Saturday, June 20, 2026

NASA Webb, Hubble Reveal History of Relic of Milky Way’s Formation

This artist’s concept shows exoplanet HD 80606 b being “roasted” as its orbit approaches periastron, the point at which it is closest to its host star, which is similar to our Sun. Artwork: NASA, ESA, CSA, Joseph Olmsted (STScI)



One well-done gas giant, coming right up! That’s the latest from researchers analyzing NASA’s James Webb Space Telescope’s observations of HD 80606 b, an exoplanet four times the mass of Jupiter with an extremely elliptical orbit that sweeps close by its Sun-like star. The research team is presenting their study and preliminary findings Tuesday at the 248th meeting of the American Astronomical Society in Pasadena, California.

“Hot Jupiters are already considered some of the most extreme exoplanets we know of, but even among that population, HD 80606 b is one of the most extreme,” said Tiffany Kataria, the study’s principal investigator at NASA's Jet Propulsion Laboratory in Southern California. “We typically think of hot Jupiters as hot gas giants sitting right next to their stars, but this planet’s highly eccentric orbit creates a completely different beast.”

As the planet plunges close to its star, Webb shows its temperature skyrockets by 1,100 degrees Fahrenheit. Previous studies have shown that radical temperature swings can cause an exoplanet's chemistry and clouds to change in real time. According to the research team, the dynamic conditions of HD 80606 b make the planet an ideal target to observe these changes with Webb’s powerful instruments.

“Observing a planet like HD 80606 b is actually very efficient because its unusual orbit, with the corresponding swings in temperature and chemical composition, allow us to gather data under varying conditions in just hours and apply those findings to other hot Jupiters or more conventional exoplanets,” said Laura C. Mayorga, co-investigator on the study and an exoplanet astronomer at the Johns Hopkins Applied Physics Laboratory in Laurel, Maryland.

Measurements of temperature and chemical composition were done with spectroscopy, a technique scientists use to break light into its component colors to reveal information about the composition, temperature, motion, and physical properties of objects in space. The team used Webb’s MIRI (Mid-Infrared Instrument) for an extended observation of HD 80606 b before, during, and after its periastron, or closest pass by its star. During periastron, the planet also passed behind the star from Webb’s perspective in what’s known as a secondary eclipse. The observation was years in the planning, as scheduling the time to catch the planet at this point was complex given its extremely elliptical 111-day orbit, and Webb’s own restrictions on where it can look during specific times of the year, based on Earth’s position in orbit around the Sun.

Researchers say they have only begun to peel back the layers of an incredibly rich dataset, but they can clearly see a dramatic shift in the exoplanet’s temperature. “Webb has shown that the planet’s increase in temperature was even more extreme than we anticipated based on Spitzer data,” said Kataria.

In fact, the planet had already been dubbed the “roasted exoplanet” and even got its own poster in NASA’s popular series. NASA’s now-retired Spitzer Space Telescope laid the groundwork of infrared observations of HD 80606 b, showing that more detailed spectroscopic data from Webb would be especially compelling.

“Spitzer did amazing work on this exoplanet, and now Webb is building on that legacy by enabling us to drill down to distinguish specific chemical signatures like methane and carbon dioxide, which is just amazing progress,” said Ryan Challener, co-author and research associate at the Cornell Center for Astrophysics and Planetary Science. “There’s so much to learn from this one dataset here — we really are just getting started deciphering what Webb has to tell us.”

The James Webb Space Telescope is the world’s premier space science observatory. Webb is solving mysteries in our solar system, looking beyond to distant worlds around other stars, and probing the mysterious structures and origins of our universe and our place in it. Webb is an international program led by NASA with its partners, ESA (European Space Agency) and CSA (Canadian Space Agency).




Details:

Last Updated: Jun 16, 2026
Location:
NASA Goddard Space Flight Center

Contact Media:

Laura Betz
NASA’s Goddard Space Flight Center
Greenbelt, Maryland

laura.e.betz@nasa.gov

Leah Ramsay
Space Telescope Science Institute
Baltimore, Maryland


Hannah Braun
Space Telescope Science Institute
Baltimore, Maryland



From Dusk Till Dawn

Artist's impression of the exoplanet WASP-121 b. It belongs to the class of hot Jupiters. Due to its proximity to the central star, the planet's rotation is tidally locked to its orbit around it. As a result, one of WASP-121 b's hemispheres always faces the star, heating it to temperatures of up to 2500 degrees Celsius. The night side is always oriented towards cold space, which is why it is 1775 degrees Celsius cooler there. © Patricia Klein and MPIA




To the point:
  • Ultrahot exoplanet, atmospheric differences: Researchers discovered clear differences in the atmosphere between the morning and evening sides of the ultrahot gas planet WASP-121 b using the James Webb Space Telescope (JWST).

