles
A large class of dark matter candidates is weakly interaction massive particles (WIMPs). WIMPs are neutral
stable particles with mass of weak scale ∼ 100 GeV, and coupling with standard model particles on weak
coupling scale α∼10−2. Candidates in WIMP class include lightest supersymmetric particles (LSPs) such as neutralinos (the linear superposition of photino, Zino and Higgsino), lightest Kaluza-Klein excitations (LKPs) from universal extra dimension models.
WIMPs may be produced in early universe as the thermal relic of Big Bang. At very early universe,
WIMPs are in equilibrium. As the temperature falls below its mχ , there are more WIMPs annihilating
into lighter particles than the converse reaction. The WIMP density drops exponentially, until the reaction
rate below the Universe expansion. Then WIMPs freeze-out from equilibrium as the thermal relic and their
co-moving number density remains fixed as the relic density. The above description can be formally modeled
by Boltzmann equation: dnχdt+3H(t)nχ=−⟨σAv⟩(n2χ−ˉn2χ)
where H is the Hubble parameter, ˉn is the equilibrium number density. The equation can be solved numerically. In the simplest case, the frozen-out temperature is about Tf∼m2χ/20 and the relic density is, Ωχh2≃3×10−27cm3s−1⟨σAv⟩
. The cross section of WIMPs is about ⟨σAv⟩∼α2m2χ(a+bv2+O(v4)). The first two terms represent s-wave and p-wave cross section respectively. v≪1, so higher order terms can be neglected. For the case of s-wave dominated annihilation, a∼O(1), then Ωχ∼10−3−10−1, where we have allowed one order of magnitude fluctuation. The cursory estimation shows, particles with weak scale mass and coupling have naturally the correct relic density as dark matter. This is called the "WIMP miracle". These properties make WIMPs the leading dark matter candidates.
Fig. 4: The WIMP relic density. The dashed line is relic density without thermal frozen-out. The solid lines are the actual relic density. The strips represents a variation of the cross section of orders of magnitude from the one with the "correct relic density".
If the orbit is circular, the speed is simply proportional to 1/√r. For general cases, however, after some derivation, the average speed, ˉv=12π∫2π0dθv(θ)=√GMa2E(2ϵ1+ϵ)π√1−ϵ,
where E(z)=∫π20(1−zsin2θ)1/2dθ is the elliptic function. Note that E(0)=π2, restoring the circular motion result. So, the average speed is proportional to 1√a where a is the semi-major axis.
Fig. 1: the semi-major axis vs. average orbital speed for solar system planets in linear coordinates
Fig. 2: the semi-major axis vs. average orbital speed for solar system planets in logarithmic coordinates
The best fit of the slope gives 29.779763 km/s/AU, which is about the earth average orbital speed. Using the data of solar mass and gravitational constant, the average eccentricity is about 0.0195386. This is the absolute value.
According to Newtonian gravity, the rotational velocity v(r) of an object is related to the mass enclosed by its orbit (integral mass): v2(r)=GM(r)r.
Rotation curves plot orbital velocity of a star vs. its distance from the center of the galaxy. Rubin et al. (1978) measured the rotation curves of various galaxies and found that the rotation curve at the edge of the luminous galaxy does not decline as expected v(r)∝1/√r. Instead, the curve is fairly flat or even increase (See Fig. 1 and Fig. 2). If Newtonian gravity is correct in these systems, there must be some invisible mass extended over the luminous part to provide gravity. These are the classical evidences of existence of dark matter.
Fig. 1: rotational curves of several spiral galaxies, with the contribution from luminous components (dashed), gas (dotted) and dark matter halo (dash-dot). The square blocks are data. The solid line is dark matter model fitting. By Begeman et al. (1991)
Fig. 2: rotation curves of several spiral galaxies. By Rubin et al. (1978)
The dark matter distribution can be inferred from the rotation curve. The flatness of rotation curves in spiral galaxies indicate an integral mass M(r)∝r1+δ. It has been shown by N-body simulation that there exists universal dark matter halo profile, ρ(r)=ρ0(r0r)γ[1+(r0a)α1+(ra)α]β−γα
Some widely used dark matter halo profiles are, Kravtsov et al. (1998)(α,β,γ)=(2,3,0.4),a=r0=10 kpc, Navarro et al.
