Gravitational Lensing: Strong, Weak and Micro: Saas-Fee Advanced Course 33
Springer Science & Business Media, Dec 30, 2006 - Science - 552 pages
The observation, in 1919 by A.S. Eddington and collaborators, of the gra- tational de?ection of light by the Sun proved one of the many predictions of Einstein’s Theory of General Relativity: The Sun was the ?rst example of a gravitational lens. In 1936, Albert Einstein published an article in which he suggested - ing stars as gravitational lenses. A year later, Fritz Zwicky pointed out that galaxies would act as lenses much more likely than stars, and also gave a list of possible applications, as a means to determine the dark matter content of galaxies and clusters of galaxies. It was only in 1979 that the ?rst example of an extragalactic gravitational lens was provided by the observation of the distant quasar QSO 0957+0561, by D. Walsh, R.F. Carswell, and R.J. Weymann. A few years later, the ?rst lens showing images in the form of arcs was detected. The theory, observations, and applications of gravitational lensing cons- tute one of the most rapidly growing branches of astrophysics. The gravi- tional de?ection of light generated by mass concentrations along a light path producesmagni?cation,multiplicity,anddistortionofimages,anddelaysp- ton propagation from one line of sight relative to another. The huge amount of scienti?c work produced over the last decade on gravitational lensing has clearly revealed its already substantial and wide impact, and its potential for future astrophysical applications.
What people are saying - Write a review
We haven't found any reviews in the usual places.
Introduction to Gravitational Lensing and Cosmology
Gravitational Lens Theory
Simple Lens Models
The Homogeneous Universe
Basics of Lensing Statistics
The Cosmological Standard Model
Strong Gravitational Lensing
Weak Gravitational Lensing
Observational Issues and Challenges
Introduction and Strong Lensing
Mass Reconstructions from Weak Lensing
Cosmic Shear Lensing by the LSS
The Mass of and Associated with Galaxies
Additional Issues in Cosmic Shear
The Mass Distributions of Galaxies
Gravitational Lens Statistics
What Happened to the Cluster Lenses?
The Role of Substructure
The Optical Properties of Lens Galaxies
Extended Sources and Quasar Host Galaxies
Does Strong Lensing Have a Future?
Other editions - View all
angular scales anisotropy aperture mass astrometric B-mode Bartelmann baryons caustic cluster comoving comoving distance components constraints correlation function corresponding cosmic shear critical curve cusp dark matter halo deflection degeneracy delay depends detected determined distance effect Einstein radius Einstein ring ellipticity estimate field finite flux ratios four-image fraction Galactic Galactic bulge gravitational lensing Hubble constant image separation isothermal Keeton Kochanek lens equation lens galaxy lens model lensing signal lightcurve linear luminosity luminosity function magnification bias mass distribution mass profile matter distribution measured Mellier method microlensing events MNRAS multiple images number density observed obtained optical panel parameters perturbations planet position potential power spectrum quadrupole quasar radial radio relative Rusin Schneider Sect shows simulations source plane stars statistics stellar strong lensing surface density surface mass density survey tangential velocity dispersion Waerbeke Wambsganss weak lensing