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| {{Gravitational Lensing}}
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| A '''gravitational lens''' refers to a distribution of plates (such as a [[galaxy cluster|cluster of galaxies]]) between a distant source (a background [[galaxy]]) and an observer, that is capable of bending (lensing) the light from the source, as it travels towards the observer. This effect is known as gravitational lensing and is one of the predictions of [[Albert Einstein]]'s [[General relativity|general theory of relativity]].
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| Although [[Orest Chwolson]] (1924) or Frantisek Klin (1936) are sometimes credited as being the first ones to discuss the effect in print, the effect is more commonly associated with [[Einstein]], who published a more famous article on the subject in 1936.
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| [[Fritz Zwicky]] posited in 1937 that the effect could allow galaxy clusters to act as gravitational lenses. It was not until 1979 that this effect was confirmed by observation of the so-called "[[Twin QSO]]" SBS 0957+561.
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| ==Description==
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| {{General relativity|cTopic=Phenomena}}
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| [[Image:Gravitational lens-full.jpg|thumb|left|225px|Bending light|Bending light around a massive object from a distant source. The orange arrows show the apparent position of the background source. The white arrows show the path of the light from the true position of the source]]
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| [[Image:Einstein cross.jpg|thumb|left|225px|In the formation known as [[Einstein's Cross]], four images of the same distant quasar appear around a foreground galaxy due to strong gravitational lensing]]
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| [[Spacetime]] around a massive object (such as a [[galaxy cluster]] or a [[black hole]]) is curved, and as a result [[light]] rays from a background source (such as a [[galaxy]]) propagating through spacetime are bent. The lensing effect can magnify and distort the image of the background source.
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| Unlike an [[lens (optics)|optical lens]], maximum 'bending' occurs closest to, and minimum 'bending' furthest from, the center of a gravitational lens. Consequently, a gravitational lens has no single [[focus (optics)|focal point]], but a focal line instead. If the (light) source, the massive lensing object, and the observer lie in a straight line, the original light source will appear as a ring around the massive lensing object. If there is any misalignment the observer will see an arc segment instead. This phenomenon was first mentioned in 1924 by the [[St. Petersburg]] physicist [[Orest Chwolson]],<ref>[http://www.abc.net.au/science/k2/moments/gmis9737.htm Gravity Lens – Part 2 (Great Moments in Science, ABS Science)]</ref> and quantified by [[Albert Einstein]] in 1936. It is usually referred to in the literature as an '''[[Einstein ring]]''', since Chwolson did not concern himself with the flux or radius of the ring image. More commonly, where the lensing mass is complex (such as a [[galaxy group]] or [[galaxy cluster|cluster]]) and does not cause a spherical distortion of space–time, the source will resemble partial arcs scattered around the lens. The observer may then see multiple distorted images of the same source; the number and shape of these depending upon the relative positions of the source, lens, and observer, and the shape of the gravitational well of the lensing object.<ref>[http://astroreview.com/issue/2012/article/black-hole-horizons-and-how-they-begin Dieter Brill, “Black Hole Horizons and How They Begin”, Astronomical Review (2012); Online Article, cited Sept.2012.]</ref>
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| There are three classes of gravitational lensing:<ref>{{cite book | title = The Galactic Supermassive Black Hole | author = Melia, Fulvio | authorlink = Fulvio Melia | publisher = Princeton University Press | year = 2007 | isbn = 0-691-13129-5 | pages = 255–256}}</ref>
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| 1. Strong lensing: where there are easily visible distortions such as the formation of [[Einstein ring]]s, arcs, and multiple images.
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| 2. [[Weak Gravitational Lensing|Weak lensing]]: where the distortions of background sources are much smaller and can only be detected by analyzing large numbers of sources to find coherent distortions of only a few percent. The lensing shows up statistically as a preferred stretching of the background objects perpendicular to the direction to the center of the lens.
