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Antimatter is an assembly of antiparticles. A cosmological antimatter population is distinct from the small secondary antiparticle populations produced by energetic collisions.

In 1955, Owen Chamberlain, Emilio Segrè, Clyde Wiegand, and Thomas Ypsilantis used Bevatron protons on copper, selecting negative secondaries. Magnetic fields selected $p=1.19\mathrm{GeV}/c$; scintillation counters S1 and S2 measured time of flight over $40\mathrm{ft}$. Cherenkov detector C1 flagged $\beta >0.79$; C2 accepted $0.75<\beta <0.78$ after material losses. S3 checked traversal. The cuts rejected negative pions.^[ref]

Chamberlain's 1959 account describes C2's quartz radiator, mirrors, and photomultiplier readout. The trigger combined delayed scintillation counter signals with C2; photographed oscilloscope traces exposed fast particles and accidental coincidences through C1 pulses or extra pulses. Reversing the magnetic fields provided a positive-proton control and revealed an alignment error. Changing selected momentum at fixed velocity acceptance tested for a proton-mass peak.^[ref]

Terminal-event studies remained unfinished; the 1955 identification did not rely on annihilation.^[ref]

The logic is useful far beyond this experiment. A magnetic field separates electric charge signs and magnetic rigidity, but particles of different rest masses can share both. A time of flight signal adds velocity, while a Cherenkov detector independently checks whether that velocity is plausible. An accidental coincidence can imitate the delay of a slow particle without being one particle traversing the apparatus. Agreement between independent measurements is therefore part of the inference, rather than a redundant decoration.

Number-changing reactions involving a relic candidate and another nearly degenerate species. If reactions interchange the species rapidly enough, the effective annihilation rate depends on their joint abundances and channels. A single-species relic estimate can then fail even for fixed candidate mass.

The line-of-sight, solid-angle integral of squared dark-matter density used for annihilation fluxes with a position-independent rate coefficient. It separates an astrophysical density model from particle yields and annihilation rates. A decay signal instead scales with a single power of density. Substructure or spatially varying velocity-dependent rates can prevent a simple smooth-density factorization.

The annihilation of an electron with a Positron, producing other particles; a common final state consists of two photons.

For an imposed equilibrium cutoff $m{c}^2=P{k}_B{T}_f$ and density $n_f=6[m{c}^2{k}_B{T}_f/(\hslash c{)}^2{]}^{3/2}{e}^{-P}$, dilution by $(T_0/T_f{)}^3$ cancels the explicit mass in the final number density. The rest-energy density still scales with particle mass. This result assumes constant entropy degrees of freedom and no post-cutoff annihilation; entropy conservation adds a factor $g_{\ast s,0}/g_{\ast s,f}$ when these assumptions are relaxed.

Gravitational evidence requires much more nonbaryonic matter than can be supplied by ordinary luminous material or by the baryon abundance permitted by nucleosynthesis. A stable, electrically neutral massive particle is a plausible cold component. Thermal production followed by cosmological particle freeze-out gives an additional motivation: an annihilation rate near a weak-interaction scale can leave an appreciable relic abundance. This is a mechanism and search hypothesis, not proof that the dark matter must be a WIMP or have any particular elastic-scattering cross section.

The plotted regions are conditional WIMP interpretations of different measurements. The experiments use different targets and distinguish signal from background differently:

The plot also includes CRESST experiment, whose cryogenic calcium-tungstate modules combine phonon and scintillation-light signals. Different nuclei contribute to its recoil interpretation. Its excess region is another conditional candidate region, not an extra confirmed detection.^[ref]

Around ten GeV, the shaded regions favour cross sections roughly $10^{-41}$–$10^{-40}\mathrm{c}{\mathrm{m}}^2$, while the XENON100 solid curve and the improved low-mass CDMS curve cut into or exclude much of those regions under the common elastic, spin-independent WIMP-nucleus scattering interpretation expressed per nucleon. There is tension within that shared model; the plot does not show mutually confirmed discoveries. electron backgrounds, threshold response, nuclear-recoil quenching factors, channeling assumptions and the halo velocity distribution can shift interpretations. Changing the interaction model can also alter target comparisons, but cannot establish a WIMP by assertion. The 100-live-day XENON100 result itself reported candidates compatible with estimated background.^[ref]

