An intermediate-mass black hole might be lurking within a dense stellar cluster — a discovery that could point toward how these oddities form.
Every Friday Bülent Kızıltan heads to a local coffee shop. There, Kızıltan (Harvard-Smithsonian Center for Astrophysics), who is a self-described “overly curious person,” meets with scientists, artists and philosophers from different disciplines across the Cambridge and Boston area. His goal is to enrich himself intellectually.
That’s how he found himself deep in conversation with a cognitive scientist one afternoon who introduced him to a mathematical tool called Kullback–Leibler divergence. Originally developed by two mathematicians and cryptanalysts at the National Security Agency in the 1950s, the tool attempts to extract information from incomplete data.
Perhaps it was the stimulating effects of the freshly brewed cup of joe, but Kızıltan quickly realized that this tool could also be used when observing a dense stellar cluster — a messy environment chockfull of hundreds of thousands of stars where the center is hidden from view. It was the first step toward a paper published today in the journal Nature that provides the best evidence yet that a globular cluster might harbor an intermediate-mass black hole.
"Weighing" a Hidden Black Hole
Few intermediate-mass black holes have been observed before. In fact, skeptics might argue that none of these black holes — which theoretically lie in the range between those that are just a few times the mass of our Sun and those that weigh millions to billions of times the Sun — even exist.
The issue is two-fold. First, there’s no obvious, direct way for these objects to form. Second, the evidence that they exist has been hazy at best.
But with this new mathematical tool in hand, Kızıltan knew he could do better. He set his eyes on the globular cluster 47 Tucanae, located roughly 15,000 light-years away in the southern constellation Tucana. The cluster, which appears roughly the size of the full Moon, is one of the most massive globular clusters in the galaxy, with millions of stars.
In order to probe those stars, Kızıltan and his colleagues first built a realistic model of 47 Tucanae. Then, they measured the locations of 25 pulsars throughout the globular cluster. These rapidly rotating neutron stars sweep electromagnetic radiation across Earth with every spin at a rate so reliable they rival atomic clocks. This (plus the fact that they emit radio waves, as opposed to visible light) enabled the team to probe deeper into the typically invisible depths of the globular cluster.
The pulsars, they found, are on the move. They’re spinning around the center of the cluster rapidly — too rapidly given the number of central stars alone. Using their new mathematical tool, Kızıltan and his colleagues compared those pulsars’ oddly quick movements with their simulation in order to determine that an intermediate-mass black hole, some 2,200 times the mass of the Sun, must be lurking in the cluster’s center, governing the pulsars’ motions.
Runaway Collisions or Dangerous Tangos?
But Cole Miller (University of Maryland), who was not involved in the study, doesn’t think that the new evidence will convince every skeptic.
“Most scientists would like to see strong evidence,” he says. “Because if these objects exist, they will have implications for the formation of the earliest massive black holes. They will have implications about stellar dynamics. And they will have implications about the evolution of very massive stars. All of this is frontier research and you don't want to be jumping on the band wagon too early.”
The main issue is that astronomers are at a loss to explain how these intermediate-mass black holes can form. Miller’s favorite hypothesis enlists runaway stellar collisions. Essentially, the heaviest stars sink to the center of the globular cluster, where they are most likely to collide and merge with other heavy stars, forming even bigger stars. And because a star’s gravitational pull increases with its size and mass, so does its chance of further stellar collisions. This effect snowballs until a massive star rests in the center of the globular cluster.
But how this massive star evolves is not fully understood, says Kayhan Gültekin (University of Michigan) who was not involved in the study. “Standard stellar theory doesn’t apply to these objects. A lot of turning this merged star-like object into a black hole is based on analogies with stellar evolution rather than detailed calculations of how it would actually evolve.”
Luckily, the competing theory doesn’t need to invoke strange astrophysics. Here, stars evolve into black holes, which sink to the center of the cluster where one enters into a binary orbit with another. Through interactions with other black holes, that duo shrinks until it merges, creating a more massive black hole. This single black hole picks up another companion and the process begins anew, until there’s only one massive black hole in the center of the globular cluster.
Unfortunately, there are issues with this theory too. In the interactions between the black hole binary and the third black hole, energy is transferred to the third black hole. And if enough energy is transferred, the third black hole could get kicked out of the system entirely — a huge problem when you’re trying to build a massive black hole.
Although there are other theories that could explain how intermediate-mass black holes arise, only these two rely on the densely packed environment of a globular cluster.
“The fact that this black hole exists in 47 Tucanae, might mean that one or both of those theories is correct,” says Gültekin, who is hopeful that both theories will receive rejuvenated attention in light of the latest discovery.
B. Kızıltan et al. “An Intermediate-Mass Black Hole in the Centre of the Globular Cluster 47 Tucanae.”Nature, February 9, 2017.