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| By measuring the shapes and orientations of large numbers of distant galaxies, their orientations can be averaged to measure the [[Shear matrix|shear]] of the lensing field in any region. This, in turn, can be used to reconstruct the mass distribution in the area: in particular, the background distribution of [[dark matter]] can be reconstructed. Since galaxies are intrinsically elliptical and the weak gravitational lensing signal is small, a very large number of galaxies must be used in these surveys. These weak lensing surveys must carefully avoid a number of important sources of [[systematic error]]: the intrinsic shape of galaxies, the tendency of a camera's [[point spread function]] to distort the shape of a galaxy and the tendency of [[atmospheric seeing]] to distort images must be understood and carefully accounted for. The results of these surveys are important for cosmological parameter estimation, to better understand and improve upon the [[Lambda-CDM model]], and to provide a consistency check on other cosmological observations. They may also provide an important future constraint on [[dark energy]].
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| 3. [[Gravitational microlensing|Microlensing]]: where no distortion in shape can be seen but the amount of light received from a background object changes in time. The lensing object may be stars in the [[Milky Way Galaxy|Milky Way]] in one typical case, with the background source being stars in a remote galaxy, or, in another case, an even more distant [[quasar]]. The effect is small, such that (in the case of strong lensing) even a galaxy with a mass more than 100 billion times [[solar mass|that of the Sun]] will produce multiple images separated by only a few [[arcsecond]]s. [[Galaxy cluster]]s can produce separations of several arcminutes. In both cases the galaxies and sources are quite distant, many hundreds of [[megaparsec]]s away from our Galaxy.
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| Gravitational lenses act equally on all kinds of [[electromagnetic radiation]], not just visible light. Weak lensing effects are being studied for the [[cosmic microwave background]] as well as [[galaxy survey]]s. Strong lenses have been observed in [[radio]] and [[x-ray]] regimes as well. If a strong lens produces multiple images, there will be a relative time delay between two paths: that is, in one image the lensed object will be observed before the other image.
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| [[Image:Black hole lensing web.gif|right|thumb|225px|Simulated gravitational lensing (black hole going past a background galaxy).]]
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| ==History==
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| According to general relativity, [[mass]] "warps" [[space–time]] to create [[gravitational field]]s and therefore bend [[light]] as a result. This theory was confirmed in 1919 during a [[solar eclipse]], when [[Arthur Eddington]] and [[Frank Watson Dyson]] observed the light from [[star]]s passing close to the [[Sun]] was slightly bent, so that stars appeared slightly out of position.
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| Einstein realized that it was also possible for [[astronomical object]]s to bend light, and that under the correct conditions, one would observe multiple images of a single source, called a '''gravitational lens''' or sometimes a '''[[gravitational mirage]]'''.
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| [[File:The most distant gravitational lens yet discovered.jpg|thumb|left|Gravitational lens discovered at [[redshift]] z = 1.53.<ref>{{cite news|title=Most distant gravitational lens helps weigh galaxies|url=http://www.spacetelescope.org/news/heic1319/|accessdate=18 October 2013|newspaper=ESA/Hubble Press Release}}</ref> ]]
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| However, as he only considered gravitational lensing by single stars, he concluded that the phenomenon would most likely remain unobserved for the foreseeable future. In 1937, [[Fritz Zwicky]] first considered the case where a [[galaxy]] could act as a source, something that according to his calculations should be well within the reach of observations.
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| It was not until 1979 that the first gravitational lens would be discovered. It became known as the "[[Twin QSO]]" since it initially looked like two identical quasistellar objects; it is officially named '''[[SBS 0957+561]]'''. This gravitational lens was discovered by [[Dennis Walsh]], [[Bob Carswell]], and [[Ray Weymann]] using the [[Kitt Peak National Observatory]] 2.1 meter [[telescope]].
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| In the 1980s, astronomers realized that the combination of CCD imagers and computers would allow the brightness of millions of stars to be measured each night. In a dense field, such as the galactic center or the Magellanic clouds, many microlensing events per year could potentially be found. This led to efforts such as [[Optical Gravitational Lensing Experiment]], or OGLE, that have characterized hundreds of such events.
