Uporedite metode

	Analiza krivih rotacije	Kinematička udaljenost	Nizovi pulsarskog merenja vremena
Oblast	Astronomija	Astronomija	Astronomija
Porodica	Process / pipeline	Process / pipeline	Process / pipeline
Godina nastanka	1970	1957	1979
Tvorac	Vera Rubin	Bert Westerhout	Stephen Detweiler
Tip	Observational kinematic method	Kinematic measurement method	Observational timing method
Temeljni izvor	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.	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.	Sazhin, M. V. (1978). Opportunities for detecting ultralong gravitational waves. Soviet Astronomy, 22, 36-38.
Drugi nazivi	Galactic Rotation Curves, Rotation Curve Method, Velocity Curve Analysis	Galactic Kinematic Distances, Rotation-Curve Distance, Kinematic Parallax	PTA, Millisecond Pulsar Timing, Pulsar Timing Residuals
Srodne	3	3	3
Sažetak	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.	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.	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.