Linked from

The 34 pages that link to Interferometry, each with the reason it gives.

• Radio astronomyRelated: Correlating signals from multiple antennas enables precise radio imaging and position measurements.

• Gravitational-wave astronomyRelated: Interferometers measure the minute distance changes caused by passing waves.

• Stellar spectroscopyCompared with: It resolves stellar sizes and surface structure rather than primarily identifying spectral features.

• Phase (waves)Related: Small path changes appear as phase changes in the resulting fringes.

• Mount Wilson ObservatoryRelated: Mount Wilson pioneered stellar interferometry to measure the apparent sizes of stars.

• PolarimetryCompared with: Interferometry compares phase and path differences rather than polarization alone.

• Stellar radiusRelated: Long-baseline observations can resolve a star’s angular diameter directly.

• WavefrontRelated: Interference patterns reveal differences between wavefronts.

• Observational astronomyRelated: It can achieve resolution beyond that of a single telescope of similar size.

• Doppler spectroscopyCompared with: It can resolve angular structure or motion through phase, rather than relying solely on wavelength shifts.

• VegaRelated: Interferometric observations helped reveal Vega’s oblate shape and temperature pattern.

• Angular diameterRelated: Interferometers measure angular diameters of stars too small for ordinary telescopes to resolve.

• Coherence (physics)Narrower topic: Coherence sets the conditions under which its interference signals remain measurable.

• AltairRelated: Interferometric observations resolved Altair's noncircular stellar disk.

• AntaresNarrower topic: Optical interferometry makes Antares's tiny angular structures observable.

• Astronomical observationRelated: Combining separated telescopes can resolve details unavailable to a single aperture.

• Laser rangefinderRelated: Interferometric range measurement can achieve finer precision but usually needs controlled optical paths.

• Albert A. MichelsonNarrower topic: Michelson’s instruments exemplify how interference becomes a precision measurement method.

• Extremely Large TelescopeCompared with: Interferometers can achieve fine resolution differently, while the ELT uses one enormous segmented aperture.

• European Southern ObservatoryRelated: It lets facilities such as the VLTI resolve details beyond a single telescope’s reach.

• Large Binocular TelescopeNarrower topic: The telescope’s two mirrors can act as separated elements in an optical interferometer.

• Young's double-slit experimentNarrower topic: The double-slit arrangement is a basic example of extracting information from fringe patterns.

• Primary mirrorCompared with: Interferometric arrays can achieve fine resolution without relying on one large primary mirror.

• Be starRelated: It can resolve the angular structure and flattening of nearby Be-star disks.

• History of opticsRelated: Interference measurements tested wave theories and later measured light with precision.

• AchernarRelated: Interferometric observations revealed Achernar’s departure from a spherical shape.

• Astronomical instrumentationCompared with: Interferometers combine separated signals to achieve capabilities unavailable to a single aperture.

• Karl Guthe JanskyRelated: Later radio astronomy used interference between antenna signals to locate sources more precisely.

• Plasma diagnosticsRelated: Plasma-induced phase shifts reveal the integrated electron density along a viewing path.

• Astronomical interferometerNarrower topic: The instrument applies this broader method to electromagnetic waves arriving from astronomical sources.

• Robert BrownRelated: Radio interferometry enabled astronomers to resolve structures near the Galactic center.

• UY ScutiRelated: It can help measure the angular diameter of a distant, unresolved star.

• History of the telescopeRelated: It offers the resolving power of widely separated instruments rather than one enormous mirror.

• Von Zeipel theoremRelated: It can map the shapes and latitude-dependent brightness of rapidly rotating stars.