For a rough dimensional event estimate, $1\mathrm{c}{\mathrm{m}}^2=10^{-4}{\mathrm{m}}^2$ givesIf a collider production cross section had this value, that small yield, before acceptance and backgrounds, would not support a likely discovery. The plotted nuclear-scattering cross section is not the LHC production cross section, however. Converting between them needs a mediator, couplings, parton distributions and production kinematics; a light stable WIMP would normally be inferred from missing transverse momentum with a visible recoil object, not a visible WIMP track. The mass makes pair production kinematically accessible, but the plot and integrated collider luminosity alone do not decide discovery probability.

For the relic estimate, define $M=m{c}^2$ and $\theta =k_{B}T$. The sharp-freeze-out relic dilution model givesAssume stable particles, no subsequent annihilation, and $RT=\mathrm{constant}$. Conserved comoving particle number then givesThe present rest-energy density and its critical fraction areThus the supplied toy model yields a cosmologically substantial density, of the right broad scale to motivate a dark-matter candidate. It is not an independent precision prediction: $P$ is imposed and the abundance depends exponentially on it. If entropy degrees of freedom change, entropy conservation instead gives an extra factor $g_{\ast s,0}/g_{\ast s,f}$ in $n_0$ when using the photon temperature. The species content needed to evaluate that correction is not supplied. A realistic calculation also follows residual annihilations with the abundance Boltzmann equation rather than stopping exactly at equilibrium freeze-out.

annihilation can produce gamma rays, charged antiparticles and neutrinos, directly or through decay and hadronization of the primary products. For self-conjugate dark matter of mass $m_{\chi }$, the annihilation rate per unit volume is $⟨\sigma v⟩{\rho }_{\chi }^2/(2m_{\chi }^2)$. For a photon yield $d{N}_{\gamma }/dE$, the optically thin flux from a chosen solid angle isUse consistent mass-energy units. The factor $1/2$ assumes identical self-conjugate particles; distinct particle-antiparticle populations require their separate number densities. A gamma-ray continuum with an endpoint near the particle mass is generic for many channels, whereas a narrow line from $\chi \chi \to \gamma \gamma$ or $\gamma Z$ would be especially distinctive but often loop suppressed. dwarf spheroidal galaxies offer high dark-matter content with limited conventional emission; the Galactic centre has a potentially larger signal and much more complicated foregrounds.

Charged Positrons and antiprotons are redistributed by magnetic fields and lose energy, so their radiation spectrum depend on propagation and cannot usually point directly to the source. annihilation electrons can also produce synchrotron and inverse-Compton radiation. dark matter captured in the Sun could produce escaping high-energy neutrinos, with the signal depending on capture, annihilation equilibrium and particle interactions. Early annihilation energy injection can alter recombination and cosmic microwave background anisotropies.

A persuasive interpretation joins particle-like spectral structure with a consistent density-dependent morphology and other channels. Pulsars, cosmic-ray interactions and unresolved sources can imitate continuum excesses. Density-profile uncertainties, substructure and velocity-dependent annihilation modify the predicted signal; a lack of a detectable line does not exclude all annihilating dark matter.

Particle candidate. A stable, electrically neutral weakly interacting massive particle can become nonrelativistic before cosmological particle freeze-out. Its annihilation rate per particle $\Gamma =n⟨\sigma v⟩$ eventually falls below the Hubble parameter; the surviving comoving number then remains approximately fixed. A weak-scale annihilation cross section can give a cosmologically significant thermal relic. This is a mechanism and a parameter-scale motivation, not a guarantee that every weakly interacting particle has the right abundance.

supersymmetry supplies neutralinos, mixtures of neutral electroweak gauginos and higgsinos. If a neutralino is the lightest supersymmetric particle and R-parity is conserved, it cannot decay solely into Standard Model particles and is stable. Its electroweak interactions can make it a WIMP. Conservation of R-parity and a neutral lightest state are additional assumptions; R-parity violation, coannihilation, composition and resonant annihilation can substantially change the conclusion.