  • Temperature and chemical variations: The evening side absorbs more infrared light due to higher temperatures caused by strong winds moving heat eastward, while water molecules decrease in the evening terminator due to high temperatures breaking them apart.

  • Planetary rotation and observation method: WASP-121 b’s synchronous rotation reveals different atmospheric regions during transit, allowing scientists to analyse changes in light absorption over time and longitude.



Astronomers find variations between the morning and the evening conditions of an ultra-hot exoplanet.

Astronomers have revealed distinct differences in atmospheric conditions between the morning and evening transition zones of the ultra-hot gas planet WASP-121 b, which separate day from night, commonly called terminators. This achievement was only possible due to the unmatched sensitivity of the James Webb Space Telescope (JWST). Led by Cyril Gapp, a PhD student at the Max Planck Institute for Astronomy (MPIA) in Heidelberg, Germany, a team of researchers detected this phenomenon, which had previously been predicted by theoretical computations.

Confirmation of variations between dusk and dawn

The discovery corresponds to an asymmetry in the absorption of infrared light received from the host star, which is partially filtered through the planet’s atmosphere during its transit. The researchers interpret this as the result of non-uniform temperatures and chemical compositions in the exoplanet’s atmosphere.

With its unprecedented observational quality, JWST gives us the most detailed glimpses into distant planets to date: By measuring how star light absorption changes as WASP-121 b rotates, we probe its atmosphere longitude by longitude. Cyril Gapp, MPIA

The data indicate that the evening terminator absorbs more light than the morning side, consistent with the commonly accepted picture of powerful winds that transport intense heat from the day to the night side. Hot winds follow the planet’s rotation eastward, which heats the evening zone. With rising temperatures, this region is bound to expand, increasing the planet’s cross-section and allowing it to absorb stellar radiation more efficiently.

Besides a general slight reduction in brightness towards the end of the transit, the data obtained by JWST’s NIRSpec (Near-infrared spectrograph) instrument also reveal an increase in the carbon monoxide (CO) signal. However, this appears to be a temperature effect, not related to an increase in carbon monoxide molecules.

In contrast, the amount of water (H2O) in the atmosphere appears to drop, which the astronomers interpret as a real decrease in water molecules. The temperatures in the upper atmosphere are high enough to break water molecules into their constituents. This result again corroborates the existence of hot winds heating the evening terminator region.

Top view of the orbit of the exoplanet WASP-121 b around its star. The planet’s rotation is synchronized to its orbit, both taking about 30 hours to complete. As a result, the planet constantly faces the star with the same side producing distinct day and night sides. The transition zones between those hemispheres are the morning and evening regions. Due to the planet’s proximity to the central star of only 1.9 stellar diameters, the planet rotates by about 30 degrees during its transit. © MPIA (CC BY 4.0)

Two extreme sides of an ultra-hot planet

To detect these minute variations, the astronomers exploited a peculiar behaviour of hot gas planets. The proximity to their host stars slowly synchronizes their spin and orbital motion via tidal forces,such that eventually one rotation takes as long as one revolution. Finally, these planets exhibit two distinct hemispheres: a hot side constantly facing the star and an opposite, darker and cooler side.

“WASP-121 b is particularly extreme, with average temperatures on the dayside hemisphere being around 2770 Kelvin, while those on the nightside are closer to about 1000 Kelvin,” co-author Tom Evans-Soma from the University of Newcastle, Australia, explains. He previously determined the planet’s temperature range and is also affiliated with MPIA. These values translate to almost 2500 degrees Celsius, or about 4525 degrees Fahrenheit, on the dayside, and approximately 725 degrees Celsius, or 1340 degrees Fahrenheit, at night.

When astronomers observe such a planet transiting in front of a star, the planet rotates slightly between the points of ingress and egress, revealing different fractions of its atmosphere. While the planet mostly presents its night side, our point of view permits glimpses beyond the dusk and dawn towards the bright dayside, depending on the transit’s progress. The zone leading the planet’s orbit corresponds to the morning side, and the one trailing is the evening side.

