Sammenlign metoder

	Astrometri (Parallakse)	Gravitationsmikrolinser	Kinematisk afstand
Fagområde	Astronomi	Astronomi	Astronomi
Familie	Process / pipeline	Process / pipeline	Process / pipeline
Oprindelsesår	1838	1986	1957
Ophavsperson	Friedrich Wilhelm Bessel	Bohdan Paczynski	Bert Westerhout
Type	Astrometric distance measurement	Observational detection method	Kinematic measurement method
Oprindelig kilde	ESA (1997). The Hipparcos and Tycho Catalogues. Astrometric and photometric star catalogue. European Space Agency Technical Reports, SP-1200.	Paczynski, B. (1986). Gravitational microlensing by the galactic halo. Astrophysical Journal, 304, 1-5.	Reid, M. J., et al. (2014). Trigonometric parallaxes of high mass star forming regions: the structure and kinematics of the Milky Way. Astrophysical Journal, 783(2), 130.
Aliasser	Stellar Parallax, Trigonometric Parallax, Parallax Distance Method	Microlensing, Gravitational Lensing Method	Galactic Kinematic Distances, Rotation-Curve Distance, Kinematic Parallax
Relaterede	3	3	3
Resumé	Astrometric parallax is the foundational geometric method for measuring distances to nearby stars, based on observing the apparent shift in a star's position as Earth orbits the Sun. First successfully demonstrated by Friedrich Wilhelm Bessel in 1838 for the star 61 Cygni, parallax remains the most direct and reliable distance measurement in astronomy, anchoring the entire cosmic distance ladder.	Gravitational microlensing is an observational technique that exploits Einstein's prediction that massive objects bend light. When a star or planet passes in front of a distant star from our perspective, its gravity acts as a lens, magnifying and distorting the background star's light. First proposed by Bohdan Paczynski in 1986, this method has discovered hundreds of exoplanets and provides unique sensitivity to low-mass planets and dark matter.	Kinematic distance is a method for estimating distances to objects in the Milky Way using their observed radial velocities and the known rotation curve of the Galaxy. Developed in the 1950s by Bert Westerhout and others, this technique enables distance determination to distant molecular clouds and masers without trigonometric parallax or individual object luminosities.