The black hole resides in the Perseus cluster, located 250 million light years from Earth. In 2002, astronomers obtained a deep Chandra observation that shows ripples in the gas filling the cluster. These ripples are evidence for sound waves that have traveled hundreds of thousands of light years away from the cluster's central black hole.

"We have observed the prodigious amounts of light and heat created by black holes, now we have detected the sound," said Andrew Fabian of the Institute of Astronomy (IoA) in Cambridge, England, and leader of the study.

In musical terms, the pitch of the sound generated by the black hole translates into the note of B flat. But, a human would have no chance of hearing this cosmic performance because the note is 57 octaves lower than middle-C (by comparison a typical piano contains only about seven octaves). At a frequency over a million billion times deeper than the limits of human hearing, this is the deepest note ever detected from an object in the Universe.

"The Perseus sound waves are much more than just an interesting form of black hole acoustics," said Steve Allen, also of the IoA and a co-investigator in the research. "These sound waves may be the key in figuring out how galaxy clusters, the largest structures in the Universe, grow."

For years astronomers have tried to understand why there is so much hot gas in galaxy clusters and so little cool gas. Hot gas glowing with X-rays should cool, and the dense central gas should cool the fastest. The pressure in this cool central gas should then fall, causing gas further out to sink in towards the galaxy, forming trillions of stars along the way. Scant evidence has been found for such a flow of cool gas or star formation. This forced astronomers to invent several different ways to explain why the gas contained in clusters remained hot, and, until now, none of was them satisfactory.

Heating caused by a central black hole has long been considered a good way to prevent cluster gas from cooling. Although jets have been observed at radio wavelengths, their effect on cluster gas was unclear since this gas is only detectable in X-rays, and early X-ray observations did not have Chandra's ability to find detailed structure.

Previous Chandra observations of the Perseus cluster showed two vast, bubble-shaped cavities in the cluster gas extending away from the central black hole. These X-ray cavities, which are bright sources of radio waves, have been formed by jets of material pushing back the cluster gas. They have long been suspected of heating the surrounding gas, but the mechanism was unknown. The sound waves, seen spreading out from the cavities in the recent Chandra observation, could provide this heating mechanism.

A tremendous amount of energy is needed to generate the cavities, as much as the combined energy from 100 million supernovae. Much of this energy is carried by the sound waves and should dissipate in the cluster gas, keeping the gas warm and possibly preventing a cooling flow. If so, the B-flat pitch of the sound wave, 57 octaves below middle-C, would have remained roughly constant for about 2.5 billion years.

Perseus is the brightest cluster of galaxies in X-rays, and therefore was a perfect Chandra target for finding sound waves rippling through the hot cluster gas. Other clusters show X-ray cavities, and future Chandra observations may yet detect sound waves in these objects.

Science Contacts:

* Prof. Andy Fabian, Institute of Astronomy, acf@ast.cam.ac.uk, +44 1223 337548 (switchboard) 337509 (direct)

* Dr. Steven Allen, Institute of Astronomy, swa@ast.cam.ac.uk, +44 1223 337548 (switchboard) 330803 (direct)

* Dr. Kim Weaver, Goddard Space Flight Center, kweaver@milkyway.gsfc.nasa.gov, 301.286.4256

* Dr. Bruce Margon, Space Telescope Science Institute, margon@stsci.edu, 410.338.4459

On the Web

News release http://www1.msfc.nasa.gov/NEWSROOM/news/releases/2003/03-152.html

Photos http://www1.msfc.nasa.gov/NEWSROOM/news/photos/2003/photos03-152.html

Animation http://www1.msfc.nasa.gov/NEWSROOM/news/video/2003/video03-152.html

Chandra Fact Sheet http://www1.msfc.nasa.gov/NEWSROOM/background/facts/axaf.htm