Interferometry allows astronomers to achieve much higher angular resolution than is possible with a single telescope, enabling them to study fine details and structures in astronomical objects.

Interferometry works by combining the light waves collected by multiple telescopes, allowing astronomers to synthesize a larger aperture and achieve finer resolution.

The baseline length is the distance between the individual telescopes in an interferometer. It determines the angular resolution and sensitivity of the interferometer.

The Michelson interferometer is a classic interferometer design commonly used for precise measurements, including the determination of the speed of light.

Long-baseline interferometers are specifically designed for high-precision astrometry, allowing astronomers to measure the positions and motions of stars with great accuracy.

Atmospheric turbulence is a major challenge in long-baseline interferometry, as it can distort the light waves and degrade the image quality.

The VLTI is a powerful interferometer array located in Chile, primarily used for high-resolution imaging of astronomical objects, including black holes and their accretion disks.

The EHT is a global network of radio telescopes designed to achieve unprecedented resolution and image the black hole at the center of our galaxy, known as Sagittarius A*.

LIGO is a large-scale interferometer designed to detect gravitational waves, ripples in spacetime predicted by Einstein's theory of general relativity.

Optical interferometry allows astronomers to achieve much higher angular resolution than is possible with a single telescope, enabling them to study fine details and structures in astronomical objects.

Optical interferometry works by combining the light waves collected by multiple telescopes, allowing astronomers to synthesize a larger aperture and achieve finer resolution.

The baseline length is the distance between the individual telescopes in an optical interferometer. It determines the angular resolution and sensitivity of the interferometer.

The Michelson optical interferometer is a classic interferometer design commonly used for precise measurements, including the determination of the speed of light.

Long-baseline optical interferometers are specifically designed for high-precision astrometry, allowing astronomers to measure the positions and motions of stars with great accuracy.

Atmospheric turbulence is a major challenge in long-baseline optical interferometry, as it can distort the light waves and degrade the image quality.