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| ==Explanation in terms of space–time curvature==
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| {{See also|Kepler problem in general relativity}}
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| In general relativity, light follows the curvature of spacetime, hence when light passes around a massive object, it is bent. This means that the light from an object on the other side will be bent towards your eye, just like an ordinary lens. Since light always moves at a constant speed, lensing changes the direction of the velocity of the light, but not the magnitude.
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| Light rays are the boundary between the future, the spacelike, and the past regions. The gravitational attraction can be viewed as the motion of undisturbed objects in a background curved ''geometry'' or alternatively as the response of objects to a ''force'' in a flat geometry. The angle of deflection is:
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| :<math>\theta = \frac{4GM}{rc^2}</math>
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| toward the mass ''M'' at a distance ''r'' from the effected radiation, where ''G'' is the [[Gravitational constant|universal constant of gravitation]] and ''c'' is the speed of light in a vacuum.
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| Since the [[Schwarzschild radius]] <math>r_\mathrm{s}</math> is defined as <math>r_\mathrm{s} = {2Gm}/{c^2}</math>, this can also be expressed in simple form as
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| :<math>\theta = 2 \frac{r_\mathrm{s}}{r}</math>
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| <gallery>
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| Image:Gravitationell-lins-4.jpg|Actual gravitational lensing effects as observed by the Hubble Space Telescope in [[Abell 1689]] – Enlarge the image to see the lensing arcs
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| Image:COSMOS 3D dark matter map.jpg|3D map of the large-scale distribution of dark matter, reconstructed from measurements of weak gravitational lensing with the Hubble Space Telescope.
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| </gallery>
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| ==Search for gravitational lenses==
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| [[File:MACS J1206.jpg|thumb|This image from the NASA/ESA Hubble Space Telescope shows the galaxy cluster [[MACS J1206]].]]
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| Most of the gravitational lenses in the past have been discovered accidentally. A search for gravitational lenses in the northern hemisphere (Cosmic Lens All Sky Survey, CLASS), done in radio frequencies using the Very Large Array (VLA) in New Mexico, led to the discovery of 22 new lensing systems, a major milestone. This has opened a whole new avenue for research ranging from finding very distant objects to finding values for cosmological parameters so we can understand the universe better.
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| [[File:Heic1401a-Abell2744-20140107.jpg|thumb|left|400px|[[Abell 2744]] [[galaxy cluster]] - [[Hubble Space Telescope#Frontier Fields program|Hubble Frontier Fields view]] (7 January 2014).<ref name="NASA-20140107">{{cite news |last1=Clavin |first1=Whitney |last2=Jenkins |first2=Ann |last3=Villard |first3=Ray |title=NASA's Hubble and Spitzer Team up to Probe Faraway Galaxies |url=http://www.jpl.nasa.gov/news/news.php?release=2014-007 |date=7 January 2014 |work=[[NASA]] |accessdate=8 January 2014 }}</ref>]]
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| A similar search in the southern hemisphere would be a very good step towards complementing the northern hemisphere search as well as obtaining other objectives for study. If such a search is done using well calibrated and well parameterized instrument and data, a result similar to the northern survey can be expected. The use of the Australia Telescope 20 GHz (AT20G) Survey data collected using the Australia Telescope Compact Array (ATCA) stands to be such a collection of data. As the data were collected using the same instrument maintaining a very stringent quality of data we should expect to obtain good results from the search. The AT20G survey is a blind survey at 20 GHz frequency in the radio domain of the electromagnetic spectrum. Due to the high frequency used, the chances finding gravitational lenses increases as the relative number of compact core objects (e.g. Quasars) are higher (Sadler et al. 2006). This is important as the lensing is easier to detect and identify in simple objects compared to objects with complexity in them. This search involves the use of interferometric methods to identify candidates and follow them up at higher resolution to identify them. Full detail of the project is currently under works for publication.