An underground test. XENON100 at Gran Sasso used a liquid-xenon target in a two-phase time projection chamber. A WIMP scattering elastically from a xenon nucleus could produce a low-energy nuclear recoil. The interaction makes prompt particle scintillation, S1, and ionization electrons. An electric field drifts the electrons upward; their extraction into xenon gas produces delayed electroluminescence, S2. The delay measures depth, while the S2 light pattern determines the transverse position. An inner fiducial volume suppresses surface backgrounds through xenon self-shielding; underground overburden reduces cosmic-ray muons, and shielding and material selection reduce radioactivity.^[ref]

The S2/S1 ratio separates most electron recoils from nuclear recoils. Gamma-source calibration maps the electron-recoil leakage; an americium–beryllium neutron source calibrates nuclear-recoil response and cut acceptance. Purity and position corrections must be measured, and selection fixed before unblinding the search region. neutrons can themselves produce single nuclear recoils, so discrimination is not perfect; material assays and transport simulations constrain this background. In the 224.6-live-day, 34-kg analysis, two candidate events were compatible with the expected $1.0\pm 0.2$ background events. The result constrained scattering cross sections rather than establishing a discovery.^[ref]

A predicted count also depends on the local dark matter halo density, distribution of velocities, recoil threshold and nuclear response. Thus a null result constrains a particle model under stated astrophysical assumptions; it does not exclude all dark matter. A collider missing-momentum signal would likewise need independent evidence for a cosmological lifetime.

Relic energy density in the stipulated freeze-out approximation. Let $M=m{c}^2=1900\mathrm{GeV}$ and $\theta =k_{B}T$. Writing the given distribution in energy units givesBy sharp-freeze-out relic dilution, after cosmological particle freeze-out conserve particle number, $n{a}^3=\mathrm{constant}$. In the approximation $aT=\mathrm{constant}$ for the background bath,Inserting the printed inputs yieldsand henceThis is approximately $93\%$ of the stipulated dark-matter energy density, $0.2\times 5=1\mathrm{GeV}{\mathrm{m}}^{-3}$, so the toy calculation gives the right order and is close to the target. At fixed $P$ the cancellation of $M$ in $n_0$ is exact for the given prefactor, while the present energy density remains proportional to $M$.

The equilibrium exponential must be evaluated at freeze-out, not at today's temperature: equilibrium no longer maintains the particle number afterward. More accurately, comoving entropy conservation gives $a^3{g}_{\ast s}{T}^3=\mathrm{constant}$ and multiplies the displayed $n_0$ by $g_{\ast s,0}/g_{\ast s,f}$, when both counts use the same bath-temperature convention. Thus $0.185$ is the constant-$g_{\ast s}$ estimate supported by the supplied toy model. A refined abundance would require additional entropy degrees of freedom and annihilation history: realistic entropy release, gradual freeze-out and the model's annihilation channels matter.

supersymmetry relates bosons and fermions through fermionic symmetry generators. A main motivation is the Lorentz scalar hierarchy problem: related boson and fermion loop contributions cancel particular ultraviolet sensitivities in an exactly supersymmetric theory. soft supersymmetry breaking leaves residual sensitivity to the superpartner scale, so a very heavy spectrum does not automatically solve naturalness. Supersymmetric matter content can also improve gauge-coupling unification, and a stable neutral lightest superpartner can be a dark-matter candidate. None of these motivations is itself experimental evidence; supersymmetry must be broken if ordinary particles and their partners have different observed masses.

If R-parity is conserved, superpartners are produced in pairs and cascades end in a stable lightest supersymmetric particle. A neutralino LSP can escape the detector, giving missing transverse momentum. Colored squarks and gluinos can generate energetic jets, sometimes b-tagged jets and leptons, plus that imbalance. An inclusive supersymmetry search classifies broad event samples by jet and lepton multiplicities, transverse momentum sums and missing momentum, without requiring a fully reconstructed decay chain.

Background controls are part of the physics argument. Lost-lepton W and top events can be constrained using lepton collider control regions; invisible-Z production can be related to visible-Z or photon samples with appropriate transfer factors. Instrumental imbalance in multijet events needs detector-quality checks and data sidebands. An excess in a collider signal region should survive uncertainty in those extrapolations, efficiencies and luminosity, with independently defined validation regions and attention to the number of searches performed.

