Editing Dark matter (section)

=== Gravitational lensing ===
One of the consequences of [[general relativity]] is the [[gravitational lens]]. Gravitational lensing occurs when massive objects between a source of light and the observer act as a lens to bend light from this source. Lensing does not depend on the properties of the mass; it only requires there to be a mass. The more massive an object, the more lensing is observed. An example is a [[galaxy cluster|cluster of galaxies]] lying between a more distant source such as a [[quasar]] and an observer. In this case, the galaxy cluster will lens the quasar.

Strong lensing is the observed distortion of background galaxies into arcs when their light passes through such a gravitational lens. It has been observed around many distant clusters including [[Abell 1689]].<ref>{{cite journal |last1=Taylor |first1=A. N. |display-authors=etal |date=1998 |title=Gravitational lens magnification and the mass of Abell&nbsp;1689 |journal=The Astrophysical Journal |volume=501 |issue=2 |pages=539–553 |arxiv=astro-ph/9801158 |bibcode=1998ApJ...501..539T |doi=10.1086/305827 |s2cid=14446661}}</ref> By measuring the distortion geometry, the mass of the intervening cluster can be obtained. In the [[weak gravitational lensing|weak]] regime, lensing does not distort background galaxies into arcs, causing minute distortions instead. By examining the apparent shear deformation of the adjacent background galaxies, the mean distribution of dark matter can be characterized. The measured mass-to-light ratios correspond to dark matter densities predicted by other large-scale structure measurements.<ref>{{cite journal |last1=Refregier |first1=A. |year=2003 |title=Weak gravitational lensing by large-scale structure |journal=[[Annual Review of Astronomy and Astrophysics]] |volume=41 |issue=1 |pages=645–668 |arxiv=astro-ph/0307212 |bibcode=2003ARA&A..41..645R |doi=10.1146/annurev.astro.41.111302.102207|s2cid=34450722 }}</ref><ref>{{cite journal |last1=Wu |first1=X. |last2=Chiueh |first2=T. |last3=Fang |first3=L. |last4=Xue |first4=Y. |date=1998 |title=A comparison of different cluster mass estimates: consistency or discrepancy? |journal=[[Monthly Notices of the Royal Astronomical Society]] |volume=301 |issue=3 |pages=861–871 |arxiv=astro-ph/9808179 |bibcode=1998MNRAS.301..861W |doi=10.1046/j.1365-8711.1998.02055.x |doi-access=free |citeseerx=10.1.1.256.8523|s2cid=1291475 }}</ref>