Last updated: September 20, 2025

Gravitational Lenses: When Spacetime Becomes a Mirage

Example of a gravitational lens observed by Hubble (cluster CL0024+1654)

Physical Principle: The Curvature of Spacetime

According to Albert Einstein’s general relativity (1915), gravity is not a force in the classical sense but a distortion of spacetime caused by the mass of objects. This curvature affects the path of light: when a light ray passes near a massive object (such as a galaxy or cluster), it is deflected, much like an optical lens. This phenomenon, called a gravitational lens, was first confirmed in 1919 during a solar eclipse, thus validating Einstein’s theory.

Types of Gravitational Lenses

Types of gravitational lenses and their characteristics
Lens Type	Description	Observation Example	Typical Visual Effect
Strong Lens	Extreme light distortion with near-perfect source-lens-observer alignment. Reveals the fine structure of matter (visible and dark).	Cluster CL0024+1654 (Hubble, 2004); Einstein Cross (quasar Q2237+0305).	Complete/partial Einstein rings, giant arcs (>10°), multiple images (up to 5).
Weak Lens	Subtle distortions of background galaxies, used to map dark matter on large scales via statistical analysis.	Dark Energy Survey (DES); Planck satellite data (cosmic microwave background).	Galaxies stretched into ellipses, preferential alignments ("cosmic shear"), weak amplification (×1.1–×2).
Microlens	Temporary effect (hours to months) caused by stellar objects (stars, black holes). No visible distortion, only amplification.	OGLE and MOA projects; discovery of exoplanets like OGLE-2005-BLG-390Lb.	Symmetric light curve, brightness peak (×2–×100), no resolved multiple images.

N.B.:
Gravitational lenses are essential tools for studying the invisible Universe.
• Dark Matter: Their effect reveals a mass 5 to 10 times greater than visible matter in galaxy clusters.
• Dark Energy: Large-scale distortions (weak lenses) help measure the acceleration of cosmic expansion.
• Early Galaxies: Amplification allows observing objects 10 to 100 times fainter than current telescope limits.

Special Case: The Einstein Ring
When a light source (star or galaxy), a massive object (lens), and the observer are perfectly aligned, light is deflected symmetrically, forming a luminous ring around the lens. This ring is a direct manifestation of the curved geometry of spacetime.

Applications in Astrophysics

Dark Matter Detection

Gravitational lenses reveal the presence of dark matter, invisible to conventional telescopes. By comparing the visible mass of a cluster (galaxies, gas) with its total mass deduced from light distortions, astronomers estimate that ~85% of the Universe’s matter is of unknown nature. Example: The Bullet Cluster (1E 0657-56) provided direct evidence of dark matter via its lensing effects.

Study of Distant Galaxies

Lenses act as natural magnifying glasses, amplifying light from distant objects (up to 50 times). This allows observing young galaxies formed only 500 million years after the Big Bang, such as GN-z11 (discovered in 2016).

Measuring Cosmic Distances

By analyzing time delays between multiple images of the same object (e.g., a quasar), scientists calculate the expansion rate of the Universe (Hubble constant). Example: The quasar RX J1131-1231 enabled an independent measurement of \( H_0 \).

Limitations and Challenges

While powerful, gravitational lenses present challenges:

Complex Modeling: The mass distribution of the lens (including dark matter) must be precise to interpret images.
Parasitic Effects: Supernovae or intergalactic gas can distort measurements.
Limited Resolution: Current telescopes (even Hubble or JWST) do not capture all subtle distortions.

Future instruments, such as the Einstein Telescope (planned for 2035), should revolutionize this field.