If you’re standing in the Southern Hemisphere on a clear night, you can see two luminous clouds offset from the Milky Way. These clouds of stars are satellite galaxies of the Milky Way, called the Small Magellanic Cloud and the Large Magellanic Cloud, or SMC and LMC.
Using newly released data from a new, powerful space telescope, University of Michigan astronomers have discovered that the southeast region, or “Wing,” of the Small Magellanic Cloud is moving away from the main body of that dwarf galaxy, providing the first unambiguous evidence that the Small and Large Magellanic Clouds recently collided. Professor of astronomy Sally Oey, lead author of the study, said:
“This is really one of our exciting results.
“You can actually see that the Wing is its own separate region that’s moving away from the rest of the SMC.”
Their results are published in The Astrophysical Journal Letters. Together with an international team, Oey and undergraduate researcher Johnny Dorigo Jones were examining the SMC for “runaway” stars, or stars that have been ejected from clusters within the SMC. To observe this galaxy, they were using a recent data release from Gaia, a new, orbiting telescope launched by the European Space Agency.
This image shows an overview of the full Small Magellanic Cloud and was composed of two images from the Digitized Sky Survey 2, which digitized photographic surveys of the night sky. (Image: Davide De Martinvia ESA via Hubble)
Gaia is designed to image stars again and again over a period of several years in order to plot their movement in real-time. That way, scientists can measure how stars move across the sky. Oey said:
“We’ve been looking at very massive, hot young stars — the hottest, most luminous stars, which are fairly rare.
“The beauty of the Small Magellanic Cloud and the Large Magellanic Cloud is that they’re their own galaxies, so we’re looking at all of the massive stars in a single galaxy.”
Arrows show the relative speed and directions of motion in the plane of the sky for the 315 targeted stars in the Small Magellanic Cloud. The red and blue colors show the relative speed in the line of sight, with red and blue corresponding to motion away from, and toward, the Earth, respectively. To the left of the dashed line is the “Wing” region, showing a bulk motion away from the rest of the galaxy. In this image, north is up and east is to the left. (Image: via Johnny Dorigo Jones)
Examining stars in a single galaxy helps astronomers in two ways: First, it provides a statistically complete sample of stars in one parent galaxy. Second, this gives astronomers a uniform distance to all the stars, which helps them measure their individual velocities. Dorigo Jones said:
“It’s really interesting that Gaia obtained the proper motions of these stars. These motions contain everything we’re looking at.
“For example, if we observe someone walking in the cabin of an airplane in flight, the motion we see contains that of the plane, as well as the much slower motion of the person walking.
“So we removed the bulk motion of the entire SMC in order to learn more about the velocities of individual stars. We’re interested in the velocity of individual stars because we’re trying to understand the physical processes occurring within the cloud.”
Oey and Dorigo Jones study runaway stars to determine how they have been ejected from these clusters. In one mechanism, called the binary supernova scenario, one star in a gravitationally bound binary pair explodes as a supernova, ejecting the other star like a slingshot. This mechanism produces X-ray-emitting binary stars.
Another mechanism is that a gravitationally unstable cluster of stars eventually ejects one or two stars from the group. This is called the dynamical ejection scenario, which produces normal binary stars. The researchers found significant numbers of runaway stars among both X-ray binaries and normal binaries, indicating that both mechanisms are important in ejecting stars from clusters.
SMC and LMC of the Milky Way
In looking at this data, the team also observed that all the stars within the Wing — that southeast part of the SMC — are moving in a similar direction and speed. This demonstrates the SMC and LMC likely had a collision a few hundred million years ago. Study contributor Gurtina Besla, an astronomer at the University of Arizona, modeled the collision of the SMC and LMC.
She and her team predicted a few years ago that a direct collision would cause the SMC Wing region to move toward the LMC, whereas if the two galaxies simply passed near each other, the Wing stars would be moving in a perpendicular direction. Instead, the Wing is moving away from the SMC, toward the LMC, said Oey, confirming that a direct collision occurred. Dorigo Jones said:
“We want as much information about these stars as possible to better constrain these ejection mechanisms.
“Everyone loves marveling at images of galaxies and nebulae that are incredibly far away. The SMC is so close to us, however, that we can see its beauty in the night sky with just our naked eye.
“This fact, along with the data from Gaia, allows us to analyze the complex motions of stars within the SMC and even determine factors of its evolution.”
Provided by: University of Michigan [Note: Materials may be edited for content and length.]
Follow us on Twitter, Facebook, or Pinterest