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| In a recent article on Science Daily (Jan. 21 2009) a team of scientists led by a cosmologist from the U.S. Department of Energy's Lawrence Berkeley National Laboratory has made major progress in extending the use of gravitational lensing to the study of much older and smaller structures than was previously possible by stating that weak gravitational lensing improves measurements of distant galaxies.<ref>[http://www.sciencedaily.com/releases/2010/01/100119172846.htm Cosmology: Weak gravitational lensing improves measurements of distant galaxies<!-- Bot generated title -->]</ref>
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| Astronomers from the [[Max Planck Institute]] for Astronomy in [[Heidelberg]], [[Germany]], the results of which are accepted for publication on Oct 21, 2013 in the [[Astrophysical Journal Letters]] (arXiv.org), have discovered the most distant gravitational lens termed as '''[[J1000+0221]]''' using [[NASA]]’s [[Hubble Space Telescope]].<ref>{{cite web|last=Sci-News.com|title=Most Distant Gravitational Lens Discovered|url=http://www.sci-news.com/astronomy/science-gravitational-lens-01478.html|publisher=Sci-News.com|accessdate=22 October 2013|date=21 Oct 2013}}</ref><ref>{{cite journal|last=van der Wel|first=A.|coauthors=et al|title=Discovery of a Quadruple Lens in CANDELS with a Record Lens Redshift|journal=ApJ Letters|year=2013|pmid=arXiv:1309.2826|accessdate=22 October 2013}}</ref>
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| A research published Sep 30, 2013 in the online edition of [[Physical Review Letters]], led by [[McGill University]] in [[Montreal]], [[Canada]], has discovered the [[B-modes]], that are formed due to gravitational lensing effect, using [[National Science Foundation]]'s [[South Pole Telescope]] and with help from the Herschel space observatory. This discovery would open the possibilities of testing the theories of how our universe originated.<ref>{{cite web|last=NASA/Jet Propulsion Laboratory|date=October 22, 2013|title=Long-sought pattern of ancient light detected|journal=ScienceDaily|accessdate=October 23, 2013|url=http://www.sciencedaily.com/releases/2013/10/131022101009.htm}}</ref><ref>{{cite journal|first=D.|last=Hanson|coauthors=S. Hoover, A. Crites, P. A. R. Ade, K. A. Aird, J. E. Austermann, J. A. Beall, A. N. Bender, B. A. Benson, L. E. Bleem, J. J. Bock, J. E. Carlstrom, C. L. Chang, H. C. Chiang, H-M. Cho, A. Conley, T. M. Crawford, T. de Haan, M. A. Dobbs, W. Everett, J. Gallicchio, J. Gao, E. M. George, N. W. Halverson, N. Harrington, J. W. Henning, G. C. Hilton, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, N. Huang, J. Hubmayr, K. D. Irwin, R. Keisler, L. Knox, A. T. Lee, E. Leitch, D. Li, C. Liang, D. Luong-Van, G. Marsden, J. J. McMahon, J. Mehl, S. S. Meyer, L. Mocanu, T. E. Montroy, T. Natoli, J. P. Nibarger, V. Novosad, S. Padin, C. Pryke, C. L. Reichardt, J. E. Ruhl, B. R. Saliwanchik, J. T. Sayre, K. K. Schaffer, B. Schulz, G. Smecher, A. A. Stark, K. T. Story, C. Tucker, K. Vanderlinde, J. D. Vieira, M. P. Viero, G. Wang, V. Yefremenko, O. Zahn, M. Zemcov|title=Detection of B-Mode Polarization in the Cosmic Microwave Background with Data from the South Pole Telescope|journal=Physical Review Letters|date=Sep 30, 2013|volume=111|series=14|doi=10.1103/PhysRevLett.111.141301}}</ref>
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| ==Measuring the weak lensing==
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| [[File:Gravitationally-lensed distant star-forming galaxy.jpg|thumb|Gravitationally-lensed distant star-forming galaxy.<ref>{{cite news|title=ALMA Rewrites History of Universe's Stellar Baby Boom|url=http://www.eso.org/public/news/eso1313/|accessdate=2 April 2013|newspaper=ESO}}</ref>]]
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| Kaiser et al. (1995), Luppino & Kaiser (1997) and Hoekstra et al. (1998) prescribed a method to invert the effects of the Point Spread Function (PSF) smearing and shearing, recovering a shear estimator uncontaminated by the systematic distortion of the PSF. This method (KSB+) is the most widely used method in current weak lensing shear measurements.
