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In 1986, Johannes Georg Bednorz and Karl Alexander Müller precipitated mixed oxalates from aqueous barium, lanthanum and copper nitrates using oxalic acid. Heating at $900{}^{\circ }\mathrm{C}$ for five hours preceded pressing at $4\mathrm{kbar}$ and reheating for sintering. X-ray diffraction resolved three phases. Rectangular pieces carried gold electrodes and indium wires; four-terminal sensing in a continuous-flow cryostat measured electrical resistance versus temperature. Annealing atmosphere and measuring electric current density were varied; larger electric current densities suppressed the drop. An onset near $35\mathrm{K}$ differed from the much lower temperature where the drop approached three orders of magnitude.^[ref]

This was evidence for possible granular superconductivity, with phase identification unfinished. The paper deferred Meissner effect and heat capacity tests; its proof note corrected bulk lanthanum/barium ratios. A resistive onset did not establish a uniform bulk superconducting transition temperature.^[ref]

Their 1987 authored lecture describes later magnetometer checks on lead, followed by magnetic susceptibility measurements: samples with a resistive drop developed diamagnetism at somewhat lower temperatures. Combining magnetic, transport and X-ray diffraction results identified barium-substituted $\mathrm{L}{\mathrm{a}}_2\mathrm{Cu}{\mathrm{O}}_4$ as the superconducting phase. These later results strengthened the case beyond the initial mixed-phase transport evidence.^[ref]

Ferdinand Reich investigated zinc minerals using chemical separation and spectrum analysis. With Hieronymus Theodor Richter, he identified indium in 1863 after finding a spectral feature inconsistent with the expected thallium. The episode illustrates how a distinctive spectral line can guide the isolation of a new chemical element.^[ref]

A scientist associated with the identification of indium.

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An experimental nuclear physicist who coauthored a 1964 comparison of allowed and unique first-forbidden beta-decay spectrum shapes. A double-lens spectrometer measured the shapes of several isotope spectra, testing whether their energy dependence followed the simplest transition models. The report concerns specific indium, potassium, rubidium, strontium and yttrium isotopes; its conclusions should not be transferred to an arbitrary isotope without checking the transition.^[ref]

Hieronymus Theodor Richter and Ferdinand Reich identified indium through spectrum analysis of material obtained from a zinc mineral. The unusual indigo-coloured spectral line distinguished the new chemical element from thallium, which Reich had initially sought. Their joint 1863 paper reported the new substance.^[ref]

A chemist associated with the identification of indium.

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Indium is the chemical element with atomic number 49 and symbol $\mathrm{In}$. It is a metal. It is a soft group-13 metal, commonly forming $+3$ compounds. Indium-containing transparent conducting oxides and indium gallium nitride illustrate how the element contributes to optical and electronic materials without behaving as a free metal.^[ref]

Indium antimonide is a narrow-gap semiconductor made of indium and antimony, with chemical formula $\mathrm{InSb}$. Its small band gap permits absorption of comparatively low-energy infrared photons, making it useful in infrared detection.

For an ideal interband threshold, $hc/\lambda$ must reach the gap; actual detector response also depends on optical coupling, carrier collection and temperature. Thermal excitation across a small band gap can supply unwanted carriers, so an operating detector's dark current is an essential measurement alongside quantum efficiency. ^[ref]

Indium oxide usually denotes indium(III) oxide, $\mathrm{I}{\mathrm{n}}_2{\mathrm{O}}_3$, a solid chemical compound of indium and oxygen. Formal oxidation states of $+3$ for indium and $-2$ for oxygen give charge balance: $2(3)+3(-2)=0$. The formula expresses the elemental ratio; it does not imply discrete molecules in the solid.^[ref]

Doping this oxide with tin produces the material family indium tin oxide, used for transparent conducting layers. Electrical and optical performance depend on charge-carrier density and preparation, so knowing the host compound's formula alone does not specify a film's conductivity.^[ref]

Polykarp Kusch and Henry Michael Foley compared hyperfine structure resonance frequencies for different electronic states of gallium, indium and sodium. Their 1948 paper reports mutually consistent departures from the ratios expected with orbital factor $1$ and spin factor $2$. Comparing several states constrained the alternative explanation of perturbed atomic levels.^[ref]