(1995) (α,β,γ)=(1,3,1),a=r0=20 kpc, Moore et al. (1999) (α,β,γ)=(1.5,3,1.5),a=r0=28 kpc and
Bergstrom et al. (1998) (α,β,γ)=(2,2,0),a=r0=3.5 kpc
Dark Matter Distribution
In summary, evidences of existence of dark matter can be found in galaxies, clusters and from cosmological probes. Cosmological observations suggest overall density fraction of invisible mass ΩDM≃0.23. Bahcall et al. (1995) collected the mass-to-light ratio on different scales (See Fig. 3). Their study shows mass-to-light ratio of dark matter on large scale structures is consistent with the cosmological constraints. This conclusion also suggests dark matter from cosmology is the same thing with the dark matter in galaxy and clusters.
Galaxy groups and clusters are structures comprising hundreds to thousands of galaxies bounded together by gravity. According to the concordance cosmology model, cluster sits on the top of the cosmos structural hierarchy. A direct evidence of existence of dark matter is that groups and clusters usually have much larger mass-to-light ratio. The average M/L in solar neighborhood is ∼5Υ⊙. In large scope, stellar and gas mass-to-light ratio ranges from 0.5Υ⊙ to 30Υ⊙. Larger than 30Υ⊙ usually cannot be explained by stars and gases. Direct probes of group and cluster mass are galaxy velocity dispersion, X-Ray and gravitational lensing.
Galaxy Velocity Dispersion and X-Ray Spectrum
Mass of group or cluster can be inferred from their dynamics. Galaxies in groups or clusters bounded together by gravitational wall can be well assumed in virial equilibrium. Applying virial theorem, ⟨ϵk⟩=−12⟨ϵp⟩
where ⟨ϵk⟩ denotes the average unit kinetic energy and ⟨ϵp⟩≃−35GMR is the average gravitational potential.
Galaxy velocities can be empirically fitted by Gaussian, exp[−(v−v0)2/2σ2v], where σv is the velocity dispersion. Thus the virial mass of the system can be estimated as, M∼53Rσ2vG,Ω∼54πσ2vGR2ρc.
90% baryons reside as intracluster media (ICM). These gases are heated to 10 to 100 MK due to gravitational energy and make good X-Ray sources. For ICM, ⟨ϵk⟩≃32kBT/μMp, where T is the temperature and μMp is the gas molecule mass. The virial mass of the system is, M∼5RGμMpkBT,Ω∼154πkBTGR2μMpρc
Kent and Gunn (1982) measured the velocity dispersion of Coma cluster and found the mass-to-light ratio M/L∼181h−150Υ⊙,Ω∼0.1, confirming Zwicky's (1933) speculation of dark mass. Carlberg et al. (1997) measured a sample of 14 clusters, containing 1150 galaxies. The average cluster virial mass-to-light ratio is 213±59hΥ⊙, corresponding to density fraction Ω∼0.19±0.1. In a number of study of our own Virgo supercluster, the velocity dispersion is determined to be around 250±20 km/s, implying Ω=0.2±0.1. For compilation of investigation of cluster masses and mass-to-light ratio, see Trimble 1987.
These are various issues using virial theorem. As the start, clusters are not totally isolated and there is no clear boundary between them. R has to be some length scale. Furthermore, the virial equilibrium assumption is also questionable, although there is no doubt that the system is equilibrating. Hence virial analysis can only provide an order of magnitude estimation. Virial mass determination can be calibrated and improved by N-body simulation.
Gravitational Lensing
Mass deflects light traveling by. Just light optical lens bends light rays, this effect can also form image, known as gravitational lensing. Although light deflection in gravitational field has been discussed by several authors notably including Newton, Laplace, Cavendish (1978), Soldner (1803) and Einstein (1911, based on equivalence principle), it was Albert Einstein (1915) first get the correct deflection angle Δθ=4GMr, following his triumph of general relativity, and related it to gravitational lensing. Using gravitational lensing to measure nebulae mass was first suggested by Zwicky (1937) and confirmed by Walsh et al. in "Twin Quasar" system in 1979. Einstein first thought gravitational lensing was too rare to be useful. However, today gravitational lensing has superseded dynamical methods, as the most powerful mean of mass measurement.
Fig. 1: geometry of gravitational lensing.
Strong Lensing In the strong lensing case, the size of the lens object is much smaller than the lens-source distance and lens-observer distance.
