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To the edge of a black hole

Astronomers have taken the closest look ever at the giant black hole in the center of the Milky Way.
Provided by the Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts
black hole
This close-up view here represents the immediate vicinity of the black hole, with the event horizon depicted as a black sphere. The surrounding disk of gas, represented by white and blue rings, whirls around the black hole. The white column over the pole of the black hole represents a jet of gas being ejected from the vicinity of the black hole at nearly the speed of light.
NASA
September 3, 2008
By combining telescopes in Hawaii, Arizona, and California, astronomers detected structure at a tiny angular scale of 37 micro-arcseconds &#8212 the equivalent of a baseball seen on the surface of the Moon, 240,000 miles distant &#8212 on the edge of a black hole. These observations are among the highest resolution ever done in astronomy.

"This technique gives us an unmatched view of the region near the Milky Way's central black hole," says Sheperd Doeleman of MIT, first author of the study that will be published in the September 4 issue of the Nature.

"No one has seen such a fine-grained view of the galactic center before," agrees coauthor Jonathan Weintroub of the Harvard-Smithsonian Center for Astrophysics (CfA). "We've observed nearly to the scale of the black hole event horizon &#8212 the region inside of which nothing, including light, can ever escape."

Using a technique called Very Long Baseline Interferometry (VLBI), a team of astronomers led by Doeleman employed an array of telescopes to study radio waves coming from the object known as Sagittarius A*. In VLBI, signals from multiple telescopes are combined to create the equivalent of a single giant telescope, as large as the separation between the facilities. As a result, VLBI yields exquisitely sharp resolution.

The Sgr A* radio emission, at a wavelength of 1.3 millimeters, escapes the galactic center more easily than emissions at longer wavelengths, which tend to suffer from interstellar scattering. Such scattering acts like fog around a streetlamp, both dimming the light and blurring details. VLBI is ordinarily limited to wavelengths of 3.5 millimeters and longer; however, using innovative instrumentation and analysis techniques, the team was able to tease out this remarkable result from 1.3-millimeters VLBI data.

The team clearly discerned structure with a 37 micro-arcsecond angular scale, which corresponds to a size of about 30 million miles (or about one-third the Earth-Sun distance) at the galactic center. With three telescopes, the astronomers could only vaguely determine the shape of the emitting region. Future investigations will help answer the question of what, precisely, they are seeing: a glowing corona around the black hole, an orbiting "hot spot," or a jet of material. Nevertheless, their result represents the first time that observations have gotten down to the scale of the black hole itself, which has a "Schwarzschild radius" of 10 million miles.

"This pioneering paper demonstrates that such observations are feasible," comments theorist Avi Loeb of Harvard University and frequent contributor to Astronomy, who is not a member of the discovery team. "It also opens up a new window for probing the structure of space and time near a black hole and testing Einstein's theory of gravity."

In 2006, Loeb and his colleague, Avery Broderick, examined how ultra-high-resolution imaging of the galactic center could be used to look for the shadow or silhouette of the supermassive black hole lurking there, as well as any "hot spots" within material flowing into the black hole. Astronomers now are poised to test those theoretical predictions.

"This result, which is remarkable in and of itself, also confirms that the 1.3-mm VLBI technique has enormous potential, both for probing the galactic center and for studying other phenomena at similar small scales," says CfA's Weintroub.

The team plans to develop novel instrumentation to make more sensitive 1.3-mm observations possible. It also hopes to develop additional observing stations, to gain extra baselines (pairings of two telescope facilities at different locations) to enhance the detail in the picture. Future plans also include observations at shorter, 0.85-mm wavelengths; however, such work will be even more challenging for many reasons, including stretching the capabilities of the instrumentation, and the requirement for a coincidence of excellent weather conditions at all sites.
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