science & techESA/Hubble

Hubble caught a nearby white dwarf bending the light of a distant star, as Einstein predicted

the gist

Einstein's general relativity says mass warps space, so light passing a massive object curves along a bent path. Stein 2051B, a white dwarf only 17 light-years away, drifted in front of a star about 5000 light-years away. Hubble observed the pair eight times over two years, and the white dwarf's gravity shifted the background star's apparent position by about 2 milliarcseconds. That is roughly the size of an ant crawling across a euro coin seen from 2300 kilometres away. Ground telescopes cannot reach this precision, so it took a space telescope to see it.

how it works

When a foreground star passes almost exactly in front of a background star, its gravity bends the background star's light toward us, making the background star appear shifted and brightened. The effect is strongest when the alignment is nearly perfect and is measured by tracking the shift over time.

so what

It is a direct test of general relativity at a scale that was out of reach for a century, with a small, nearby star providing the lens. The method can also detect objects that give off no light.

fun fact

A white dwarf is the dense leftover core of a Sun-like star, after it has shed its outer layers.

more on this

background

Gravitational microlensing is an astronomical phenomenon caused by the gravitational lens effect. It can be used to detect objects that range from the mass of a planet to the mass of a star, regardless of the light they emit. Typically, astronomers can only detect bright objects that emit much light (stars) or large objects that block background light (clouds of gas and dust). These objects make up only a minor portion of the mass of a galaxy. Microlensing allows the study of objects that emit little or no light.

When a distant star or quasar gets sufficiently aligned with a massive compact foreground object, the bending of light due to its gravitational field, as discussed by Albert Einstein in 1915, leads to two distorted images (generally unresolved), resulting in an observable magnification. The time-scale of the transient brightening depends on the mass of the foreground object as well as on the relative proper motion between the background 'source' and the foreground 'lens' object.

From Wikipedia: Gravitational microlensing (CC BY-SA 4.0) ↗

ESA/Hubble · CC BY 4.0

Image: NASA, ESA, and K. Sahu (STScI)