Apart from recording the measured brightness variation over time, spectrographs break light into smaller components, which physicists call a spectrum, much as a prism produces a rainbow-like distribution of colours. Since atmospheric gases absorb light at distinct colours or wavelengths, a detailed analysis reveals their chemical composition.

Elapsed time converts to longitude

Hence, the variation along the direction of rotation translates into a time-dependent change of the filtered signal. In the case of WASP-121 b the rotation angle during a full transit amounts to about 30 degrees, which is sufficient to probe the morning (dawn) and evening (dusk) terminators with high precision in longitude.

Astronomers usually average the measurements over the entire transit to achieve a clearer signal. However, to determine how the signal changes during the planet’s trajectory across the star, Gapp and his colleagues allowed for a temporal variation while the planet rotates. By applying statistical methods, they found that their procedure provides a significantly better fit to the data, indicating that they indeed detected a significant variation.

Notable gaps in atmospheric models

To verify the measured temperatures that would cause local expansion, the astronomers ran models simulating heat distribution in the upper layers of a gas planet, depending on the planet's properties and the constellation of the planet and its host star. While these atmospheric models confirmed the asymmetric effect caused by spatial temperature variations, the data revealed a larger signal amplitude than the models predicted.

The astronomers suspected that cooling mechanisms at the morning terminator might be at work that the models didn’t account for. Previous studies have indicated that clouds may be present, albeit composed not of water droplets but of minerals such as silicates. Clouds can efficiently shield infrared light emitted from hot gaseous layers below, mimicking lower temperatures. Infamously, simulating the physics of clouds, condensation, and evaporation in a dynamic environment is hard. Therefore, physical models commonly applied to exoplanet atmospheres, such as the one used in this study, do not account for clouds, which can yield unrealistic results.

After tweaking the simulation to better approximate the effect of clouds on infrared radiation from deeper layers, the results were more consistent with observations. However, only more sophisticated models will be able to confidently confirm the presence of clouds.

A blueprint for future studies

Model updates will also improve future investigations using this method. The astronomers have already identified additional suitable targets within the required temperature range and rotation speed to successfully probe the terminator regions. This will help them establish a sample of ultrahot gas planets, revealing their longitudinal structure, and potentially discover similarities and differences among these extreme worlds.

Additional information

MPIA astronomers involved in this study were Cyril Gapp (also Heidelberg University), Thomas M. Evans-Soma (also University of Newcastle, Australia), and Eva-Maria Ahrer.

Other researchers were: Aurélien Falco (Sorbonne Université, Paris, France), David K. Sing (Johns Hopkins University, Baltimore, USA), Shashank Dholakia (University of Queensland, St. Lucia, Australia), Vivien Parmentier (Université de la Côte d’Azur, Nice, France), Jérémy Leconte (Université Bordeaux, France), and Guangwei Fu (Johns Hopkins University).

The JWST observations used in this study were conducted as part of GO program #1729 (PI: Thomas Evans-Soma, Co-PI: Tiffany Kataria) titled “A NIRSpec Phase Curve for the ultrahot Jupiter WASP-121b” and GTO program #1201 (PI: David Lafreniere) labelled “NIRISS Exploration of the Atmospheric diversity of Transiting exoplanets (NEAT).”

NIRSpec (Near Infrared Spectrograph) was built by European industry to the European Space Agency’s (ESA) specifications and managed by the ESA JWST Project at ESTEC (European Space Research and Technology Centre), the Netherlands. The prime contractor was Airbus Defence and Space in Ottobrunn, Germany. MPIA contributed to the development and manufacture of NIRSpec’s filter and grating wheels. The NIRSpec detector and micro-shutter array subsystems were provided by NASA’s Goddard Space Flight Center (GSFC).

The James Webb Space Telescope is the world’s leading observatory for space research. It is an international programme led by NASA and its partners ESA and CSA (Canadian Space Agency).




Contacs:

Dr. Markus Nielbock
Press and outreach officer
Tel:
+49 6221 528-134
Email: pr@mpia.de
MPIA press team
Max Planck Institute for Astronomy, Heidelberg, Germany

Cyril Gapp
Tel:
+49 6221 528-328
Email: gapp@mpia.de
Cyril Gapp / MPIA
Max Planck Institute for Astronomy, Heidelberg, Germany

Dr. Thomas M. Evans-Soma
Tel:
+61 2 4055-3229
Email: tom.evans-soma@newcastle.edu.au
Homepage Thomas Evans-Soma
School of Information and Physical Sciences, The University of Newcastle, Callaghan, Australia
Max-Planck-Institut für Astronomie, Heidelberg, Deutschland