The image angle θ and source angle β is related through deflection angle α (See the geometry configuration in Fig. 1), →β=→θ−DdsDsΔ→α(→θ)≡→θ−→α(→θ).
The vector hats indicate the 2D nature of these angles. Different →θ may result the same →β, reflecting the possibility of multi-image formation. Under the weak field approximation and thin lens approximation, the deflection angle, →α=4GDdsDs∫d3x′ρ(x′)→ζ−→ζ′(→ζ−→ζ′)2≡4GDdsDs∫d2ζ′Σ(→ζ′)→ζ−→ζ′(→ζ−→ζ′)2,
where →ζ and →ζ′ are projected position vectors. It is convenient to use angular parameters, →α(→θ)=4G∫d2θ′σ(→θ′)→θ−→θ′(→θ−→θ′)2=∇ψ(→θ),
where σ(→θ)≡Σ(Dd→θ′)DdsDd/Ds is the projected density, ψ=4G∫d2θ′σ(→θ′)ln|→θ−→θ′| is angular potential. It can be shown it satisfies Poisson equation, ∇2ψ(→θ)=8πGσ(→θ).
The local image distortion (See Fig. 2) is related to the Jacobian matrix, ∂βi/∂θj=δij−∂2ψ∂θi∂θj=1ij−(κ+γ1γ2γ2κ−γ1)ij
Fig. 2: meaning of distortion parameters, γ≡γ1+iγ2. Figure from Wikipedia.
The resulted image would a ring, arc, or multiple images depending on the relative position and shapes of the lens and source (See Fig. 3).
Fig. 3: images of strong lensing. Left: An Einstein ring; Right: An Einstein cross.
As an example, consider Einstein ring (Fig 3a). It occurs when the lens, source and the observer align on a straight line (β=0). The total mass of the lens system is M=dSdL4G(dS−dL)θ2E
where d is angular diameter distance and θE is the angular radius of the ring.
For more general strong lensing, the mass distribution of the lens can be reconstructed from reasonable modeling of the lens and source (see for Koopmans (2005) more technical details). Reconstruction of mass map (See Fig. 4) of CL0024+1654 from strong lensing by Type et al. (1998) shows 98% of the cluster mass is dark matter in 35h−1 kpc core.
Fig. 4: mass reconstruction of CL0024+1654 from strong lensing. Galaxies are shown in blue, dark matter distribution is shown in orange.
weak lensing In weak lensing, light is deflected by large number of non-uniformly distributed mass a long its path. Thus the thin lens approximation fails. The Jacobi matrix has to be generalized as, ∂βi/∂θj=δij−∫χh0dχg(χ)∂2Ψ∂ζi∂ζj,
where ζ is transverse distance, Ψ is Newtonian potential, χ is the comoving distance. The weight function is g(χ)=2r∫χhχdχ′n(χ′)r(χ−χ′)/r(χ′), where n(χ) is normalized lensing object distribution, r=dA/(1+z),dA is the angular diameter distance, χh is the comoving distance to the horizon.
The image of the background galaxy is slightly distorted, known as cosmic shear. Statistical characteristics of the cosmic shear field provide valuable information of the lens system. Detailed projected mass can be reconstructed from it. Because the cosmic shear is only a few percent effect, it requires careful image processing. It turns out the point spread function (PSF) is one of the major sources of image distortion, which has to be corrected.
Cosmic shear has been observed by Van Waerbeke et al. (2000), Bacon et al. (2000) and Wittman et al.(2000). The observation is consistent with prediction from Λ-CDM model. Clowe et a. (2006) compared the optical and X-Ray image with weak lensing mass reconstruction of a merging cluster system 1E0657-556, and suggested the > 70% system mass is dark matter (See Fig. 5). The Hubble Space Telescope (HST) Cosmic Evolution Survey (COSMOS) project (2004 - 2005) led by Scoville measured 1.637 square degrees region, shape of half million distant galaxies, and used their distortion image to reconstruct the projected mass and mass evolution with redshift (See Fig. 6 and 7).
Fig. 5: observation of 1E0657-556. Left: optical band; Right: X-Ray band. The mass contours are reconstructed from weak lensing.
Fig. 6: Large scale structure mass distribution from COSMOS project. The total projected mass from weak lensing, is shown as contours in a and gray level in b c d; Stellar mass in blue; galaxy number density in yellow; hot gass in red.
