Σύγκριση μεθόδων

	Φωτομετρία Διέλευσης	Αστρομετρία (Παράλλαξη)	Προσαρμογή Φασματικής Ενεργειακής Κατανομής (SED Fitting)
Πεδίο	Αστρονομία	Αστρονομία	Αστρονομία
Οικογένεια	Process / pipeline	Process / pipeline	Process / pipeline
Έτος προέλευσης	1984	1838	2003
Δημιουργός	William Borucki	Friedrich Wilhelm Bessel	Gustavo Bruzual
Τύπος	Observational photometric pipeline	Astrometric distance measurement	Analysis and modeling method
Θεμελιώδης πηγή	Borucki, W. J., & Summers, A. L. (1984). The photometric method of detecting other planetary systems. Astrophysical Journal, 281, 537-553.	ESA (1997). The Hipparcos and Tycho Catalogues. Astrometric and photometric star catalogue. European Space Agency Technical Reports, SP-1200.	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.
Εναλλακτικές ονομασίες	Photometric Transit Method, Planetary Transit Detection	Stellar Parallax, Trigonometric Parallax, Parallax Distance Method	SED Analysis, Spectral Energy Distribution Method, Photometric Redshift
Συναφείς	3	3	3
Σύνοψη	Transit photometry is an observational technique that detects exoplanets by monitoring the periodic dips in stellar brightness as planets cross in front of their host stars. First systematized by William Borucki in 1984, this method became the most successful exoplanet detection technique, with the Kepler space telescope discovering thousands of confirmed exoplanets using this approach.	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.	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.