PTAs do not detect gravitational waves in the same way as observatories such as LIGO, Virgo, or KAGRA. Instead of using kilometer-scale laser interferometers to sense waves with frequencies of hundreds of hertz, PTAs turn the Galaxy into a vast detector. They observe millisecond pulsars—rapidly rotating neutron stars whose radio pulses arrive with extraordinary regularity. A passing gravitational wave slightly stretches and compresses spacetime, changing the apparent arrival times of those pulses by tiny amounts. When dozens of pulsars are monitored over many years, correlated timing variations can reveal a stochastic background: not one isolated cosmic collision, but the combined signal of countless unresolved sources. International PTA collaborations have reported compelling evidence for such a background at nanohertz frequencies, where the leading explanation is a population of orbiting supermassive black-hole binaries.

These binaries are expected to form when galaxies merge and bring their central black holes together. As the two black holes orbit, they emit gravitational radiation and gradually lose energy, causing their separation to shrink. The most powerful sources in the nanohertz band are expected to contain black holes with total masses of roughly a billion times that of the Sun or more. Yet this explanation immediately raises a difficult question. If the Universe’s largest black holes grew from smaller ancestors, how could those initial seeds become so massive so quickly? Observations by the James Webb Space Telescope and the Chandra X-ray Observatory have identified unexpectedly massive black-hole candidates at very high redshifts, intensifying the debate over whether ordinary stellar remnants could have assembled the earliest giants rapidly enough.

In their Physical Review D study, Ghodla and Ilie examine whether the origin of those seeds could influence the gravitational-wave background billions of years later. Their analysis follows the subsequent evolution of black holes formed through two proposed early-Universe channels. The first is direct collapse, in which enormous clouds of primordial gas avoid fragmenting into ordinary stars and collapse almost directly into black holes. The second involves supermassive Dark Stars, hypothetical primordial objects powered not mainly by nuclear fusion but by energy released through interactions involving dark matter. In the WIMP dark-matter scenario explored by the researchers, dark-matter heating could support a large, relatively cool and extended star while it continues to draw in gas. Such an object might grow to a mass of a million Suns or more before ultimately collapsing into a massive black-hole seed.

The importance of these two channels lies not only in the size of their seeds, but also in their expected abundance. A larger initial black hole can reduce the amount of subsequent growth required to reach the masses observed in the modern Universe. However, a sufficiently numerous population of massive seeds could also produce too many later mergers, creating a gravitational-wave background stronger than the one measured by PTAs. The researchers therefore model the halos hosting the early seeds, track the cosmic growth and merger histories of their black-hole descendants, and calculate the gravitational-wave spectrum expected from the resulting binary population. Their calculations indicate that supermassive Dark-Star remnants with a number density of approximately 10^-3 per cubic megaparsec could make a substantial, potentially dominant contribution to the observed nanohertz signal.

The direct-collapse scenario examined in the study produces a markedly weaker background. The reason is primarily demographic: the direct-collapse black holes considered by the researchers are expected to be far rarer, with characteristic number densities near 10^-6 per cubic megaparsec. Even if individual seeds are massive, too few of them would eventually find partners, form binaries, and merge in sufficient numbers to generate a strong stochastic signal. By contrast, a more abundant population of Dark-Star remnants would provide many more opportunities for descendant black holes to enter galactic nuclei, pair up after galaxy mergers, and radiate gravitational waves. The difference illustrates how a gravitational-wave background can depend not only on the mass of the sources, but also on the population statistics and environments in which those sources formed.

The study also turns PTA measurements into a possible census of objects that existed when the Universe was less than a few hundred million years old. For the models considered, seed densities in the approximate range of 10^-2 to 10^-1 per cubic megaparsec would begin to overproduce the measured gravitational-wave background. The exact limit depends strongly on the dark-matter halo masses associated with the seeds, because the halo environment affects black-hole growth, galaxy assembly, merger rates, and the eventual mass distribution of the binaries. In this sense, PTAs could constrain a population at redshifts greater than 10 even though the mergers responsible for most of the signal take place much later, after billions of years of cosmic evolution.

