Astronomers Use New Method To Weigh Giant Black Holes
How do you weigh the biggest black holes in the universe? One answer now comes from a completely new and independent technique that astronomers have developed using data from NASA’s Chandra X-ray Observatory.
By measuring a peak in the temperature of hot gas in the center of the giant elliptical galaxy NGC 4649, scientists have determined the mass of the galaxy’s supermassive black hole. The method, applied for the first time, gives results that are consistent with a traditional technique.
Astronomers have been seeking out different, independent ways of precisely weighing the largest supermassive black holes, that is, those that are billions of times more massive than the Sun. Until now, methods based on observations of the motions of stars or of gas in a disk near such large black holes had been used.
“This is tremendously important work since black holes can be elusive, and there are only a couple of ways to weigh them accurately,” said Philip Humphrey of the University of California at Irvine, who led the study. “It’s reassuring that two very different ways to measure the mass of a big black hole give such similar answers.”
NGC 4649 is now one of only a handful of galaxies for which the mass of a supermassive black hole has been measured with two different methods. In addition, this new X-ray technique confirms that the supermassive black hole in NGC 4649 is one of the largest in the local universe with a mass about 3.4 billion times that of the Sun, about a thousand times bigger than the black hole at the center of our galaxy.
The new technique takes advantage of the gravitational influence the black hole has on the hot gas near the center of the galaxy. As gas slowly settles towards the black hole, it gets compressed and heated. This causes a peak in the temperature of the gas right near the center of the galaxy. The more massive the black hole, the bigger the temperature peak detected by Chandra.
This effect was predicted by two of the co-authors — Fabrizio Brighenti from the University of Bologna, Italy, and William Mathews from the University of California at Santa Cruz — almost 10 years ago, but this is the first time it has been seen and used.
“It was wonderful to finally see convincing evidence of the effects of the huge black hole that we expected,” said Brighenti. “We were thrilled that our new technique worked just as well as the more traditional approach for weighing the black hole.”
The black hole in NGC 4649 is in a state where it does not appear to be rapidly pulling in material towards its event horizon, nor generating copious amounts of light as it grows. So, the presence and mass of the central black hole has to be studied more indirectly by tracking its effects on stars and gas surrounding it. This technique is well suited to black holes in this condition.
“Monster black holes like this one power spectacular light shows in the distant, early universe, but not in the local universe,” said Humphrey. “So, we can’t wait to apply our new method to other nearby galaxies harboring such inconspicuous black holes.”
These results will appear in an upcoming issue of The Astrophysical Journal. NASA’s Marshall Space Flight Center, Huntsville, Ala., manages the Chandra program for the agency’s Science Mission Directorate. The Smithsonian Astrophysical Observatory controls science and flight operations from the Chandra X-ray Center in Cambridge, Mass.
Image Caption: A composite image from NASA’s Chandra X-ray Observatory (shown in purple) and Hubble Space Telescope (blue) shows the giant elliptical galaxy NGC 4649. By applying a new technique, scientists used Chandra data to measure the black hole at its center to be about 3.4 billion times more massive than the Sun. The value from this X-ray technique is consistent with a more traditional method using the motions of stars near the black hole. NGC 4649 is now one of only a handful of galaxies for which the mass of a supermassive black hole has been measured with two different methods. Credit: X-ray: NASA/CXC/Univ. of California Irvine/P.Humphrey et al.; Optical: NASA/STScI
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