Fig. 7: Three-dimensional reconstruction of the dark matter
distribution from COSMOS project.
microlensing microlensing is a gravitational lensing by pass-by massive compact astronomical objects that causes background light source apparent brightening in a certain a mount of time (several months to years). Microlensing involves small and usually faint lenses such as dwarfs and blackholes. It provides a major mean to detect massive compact astronomical halo objects (MACHOs) including planets, red, brown and black dwarfs, neutron stars and black holes etc. Microlensing is very useful for baryonic dark matter detection. However, two surveys of MACHOs shows that they are insignificant of the overall halo mass.
Evidences of dark matter can be tracked back to Oort (1932) and Zwicky (1933). In 1970s, study of galaxy rotation curves shows clear evidence of missing mass. Since then, overwhelming evidences, direct or indirect, emerge from galaxy velocity dispersion, cluster X-Ray spectroscopy, strong and weak gravitational lensing, N-body simulation, large scale structure, comic microwave background (CMB), baryon acoustic oscillation (BAO), Type-Ia supernovae (SNe) and Ly-α forest.
The concordant cosmology model Λ-CDM postulates existence of significant amount of dark energy and cold dark matter. Λ stands for Einstein's cosmology constant, i.e. dark energy; CDM stands for cold dark matter. Many other competing cosmology models, such as CHDM, OCDM, SCDM and τCDM, also require some amount of dark matter. The success of CDM cosmology models forces people to take their postulates seriously.
Modern cosmology is based on three observation facts of the universe: in large scales (≳ 10 Mpc ), the universe is homogeneous (See Fig. 0), isotropic and the Doppler-shift velocity of an observable object is proportional to their distance to the earth. The third observation is well known as Hubble's law. The proportionality of the recession velocity to the distance v/d=H(t) is called Hubble's parameter. The current value is called Hubble constant, H0=71±4 km/(s⋅Mpc). Two dimensionless constants are frequently used, h=H0/100 km/(s⋅Mpc) and h50=H0/50 km/(s⋅Mpc). Hubble's law implies the universe is undergoing a homogeneous expansion.
Fig. 0: Density fluctuations vs scale. Image from Sloan Digital Sky Survey project.
To generalize our limited knowledge of the universe, one also need to adopt a modern version of Copernican principle, formally termed Cosmological Principle. Cosmological principle extends the three observation facts to the whole observable universe. Mathematically it assigns the universe a symmetry and leads to Robertson-Walker (RW) metric: ds2=−dt2+a2(t)(dr21−kr2+r2dΩ2θ,ϕ),
where r is called comoving distance, a(t) is called scalar factor and related to Hubble parameter H(t)=˙a/a. RW metric describes three classes of universe, open (k<0), flat (k=0) and close (k>0).
Fig. 1: three types of universe, closed, open and flat. According to General Relativity, the geometry of the universe is determined by the ratio Ω0 of the total energy density and the critical density. Credit: NASA/WMAP Science Team
According to Einstein's Equation of Field (EEF), the geometry of the universe if ultimately determined by the mass distribution Tμν and probably also cosmological constant Λ. EEF implies: (˙aa)2+ka2=8πG3c2(ρ+ρΛ)2¨aa+(˙aa)2+ka2=8πGc2(ρΛ−p/c2),
where ρ is the total energy density, p is the pressure owing to ρ and the motion, ρΛ=Λ/8πG is known as dark energy.
Similarly, introduce Hubble densityρH≡38πGH2 and curvature densityρk=−3k8πG, total energy density ρ0=ρ+ρΛ. The current value of Hubble density is called critical density ρc≡38πGH20. It is convenient to work with dimensionless density ratios Ωi=ρi/ρc, also known as density fractions or relic fractions. EEFs become, 1=Ωk+Ω0¨aa=−H202∑iΩi(1+3wi).