The calculations further support the conclusion that binaries with total black-hole masses above about 10^9 solar masses dominate the predicted PTA signal. Lower-mass systems can be numerous, but their individual gravitational-wave emission is substantially weaker, and their combined contribution at nanohertz frequencies is comparatively limited. This mass dependence offers an important physical explanation for why early massive seeds are so relevant. If the first black holes were born with enough mass—or grew rapidly enough—to become members of extremely massive binary systems, their descendants could leave a measurable imprint on today’s pulsar timing data. If instead the early Universe produced mostly small seeds, later growth and mergers would have to build the largest black holes, potentially changing both the amplitude and the shape of the gravitational-wave background.

The implications extend beyond one proposed type of primordial star. A successful explanation of the PTA signal must be tested against observations of galaxy populations, black-hole masses, quasar activity, dark matter, and the timing data themselves. Future PTA observations should improve the measurement of the background’s amplitude and spectral shape, while larger pulsar samples and longer observing campaigns may help identify departures from the simplest population models. At the same time, JWST and other observatories will continue searching for black holes and luminous galaxies at cosmic dawn. If the gravitational-wave background is stronger or structured in a way that favors an abundant population of massive descendants, it could provide indirect evidence that supermassive Dark Stars once existed—even if the original stars are too distant and faint to observe directly.

The proposed scenario is therefore a striking example of how the Universe can preserve ancient history in unexpected forms. A dark-matter-powered object that vanished at the beginning of cosmic time might be impossible to see today, yet its collapsed remnant could grow inside a galaxy, merge with another supermassive black hole, and contribute to spacetime vibrations detected by pulsars in the present-day Milky Way. “Pulsar timing arrays are usually thought of as probes of supermassive-black-hole binaries in the relatively recent Universe,” Cosmin Ilie said. “What our work shows is that the signal may also contain information about how the ancestors of those black holes formed at cosmic dawn.” If future measurements confirm the connection, the nanohertz sky could become a new archaeological record of the first black-hole seeds—and a powerful test of the exotic physics that may have shaped the earliest luminous objects in existence.

Subject of Research: Early supermassive black-hole seeds, supermassive Dark Stars, direct-collapse black holes, and the nanohertz gravitational-wave background detected by Pulsar Timing Arrays.

Article Title: Reconstructing PTA measurements via early seeding of supermassive black holes

News Publication Date: 19-Aug-2026

Web References: https://doi.org/10.1103/hvfd-8fkr

References: Ghodla, S. and Ilie, C., “Reconstructing PTA measurements via early seeding of supermassive black holes,” Physical Review D, published 17 August 2026.

Image Credits: Ghodla and Ilie, Physical Review D (2026).

Keywords

Supermassive black holes, Dark Stars, direct-collapse black holes, gravitational waves, Pulsar Timing Arrays, nanohertz astronomy, cosmic dawn, dark matter, black-hole seeds, galaxy mergers, James Webb Space Telescope, astrophysics

Supermassive black holes, often billions of times the mass of our Sun, serve as the gravitational anchors at the centers of most galaxies, including our own Milky Way. When actively accreting matter, these cosmic behemoths blaze as quasars, some of the brightest and most energetic objects observable in the universe. Quasars emit copious radiation as gas and dust spiral inward, heated to extreme temperatures in their accretion disks. This light flickers irregularly as the black hole feeds, a phenomenon providing key insights into the dynamics of accretion and black hole growth. The detection of such flickering from one of the universe’s earliest quasars marks a significant milestone in astrophysics.

The quasar flicker detected by the MIT-led team represents the earliest known variability observed from such an object, emerging from what astronomers term the “cosmic dawn.” This period, occurring roughly 850 million years post-Big Bang, was thought to host only nascent galaxies and immature black holes. Contradicting previous assumptions, the observed quasar exhibited variability patterns similar to those found in more contemporary quasars, suggesting that the physical processes governing black hole accretion were already established at these primordial times.

Gene Leung, a postdoctoral researcher at MIT’s Kavli Institute for Astrophysics and Space Research, explains that prior detections of quasars from the early universe showed bright, steady light sources but lacked the tell-tale flickering patterns that reveal underlying accretion processes. The detection of flicker is critical because it directly relates to fluctuations in how material is ingested by the black hole. Such fluctuations imprint themselves in the light output, encoding information about the accretion disk’s geometry and the feeding mechanisms at work.

