The merging of two supermassive black holes is a phenomenon that has long been predicted, though never directly observed. One theory put forth by astronomers is that these systems are so massive that they deplete their host galaxy of the stellar material needed to drive their merger. Using archival data from the Gemini North telescope, a team of astronomers have found a binary black hole that provides strong evidence supporting this idea. The team estimates the binary’s mass to be a whopping 28 billion times that of the Sun, qualifying the pair as the heaviest black hole binary ever measured. Not only does this measurement give valuable context to the formation of the binary system and the history of its host galaxy, but it supports the long-standing theory that the mass of a supermassive black hole binary plays a key role in stalling supermassive black hole mergers. Credit: NOIRLab/NSF/AURA/J. daSilva/M. Zamani
Data from Gemini North provide possible explanation for supermassive binary black hole’s halted merger.
Using archival data from the Gemini North telescope, a team of astronomers have measured the heaviest pair of supermassive black holes ever found. The merging of two supermassive black holes is a phenomenon that has long been predicted, though never observed. This massive pair gives clues as to why such an event seems so unlikely in the Universe.
Nearly every massive galaxy hosts a supermassive black hole at its center. When two galaxies merge, their black holes can form a binary pair, meaning they are in a bound orbit with one another. It’s hypothesized that these binaries are fated to eventually merge, but this has never been observed.[1] The question of whether such an event is possible has been a topic of discussion amongst astronomers for decades. In a recently published paper in The Astrophysical Journal, a team of astronomers presented new insight into this question.
Using archival data from the Gemini North telescope, one half of the International Gemini Observatory, operated by NSF’s NOIRLab, a team of astronomers have measured the heaviest pair of supermassive black holes ever found. The merging of two supermassive black holes is a phenomenon that has long been predicted, though never observed. This massive pair gives clues as to why such an event seems so unlikely in the Universe.
Unprecedented Insights From Gemini North
The team used data from the Gemini North telescope in Hawai‘i, one-half of the International Gemini Observatory operated by NSF’s NOIRLab, which is funded by the U.S. National Science Foundation, to analyze a supermassive black hole binary located within the elliptical galaxy B2 0402+379. This is the only supermassive black hole binary ever resolved in enough detail to see both objects separately,[2] and it holds the record for having the smallest separation ever directly measured — a mere 24 light-years.[3]
While this close separation foretells a powerful merger, further study revealed that the pair has been stalled at this distance for over three billion years, begging the question; what’s the hold-up?
The Challenge of Binary Black Hole Mergers
To better understand the dynamics of this system and its halted merger the team looked to archival data from Gemini North’s Gemini Multi-Object Spectrograph (GMOS), which allowed them to determine the speed of the stars within the vicinity of the black holes. “The excellent sensitivity of GMOS allowed us to map the stars’ increasing velocities as one looks closer to the galaxy’s center,” said Roger Romani, Stanford University physics professor and co-author of the paper. “With that, we were able to infer the total mass of the black holes residing there.”
The team estimates the binary’s mass to be a whopping 28 billion times that of the Sun, qualifying the pair as the heaviest binary black hole ever measured. Not only does this measurement give valuable context to the formation of the binary system and the history of its host galaxy, but it supports the long-standing theory that the mass of a supermassive binary black hole plays a key role in stalling a potential merger.[4]
“The data archive serving the International Gemini Observatory holds a gold mine of untapped scientific discovery,” says Martin Still, NSF program director for the International Gemini Observatory. “Mass measurements for this extreme supermassive binary black hole are an awe-inspiring example of the potential impact from new research that explores that rich archive.”
Formation and Future of the Binary System
Understanding how this binary formed can help predict if and when it will merge — and a handful of clues point to the pair forming via multiple galaxy mergers. The first is that B2 0402+379 is a ‘fossil cluster,’ meaning it is the result of an entire galaxy cluster’s worth of stars and gas merging into one single massive galaxy. Additionally, the presence of two supermassive black holes, coupled with their large combined mass, suggests they resulted from the amalgamation of multiple smaller black holes from multiple galaxies.
Following a galactic merger, supermassive black holes don’t collide head-on. Instead they begin slingshotting past each other as they settle into a bound orbit. With each pass they make, energy is transferred from the black holes to the surrounding stars. As they lose energy, the pair is dragged down closer and closer until they are just light-years apart, where gravitational radiation takes over and they merge. This process has been directly observed in pairs of stellar-mass black holes — the first ever recorded instance being in 2015 via the detection of gravitational waves — but never in a binary of the supermassive variety.
A Stalled Merger and Potential for Future Union
With new knowledge of the system’s extremely large mass, the team concluded that an exceptionally large number of stars would have been needed to slow the binary’s orbit enough to bring them this close. In the process, the black holes seem to have flung out nearly all the matter in their vicinity, leaving the core of the galaxy starved of stars and gas. With no more material available to further slow the pair’s orbit, their merger has stalled in its final stages.
“Normally it seems that galaxies with lighter black hole pairs have enough stars and mass to drive the two together quickly,” said Romani. “Since this pair is so heavy it required lots of stars and gas to get the job done. But the binary has scoured the central galaxy of such matter, leaving it stalled and accessible for our study.”
Whether the pair will overcome their stagnation and eventually merge on timescales of millions of years, or continue in orbital limbo forever, is yet to be determined. If they do merge, the resulting gravitational waves would be a hundred million times more powerful than those produced by stellar-mass black hole mergers. It’s possible the pair could conquer that final distance via another galaxy merger, which would inject the system with additional material, or potentially a third black hole, to slow the pair’s orbit enough to merge. However, given B2 0402+379’s status as a fossil cluster, another galactic merger is unlikely.
“We’re looking forward to follow-up investigations of B2 0402+379’s core where we’ll look at how much gas is present,” says Tirth Surti, Stanford undergraduate and the lead author on the paper. “This should give us more insight into whether the supermassive black holes can eventually merge or if they will stay stranded as a binary.”
NotesWhile there is evidence of supermassive black holes coming within a few light-years of each other, it seems none have been able to overcome that final distance. The question of whether such an event is possible is known as the final-parsec problem and has been a topic of discussion amongst astronomers for decades. Previous observations have been made of galaxies containing two supermassive black holes, but in these cases, they are thousands of light-years apart — too far to be in a bound orbit with one another like the binary found in B2 0402+379.Other black hole-powered sources exist with possible smaller separations, though these have been inferred using indirect observations and therefore can best be classified as candidate binaries.This theory was first put forth in 1980 by Begelman et al. and has long been argued to occur based on decades of observations of the centers of galaxies.
Reference: “The Central Kinematics and Black Hole Mass of 4C+37.11” by Tirth Surti, Roger W. Romani, Julia Scharwächter, Alison Peck and Greg B. Taylor, 5 January 2024, The Astrophysical Journal.
DOI: 10.3847/1538-4357/ad14fa
The team is composed of: Tirth Surti (Kavli Institute for Particle Astrophysics and Cosmology, Stanford University), Roger W. Romani (Kavli Institute for Particle Astrophysics and Cosmology, Stanford University), Julia Scharwächter (Gemini Observatory/NSF’s NOIRLab), Alison Peck (University of Maryland) and Greg B. Taylor (University of New Mexico, Albuquerque).
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