An exclusive supersymmetry search targets a more specific production mode and decay pattern. Electroweak chargino-neutralino production can yield three leptons plus missing momentum; a cascade through a slepton can yield a dilepton invariant-mass edge that constrains mass combinations. Such searches often have cleaner backgrounds but depend more strongly on branching fractions and intermediate masses. An endpoint does not necessarily determine every absolute mass without additional observables.

Different spectra require different strategies. For a compressed supersymmetric spectrum, small parent-daughter mass differences make the visible decay products soft. initial-state radiation can recoil against the pair and provide a trigger, supplemented by soft-lepton reconstruction. The ATLAS compressed-spectrum study explicitly uses small neutralino mass differences and initial-state radiation to define a dedicated search rather than applying a hard-lepton selection indiscriminately.^[ref] If R-parity is violated, the LSP can decay visibly, so high-multiplicity jet or lepton channels may matter more than large missing momentum. CMS separately studied hadronic and leptonic final states for this reason.^[ref] Long-lived particles instead motivate displaced vertices, disappearing tracks, abnormal ionization or time-of-flight measurements. Thus there is no single model-independent missing-energy cut that covers every supersymmetric spectrum.

For the hypothetical relic-density calculation, use the supplied distribution and retain its prefactor exactly. Put $M=m{c}^2$, $\Theta =k_{B}T$ and ${\Theta }_0=k_B{T}_0$. Thennumber density, denoted $N$ in the paper, is written $n$ here to distinguish it from a total particle count. The cosmological particle freeze-out temperature in energy units isAssume a stable nonrelativistic relic, negligible further annihilation and $aT=\mathrm{constant}$ after cosmological particle freeze-out, using sharp-freeze-out relic dilution. Its comoving particle number is conserved, soThe particle mass cancels from this present number density under the stated approximation. Its present rest-energy density is $M{n}_0$, not merely $n_0$:This is only 0.371% of the critical density, not a universe-closing component. The correct further comparison is with the measured dark-matter fraction, not an assumption that all critical density must be dark matter. In standard cosmology this abundance would be a small subcomponent, despite a possible collider discovery.

The exponential freeze-out sensitivity makes the result highly sensitive to $P$. Also, thermal entropy release means $aT$ is not exactly constant through the whole cosmic history. If total comoving entropy is conserved, the above number density acquires a factor $g_{\ast s,0}/g_{\ast s,f}$, involving entropy degrees of freedom. Those degrees of freedom and a full annihilation history are not given, so no precise correction is justified from the supplied data.

Establishing the nature of dark matter would require more than measuring a missing particle's collider mass. Measure its spin, charges, interactions, decay lifetime or stability limits, and annihilation or coannihilation processes; compare the resulting relic calculation with cosmological observations. Seek compatible direct nuclear-recoil signals and indirect annihilation or decay products, while controlling astrophysical and detector backgrounds. A collider-invisible lifetime need not be cosmologically long, and nonthermal production could change the abundance. A consistent particle identity, cosmological abundance and independent non-collider evidence are needed to connect the hypothetical discovery to the dark matter.

The charged weak current contains $\bar{\psi }{\gamma }^{\mu }{P}_L\psi$. For an ultrarelativistic external fermion, it selects negative helicity; its antifermion partner has positive helicity. Wrong-helicity charged-current amplitudes vanish in the massless limit and are suppressed by powers of $m/E$ at finite mass. The active neutrino is consequently left-helicity and its antineutrino right-helicity in this limit.

This is a charged-current statement, not a prohibition on every right-helicity Standard Model fermion. Electromagnetic and strong vector interactions act on both chiralities and conserve helicity along a massless fermion line. A neutral-current $Z$ vertex also couples to both charged-fermion chiralities with unequal strengths. For example, a right-helicity electron can scatter electromagnetically: it is not excluded from the Standard Model. In vector-current pair annihilation the massless fermion and antifermion have opposite helicities; a purely charged-current vertex keeps only the left-fermion/right-antifermion choice. Yukawa interactions connect left and right fields and must be distinguished from these vector-current selection rules.

