Krahasoni metodat

	Paralaksa (Astrometri)	Mikrolensimi Gravitacional	SED Fitting
Fusha	Astronomi	Astronomi	Astronomi
Familja	Process / pipeline	Process / pipeline	Process / pipeline
Viti i origjinës	1838	1986	2003
Krijuesi	Friedrich Wilhelm Bessel	Bohdan Paczynski	Gustavo Bruzual
Lloji	Astrometric distance measurement	Observational detection method	Analysis and modeling method
Burimi themelues	ESA (1997). The Hipparcos and Tycho Catalogues. Astrometric and photometric star catalogue. European Space Agency Technical Reports, SP-1200.	Paczynski, B. (1986). Gravitational microlensing by the galactic halo. Astrophysical Journal, 304, 1-5.	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.
Emërtime të tjera	Stellar Parallax, Trigonometric Parallax, Parallax Distance Method	Microlensing, Gravitational Lensing Method	SED Analysis, Spectral Energy Distribution Method, Photometric Redshift
Të lidhura	3	3	3
Përmbledhja	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.	Gravitational microlensing is an observational technique that exploits Einstein's prediction that massive objects bend light. When a star or planet passes in front of a distant star from our perspective, its gravity acts as a lens, magnifying and distorting the background star's light. First proposed by Bohdan Paczynski in 1986, this method has discovered hundreds of exoplanets and provides unique sensitivity to low-mass planets and dark matter.	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.