Weak gravitational lensing

Big things in space bend light.

When light passes near a heavy object, it bends. This can make far things look stretched.

Sometimes the stretch is very small. We cannot see it in just one star or galaxy.

But we can look at many far things at once. We look for a pattern in their shapes.

This helps us find where heavy things are hiding. It is a way to map the sky.

Space is filled with heavy objects. These objects can bend light. This is called gravitational lensing.

Sometimes, this bending is very strong. It can make light look like giant arcs.

But most of the time, the bending is very weak. We cannot see it by looking at one single object. We must look at many far objects at once. We look for a pattern in their shapes. This is called weak gravitational lensing.

When light passes a heavy mass, it changes. One part of this change is called convergence. This makes the far objects look bigger. Another part is called shear. This stretches the objects into long shapes.

Measuring this is hard. Galaxies are not perfect circles. They already have their own shapes. This can hide the lensing signal. Scientists must study many galaxies to find the true pattern. They also must fix errors from the air or the telescope.

This way of mapping helps us find mass. It even helps us find dark matter. Dark matter is a type of mass we cannot see directly.

Astronomers use a clever way to map mass in space. It is called weak gravitational lensing. This happens because mass bends the path of light. This idea comes from a rule called general relativity. When light passes near a heavy object, its path curves. In some cases, this creates giant arcs or many images. These are called strong lensing effects. However, most light in the universe follows a weaker path. We call this the weak lensing regime. In this state, you cannot see the bend by looking at just one object.

To see this, scientists look for a pattern in many objects. This process uses two main changes to light. The first is called convergence. This term means the background objects look larger in size. The second is called shear. This term means the objects look stretched around the heavy mass. To find this, researchers measure the shapes of many distant galaxies. They look for a systematic alignment in those shapes. They must combine many measurements to average out something called shape noise. This noise happens because galaxies are not naturally perfect circles.

This field grew thanks to many important researchers. J. Anthony Tyson pioneered this work in the 1990s. He performed the first cluster weak lensing analysis in 1990. He found a pattern of shapes behind two specific clusters. These clusters were named Abell 1689 and CL 1409+524. Earlier, Roger Lynds and Vahe Petrosian found bright arcs in the late 1970s. They published their work in 1986. Later, Genevieve Soucail proposed a lensing idea for Abell 370 in 1987. These discoveries helped us understand how to map the invisible parts of space.

Measuring these shapes is a very hard job. Telescopes and the air can smear the images. This smearing is called the point spread function. It can make small objects look rounder than they are. It can even create fake patterns that look like lensing. Scientists use stars in our own galaxy to fix this. They build a model to show how the telescope changes the light. They also need to know the distance to the objects. They often use something called photometric redshifts to estimate these distances.

Weak lensing helps us see things we cannot touch. It can reveal the mass of huge galaxy clusters. These clusters are the largest bound structures in the universe. About 80% of a cluster is made of dark matter. We cannot see dark matter, but lensing shows where it is. A famous example is the Bullet Cluster. By comparing lensing maps to light and gas, we learn about the universe. This helps us test different ideas about how gravity works. It is a powerful tool for studying the whole cosmos.

Weak gravitational lensing is a vital technique used in astronomy to map how mass is distributed across the universe. This phenomenon is based on the principles of general relativity. According to this theory, any mass will bend the path of light passing near it. This bending effect is known as gravitational lensing. While some instances of lensing produce dramatic results like giant arcs or multiple images, these are called strong lensing. Most light traveling through space follows a much subtler path. This is known as the weak lensing regime. In this regime, the deflection of light is too small to detect by looking at a single background object. Instead, astronomers must look for a systematic alignment of many background sources around a foreground mass.

To understand how this works, we can look at the two specific ways light is transformed. The first part is called convergence. Convergence acts as a magnification, increasing the apparent size of background objects. The second part is called shear. Shear stretches the images of background objects tangentially around the foreground mass. To measure this, scientists must determine the ellipticities, or the oval shapes, of many distant galaxies. They then look for a statistical pattern in these shapes. A major obstacle is shape noise. This occurs because galaxies are not naturally perfect circles. Their intrinsic ellipticity is often much larger than the shear caused by lensing. In fact, the natural shape can be 3 to 300 times greater than the lensing effect. To overcome this, researchers combine measurements from many galaxies to average out the noise.

Another significant technical challenge is the point spread function, or PSF. This refers to the smearing of images caused by the telescope or the Earth's atmosphere. This smearing can make small, stretched objects appear more rounded. This destroys important information about their true shape. Even worse, the PSF can add a small amount of non-random ellipticity to an image. This can mimic a real lensing signal. To correct for this, astronomers build a model of how the telescope varies across the field. They use stars within our own galaxy to measure the PSF directly. By interpolating between these stars, they can reconstruct the true shapes of the distant galaxies.

The history of this field is marked by several key discoveries. In the late 1970s, Roger Lynds and Vahe Petrosian discovered giant luminous arcs in galaxy clusters. They published these findings in 1986, though they did not yet know the cause. In 1987, Genevieve Soucail and her team identified a blue ring-like structure in Abell 370. They were the first to propose that gravitational lensing was the cause. The first true weak lensing analysis was conducted in 1990 by J. Anthony Tyson. Tyson and his collaborators detected a coherent alignment of galaxies behind the clusters Abell 1689 and CL 1409+524. This work pioneered the use of statistical methods to map mass. Later, in 2006, David Wittman published the first sample of clusters detected solely through lensing signals.

Weak lensing is incredibly useful for studying galaxy clusters, which are the largest gravitationally bound structures in the universe. These clusters are mostly made of dark matter, which accounts for approximately 80% of their content. Because lensing does not depend on how much light a cluster emits, it allows scientists to measure mass without knowing the cluster's composition or dynamical state. This can reveal "dark clusters" that contain dark matter but very little visible matter. A famous example is the Bullet Cluster. By comparing lensing mass maps with observations of gas and stars, scientists can test different models of the universe, such as Λ-Cold Dark Matter (Λ-CDM). These studies help us understand the interplay between dark matter and visible matter.

There is also a specific type of measurement called galaxy-galaxy lensing. In this case, the foreground object is an individual field galaxy rather than a massive cluster. This produces a "mid-range" signal. It is weaker than cluster lensing but stronger than the cosmic shear found in the large-scale structure of the cosmos. J. Anthony Tyson first suggested this concept in 1984. While early results were inconclusive, evidence was tentatively found in 1996. By the year 2000, the first statistically significant results were published. Today, this technique is widely used to help determine the physical characteristics of individual galaxies.

Finally, weak lensing serves as a powerful tool for understanding the entire cosmos. The number of clusters found at different masses and redshifts can help scientists constrain cosmological parameters. However, this is difficult because projections along the line of sight can create false positives. Astronomers also use a technique called stacking to calibrate the relationship between mass and observable light. By combining signals from many clusters, they can create a more robust measurement. As telescopes become more advanced, weak lensing will continue to be a precision probe for the history and structure of our universe.