Unexpectedly, the flickering quasar’s accretion disk appeared surprisingly flat and thin, resembling a “pancake” rather than the puffier, chaotic structures anticipated for black holes at such early stages of growth. This finding puzzles astronomers, as conventional wisdom suggests that youthful black holes in the young universe should exhibit turbulent, unstable accretion disks, reflecting ongoing rapid growth phases. Instead, this quasar’s disk mirrors the more orderly structures typically associated with mature, settled black holes.

Anna-Christina Eilers, an assistant professor of physics at MIT and a co-author on the study, interprets this evidence as suggesting that the tumultuous, rapid growth stages of supermassive black holes precede the luminous quasar phase visible to current telescopes. In other words, the messy early feeding epochs might occur so swiftly and early that by the time we observe the quasar’s brilliant light, the black hole’s accretion disk has already stabilized into a flat, well-organized structure.

This revelation adds to one of cosmology’s deepest enigmas: How did supermassive black holes form and reach immense mass so quickly in the early universe? The presence of such sophisticated accretion disks at cosmic dawn implies that significant growth and structural organization happened on remarkably short timescales, challenging existing models of black hole evolution and opening new avenues for theoretical and observational research.

Detecting flickering from such a distant quasar was a formidable technical challenge. Owing to cosmic expansion, the quasar’s emitted light is not only stretched to longer, infrared wavelengths — a phenomenon known as redshift — but its temporal flickering expands correspondingly. What might be a variation over weeks in the quasar’s frame becomes a gradual fluctuation observed over many months or years from Earth. This necessitated infrared observations over extended durations with high sensitivity.

The team turned to data collected by NASA’s NEOWISE mission, a space-based infrared survey telescope with a 14-year archive monitoring the entire sky at infrared wavelengths. High-quality, time-resolved infrared data provided the ideal dataset to detect the subtle, long-term flickering signal from the distant quasar. Utilizing refined data processing techniques developed by former MIT postdoc Kishalay De, now at Columbia University, the researchers extracted the earliest evidence of quasar variability from the cosmic dawn.

The flickering exhibited stochastic variations in brightness by up to 20 percent, equivalent to luminosity shifts of approximately 2 trillion times that of our Sun. Such variations imply fluctuating accretion rates and provide a rare glimpse into the black hole’s feeding habits in an epoch close to the universe’s infancy. By analyzing flicker behavior across multiple wavelengths, the researchers could infer temperature gradients within the disk, enabling them to map its structure and confirm its thin, flat morphology.

This discovery not only underscores that the physical mechanics of black hole accretion recognized in the modern universe were already in place shortly after the Big Bang but also poses profound implications for models of galaxy and black hole coevolution. Supermassive black holes exert powerful influence on their host galaxies, regulating star formation and galactic growth through energetic feedback processes. Understanding how early black holes matured thus impacts our grasp of galaxy formation and evolution across cosmic time.

Looking ahead, the team aims to push observational boundaries even further, seeking to identify flickering quasars at even earlier times. Capturing the nascent stages of black hole development promises to unravel the initial phases of black hole assembly and accretion disk formation. Such insights will illuminate the conditions prevailing in the first billion years and potentially solve the mystery of how black holes achieved such enormous masses so rapidly after the dawn of the universe.

Funded in part by NASA, this study represents a collaborative effort between MIT Kavli and multiple global institutions. It advances our cosmic understanding through innovative reuse of archival data and sets a benchmark for future infrared time-domain surveys. The insights gained from this flickering quasar discovery herald a new era in the study of black hole physics, galaxy evolution, and the earliest chapters of cosmic history.

Written by Jennifer Chu, MIT News

Subject of Research: Early Universe Quasar Variability and Supermassive Black Hole Accretion Disk Structure

Article Title: “Discovery of Cosmic Dawn Quasar Variability and Early Accretion Disk Signatures”

News Publication Date: 2024

Web References: http://dx.doi.org/10.1038/s41550-026-02897-4

Image Credits: NASA/JPL-Caltech

Keywords

Quasar flickering, supermassive black holes, cosmic dawn, accretion disk, early universe, NEOWISE, infrared astronomy, black hole growth, galaxy evolution, cosmic redshift, astrophysics, variability detection