cúmulo de galaxias Abel 370, ubicado a unos 4 mil millones de años luz de distancia, contiene una asombrosa variedad de varios cientos de galaxias unidas por la gravedad mutua. Enredados entre las galaxias hay arcos de luz azul de aspecto borroso. Estas son en realidad imágenes distorsionadas de galaxias distantes detrás del cúmulo. Estas galaxias distantes son demasiado débiles para que el Hubble las vea directamente. En cambio, la gravedad del cúmulo actúa como una enorme lente hacia el espacio que magnifica y estira las imágenes de las galaxias de fondo como un divertido espejo. Casi 100 galaxias distantes tienen múltiples imágenes causadas por el efecto de lente. El ejemplo más sorprendente es el «dragón», una característica extendida que probablemente son varias imágenes repetidas de una sola galaxia espiral de fondo estirada a lo largo de un arco. Los astrónomos eligieron Abell 370 como objetivo para el Hubble porque los efectos de las lentes gravitacionales se pueden usar para sondear las galaxias distantes que habitaron el universo primitivo. Crédito: NASA, ESA, J. Lutz y el equipo HFF (STScI)
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Cuando se lleva a los extremos, la ternura puede crear algunos efectos visuales interesantes.[{» attribute=»»>Hubble Space Telescope is well suited to observing. Einstein’s general theory of relativity describes how mass concentrations distort the space around them. A gravitational lens can occur when a huge amount of matter, like a cluster of galaxies, creates a gravitational field that distorts and magnifies the light from distant galaxies that are behind it but in the same line of sight. The effect is like looking through a giant magnifying glass. It allows researchers to study the details of early galaxies too far away to be seen with current technology and telescopes.
Smaller objects, like individual stars, can also act as gravitational lenses when they pass in front of more distant stars. For a few days or weeks, light from the more distant star temporarily appears brighter because it is magnified by the gravity of the closer object. This effect is known as gravitational microlensing.
The gravity of a luminous red galaxy (LRG) has gravitationally distorted the light from a much more distant blue galaxy. More typically, such light bending results in two discernible images of the distant galaxy, but here the lens alignment is so precise that the background galaxy is distorted into a horseshoe – a nearly complete ring. Credit: ESA/Hubble & NASA
The simplest type of gravitational lensing occurs when there is a single concentration of matter at the center, such as the dense core of a galaxy. The light of a distant galaxy is redirected around this core, often producing multiple images of the background galaxy. When the lensing approaches perfect symmetry, a complete or almost-complete circle of light is produced, called an Einstein ring. Hubble observations have helped to greatly increase the number of Einstein rings known to astronomers.
More complex gravitational lensing arises in observations of massive clusters of galaxies. While the distribution of matter in a galaxy cluster generally does have a center, it is never circularly symmetric and can be significantly lumpy. Background galaxies are lensed by the cluster and their images often appear as short, thin “lensed arcs” around the outskirts of the cluster.
These lensed images also act as probes of the matter distribution in the galaxy cluster. The results indicate that most of the matter in a galaxy cluster is not in the visible galaxies or hot gas around them and does not emit light, and is thus called dark matter. The distribution of lensed images reflects the distribution of all matter, both visible and dark. Hubble’s images of gravitational lensing have been used to create maps of dark matter in galaxy clusters.
On the left is a Hubble Space Telescope image of the galaxy cluster Cl 0024+17. On the right is the same image overlaid with a map of the cluster’s mass distribution. The ring-like structure evident in the map is one of the strongest pieces of evidence to date for the existence of dark matter. Credit: NASA, ESA, M. J. Jee and H. Ford (Johns Hopkins University)
In turn, a map of the matter in a galaxy cluster helps provide a better understanding and analysis of the gravitationally lensed images. A model of the matter distribution can help identify multiple images of the same galaxy or predict where the most distant galaxies are likely to appear in a galaxy cluster image. Astronomers work between the gravitational lenses and the cluster matter distribution to improve our understanding of both.
Because very distant galaxies are very faint, gravitational lenses extend Hubble’s view deeper into the universe. Gravitational lensing not only distorts the image of a background galaxy, it can amplify its light. Looking through a lensing galaxy cluster, Hubble can see fainter and more distant galaxies than otherwise possible. It is like having an extra lens that is the size of the galaxy cluster. The Frontier Fields project has examined multiple galaxy clusters, measured their lensing and matter distribution and identified a collection of these most distant galaxies.
The diverse, lensed images of crosses, rings, arcs, and more are both intriguing and informative. Gravitational lensing probes the distribution of matter in galaxies and clusters of galaxies, and enables observations of the distant universe. Hubble’s data also provide a basis and guide for the James Webb Space Telescope, whose infrared observations complement those of Hubble.
Learn more about gravitational lensing.
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