When the James Webb Space Telescope (JWST) turned its powerful infrared eyes toward the absolute edges of observable space, it began uncovering a mysterious class of objects that baffled astronomers. Dubbed “little red dots” (LRDs) due to their compact morphology and exceptionally red colors, these distant cosmic beacons appeared to harbor supermassive black holes far too large to exist so early in cosmic time. Standard models of cosmic evolution simply could not explain how black holes boasting millions or billions of solar masses could assemble within the first few hundred million years following the Big Bang.
Now, a team of international researchers using JWST’s Near-Infrared Spectrograph (NIRSpec) instrument as part of the “Mirage or Miracle” (MoM) survey has discovered a singular object that may resolve this long-standing paradox. Located just 660 million years after the Big Bang (at a redshift of $z = 7.7569$), the newly identified object—named MoM-BH-1*—represents the earliest known “black hole star” ever observed.
Unlike typical quasars, MoM-BH*-1 is not obscured by a heavy shroud of cosmic dust. Instead, it is an early, rapidly growing supermassive black hole enveloped within an extraordinarily dense, turbulent cocoon of pure gas. This discovery provides direct empirical evidence for super-Eddington accretion—a theoretical mechanism long hypothesized to fuel supra-exponential black hole growth in the infant universe—and fundamentally recalibrates how astronomers measure the masses of early cosmic monsters.
The Anatomy of a Cosmic Miracle
MoM-BH*-1 stood out instantly in deep extragalactic survey images of the Ultra Deep Survey (UDS) field as the single reddest object across a 250-square-arcminute region. While remarkably luminous at longer infrared wavelengths, the source virtually vanished at shorter wavelengths.
When the researchers analyzed its spectrum, they discovered an array of extreme physical features that defied conventional stellar physics. First, the object exhibits a massive spectral “Balmer break”—a sharp drop in light intensity—of $7.7_{-1.4}^{+2.3}$, far exceeding the theoretical maximum break strength of 3 to 5 for a dust-free galaxy made purely of stars, thereby ruling out stars as the primary source of its optical light. Additionally, non-resonant hydrogen emission lines like $\text{H}\beta$ and $\text{H}\gamma$ display deep absorption troughs at line center, requiring hyper-dense gas environments with densities exceeding $10^9 \text{ cm}^{-3}$. The source also features remarkably broad $\text{H}\beta$ emission lines with symmetric double peaks mirrored around the systemic redshift. Finally, imaging confirms extreme compactness, with light concentrated within a radius of less than 100 parsecs (roughly 325 light-years), matching point-source morphologies expected of an active galactic nucleus (AGN).
To explain these singular characteristics, the research team performed extensive spectral modeling using the Cloudy synthesis code by embedding a classical AGN accretion disk inside an idealized gas cloud spanning approximately 40 astronomical units (AU)—about the size of our solar system. The model revealed that an extreme gas column density ($\sim 10^{25.8} \text{ cm}^{-2}$) with turbulent velocities near 500 km/s perfectly reproduces the spectral features, including the deep Balmer break and the broad absorption lines, without needing significant amounts of dust.
As lead author Rohan Naidu, an astronomer at the University of Hawaiʻi’s Institute for Astronomy, explained in editorial interviews:“The spectrum we detected is our best evidence of a cloak of gas feeding an early-forming black hole. Because of its spectrum and with a nod to the survey’s name, we dubbed the object ‘MoM-BH-1.’ We modeled MoM-BH*-1 as a miniature supermassive black hole in the earliest phases of its evolution, enshrouded by extremely dense, turbulent gas that forms a dust-free envelope around it.”
Naidu further underscored the uniqueness of the discovery:“MoM (Mirage or Miracle)-BH-1 is so swaddled within shrouds of dense gas that it effectively radiates in a manner reminiscent of stellar phenomena. It is a very special thing to find an object with no comparison given the vast stores of data on billions of stars, galaxies, and black holes that we have in our archival databases. MoM-BH*-1 is one in a billion!”
Feeding Beyond the Limit: How Early Black Holes Grow
A central mystery of early cosmology is the “eddington limit”—a physical balance point where the outward radiation pressure of an accreting black hole balances the inward pull of gravity, theoretically capping how fast a black hole can feed. Standard Eddington-limited growth requires hundreds of millions of years for a small seed black hole to reach a billion solar masses, a timeline that conflicts with observations of giant quasars existing just 700 million years after the Big Bang.
Theoretical astrophysicists have proposed that early black holes could bypass this limit through super-Eddington accretion. Under this framework, if a seed black hole is buried within an extremely dense, spherically symmetric gas cloud or nuclear star cluster, the dense gas layer traps or convective-cools the radiation before it can escape. Gravity overcomes radiation feedback, allowing gas to pour onto the black hole at supra-exponential rates.
MoM-BH*-1 offers the first direct observational snapshot of this exact theoretical setup in action. Wrapped in a Compton-thick cocoon of hydrogen gas, the black hole is caught mid-burst in a hyper-feeding phase.
