Open AccessStrong gravitational lensing by multiple galaxies
Author(s) -
Möller Ole,
Blain A.W.
Publication year - 2001
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2001.04727.x
Subject(s) - physics , gravitational lens , strong gravitational lensing , lens (geology) , gravitational lensing formalism , magnification , astrophysics , galaxy , weak gravitational lensing , line of sight , simple lens , redshift , cosmology , astronomy , optics , cylindrical lens
We discuss strong gravitational lensing by multiple objects along any line of sight. The probability for strong gravitational lensing by more than one lens is small, but a number of strong lens systems in which more than one separate lens contribute significantly to the lensing potential will be detected in the large sample of lens systems compiled with new instruments. Using multi‐lens ray‐tracing, we estimate the likelihood for gravitational lensing by two lenses at different redshifts and investigate typical image geometries and magnification cross‐sections. We find that, for a cosmology with and , about one in 20 lens systems consist of two lenses with merging caustics. Multiple lens systems differ from single lenses as the presence of a second lens in close proximity along the line of sight leads to a strongly asymmetric potential, which increases the multiple imaging cross‐section and significantly changes the image configuration. The external shear induced by a second nearby galaxy, group or cluster can significantly affect image positions even for more widely separated lens pairs. Both of these effects must be accounted for in lens modelling. We also show how the presence of aligned discs in the pair of lensing galaxies can lead to very large high‐magnification cross‐sections. Lensing by more than one galaxy along the line of sight can lead to interesting image configurations. Such systems will be important in future, both for constraining lens models of individual systems and for statistical lensing.