Comparer des méthodes

	Parallaxe astrométrique	Distance cinématique	Ajustement de la DSE
Domaine	Astronomie	Astronomie	Astronomie
Famille	Process / pipeline	Process / pipeline	Process / pipeline
Année d'origine	1838	1957	2003
Auteur d'origine	Friedrich Wilhelm Bessel	Bert Westerhout	Gustavo Bruzual
Type	Astrometric distance measurement	Kinematic measurement method	Analysis and modeling method
Source fondatrice	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.	Bruzual, G., & Charlot, S. (2003). Stellar population synthesis at arbitrary metallicity with the Bruzual & Charlot models. Monthly Notices of the Royal Astronomical Society, 344(3), 1000-1028.
Alias	Stellar Parallax, Trigonometric Parallax, Parallax Distance Method	Galactic Kinematic Distances, Rotation-Curve Distance, Kinematic Parallax	SED Analysis, Spectral Energy Distribution Method, Photometric Redshift
Apparentées	3	3	3
Résumé	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.	Spectral Energy Distribution (SED) fitting is the technique of comparing observed photometric measurements of galaxies across many wavelengths against theoretical predictions from stellar population synthesis models. By fitting models to observations, astronomers estimate galaxy properties including redshift, mass, age, star formation rate, and dust content without requiring expensive spectroscopic observations.