Binge Eating Black Hole Jets Caught

“There are four black hole binaries within our own galaxy that have been observed accreting at these extreme rates,” said Matthew Middleton, an astronomer at the Anton Pannekoek Astronomical Institute in Amsterdam. “Gas and dust in our own galaxy interfere with our ability to probe how matter flows into ULXs, so our best glimpse of these processes comes from sources located out of the plane of our galaxy, such as those in M31.”

As gas spirals toward a black hole, it becomes compressed and heated, eventually reaching temperatures where it emits X-rays. As the rate of matter ingested by the black hole increases, so does the X-ray brightness of the gas. At some point, the X-ray emission becomes so intense that it pushes back on the inflowing gas, theoretically capping any further increase in the black hole’s accretion rate. Astronomers refer to this as the Eddington limit, after Sir Arthur Eddington, the British astrophysicist who first recognized a similar cutoff to the maximum luminosity of a star.

This image composites XMM-Newton X-ray data onto an optical view of the Andromeda galaxy; the ULX is circled. Colors in the XMM image correspond to different X-ray energies: 0.2 to 1 keV (red), 1 to 2 keV (green) and 2 to 4.5 keV (blue).

Credit (background): Bill Schoening, Vanessa Harvey/REU program/NOAO/AURA/NSF
Credit (inset): ESA/M. Middleton et al.

“Black-hole binaries in our galaxy that show accretion at the Eddington limit also exhibit powerful radio-emitting jets that move near the speed of light,” Middleton said. Although astronomers know little about the physical nature of these jets, detecting them at all would confirm that the ULX is accreting at the limit and identify it as a stellar mass black hole.

The European Space Agency’s XMM-Newton observatory first detected the ULX, dubbed XMMU J004243.6+412519 after its astronomical coordinates, on Jan. 15. Middleton and a large international team then began monitoring it at X-ray energies using XMM-Newton and NASA’s Swift satellite and Chandra X-ray Observatory. The scientists conducted radio observations using the Karl G. Jansky Very Large Array (VLA) and the continent-spanning Very Long Baseline Array, both operated by the National Science Foundation in Socorro, N.M., and the Arcminute Microkelvin Imager Large Array located at the Mullard Radio Astronomy Observatory near Cambridge, England.

In a paper published online by the journal Nature on Wednesday, Dec. 12, the scientists reveal their successful detection of intense radio emission associated with a jet moving at more than 85 percent the speed of light. VLA data reveal that the radio emission was quite variable, in one instance decreasing by a factor of two in just half an hour. 

Black holes have been conclusively detected in two varieties: “lightweight” ones created by stars and containing up to a few dozen times the sun’s mass, and supermassive “heavyweights” of millions to billions of solar masses found at the centers of most big galaxies. Astronomers have debated whether many ULXs represent hard-to-find “middleweight” versions, containing hundreds to thousands of solar masses. 

ESA/M. Middleton et al.

“The discovery of jets tells us that this particular ULX is a typical stellar remnant about 10 times the mass of the sun, swallowing as much material as it possibly can,” Middleton said. “We may well find jets in ULXs with similar X-ray properties in other nearby galaxies, which will help us better understand the nature of these incredible outflows.”

Commenting on the findings on behalf of the Swift team, Stefan Immler at NASA’s Goddard Space Flight Center in Greenbelt, Md., noted that it was almost exciting enough for astronomers to witness a new ULX so close to home, even if “close” is a few million light-years away. “But detecting the jets is a real triumph, one that will allow us to study the accretion process of these elusive black hole candidates in never-before-seen detail,” he said.