A Dual Quasar Shines Light on Two Supermassive Black Holes on a Collision Course Inside a Galaxy Merger
Maunakea, Hawaiʻi – Astronomers have made a rare discovery in the early universe involving two actively feeding supermassive black holes – or quasars – just 10,000 light-years apart from each other, that are on the verge of a colossal collision.
Using a suite of space- and ground-based telescopes, including two Maunakea Observatories in Hawaiʻi – W. M. Keck Observatory and Gemini North – the researchers found the pair of black holes embedded within two galaxies that merged when the universe was just 3 billion years young.
The study, led by the University of Illinois at Urbana-Champaign, is published in today’s issue of the journal Nature.
Finding such a system is difficult because of the challenge distinguishing two black holes individually when they are so close together. But in this particular system, called J0749+2255, both black holes were on a feeding frenzy, devouring gas and dust that became heated at such high temperatures, the duo produced a massive fireworks show. This activity is called a quasar, a phenomenon that happens when black holes emit an enormous amount of light across the electromagnetic spectrum as they feast.
J0749+2255 is highly unusual because the system has not one, but two quasars that are active at the same time, and are close enough that they will eventually merge.
“We don’t see a lot of double quasars at this early time in the universe. And that’s why this discovery is so exciting,” said graduate student Yu-Ching Chen of the University of Illinois at Urbana-Champaign, lead author of this study.
ESA’s (European Space Agency) Gaia space observatory first detected the unresolved double quasar, capturing images that indicate two closely aligned beacons of light in the young universe. Chen and his team then used NASA’s Hubble Space Telescope to verify the points of light were in fact coming from a pair of supermassive black holes.
Multi-wavelength observations followed; using Keck Observatory’s second generation Near-Infrared Camera (NIRC2) paired with its adaptive optics system, as well as Gemini North, NASA’s Chandra X-ray Observatory, and the Very Large Array network of radio telescopes in New Mexico, the researchers confirmed the double quasar was not two images of the same quasar created by gravitational lensing.
“The confirmation process wasn’t easy and we needed an array of telescopes covering the spectrum from X-rays to the radio to finally confirm that this system is indeed a pair of quasars, instead of, say, two images of a gravitationally lensed quasar,” said co-author Yue Shen, an astronomer at the University of Illinois.
Because telescopes peer into the distant past, this double quasar no longer exists. Over the intervening 10 billion years, their host galaxies have likely settled into a giant elliptical galaxy, like the ones seen in the local universe today. And the quasars have merged to become a gargantuan, supermassive black hole at its center.
The nearby giant elliptical galaxy, M87, has a monstrous black hole weighing 6.5 billion times the mass of our Sun. Perhaps this black hole grew from one or more galaxy mergers over the past billions of years.
There is increasing evidence that large galaxies are built up through mergers. Smaller systems come together to form bigger systems and ever larger structures. During that process there should be pairs of supermassive black holes formed within the merging galaxies.
“Knowing about the progenitor population of black holes will eventually tell us about the emergence of supermassive black holes in the early universe, and how frequent those mergers could be,” said Chen.
“We’re starting to unveil this tip of the iceberg of the early binary quasar population,” said co-author Xin Liu of the University of Illinois at Urbana-Champaign. “This is the uniqueness of this study. It is actually telling us that this population exists, and now we have a method to identify double quasars that are separated by less than the size of a single galaxy.”
- “Hubble Unexpectedly Finds Double Quasar in Distant Universe” – STScI Press Release
- “Dual Quasars Blaze Bright at the Center of Merging Galaxies” – Gemini North, one half of the International Gemini Observatory, operated by NSF’s NOIRLab Press Release
The Near-Infrared Camera, second generation (NIRC2) works in combination with the Keck II adaptive optics system to obtain very sharp images at near-infrared wavelengths, achieving spatial resolutions comparable to or better than those achieved by the Hubble Space Telescope at optical wavelengths. NIRC2 is probably best known for helping to provide definitive proof of a central massive black hole at the center of our galaxy. Astronomers also use NIRC2 to map surface features of solar system bodies, detect planets orbiting other stars, and study detailed morphology of distant galaxies.
ABOUT ADAPTIVE OPTICS
W. M. Keck Observatory is a distinguished leader in the field of adaptive optics (AO), a breakthrough technology that removes the distortions caused by the turbulence in the Earth’s atmosphere. Keck Observatory pioneered the astronomical use of both natural guide star (NGS) and laser guide star adaptive optics (LGS AO) and current systems now deliver images three to four times sharper than the Hubble Space Telescope at near-infrared wavelengths. AO has imaged the four massive planets orbiting the star HR8799, measured the mass of the giant black hole at the center of our Milky Way Galaxy, discovered new supernovae in distant galaxies, and identified the specific stars that were their progenitors. Support for this technology was generously provided by the Bob and Renee Parsons Foundation, Change Happens Foundation, Gordon and Betty Moore Foundation, Mt. Cuba Astronomical Foundation, NASA, NSF, and W. M. Keck Foundation.
ABOUT W. M. KECK OBSERVATORY
The W. M. Keck Observatory telescopes are among the most scientifically productive on Earth. The two 10-meter optical/infrared telescopes atop Maunakea on the Island of Hawaii feature a suite of advanced instruments including imagers, multi-object spectrographs, high-resolution spectrographs, integral-field spectrometers, and world-leading laser guide star adaptive optics systems. Some of the data presented herein were obtained at Keck Observatory, which is a private 501(c) 3 non-profit organization operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the Native Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.