The key quantity is the Lyman continuum escape fraction, written by astronomers as fesc^LyC. Lyman continuum photons are the highest-energy ultraviolet photons that massive stars can produce, with wavelengths shorter than 912 angstroms, the ionization threshold of hydrogen. Only photons at these energies can ionize intergalactic hydrogen, yet within a star-forming galaxy they face a gauntlet of obstacles: vast reservoirs of neutral hydrogen and interstellar dust that absorb them long before they can reach the galactic frontier. The abundance of ultraviolet-bright, compact star-forming galaxies observed at early cosmic times by JWST suggests that the sheer output of ionizing photons from massive stars alone could have reionized the universe, but only if a sufficiently large fraction of those photons actually escaped. Measuring that fraction directly at high redshift is nearly impossible, because intervening hydrogen absorbs the Lyman continuum before it reaches our telescopes.

This is why local analogues matter. The Low-redshift Lyman Continuum Survey, or LzLCS, and its extension known as LzLCS+ have assembled a sample of nearby compact, highly star-forming galaxies whose properties resemble those of reionization-era systems: intense star formation packed into regions smaller than a kiloparsec, low metallicity, and high ionization states of their gas. Crucially, for these nearby objects, the Hubble Space Telescope’s Cosmic Origins Spectrograph can detect escaping Lyman continuum photons directly, giving researchers ground truth about fesc^LyC that no high-redshift survey can currently provide.

In the new work, Carr and colleagues focused on six of these local galaxies that are otherwise strikingly similar to one another, but that span a range of starburst ages and Lyman continuum escape fractions. The six objects, with designations such as J103344+635317, J105331+523753, J144010+461937 and J154050+572442, were observed with medium-resolution far-ultraviolet spectroscopy, drawing on archival HST programmes and new imaging from the LaCOS survey. The power of the approach lies in its simultaneity: within a single spectrum, the team could read off both the age of the stellar population and the kinematics of the gas, allowing them to trace the launch of a galactic wind through individual absorption lines while directly measuring how many ionizing photons were escaping.

The technical trick is that different ultraviolet spectral features encode different physical information. Stellar-wind doublets such as N V at 1239 and 1243 angstroms and O VI at 1032 and 1038 angstroms are exquisitely sensitive to the ages of the youngest stellar populations, because only the most massive stars launch powerful radiation-driven winds, and those stars die within a few million years. Photospheric features, by contrast, trace stellar metallicity. On the galactic side, absorption lines imprinted by outflowing interstellar gas, including H I Ly-beta at 1026 angstroms and C II at 1036 angstroms, record the velocity structure and column density of material along the line of sight. By fitting stellar population synthesis models with the FiCUS spectral fitting code and modeling radiative transfer with the publicly available SALT semi-analytic line transfer code, the team disentangled these stellar and interstellar components.

The result is a clear evolutionary sequence. In the youngest systems, with stellar populations younger than roughly three million years, Lyman continuum escape peaks. At this stage, the galaxy is flooded with intense radiation from its most massive stars, and strong stellar winds from those stars are carving channels through the neutral gas, but a fast large-scale galactic wind has not yet developed. The youngest starbursts are, somewhat counterintuitively, the best leakers. Then, as the starburst ages past three million years, the first core-collapse supernovae detonate, injecting enormous mechanical energy into the surrounding medium and launching a faster, more massive multiphase wind. These more evolved systems show absorption features of greater equivalent width, higher outflow velocities and higher dust content, and their Lyman continuum escape fractions are correspondingly suppressed.

The statistical support for this picture is striking. The 90th percentile outflow velocity, v90, and the equivalent width of the H I 1026 angstrom absorption line both show strong anti-correlations with the Lyman continuum escape fraction, with a Kendall rank correlation coefficient of tau equal to minus 0.87 and a p-value of 0.02. Monte Carlo resampling confirmed that these relations remain robust against measurement uncertainties. Even more remarkable, the fraction of stellar light contributed by populations between three and ten million years old shows a nearly perfect monotonic correlation with escape fraction, tau equal to 1.0 with a p-value of 0.00, although the authors caution that uncertainties in the stellar ages make the strength of this particular correlation less well constrained.

