X-ray binaries are among the brightest non-explosive beacons in the universe. In these systems, a compact object, either a black hole, a neutron star or a white dwarf, strips gas from a companion star and heats it to millions of degrees as it spirals inward, outshining the Sun by factors of millions. Typical X-ray binaries radiate most of their energy above 0.3 kiloelectronvolts, an energy range where missions such as ROSAT, XMM-Newton and Chandra have been highly sensitive. Cooler accreting sources, whose emission peaks in the extreme ultraviolet between roughly 912 and 100 angstroms, present a fundamentally harder problem: interstellar hydrogen absorbs extreme-ultraviolet photons efficiently across most of the sky, and no dedicated extreme-ultraviolet survey mission has operated since the 1990s. As a result, sources whose output is concentrated in this band have been systematically undercounted, despite theoretical predictions that they should exist in substantial numbers.

The new study took a direct approach to this gap. Rather than relying on standard survey catalogs, which typically classify sources using hardness ratios computed over conventional X-ray bands, the team reprocessed Chandra observations of nearby galaxies and specifically searched for point-like, non-nuclear sources detected primarily or exclusively in the 0.15 to 0.3 kiloelectronvolt band. This required careful accounting for a subtle instrumental effect: Chandra’s sensitivity at the softest energies has gradually declined over the decades since its launch, particularly in the lowest energy channels. By quantifying this evolution using the galaxy cluster Abell 1795 as a calibration reference, and fitting the decline in soft-band count rates as a function of observing epoch, the researchers ensured that a source appearing faint in soft X-rays in an early observation was not simply a casualty of changing detector response.

What emerged from the search was a population of sources unlike anything in the standard X-ray binary zoo. The most luminous examples radiate close to the canonical 10^38 erg per second Eddington-level output associated with accretion onto a stellar-mass compact object, but they do so in a band so narrow that standard surveys, tuned to harder photons, often register nothing at all. Spectral modeling indicates that the observed X-ray emission is only the tip of the iceberg. For blackbody temperatures in the range implied by the observed colors, the bolometric correction is large, meaning that the total energy output, most of which emerges in the extreme ultraviolet, is likely several times higher than what the X-ray band alone reveals. For accretion-disk models the correction is estimated at roughly three to four times larger than for a pure blackbody at comparable temperatures. By this measure, hypersoft sources rank among the most energetic steady objects in their host galaxies.

The galaxies hosting the newly identified sources include well-observed nearby systems such as NGC 3379 and NGC 4472, two elliptical galaxies in the Virgo region with deep Chandra monitoring records, as well as the spiral galaxy M101. In NGC 4472, repeated observations across three different epochs revealed at least two hypersoft sources displaying recurrent or potentially persistent behavior, demonstrating that these are not one-off flares but stable or repeatable emitters. Variability analysis of the sources in NGC 3379 likewise shows that their soft emission persists on timescales long enough to be captured multiple times, ruling out the possibility that they are transient artifacts or background fluctuations. Their point-like morphology and off-nuclear locations distinguish them from diffuse hot gas and from active galactic nuclei, placing them squarely in the category of compact accreting binaries.

The physical nature of these sources remains an open question, but the authors propose that hypersoft sources represent X-ray binaries spanning several classes rather than a single type of object. One leading possibility is that many are accreting white dwarfs, including post-nova systems in which a white dwarf continues to burn hydrogen stably or quasi-stably on its surface after a classical nova eruption. Such systems are of special interest because sufficiently massive accreting white dwarfs are considered strong candidate progenitors of type Ia supernovae, the standardizable candles used to measure cosmic expansion. The classical supersoft sources discovered by ROSAT in the early 1990s in the Large Magellanic Cloud and M31 fit this general picture, with effective temperatures near a few tens of electronvolts, but the new hypersoft population appears to extend to even softer spectra, suggesting either lower temperatures, higher absorbing columns, or different accretion geometries than previously cataloged supersoft sources.

Accreting black holes may also inhabit the hypersoft class. Theoretical work on ultraluminous X-ray sources has long anticipated that super-Eddington or near-Eddington accretion onto stellar-removal black holes could produce cool, disk-dominated spectra peaking at extreme-ultraviolet energies, and at least one ultraluminous ultraviolet source has been directly detected in a nearby galaxy. If a meaningful fraction of hypersoft sources turn out to host black holes, they would provide a new window on the physics of accretion at the softest observable energies and could refine population models of stellar-mass black holes in galaxies. Conversely, if most are white-dwarf systems, they would constrain the rates at which type Ia supernova progenitors evolve in both old and young stellar populations, a longstanding puzzle given that elliptical galaxies like NGC 3379 and NGC 4472 host these sources despite lacking recent star formation.

Beyond their identity, hypersoft sources may matter for galaxy evolution in a more diffuse way. The extreme-ultraviolet photons that dominate their output are capable of ionizing helium and other species in the surrounding interstellar medium, and recent theoretical work has argued that supersoft sources contribute significantly to nebular He II line emission in star-forming galaxies, a spectral feature whose origin has long been debated. If hypersoft sources are as numerous as the new survey technique suggests, their cumulative ionizing output could help explain puzzling emission lines observed in nearby galaxies and might even leave an imprint on the absorption signatures seen in the spectra of very distant, young star-forming galaxies observed by the James Webb Space Telescope. In effect, these dim-seeming objects could be quiet but consequential players in the energy budget of the interstellar gas.

The discovery also carries a practical lesson for observational astronomy. Hypersoft sources evaded detection not because they are rare or faint but because standard survey pipelines, calibrated to the energy bands where most X-ray binaries shine, were effectively blind to them. The researchers point out that Chandra’s declining soft-band sensitivity means that future searches should prioritize the earliest, deepest archival observations, when the observatory’s extreme-ultraviolet-adjacent response was at its best. All of the data and code underlying the new catalog have been released through the Chandra Data Archive and Zenodo, allowing other teams to extend the hunt to additional galaxies. As follow-up observations with optical telescopes, ultraviolet missions and eventually next-generation X-ray observatories home in on individual hypersoft sources, astronomers may find that a significant fraction of the universe’s luminous accreting binaries has been waiting, softly glowing, just below the threshold of notice.

Subject of Research: Discovery of hypersoft X-ray sources, a new low-energy class of luminous accreting cosmic emitters

Article Title: Hypersoft X-ray sources as a low-energy class of luminous cosmic emitter

Article References: Muhibullah, M., Irwin, J. A., & Di Stefano, R. (2026). Hypersoft X-ray sources as a low-energy class of luminous cosmic emitter. Nature Astronomy. https://doi.org/10.1038/s41550-026-02959-7

Image Credits: AI Generated

DOI: 10.1038/s41550-026-02959-7

Keywords: hypersoft X-ray sources, X-ray binaries, extreme ultraviolet, accreting white dwarfs, type Ia supernovae, Chandra X-ray Observatory, black holes, NGC 4472, NGC 3379, M101, supersoft sources, galaxy evolution