Moreover, the object sits just 60 proper kiloparsecs away from a neighbor galaxy that is roughly ten times more massive. Theoretical models of direct-collapse black hole seeds suggest that proximity to a nearby star-forming galaxy generates an intense ionizing flux, suppressing the formation of molecular hydrogen gas and enabling primordial gas clouds to collapse directly into black hole seeds.
Demystifying “Little Red Dots” and Recalibrating Black Hole Masses
The discovery of MoM-BH*-1 carries profound implications for the broader population of “little red dots” discovered across the high-redshift universe. Previously, astronomers struggled to model LRDs because their spectral energy distributions (SEDs) exhibited a hybrid behavior: V-shaped continua that appeared faint and blue in the ultraviolet, but dramatically steep and red in the rest-optical. To account for this, prior studies assumed LRDs contained massive amounts of cosmic dust that heavily attenuated the central black hole. Consequently, when applying standard velocity scaling relations to calculate central black hole masses, scientists inferred that early black holes were wildly “overmassive”—comprising up to 10% of their host galaxy’s total mass, compared to the 0.01% observed in the modern universe.
MoM-BH*-1 proves that this narrative needs a major update by demonstrating that the steep red continuum is driven by hydrogen gas opacity and atomic scattering rather than dust absorption. Furthermore, H$\beta$ line emission behaves similarly to Lyman-$\alpha$ radiation, undergoing resonant scattering within the dense gas atmosphere so that observed line widths reflect optical scattering through a gas envelope rather than pure gravitational motion within a broad-line region. Because line widths and dust corrections were previously overestimated, calculated black hole masses in LRDs may actually be exaggerated by 1 to 2 orders of magnitude (up to 100 times too high).
When treating MoM-BH*-1 as an unattenuated template for the core black hole and combining its light with that of a typical UV-bright host galaxy, the combined spectrum yields a perfect match for classic LRDs. The host galaxy dominates the UV light, while the gas-enshrouded black hole dominates the optical light. Correcting for these gas-scattering effects brings early black hole masses back into alignment with local cosmic scaling relations.
A Window into Cosmic Dawn
Co-author Jorryt Matthee, an assistant professor at the Institute of Science and Technology Austria (ISTA), emphasized the significance of probing these extreme early environments:“Until now, we have known very little about how these supermassive black holes formed. In addition, some quasars found in the early Universe seemed far too massive to exist, which led astronomers to call them ‘problematic quasars.’ The Mirage or Miracle survey was designed specifically to target sources considered ‘risky,’ meaning they could either be amazing discoveries or just interlopers. Far from a mirage, this might well be a cosmic miracle.”
With evidence of photometric variability—a 30% flux increase over just two rest-frame months—MoM-BH*-1 is set to become a prime candidate for long-term monitoring by JWST and future observatories. By peeling back the gas shroud around this ancient “black hole star,” astronomers have finally glimpsed the engine room of supermassive black hole growth at the dawn of time.
Endnotes & References
Naidu, R. P., Matthee, J., Katz, H., de Graaff, A., Oesch, P. A., Smith, A., Greene, J. E., et al. (2026). A gas-enshrouded and gas-reddened black hole at cosmic dawn. Nature, 656, 329–335. https://doi.org/10.1038/s41586-026-10846-4
Institute of Science and Technology Austria / EurekAlert! (2026, August 12). Mirage or miracle? JWST finds earliest known ‘black hole star’ at cosmic dawn. Press Release. https://www.eurekalert.org/news-releases/1139484
Quantum Zeitgeist. (2026, August 12). First Black Hole From Cosmic Dawn Is Gas-shrouded And Reddened. https://quantumzeitgeist.com/james-webb-black-hole-cosmic-dawn/
Gizmodo / Passant Rabie. (2026, August 12). Astronomers Discover a Brand-New Type of Object: Part Black Hole, Part Star. https://gizmodo.com/astronomers-discover-a-brand-new-type-of-object-part-black-hole-part-star-2000797643
Inayoshi, K., & Maiolino, R. (2025). Extremely dense gas around little red dots and high-redshift active galactic nuclei: a non-stellar origin of the Balmer break and absorption features. The Astrophysical Journal Letters, 980, L27.
Ji, X., et al. (2025). BlackTHUNDER – a non-stellar Balmer break in a black hole-dominated little red dot at z = 7.04. Monthly Notices of the Royal Astronomical Society, 544, 3900–3935.
Alexander, T., & Natarajan, P. (2014). Rapid growth of seed black holes in the early universe by supra-exponential accretion. Science, 345(6202), 1330–1333.
Coughlin, E. R., & Begelman, M. C. (2024). Quasi-stars as a means of rapid black hole growth in the early Universe. The Astrophysical Journal, 970, 158.
Matthee, J., et al. (2024). Little red dots: an abundant population of faint active galactic nuclei at z ~ 5 revealed by the EIGER and FRESCO JWST surveys. The Astrophysical Journal, 963, 129.
Reines, A. E., & Volonteri, M. (2015). Relations between central black hole mass and total galaxy stellar mass in the local Universe. The Astrophysical Journal, 813, 82.
COPY II (2-3 PARAGRAPHS)
IMAGE CREDIT: NASA.
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