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| 強重力レンズ効果× | 天体測量（年周視差）× | |
|---|---|---|
| 分野 | 天文学 | 天文学 |
| 系統 | Process / pipeline | Process / pipeline |
| 提唱年≠ | 1964 | 1838 |
| 提唱者≠ | Sjur Refsdal | Friedrich Wilhelm Bessel |
| 種類≠ | Observational measurement method | Astrometric distance measurement |
| 原典≠ | Refsdal, S. (1964). On the possibility of determining Hubble's parameter and the masses of galaxies from the gravitational lens effect. Monthly Notices of the Royal Astronomical Society, 128(4), 307-311. DOI ↗ | ESA (1997). The Hipparcos and Tycho Catalogues. Astrometric and photometric star catalogue. European Space Agency Technical Reports, SP-1200. link ↗ |
| 別名 | Strong Lensing, Gravitational Lens, Einstein Ring | Stellar Parallax, Trigonometric Parallax, Parallax Distance Method |
| 関連 | 3 | 3 |
| 概要≠ | Strong gravitational lensing occurs when massive objects (clusters, galaxies) bend light so strongly that multiple images of distant sources appear, or complete rings (Einstein rings) form. Proposed by Sjur Refsdal in 1964 and first observed in 0957+561 in 1979, strong lensing provides direct measurements of lens masses and cosmic distances independent of the distance ladder. | 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. |
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