Compara mètodes

	Distància cinemàtica	Paral·laxi astromètrica	Xarxa d'observació de púlsars	Anàlisi de corbes de rotació
Camp	Astronomia	Astronomia	Astronomia	Astronomia
Família	Process / pipeline	Process / pipeline	Process / pipeline	Process / pipeline
Any d'origen	1957	1838	1979	1970
Autor original	Bert Westerhout	Friedrich Wilhelm Bessel	Stephen Detweiler	Vera Rubin
Tipus	Kinematic measurement method	Astrometric distance measurement	Observational timing method	Observational kinematic method
Font seminal	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.	ESA (1997). The Hipparcos and Tycho Catalogues. Astrometric and photometric star catalogue. European Space Agency Technical Reports, SP-1200.	Sazhin, M. V. (1978). Opportunities for detecting ultralong gravitational waves. Soviet Astronomy, 22, 36-38.	Vera C. Rubin & W. Kent Ford Jr. (1970). Rotation of the Andromeda Nebula from a Spectroscopic Survey of Emission Regions. Astrophysical Journal, 159, 379-403.
Àlies	Galactic Kinematic Distances, Rotation-Curve Distance, Kinematic Parallax	Stellar Parallax, Trigonometric Parallax, Parallax Distance Method	PTA, Millisecond Pulsar Timing, Pulsar Timing Residuals	Galactic Rotation Curves, Rotation Curve Method, Velocity Curve Analysis
Relacionats	3	3	3	3
Resum	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.	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.	A pulsar timing array uses multiple millisecond pulsars as a distributed network of gravitational wave detectors across the galaxy. Proposed theoretically by Stephen Detweiler in 1979, this method exploits the extraordinary timing precision of pulsars to detect the subtle spacetime distortions caused by gravitational waves. In 2023, the first evidence for a stochastic background of gravitational waves was announced using pulsar timing arrays.	Galaxy rotation curve analysis is the technique of measuring how orbital velocities change with distance from the center of a galaxy. Pioneered by Vera Rubin and W. Kent Ford Jr. in 1970, rotation curves revealed one of astronomy's great mysteries: galaxies rotate too fast to be held together by their visible stars alone, providing direct evidence for dark matter.