Original publication

Cyril Gapp, Aurélien Falco, Thomas M. Evans-Soma, et al. (incl. Eva-Maria Ahrer)
Atmospheric asymmetries in WASP-121 b revealed by rotational transits detected with JWST
Nature Astronomy (2026). DOI: 10.1038/s41550-026-02887-6


Source



Orbit of WASP-121 b around its host star (Video)
This animation illustrates the orbit of the exoplanet WASP-121 b around its host star, as well as its tidal locking. The perspective shifts from a top-down view of the orbit to the alignment during observation. During the transit, it becomes apparent that at the beginning and the end of the passage, a portion of the planet's illuminated dayside appears as a narrow crescent. T. Müller (MPIA/HdA)



Downloads

mpia-pm_wasp121b_2026_animation1080p (8.3 MB)

mpia-pm_wasp121b_2026_animation4k 21.22 MB

mpia-pm_wasp121b_2026_fig1_de 455.47 kB

mpia-pm_wasp121b_2026_fig1_en 455.92 kB

mpia-pr_wasp-121b_mikal-evans_2022_teaser 1.6 MB


Friday, June 19, 2026

The Neutron Star That Doesn't Stop Spinning Up

A combined optical, H-alpha, and X-ray image of NGC 7793, indicating the position of the remarkably bright X-ray source P13. Image credit: NASA/CXC/ESO/VLT/NOAO/AURA/NSF/Univ of Strasbourg/M. Pakull et al. Download Image



Last week, NuSTAR performed the first of two planned observations of the ultraluminous X-ray source NGC 7793 P13. Like its fellow ultraluminous source M82 X-2, P13 is a pulsar, meaning that its extraordinary luminosity comes from extreme levels of accretion onto a tiny neutron star, and its spin period decreases over time as the accreting material spins it up by adding angular momentum. Every now and again, P13 appears to fade dramatically in brightness but, unusually for this class of objects, when it returns to its usual luminosity again its rate of spin has increased further rather than slowing down, suggesting that it doesn't stop spinning up even when it is in a faint state. Additionally, this binary system has an orbital period a little over 60 days long, with a variation in the ultraviolet emission that is very slightly out of sync with it, which might indicate some unusual interaction between different parts of the accreting system. These NuSTAR observations will continue to track its changing period over time, helping to piece together the shape of this system and the reasons for its strange behavior.

Author: Hannah Earnshaw (NuSTAR Project Scientist, Caltech)



Hunting for the Source of Superfast Electrons with NuSTAR

A multi-wavelength image of the supernova remnant shell of PWN G0.9+0.1, combining high-energy X-ray data from NuSTAR (green), low-energy X-ray data from XMM-Newton (blue), and radio data from MeeRKAT (red). The pulsar remnant of the supernova explosion is the compact X-ray source at the center of the image, while the brighter cnewsompact X-ray source to the lower right is unrelated. The radio data shows the shape of the nebula, as well as the fainter outer shell of the supernova remnant. Image credit: Brunelli et al. (2026)/MeerKAT (Heywood et al. 2022)/H. Earnshaw.
Download Image



Earth is continuously bombarded with cosmic rays—particles such as protons and electrons flying through space incredibly fast. The faster a particle travels, the more energy it has, and a small fraction of these cosmic rays have energies greater than a petaelectronvolt, or PeV. This is about the energy of a buzzing housefly, which might not seem like a lot, but it's all contained in one single, incredibly energetic electron moving at mind-blowing, relativistic speed. Accelerating electrons to such extreme speeds takes a cosmic-scale particle accelerator, which astronomers have nicknamed a 'PeVatron'. But what kind of astronomical source could be capable of such a feat?

Pulsar wind nebulae are some of the most fascinating objects in our Galaxy. They are created in the aftermath of a supernova, the explosion of a massive star at the end of its life when it has exhausted its fuel supply. Supernovae usually leave behind a compact remnant, either a black hole or a neutron star, and a rapidly spinning neutron star can appear to pulse, almost like a light house. This inspired the term “pulsar” to describe such remnants. A rapidly spinning pulsar will illuminate the extended bubble of outflowing material from the explosion, producing highly energetic particles accelerated by the strong magnetic field of the nebula. Pulsar wind nebulae can be detected at X-ray and even gamma-ray energies, making these cosmic powerhouses ideal candidates in the hunt for PeVatrons.

