Σύγκριση μεθόδων

	Ανάλυση Καμπύλης Περιστροφής	Αστρομετρία (Παράλλαξη)	Κινηματική Απόσταση
Πεδίο	Αστρονομία	Αστρονομία	Αστρονομία
Οικογένεια	Process / pipeline	Process / pipeline	Process / pipeline
Έτος προέλευσης	1970	1838	1957
Δημιουργός	Vera Rubin	Friedrich Wilhelm Bessel	Bert Westerhout
Τύπος	Observational kinematic method	Astrometric distance measurement	Kinematic measurement method
Θεμελιώδης πηγή	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.	ESA (1997). The Hipparcos and Tycho Catalogues. Astrometric and photometric star catalogue. European Space Agency Technical Reports, SP-1200.	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.
Εναλλακτικές ονομασίες	Galactic Rotation Curves, Rotation Curve Method, Velocity Curve Analysis	Stellar Parallax, Trigonometric Parallax, Parallax Distance Method	Galactic Kinematic Distances, Rotation-Curve Distance, Kinematic Parallax
Συναφείς	3	3	3
Σύνοψη	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.	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.	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.