The leading subprocess is $u\bar{d}\to W^{+}$. There are two beam assignments, and charge conjugation relates antiproton PDFs to proton PDFs. ThereforeIn a narrow-width leading-order normalization the prefactor is $\pi g^2/(12s)$ when $|V_{ud}|=1$; only the PDF dependence is needed for the fractions below.

Write the common sea PDF as $S=\bar{u}=\bar{d}=\bar{s}=\bar{c}=\Sigma /8$. The Valence and sea decomposition of proton-antiproton W production gives the three parton luminositiesThe factor two in the sea-sea term includes both beam assignments. The antiproton's valence antiquarks make valence-valence Annihilation possible.

The charged-current process iswith a $t$-channel $W^{-}$ emitted at the electron-to-neutrino vertex and absorbed at the antimuon-to-antineutrino vertex. It is not an $s$-channel Annihilation of the unlike-flavour charged leptons into one $W$.

At high momentum transfer the incident electron's left-chiral fraction tends to $4/5$. In the collision centre-of-mass frame, the incoming antimuon moves along $-z$ and its charged-current allowed right helicity has spin along $-z$. A rest-frame spin at Angle $\theta$ to $+z$ projects onto that spin direction with probability ${\sin }^2(\theta /2)$. Therefore, if ${\sigma }_0$ denotes the cross section for a pure left-helicity electron and fully selected antimuon spin,It vanishes at $\theta =0$ in the ultrarelativistic selection limit and is maximal at $\theta =\pi$. Finite-mass corrections can fill the suppressed orientation. The absolute normalization depends on beam energy and the exchanged-boson propagator; the spin-angle dependence is what is fixed here.

Useful examples with no net quark flavor are the eta c meson ${\eta }_c=c\bar{c}$ and the eta b meson ${\eta }_b=b\bar{b}$. Examples with nonzero quark flavor are the kaon $K^{+}=u\bar{s}$ and the D meson $D^{+}=c\bar{d}$. These are pseudoscalar mesons: in the lowest quark model configuration the constituent spins combine to $S=0$, the relative orbital angular momentum is $L=0$, and the total angular momentum and parity are $J^P=0^{-}$. For the self-conjugate examples, meson parity and charge conjugation also gives $C=(-1{)}^{L+S}=+1$. Electrical neutrality alone would not imply zero net quark flavor; for example $K^0=d\bar{s}$ has strangeness.

Restoring reduced Planck constant, decay width and mean lifetime satisfy $\Gamma \tau =\hslash$. Thus the representative numbers correspond toThe mean lifetimes differ by at least $3.0\times 10^{10}$. Hidden-heavy-flavor quarkonium can undergo quark-antiquark annihilation into gluons, followed by hadronization. A $0^{-+}$ color-singlet state can annihilate into two gluons. A lightest open-flavor meson cannot simply annihilate through the strong interaction, which conserves net quark flavor. With no lighter accessible final state carrying that flavor, it must undergo a weak interaction changing a constituent's flavor. The small weak interaction amplitude, CKM matrix factors and available Lorentz-invariant phase space produce a much smaller decay width.

Qualification. A decay width of order tens of MeV is not a universal property of flavor-neutral pseudoscalar mesons. The neutral pion has $\Gamma \simeq 7.8\mathrm{eV}$ and decays predominantly by the electromagnetic interaction, a concrete counterexample. Its mass lies below the lightest allowed hadronic final state. The examples above illustrate the intended annihilation-versus-open-flavor comparison; the numerical scale depends on thresholds and selection rules.^[ref]

Positronium is the electromagnetic bound state of an electron and a Positron. Their equal masses give reduced mass $m_e/2$, half the hydrogenic Rydberg binding scale and approximately twice the electron-proton separation of hydrogen. Its spin singlet and triplet differ in hyperfine energy; annihilation also affects their physical lifetimes and splitting.

In a stable-particle approximation with negligible later annihilation, comoving particle number is conserved and physical number density falls as $a^{-3}$. Replacing scale-factor ratios by photon-temperature ratios additionally assumes no change in the entropy degrees of freedom.