Stacked spectra of the broader LzLCS+ sample reinforce the conclusion. When Carr and colleagues combined the spectra of compact, highly star-forming galaxies split into strong leakers with escape fractions of twenty percent or more, weak leakers between five and twenty percent, and non-leakers below five percent, they found that strong leakers host the narrowest H I absorption profiles, while the C II profiles reveal that non-leakers drive the fastest outflows, followed by weak leakers. In other words, the galaxies with the most vigorous supernova-driven winds are precisely the ones leaking the fewest ionizing photons. This seems paradoxical at first glance, since winds are often invoked as the mechanism that clears escape channels. The resolution is timing: winds help open pathways, but once they launch and become heavily mass-loaded, they load the line of sight with dense, absorbing material that blocks Lyman continuum photons.

The broader implications reach to the very beginning of galaxy formation. Reionization simulations have long wrestled with the question of whether radiation pressure, stellar winds or supernovae dominate the regulation of ionizing photon escape, and theoretical models differ on when in a starburst’s life the escape fraction peaks. The new observations suggest that in compact star-forming galaxies, the critical window opens almost immediately, within the first three million years of star formation, and closes over the following several million years as supernova-driven winds launch and mass-load during the first ten million years. Because JWST is now detecting galaxies at redshifts greater than ten, whose starbursts may be only a few million years old, this timing matters enormously for interpreting whether the early universe had enough escaping photons to complete reionization, or whether additional sources such as delayed photons from binary star evolution are required.

The study also delivers practical tools for the high-redshift frontier. Indirect estimators of the Lyman continuum escape fraction, such as the far-ultraviolet continuum slope and nebular emission-line ratios, are calibrated against local measurements, and understanding how escape evolves with starburst age sharpens those calibrations. The team cross-checked their outflow velocity measurements against independent estimates derived from the [O III] 5007 line and the Mg II doublet in other surveys, finding broad agreement. All of the HST and XMM-Newton data underpinning the work are publicly available in the Mikulski Archive for Space Telescopes and the XMM-Newton Science Archive, and both analysis codes, SALT and FiCUS, are openly accessible on GitHub, inviting the community to test and extend the emerging picture. For now, the message is elegantly simple: the youngest, most violently radiative starbursts are the universe’s best window manufacturers, and their own supernova explosions are what, a few million years later, shut the window.

Subject of Research: Lyman continuum photon escape and its suppression by the onset of galactic winds in compact star-forming galaxies

Article Title: Lyman continuum escape during the onset of galactic winds in compact starbursts

Article References: Carr, C., Cen, R., McCandliss, S., Ford, J., Saldana-Lopez, A., Scarlata, C., Huberty, M. S., Jaskot, A., Flury, S., Oey, M. S., Amorín, R. O., Borthakur, S., Haye, M., Heckman, T., Ji, Z., Komarova, L., Reste, A. L., Leclercq, F., Marques-Chaves, R., … Xu, X. (2026). Lyman continuum escape during the onset of galactic winds in compact starbursts. Nature Astronomy. https://doi.org/10.1038/s41550-026-02999-z

Image Credits: AI Generated

DOI: 10.1038/s41550-026-02999-z

Keywords: Lyman continuum, galactic winds, starburst galaxies, reionization, Hubble Space Telescope, stellar feedback, supernovae, escape fraction, ultraviolet spectroscopy, LzLCS, interstellar medium, early universe

The scale of the computational challenge is staggering. Temperature contrasts in astrophysical multiphase systems span roughly ten orders of magnitude, and the cold gas, while dense, can be scattered in tiny structures across enormous volumes. Observations suggest cold clouds in the circumgalactic medium may be as small as tens of parsecs. To fully resolve such structures across a Milky Way-sized halo would require more than a quadrillion resolution elements, a number so vast that no supercomputer on Earth comes close. As a result, cold gas quantities in typical cosmological simulations remain unconverged, and researchers have had to resort to a hierarchy of idealized experiments, from turbulent mixing layers to cloud-crushing simulations, each isolating one piece of the physics.

One of the central results the review highlights concerns the survival of cold clouds blasted by hot winds, the classic ‘cloud crushing’ problem. In the absence of cooling, a cold cloud embedded in a supersonic wind is shredded by Kelvin-Helmholtz and Rayleigh-Taylor instabilities on a characteristic crushing time. Worse, the drag time needed to accelerate the cloud is far longer than the destruction time, giving rise to the long-standing ‘entrainment problem’: how can cold gas be flung to hundreds or even thousands of kilometers per second in galactic winds if it should be destroyed before it can accelerate? The answer, it turns out, lies in radiative cooling. When mixed gas at the interface cools faster than the cloud is disrupted, hot gas condenses onto the cold phase, allowing clouds not only to survive but to grow in mass as they are carried along.