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| Galaxies have random rotations and inclinations. As a result, the shear effects in weak lensing need to be determined by statistically preferred orientations. The primary source of error in lensing measurement is due to the convolution of the PSF with the lensed image. The KSB method measures the ellipticity of a galaxy image. The shear is proportional to the ellipticity. The objects in lensed images are parameterized according to their weighted quadrupole moments. For a perfect ellipse, the weighted quadrupole moments are related to the weighted ellipticity. KSB calculate how a weighted ellipticity measure is related to the shear and use the same formalism to remove the effects of the PSF.
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| KSB’s primary advantages are its mathematical ease and relatively simple implementation. However, KSB is based on a key assumption that the PSF is circular with an anisotropic distortion. It’s fine for current cosmic shear surveys, but the next generation of surveys (e.g. LSST) may need much better accuracy than KSB can provide. Because during that time, the statistical errors from the data are negligible, the systematic errors will dominate.
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| ==Historical papers and references==
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| * {{cite journal | first = O | last = Chwolson | title = Über eine mögliche Form fiktiver Doppelsterne | journal = Astronomische Nachrichten | volume = 221 | issue = 20 | pages = 329 | year = 1924 | bibcode = 1924AN....221..329C | doi = 10.1002/asna.19242212003}}
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| * {{cite journal | first = Albert | last = Einstein | authorlink = Albert Einstein | title = Lens-like Action of a Star by the Deviation of Light in the Gravitational Field | journal = Science | volume = 84 | pages = 506–7 | year = 1936 | doi = 10.1126/science.84.2188.506 | pmid = 17769014 | issue = 2188 | jstor=1663250|bibcode = 1936Sci....84..506E }}
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| * {{cite journal | first = Jürgen | last = Renn | coauthors = Tilman Sauer and John Stachel | title =The Origin of Gravitational Lensing: A Postscript to Einstein's 1936 Science paper | journal = Science | volume = 275 | pages = 184–6 | year = 1997 | doi = 10.1126/science.275.5297.184 | pmid =8985006 | issue = 5297|bibcode = 1997Sci...275..184R }}
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| ==References==
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| ;Notes
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| {{Reflist}}
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| ;Bibliography
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| * "''[http://www.sciencenews.org/view/generic/id/33082/title/Math_Trek__Accidental_astrophysicists Accidental Astrophysicists]''". Science News, June 13, 2008.
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| * "''[http://www.cinespa.ucr.ac.cr/software/xfgl/index.html XFGLenses]''". A Computer Program to visualize Gravitational Lenses, Francisco Frutos-Alfaro
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| * "''[http://web.archive.org/web/20070929124804/http://www.btinternet.com/~Boughen/G-LenS G-LenS]''". A Point Mass Gravitational Lens Simulation, Mark Boughen.
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| * Newbury, Pete, "''[http://www.iam.ubc.ca/old_pages/newbury/lenses/lenses.html Gravitational Lensing]''". Institute of Applied Mathematics, The University of British Columbia.
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| * Cohen, N., "Gravity's Lens: Views of the New Cosmology", Wiley and Sons, 1988.
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| * "''[http://cfa-www.harvard.edu/~rschild/qgl.html Q0957+561 Gravitational Lens]''". Harvard.edu.
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| * "''[http://imagine.gsfc.nasa.gov/docs/features/news/grav_lens.html Gravitational lensing]''". Gsfc.nasa.gov.
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| * Bridges, Andrew, "''[http://www.signonsandiego.com/news/science/20040215-1033-ca-farthestgalaxy.html Most distant known object in universe discovered]''". [[Associated Press]]. February 15, 2004. (Farthest galaxy found by gravitational lensing, using Abell 2218 and Hubble Space Telescope.)
