Linganisha mbinu

	Umbali wa Kine matiki	Kipima Muda cha Pulsar
Nyanja	Astronomia	Astronomia
Familia	Process / pipeline	Process / pipeline
Mwaka wa asili	1957	1979
Mwanzilishi	Bert Westerhout	Stephen Detweiler
Aina	Kinematic measurement method	Observational timing method
Chanzo asilia	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.
Majina mbadala	Galactic Kinematic Distances, Rotation-Curve Distance, Kinematic Parallax	PTA, Millisecond Pulsar Timing, Pulsar Timing Residuals
Zinazohusiana	3	3
Muhtasari	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.