New analysis leads to a fundamentally different view of supermassive black holes

Located in the center of galaxies, supermassive black holes are millions or even billion times more massive than our Sun. With their extreme gravitational pull, they are able to engulf vast amounts of gas, dust, and perhaps even stars that wander into their vicinity.

Physics tells us that this material tends to form a disk as it is drawn towards the black hole in a phenomenon called “accretion”. Now these accretion disks are some of the most uninviting, violent places in the known Universe, with velocities approching the speed of light, and temperatures far in excess of the surface of our Sun. This heat produces radiation which we see as light, but the conversion of heat to light is so efficient — about 30 times more efficient than nuclear fusion — that physicists don’t quite understand how.

Hungry cosmic behemoths

The dietary patterns of black holes have wide range. Some, like the one in our own Galaxy, aren’t very hungry and don’t seem to have accretion disks. But we see other galaxies with ravenous hunger whose supermassive black holes have grown extremely hot accretion disks so bright that they outshine all of the stars in their galaxy.

Only recently have we obtained our first picture of an accretion disk from the Event Horizon Telescope, a worldwide network of radio telescopes. However, this accretion disk belongs to a very nearby galaxy. We cannot repeat this experiment with more distant galaxies as the disks are simply too small and so are unresolved, even by the largest telescopes.

Variability is key

Fortunately another method of probing the size and structure of distant accretion disks seems promising: Although we cannot resolve the disks' various components, we can study how its intensity varies in time. By studying the variations in the disks' light we can piece together a picture of the accretion disks of even the most distant galaxies.

This is what DAWN PhD Fellow John Weaver has done, looking into past observations of more than 9,000 galaxies with bright accretion disks — the so-called quasars — from the observational program "Sloan Digital Sky Survey".

When the source is not resolved, the observed light from the accretion disk will be “contaminated” by light from the galaxy hosting the black hole. This unwanted light from the host galaxies has largely been ignored by previous studies. However, by using a new model for the variations in the quasar light, John Weaver and his collaborator Keith Horne, professor of astronomy at the University of St Andrews, were able to separate the light of the accretion disk from that of the host galaxy.

In other words, the model allowed them to more directly see the light from the accretion disk around supermassive black holes, even in galaxies billions of lightyears away.

Obscured by dust

What Weaver and Horne found was that cosmic dust near the accretion disk was likely blocking their view. Using several different models of cosmic dust to account for, and remove, its obscuring effects, they were able to determine how hot the accretion disk is, both near the black hole and far from it at the edges of the disk.

This difference in temperature between the hot inner disk and the cold outer disk has been theoretically predicted. However, what Weaver and Horne found observationally was a very different picture of the temperature of the disk: the disks turned out to be even hotter near the black hole than predicted. These unexpected findings were published today in the Monthly Notices of The Royal Astronomical Society and suggest that our assumptions and theoretical models need to be revised — with consequences for our understanding of supermassive black holes altogether.

Not only do we have more to learn about supermassive black holes, but the variations in their ravenous hunger are a marvelous demonstration that our Universe is a far more dynamic place than one would expect looking at the static night time sky.

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