The main contributions for Ω0 include dark energy ΩΛ, dark matter ΩDM (cold ΩCDM, warm ΩWDM and/or hot ΩHDM), neutrinos Ων, baryonic matter Ωb and mosmic microwave background radiation (photons) ΩR etc. wi=pi/ρi is called equation of state. For idea gas, wi are constants, which is indeed true in cosmology since the typical density is only ρc∼10−26kg/m3. For non-relativistic matters such as baryons and cold dark matter, w=v2s/c2≃0, where vs is the speed of sound in such a matter medium. For relativistic particles such as photons, neutrinos and hot dark matter, w=1/3. Energy conservation ∇νTμν=0 (also implied from EEFs) implies ρ(t)∝a−3(1+w). Dark matter density ρΛ stays constant while the universe expands, implying wΛ=−1. In some other models, there exists another hypothetical energy similar to dark energy, called quintessence. Quintessence may have w≤−1. Measurement of the deviation of wΛ from -1 provides information of existence of quintessence.
In summary, the geometry of the universe is determined by the energy density ratio Ω0; the acceleration of the universe expansion is determined by the relative abundance of energy and matter. Conversely, we can determine the values of these density ratios by measuring the observables associated with the cosmos geometry and/or expansion acceleration. The existence of dark matter as well as dark energy thus is measurable.
The density of a galaxy and other astronomical structures can be obtained from their mass-to-light ratio. As we will see in following sections, it may provide direct evidence of existence of dark matter. Given the mass-to-light ratio Υ (V-band), the density fraction Ω=(6.12±2.16)×10−4h−1Υ/Υ⊙. Typical cluster mass-to-light ratio is 200 - 300 Υ⊙, indicating a density fraction 0.17 - 0.26.
The geometry of the universe affects the anisotropy of the CMB power spectrum. Cosmic Background Explorer(COBE) (1989 - 1996) and Wilkinson Microwave Anisotropy Probe (WMAP) (2001 - ) and others measured the full sky CMB angular power spectrum (See Fig. 2 & 3).
Fig. 2: 7 years WMAP full sky image of CMB. Credit: NASA/WMAP Science Team
Fig. 3: the angular power spectrum of CMB from WMAP. Credit: NASA/WMAP Science Team
The deviation of high red-shift Type-Ia supernovae from standard candle reflects the acceleration of the universe expansion. In 1998, High-Z supernova Search Team and Supernova Cosmology Project report evidence that the universe expansion is accelerating (See Fig 4).
Fig. 4: measurement of high-z supernovae magnitudes vs. red-shift z.
Similar to CMB fluctuation, BAO is the fluctuation of baryon density in the universe. Sloan Digital Sky Survey (SDSS) project provides an image of the distribution of matter (See Fig. 5). SDSS Team report discovery of baryon acoustic peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies, which provides information of cosmology model parameters (See Fig. 6).
Fig. 5: a SDSS map of local galaxies. See a 3D map of SDSS-III galaxies below.
Fig. 6: SDSS galaxies two point correlation function vs. distance. The magenta curve is pure CDM model Ωmh2=0.105, which lacks acoustic peak at around 100 Mpc/h. Other models are green, red, blue Ωmh2=0.12,0.12,0.14,0.15. All models take Ωbh2=0.024,n=0.98.
Combine all these cosmological probes, the current data suggest (See Fig. 7), ΩΛ≃0.73,ΩM≃0.27,ΩR≃6×10−5,Ων<0.0062,Ω0≃1.00,wΛ≃−1±0.053.
This result is also consistent with the typical mass-to-light ratios measured in galaxies and clusters. We conclude from these data: (1): our universe is ( at least close to ) a flat universe (k≃0); (2): there is significant amount of dark energy (ΩΛ>ΩM≫Ωothers); (3): The universe expansion is accelerating (¨a/a>0).
Fig. 7: ΩΛ vs. ΩM using compilation of various cosmological probes.
Modern cosmology postulates the universe is born in a big bang in around 13.7 billion years ago. The early universe is in equilibrium at very high temperature. As it expands, temperature drops, the number of heavier particles drops, until their annihilation rates below the universe expansion rate. Thus they freeze out from reaction and become the relic. The big bang nucleosynthesis predicts abundance of elements based on the baryon-to-photon ratio η. Measurement of element relative ratios determines η, hence the baryon relic density, since photon relic density is known from CMB. The current data suggest, Ωbh2=0.0214±0.0020(9.3%).
Now the evidence of dark matter arises: ΩM≃0.3 but Ωb≃0.04, suggesting there are significant amount of dark matter ΩCDM≃0.23 (See Fig. 8).
Fig. 8: the contents of the universe. Credit: NASA/WMAP Science Team.
