Comparar métodos
Revisa los métodos seleccionados uno junto a otro; las filas que difieren aparecen resaltadas.
| Microlente gravitacional× | Lentes gravitacionales débiles× | |
|---|---|---|
| Campo | Astronomía | Astronomía |
| Familia | Process / pipeline | Process / pipeline |
| Año de origen≠ | 1986 | 1992 |
| Autor original≠ | Bohdan Paczynski | Nick Kaiser |
| Tipo≠ | Observational detection method | Observational measurement method |
| Fuente seminal≠ | Paczynski, B. (1986). Gravitational microlensing by the galactic halo. Astrophysical Journal, 304, 1-5. DOI ↗ | Kaiser, N. (1992). Weak gravitational lensing of distant galaxies. Astrophysical Journal, 388, 272-286. DOI ↗ |
| Alias≠ | Microlensing, Gravitational Lensing Method | Weak Lensing, Cosmic Shear, Lensing Distortion |
| Relacionados | 3 | 3 |
| Resumen≠ | 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. | 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. |
| ScholarGateConjunto de datos ↗ |
|
|