This insight has been crystallized into a simple survival criterion: clouds endure if the cooling time of the mixed gas is shorter than their destruction time, which can be recast as a minimum cloud size of roughly a few parsecs under typical wind conditions. Simulations show that surviving clouds grow continuously through cooling-driven mass transfer in their turbulent wakes, and that this same mixing efficiently transfers momentum, accelerating even dense molecular clouds entrained in galactic outflows. Magnetic fields, once heralded as a potential savior of the entrainment problem, help but are not sufficient on their own for the high density contrasts typical of real astrophysical clouds; combined with cooling, however, they shift the survival threshold by orders of magnitude.

The review also delves into thermal instability, the classic mechanism by which a hot medium can spontaneously fragment into a cold, clumpy phase. When radiative cooling increases as temperature drops, small density perturbations run away into dense clumps. In stratified halo atmospheres, precipitation occurs when the ratio of cooling time to free-fall time falls below a critical value of order ten, a criterion modified by turbulence, halo rotation, magnetic fields and cosmic rays. A related and still contentious question is whether cooling clouds ‘shatter’ into a characteristic scale of tiny fragments or instead undergo a violent pulsation dubbed ‘splattering’ before fragmenting, with recent three-dimensional simulations tending to favor the latter picture.

Scaling up, the review surveys supernova-driven bubbles, stratified ‘tall box’ simulations of galaxy disks, and fully global models of dwarf and Milky Way-mass galaxies. A consistent picture emerges: most outflowing mass travels in the warm phase at around 10,000 Kelvin, while most of the energy is carried by the hot, million-degree gas. Hot gas mass loading factors hover near 0.1 across a wide range of star formation rates, and warm outflows in massive galaxies tend to fall back as fountain flows rather than escaping. Including cosmic rays transforms these results, converting fountains into steady, cooler, denser winds that can double the outflowing mass and substantially reshape the circumgalactic medium.

At the largest scales, the review examines how simulations handle the circumgalactic and intracluster media. In cluster cores, jets from supermassive black holes stir turbulence that triggers local thermal instability, producing ‘chaotic cold accretion’ in which cold filaments rain onto the central galaxy and feed the black hole in a self-regulating cycle. In cosmological zoom-in simulations, a recent revolution has come from ‘super-Lagrangian’ refinement schemes that boost resolution specifically in the halo, reaching below 100 parsecs in the circumgalactic medium. These enhanced-resolution models consistently show more and smaller cool clouds, higher covering fractions of cool gas, and non-converged cloud mass functions, confirming that cold gas structure in halo simulations is far from fully resolved.

What emerges most clearly from this comprehensive synthesis is that the diverse simulation approaches, from idealized mixing layers to full cosmological models, are not competitors but complementary layers of a single framework. Small-scale experiments provide the physical intuition, survival criteria and subgrid prescriptions that large-scale simulations need; large-scale simulations in turn supply the realistic boundary conditions, pressures and turbulence levels under which the small-scale physics operates. The ultimate arbiter, the authors stress, is observation, and connecting simulations to real spectra, emission maps and absorption measurements through radiative transfer remains one of the field’s most demanding tasks.

The challenges ahead are formidable: achieving numerical convergence in multiphase diagnostics, capturing the interplay of magnetic fields, conduction, viscosity and cosmic rays, and resolving the critical scales that govern whether cold gas survives, grows or shatters. But the trajectory is clear. GPU-accelerated codes, adaptive refinement targeted at cooling lengths, and a maturing theoretical framework are converging on a unified picture of the multiphase Universe, one simulation at a time.

Subject of Research: Numerical simulations of multiphase gas dynamics in the interstellar, circumgalactic and intracluster media

Article Title: Simulations of multi-phase gas in and around galaxies

Article References: Gronke, M., & Schneider, E. E. (2026). Simulations of multi-phase gas in and around galaxies. Living Reviews in Computational Astrophysics, 12(1), Article 2. https://doi.org/10.1007/s41115-026-00025-7

Image Credits: AI Generated

DOI: 10.1007/s41115-026-00025-7

Keywords: multiphase gas, galaxy simulations, circumgalactic medium, thermal instability, galactic winds, cloud crushing, turbulent mixing layers, computational astrophysics, radiative cooling, cosmic rays, supernova feedback, Kelvin-Helmholtz instability