gravitational lens

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Gravitational lensing

gravitational lens

A concept arising from the fact that a gravitational field bends light, and hence a concentration of mass can focus light rays in a manner similar to that of a lens. In the illustration, the observer at O sees two apparent images S′ of the background source S caused by lensing effects of the intervening galaxy. The theory of gravitational lensing was discussed by both Einstein and Lodge in 1919, and its applications to cosmology realized by Zwicky in 1937, but the first known gravitational lens (the double quasar) was not discovered until 1979. Lensing by a smooth mass distribution such as a galaxy or a cluster of galaxies is known as macrolensing, and can occur in several forms.

The simplest form of gravitational lensing is where a pointlike background source, usually a quasar, is split into multiple images, the location and number of which are dependent on the relative geometry of the source and lens. The lens will distort and concentrate the original path of the light, so that an image will also appear brighter, or magnified. Different images forming a multiple system may have their luminosities magnified by different factors. Cases of double, triple and even quadruple lensing have been found (e.g. the Cloverleaf and the Einstein cross). In most cases the lensing galaxy is not observed. Theoretical models of gravitational lensing predict that there should always be an odd number of images so both the double and quadruple systems are expected to have a central image that is too faint to be detected.

If the background object is a distant galaxy that is itself extended, the lensed images are smeared out into long luminous arcs several arc seconds long. Such arcs are commonly observed in the core of rich clusters of galaxies, usually elongated tangentially to the cluster center and bluer in color than the cluster member galaxies. In several clusters many tens of smaller arclets are seen, which originate from weak lensing of background galaxies that are not so strongly magnified. The most extreme case of gravitational lensing is observed when an extended background source is exactly aligned with a symmetrical lens. The lensed image takes the form of an Einstein ring.

The alteration in the light path to the quasar will result in different times of flight for each image. If the quasar itself is variable, then a corresponding time delay for the brightening to be seen in each component of the image may be measured. The difference in the light travel time is related to the inverse of the Hubble constant, so it is theoretically possible to estimate H 0 from such time delays. In practice, precise modeling of the lens geometry is required before H 0 can be well constrained.

It is possible that individual stars in a lensing galaxy can cross the light path to the quasar and cause fluctuations in image brightness known as microlensing. This effect can also be seen when objects known as MACHOs in the galactic halo lens the light from an extragalactic star to cause a large amplification in its brightness, although such events are very rare.

gravitational lens

[‚grav·ə′tā·shən·əl ′lenz]
(astronomy)
A massive galaxy or other massive object whose gravitational field focuses light from a distant quasar near or along its line of sight, giving a double or multiple image of the quasar.
References in periodicals archive ?
The speaker showed images of gravitational lenses which had been taken using the Hubble Space Telescope (HST), and explained that these images provided direct evidence for the presence of dark matter in the lensing galaxies.
Of the 10,000 which were spotted, only 20 examples of gravitational lenses were seen.
One key difference between telescope lenses and gravitational lenses was that whilst the former were carefully figured to produce focused images, the latter were less painstakingly constructed, and tended to produce multiple distorted images, often stretched out into arc-like shapes.
The Adler's next citizen science project is Space Warps, which asks for the public's help in finding gravitational lenses in deep space.
For instance, astronomers can measure the density of small galaxies or the cores of larger galaxies by determining how well they act as gravitational lenses.
The distorted image of the galaxy is repeated several times in the foreground lensing cluster, as is typical of gravitational lenses.
This led them to suspect that the galaxies seen in visible light might be gravitational lenses magnifying much more distant galaxies seen by Herschel.
Tyson adds that the prevalence of gravitational lenses provides another test of whether or not the universe has revved up the rate at which it is expanding, as recent studies of distant supernovas have indicated (SN: 4/7/01, p.
Since then, astronomers have used gravitational lenses in many ways, including studying dark matter and as "Nature's Telescope" to investigate galaxies in the distant universe
The astronomers recently focused on three massive, relatively nearby clusters of galaxies known to act as gravitational lenses.
Gravitational lenses could also be used to transmit signals, amplifying them so they could travel further and potentially reach distant civilizations.
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