Сравнение методов
Просматривайте выбранные методы рядом; строки с различиями подсвечены.
| Сильное гравитационное линзирование× | Слабое гравитационное линзирование× | |
|---|---|---|
| Область | Астрономия | Астрономия |
| Семейство | Process / pipeline | Process / pipeline |
| Год появления≠ | 1964 | 1992 |
| Автор метода≠ | Sjur Refsdal | Nick Kaiser |
| Тип | Observational measurement method | Observational measurement method |
| Основополагающий источник≠ | 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 ↗ | Kaiser, N. (1992). Weak gravitational lensing of distant galaxies. Astrophysical Journal, 388, 272-286. DOI ↗ |
| Другие названия | Strong Lensing, Gravitational Lens, Einstein Ring | Weak Lensing, Cosmic Shear, Lensing Distortion |
| Связанные | 3 | 3 |
| Сводка≠ | 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. | Weak gravitational lensing occurs when light from distant sources bends slightly as it travels through the universe, passing through the gravitational fields of matter concentrations. Proposed theoretically by Nick Kaiser in 1992, this subtle effect has become one of the most powerful cosmological probes, directly revealing the distribution of all matter (dark and luminous) across cosmic distances. |
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