مقایسهٔ روش‌ها

	فاصله سینماتیکی	آرایه زمان‌سنجی تپ‌اختر	تحلیل منحنی چرخش
حوزه	نجوم	نجوم	نجوم
خانواده	Process / pipeline	Process / pipeline	Process / pipeline
سال پیدایش	1957	1979	1970
پدیدآور	Bert Westerhout	Stephen Detweiler	Vera Rubin
نوع	Kinematic measurement method	Observational timing method	Observational kinematic method
منبع بنیادین	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.	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.
نام‌های دیگر	Galactic Kinematic Distances, Rotation-Curve Distance, Kinematic Parallax	PTA, Millisecond Pulsar Timing, Pulsar Timing Residuals	Galactic Rotation Curves, Rotation Curve Method, Velocity Curve Analysis
مرتبط	3	3	3
خلاصه	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.	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.