เปรียบเทียบวิธี

	ไมโครเลนส์ความโน้มถ่วง	ระยะทางจลนศาสตร์	การปรับแบบจำลองการกระจายพลังงานเชิงสเปกตรัม (SED Fitting)
สาขาวิชา	ดาราศาสตร์	ดาราศาสตร์	ดาราศาสตร์
ตระกูล	Process / pipeline	Process / pipeline	Process / pipeline
ปีกำเนิด	1986	1957	2003
ผู้ริเริ่ม	Bohdan Paczynski	Bert Westerhout	Gustavo Bruzual
ประเภท	Observational detection method	Kinematic measurement method	Analysis and modeling method
แหล่งต้นตำรับ	Paczynski, B. (1986). Gravitational microlensing by the galactic halo. Astrophysical Journal, 304, 1-5.	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.
ชื่อเรียกอื่น	Microlensing, Gravitational Lensing Method	Galactic Kinematic Distances, Rotation-Curve Distance, Kinematic Parallax	SED Analysis, Spectral Energy Distribution Method, Photometric Redshift
ที่เกี่ยวข้อง	3	3	3
สรุป	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.	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.