A new 3D map of the Milky Way reveals our galaxy's warped shape in unprecedented detail
- A large-scale 3D map of the Milky Way shows its warped shape with a new level of detail and accuracy.
- Researchers measured the distances between our sun and 2,400 stars to map their three-dimensional coordinates across the Milky Way.
- Scientists still don't know how our galaxy and others like it ended up with these warped S-curve shapes.
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We sit along an outer arm of a massive, spiraling disk of gas, dust, and a billion stars. In the right place at the right time, you can see it as a spilled-milk streak across the night sky: the Milky Way.Recently, researchers at the University of Warsaw in Poland measured the distances between thousands of stars and our sun to chart the stars' three-dimensional coordinates across the Milky Way. The result is an unprecedented large-scale 3D map of the galaxy. And that map shows that the edges of the Milky way bend slightly, giving it a warped S shape.
Over the last 50 years, scientists have determined that the Milky Way is not flat like they once thought, but curves at the edges. The first 3D map of the galaxy that showed this warped curve was published in February by researchers from the Chinese Academy of Sciences in Beijing.The Warsaw team used the same technique as the Beijing scientists for their new map, but factored in data from over 1,000 more stars, some as remote as the boundary of the Milky Way's disk.
The new map provides a larger-scale picture of our galaxy in more detail.
Mapping distant stars reveals a bend in the galaxy
"The internal structure and history of the Milky Way are still far from being well understood, in part because it is extremely difficult to measure distances to stars in the outer regions of our galaxy," Dorota Skowron, the study's lead author, said in the video.
To make these difficult measurements, Skowron's team looked for "cepheid" stars."Cepheids are young, pulsating, supergiant stars," she said.
Cepheids are easy to study because they pulsate at regular intervals and burn hundreds (or sometimes thousands) of times brighter than our sun. Researchers can measure the distance of a cepheid star with an accuracy of more than 95% by using the star's pulsation patterns to determine its luminosity. They can then calculate distance by comparing that luminosity with how bright the star looks from Earth.
The pulsation patterns also allow scientists to estimate the stars' ages.So Skowron and her team measured the distances between our sun and 2,400 of these cepheid stars.
The locations of these cepheid stars illustrate the way the Milk Way's disk curves away from its center in more detail and with more precision than ever before.Other galaxies show similar warping, but scientists still haven't figured out why. The Beijing researchers thought forces from the Milky Way's spinning, massive inner disk of stars may have caused the warping, but Mroz suggested other influences that could be at play.
"Warping may have been caused by the past interactions with satellite galaxies, interactions with intergalactic gas, or dark matter," he said.
Simulations and maps could unearth galactic historyIn their observations, the Warsaw researchers also noticed that clusters of similar-aged cepheids follow the shape of the galaxy's spiral. Younger stars appear to be clustered closer to the middle, and older stars are spread out across the edges.
The researchers guessed that the clustered cepheids may have formed together, so they created a simulation of three waves of star formation to test that theory. The results of the simulation look remarkably similar to the real map.
The image below compares that simulation (left) with the researchers' actual map of the cepheids (right). The oldest stars, shown in red, are 400 million years old, while the youngest, in blue, are 30 million years old. The little sun symbol marks the location of our own solar system.
More research like this to map the ages and locations of stars in the Milky Way could can help scientists piece together how our galaxy formed.
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