مقایسهٔ روش‌ها

	اخترسنجی (اختلاف منظر)	طیف‌سنجی عبوری سیارات فراخورشیدی	برازش توزیع انرژی طیفی (SED Fitting)
حوزه	نجوم	نجوم	نجوم
خانواده	Process / pipeline	Process / pipeline	Process / pipeline
سال پیدایش	1838	2002	2003
پدیدآور	Friedrich Wilhelm Bessel	David Charbonneau	Gustavo Bruzual
نوع	Astrometric distance measurement	Spectroscopic observational method	Analysis and modeling method
منبع بنیادین	ESA (1997). The Hipparcos and Tycho Catalogues. Astrometric and photometric star catalogue. European Space Agency Technical Reports, SP-1200.	Charbonneau, D., Brown, T. M., Noyes, R. W., & Gilliland, R. L. (2002). Detection of an atmospheric trace constituent in the transmission spectrum of a distant extrasolar planet. Astrophysical Journal, 568(1), 377-384.	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.
نام‌های دیگر	Stellar Parallax, Trigonometric Parallax, Parallax Distance Method	Transmission Spectrum, Atmospheric Spectroscopy, Transit Spectroscopy	SED Analysis, Spectral Energy Distribution Method, Photometric Redshift
مرتبط	3	3	3
خلاصه	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.	Transmission spectroscopy is a technique for studying the atmospheres of exoplanets by analyzing the light passing through the planetary atmosphere during transit. Pioneered by David Charbonneau in 2002 with the detection of sodium in HD 209458b's atmosphere, this method has become the primary tool for characterizing exoplanet atmospheres and searching for biosignatures.	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.