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| * [http://sciencecareers.sciencemag.org/career_development/previous_issues/articles/2006_05_12/analysing_corporations_and_the_cosmos/(parent)/12100 Analyzing Corporations ... and the Cosmos] An unusual career path in gravitational lensing.
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| * "''[http://cfa-www.harvard.edu/castles HST images of strong gravitational lenses]''". Harvard-Smithsonian Center for Astrophysics.
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| * "''[http://uk.arxiv.org/abs/astro-ph/0404309 A planetary microlensing event]''" and "''[http://arxiv.org/abs/astro-ph/0505451 A Jovian-mass Planet in Microlensing Event OGLE-2005-BLG-071]''", the first [[Extrasolar planet|extra-solar planet]] detections using microlensing.
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| * [http://xstructure.inr.ac.ru/x-bin/theme3.py?level=2&index1=-188353 Gravitational lensing on arxiv.org]
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| * [http://www.aoc.nrao.edu/~smyers/class.html NRAO CLASS home page]
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| * [http://www.atnf.csiro.au/research/AT20G AT20G survey]
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| * [http://cdsads.u-strasbg.fr/full/1981Ap%26SS..78..199B ''A diffraction limit on the gravitational lens effect'' (Bontz, R. J. and Haugan, M. P. "Astrophysics and Space Science" vol. 78, no. 1, p. 199-210. August 1981)]
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| ;Further reading
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| * {{cite journal
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| | author = Blandford & Narayan
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| | year = 1992
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| | title = Cosmological applications of gravitational lensing
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| | journal = ARA&A
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| | pages = 311–358
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| | issue = 1
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| | volume = 30
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| | bibcode = 1992ARA&A..30..311B
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| | doi = 10.1146/annurev.aa.30.090192.001523
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| | last2 = Narayan
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| | first2 = R
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| }}
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| * {{cite journal|title=Weak Gravitational Lensing|author=Matthias Bartelmann and Peter Schneider|date=2000-08-17|format=PDF|url=http://www.mpa-garching.mpg.de/Lenses/WLRevEls.pdf}}
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| * {{Cite journal | first1=Dmitry | last1=Khavinson | first2=Genevra | last2=Neumann | url=http://www.ams.org/notices/200806/tx080600666p.pdf | title=From Fundamental Theorem of Algebra to Astrophysics: A "Harmonious" Path | journal=Notices | publisher=AMS |date=June–July 2008 | volume=55 | issue=6 | pages=666–675 | postscript=<!--None-->}}.
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| * {{cite book | first1=Arlie O. | last1=Petters | authorlink = Arlie Petters | first2=Harold | last2=Levine | first3=Joachim | last3=Wambsganss | url=http://www.springer.com/birkhauser/physics/book/978-0-8176-3668-5 | title=Singularity Theory and Gravitational Lensing | series=Progress in Mathematical Physics | volume=21 | publisher=Birkhäuser | year=2001 }}
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| * [http://www.matnat.uio.no/proveforelesninger/g-i/haugan-stein-vidar-hagfors.xml ''Tools for the evaluation of the possibilities of using parallax measurements of gravitationally lensed sources'' (Stein Vidar Hagfors Haugan. June 2008)]
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| ==External links==
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| {{Commons category|Gravitational lensing}}
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| * [http://www.pdxjustice.org/node/54 Video: Evalyn Gates – Einstein's Telescope: The Search for Dark Matter and Dark Energy in the Universe], presentation in Portland, Oregon, on April 19, 2009, from the author's recent book tour.
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| * [http://www.astronomycast.com/stars/episode-37-gravitational-lensing/ Audio: Fraser Cain and Dr. Pamela Gay – Astronomy Cast: Gravitational Lensing, May 2007]
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| ==Featured in science-fiction works==
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| * [http://www.davidbrin.com/existence.html Existence, by David Brin, 2012]
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| {{Relativity}}
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| {{DEFAULTSORT:Gravitational Lens}}
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| [[Category:Astrophysics]]
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| [[Category:Effects of gravitation]]
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