The Rabi molecular beam magnetic resonance experiment explains the readout principle: a resonant transition changes an atom's magnetic response, and hence its transmitted beam signal. Kusch describes rapidly interchangeable ovens, several radio frequency oscillators and careful field homogenization. Measurements taken during monotonic field drift were reduced to a common field.^[ref]

Real hyperfine structure lines are not simply bare electronic $g_J$ times field. Nuclear magnetic moments, known interaction constants and nonlinear field dependence enter the inference.^[ref] Field homogeneity controls line broadening; alternating species addresses drift. Neither control removes an error in the atomic model. The beauty of the comparison is the separation of two problems: cancelling a shared calibration scale and testing whether several physical systems imply the same electron spin g-factor.

The large rises mark the opening of Ga and As K-shell photoionization channels at their respective thresholds. Above each edge, the outgoing photoelectron interferes with waves backscattered by neighboring atoms; that interference modulates the absorption transition probability. Near-edge resonances and multiple scattering require a different level of treatment from the simple high-energy single-scattering formula. Ga has four As nearest neighbors, while As has four Ga nearest neighbors, so the two edges sample different central atoms and scattering factors even though they probe the same nearest-neighbor bond lengths.

Write $k=\sqrt{2m_e(E-E_0)}/\hslash$ and $\chi =(\mu -{\mu }_0)/{\mu }_0$ relative to a smooth atomic background. The phase $2k{R}_j+{\varphi }_j(k)$ includes the outward-and-return propagation distance and atomic phase shifts. The factor $R_j^{-2}$ describes geometrical spreading; the backscattering amplitude depends on the neighbor species. The exponential $e^{-2R_j/\lambda (k)}$ accounts for loss of coherent photoelectron propagation. Averaging over Gaussian bond-length fluctuations gives $⟨e^{2ik\delta R}⟩=e^{-2k^2{\sigma }_j^2}$.

The printed polarization factor needs a notation correction: for K-shell dipole absorption it is proportional to $({\hat{\mathbf{R}}}_j\cdot \mathbf{ϵ}{)}^2={\cos }^2{\theta }_j$, not literally the cosine of a dimensional vector dot product. Four equivalent tetrahedral bonds have an isotropic sum of these projection weights. If the sum is over shells rather than individual neighbors, it also needs the coordination number. A common conventional amplitude contains $S_0^2{f}_j(k)/(k{R}_j^2)$; omitted normalization and $1/k$ factors must be absorbed in the printed $f_B$ convention rather than silently changing its dimensions.

These are the ingredients of extended X-ray absorption fine structure. A shell fit uses calculated or reference scattering amplitudes and phases, and refines bond distances, coordination and mean-square relative disorder together with an edge-energy correction. Fourier transformation separates approximate distance contributions, but the uncorrected peak position is shifted by the scattering phase and is not an exact bond length.^[ref]

Sample A has the larger Ga–As bond length. Its oscillations advance slightly faster with $k$: at higher $k$ its corresponding maxima lie to the left of B's. Reading several full cycles gives approximate periods $\Delta k_A\simeq 1.47{\mathring{\mathrm{A}}}^{-1}$ and $\Delta k_B\simeq 1.50{\mathring{\mathrm{A}}}^{-1}$. In the constant/common-phase-slope estimate, $R\propto 1/\Delta k$, soThis is a rough percent-level difference, not a precise fitted strain. Nonconstant atomic phase shifts affect the absolute distance inferred from a period and also limit this fractional estimate. The graph does not establish which alloy has which indium concentration or how much its bulk lattice parameter changed. Local Ga–As relaxation need not follow a uniform bulk strain exactly.

Low temperature reduces thermal relative motion, preserving high-$k$ oscillations and separating small phase changes more clearly. It does not remove zero-point motion or static alloy disorder. To obtain an illustrative disorder estimate, take the high-$k$ envelope of the plotted $k\chi (k)$ to fall from about $0.19$ at $k=7.5{\mathring{\mathrm{A}}}^{-1}$ to $0.12$ at $k=10.4{\mathring{\mathrm{A}}}^{-1}$. If other envelope factors vary slowly over this interval,The value is only an order-of-magnitude, model-dependent reading: the backscattering amplitude, mean free path and normalization have not been independently removed. In particular, ${\sigma }^2$ is the bond-projected mean-square relative displacement,including correlations and static disorder. It is not uniquely either atom's mean-square displacement. Equal uncorrelated projected displacements would each contribute ${\sigma }^2/2$, but that extra assumption is not supplied by the figure.

Spectrum analysis identifies substances by the positions and patterns of characteristic spectral lines, rather than by the overall colour of a flame alone. A small amount of a suitable salt is introduced into a hot, weakly luminous flame. In the historical prism spectroscope, light enters a narrow slit, a collimator makes the emerging rays nearly parallel, a prism separates them by wavelength, and an observing telescope shows images of the slit at different spectral positions. A reference scale or comparison spectrum makes positions reproducible.

A clean platinum wire and reagent blank help distinguish the sample's signal from contamination. A reference sample establishes the expected positions, while repeated cleaning and testing check whether an unfamiliar line belongs to the sample. Several substances can be recognized in one mixture because their characteristic line patterns can coexist, although overlapping lines and changing excitation conditions complicate identification. Robert Bunsen and Gustav Kirchhoff's original account explicitly emphasizes the faint background of the flame, the prism instrument and the characteristic patterns of alkali and alkaline-earth salts.^[ref]

In modern terms, emission lines arise when excited chemical atoms or ions release photons at energies corresponding to allowed differences between energy levels:The quantum mechanics behind this equation is a later explanation, not the theory available to an 1866 candidate. Similarly, absorption lines appear when a cooler foreground gas removes particular wavelengths from a brighter background. Agreement between laboratory line positions and dark lines in the solar spectrum permits identification of constituents of the solar atmosphere without bringing a solar sample into the laboratory. It does not establish the detailed chemical constitution of every layer of the Sun.

By December 1866, striking examples included caesium (1860), rubidium (1861), thallium (1861) and indium (1863). The first two were recognized in the work of Robert Bunsen and Gustav Kirchhoff, using conspicuous blue and deep-red spectral features respectively. William Crookes recognized the characteristic green line associated with thallium, while Ferdinand Reich and Hieronymus Theodor Richter identified indium through its indigo-blue spectral signature. These observations motivated chemical separation and further characterization; an unexpected line by itself is a clue to a new chemical element, not a complete proof.^{[ref][ref][ref][ref]}

The corresponding recognition of familiar chemical elements in the solar spectrum opened stellar chemical analysis. Later discoveries such as solar helium should not be credited to the 1866 state of the subject.

Daniel Tsui, Horst Störmer and Arthur Gossard reported the effect in 1982. They grew gallium arsenide–aluminium gallium arsenide layers by molecular beam epitaxy, separating the two-dimensional electron gas from its semiconductor doping. They cut Hall bars and made indium contacts. Low-field measurements established number density and charge carrier mobility. A perpendicular magnetic field sweep measured transverse and longitudinal sheet resistivities at several temperatures. Cooling sharpened the plateau near $3h/e^2$ and the longitudinal minimum at filling factor $1/3$; integer plateaus provided an internal comparison. The longitudinal minimum remained finite at the lowest temperature: zero-temperature vanishing was unresolved. This established anomalous transport, without directly measuring excitation electric charge.^[ref]

The two readouts test different statements. A single intersection with $R_H=3R_K$ would also occur on the smooth classical relation $R_H=B/(n_{s}e)$ at $n_{s}h/(eB)=1/3$. A quantum Hall plateau instead persists over a magnetic field interval. Comparing transverse and longitudinal signals helps distinguish that plateau from a contact-placement artefact; the quantum Hall conductivity tensor inversion quantifies the contamination when longitudinal sheet resistivity is nonzero.

Later, 1997 shot noise measurements associated with quantum tunnelling at filling factor $1/3$ tested the excitation electric charge separately, finding $e/3$. That is a different observable from a Hall plateau.^[ref]