Dr. Kaya Mori of Columbia University is leading a large program with NASA’s NuSTAR X-ray satellite to hunt for PeVatrons in pulsar wind nebulae in our Galaxy. NuSTAR is the first satellite to focus high-energy X-ray photons, making it the most sensitive instrument for studying the Universe at X-ray energies above 10 keV, roughly the energy of X-ray machines you'd find at a hospital. One of the nebulae studied is this program is G0.9+0.1, a young supernova remnant in the Galactic Center. In a recent paper published in the Astrophysical Journal led by PhD student Giulia Brunelli at INAF Bologna, high-energy X-ray data from NuSTAR is combined with multiwavelength data from radio and gamma-ray observatories. Modeling these observations, the team determined that this pulsar wind nebula is very young—about 2,200 years old—and capable of accelerating electrons up to 2 PeV. This makes G0.9+0.1 a compelling PeVatron candidate, meaning that it—and perhaps other pulsar wind nebulae churning away in the Galactic Center—may be one of the objects responsible for some of the highest-energy particles arriving at Earth.



Thursday, June 18, 2026

How Galaxies Keep the Fuel Flowing

Montage of the NOEMA Telescopes and the detected massive disk galaxies with spiral arms and bars that actively transported cold gas inward. © Jean-Baptiste Jolly



Spiral Arms and Bars Drive Gas Transport at Cosmic Noon

Studies from the Infrared & Submillimeter Astronomy Group at the Max Planck Institute for Extraterrestrial Physics (MPE) using NOEMA and JWST reveal that during cosmic noon, massive disk galaxies with spiral arms and bars actively transported cold gas inward. This process sustained star formation by distributing gas efficiently across galactic disks, challenging previous views of early chaotic galaxies.

Galaxies need a continuous supply of cold gas to form new stars. This was especially true during "cosmic noon", roughly 8 to 10 billion years ago, when galaxies across the universe were forming stars at rates far exceeding those seen today. A key question in galaxy evolution is therefore how this gas was distributed within galaxies, and how it was transported from the outer disk into the regions where stars, bulges, and central black holes form and grow. Two new studies from the NOEMA3D survey, led by the Infrared-Submillimeter-Astronomy Group at the Max Planck Institute for Extraterrestrial Physics (MPE) and collaborators, now provide one of the clearest observational views yet of these processes.

Using the NOrthern Extended Millimeter Array (NOEMA), a radio interferometer located in the French Alps, the team obtained the deepest millimeter-wave observations to date of cold molecular gas — traced via CO emission — in ten massive, star-forming galaxies at redshifts z ~ 1.1–1.6. With integration times of typically more than 20 hours per galaxy, the NOEMA3D survey resolves both the distribution and kinematics of molecular gas on kiloparsec scales. These observations were combined with high-resolution infrared imaging from the James Webb Space Telescope (JWST), which reveals the underlying stellar structure of the same galaxies in unprecedented detail.

What JWST shows is itself striking: many of these distant systems are not the chaotic, merger-dominated objects that early galaxies were long assumed to be. Instead, they are well-ordered disk galaxies with clear spiral arms and, in four out of ten cases, bars. Structural features previously thought to be rare or absent at these redshifts.

The NOMA3D sample: 10 large massive galaxies on the star forming main sequence, at 1.1 < z < 1.6, showing clear spiral arms and for 4 of them bars. © Jean-Baptiste Jolly


G4_38065 is a massive spiral galaxy at z = 1.12. The velocity residuals, obtained by subtracting a model velocity map from the observed one, show clear patterns along the spiral arms which we interpret as inflowing gas refueling the galaxy. © Jean-Baptiste Jolly

Cold Gas Distribution Supports Star Formation Across Galactic Disks

The first study analyzes the kinematics of the molecular gas. All ten galaxies show ordered rotation consistent with a rotating disk. But after subtracting the best-fitting disk model, coherent velocity residuals remain in nearly every system, gas motions that cannot be accounted for by simple rotation alone. These residuals reach typical in-plane velocities of 50 to 100 km/s, substantially larger than comparable non-circular motions in nearby disk galaxies. Crucially, they are spatially correlated with the non-axisymmetric structures seen in the JWST images: spiral arms and bars. “For the first time, we can directly link spiral arms and bars to the motions of cold gas within galaxies,” says Jean-Baptiste Jolly. “This provides compelling evidence that these structures were already driving gas transport when the Universe was at the peak of its star-forming activity.”.

Spiral arms and bars are therefore not merely aesthetic features in galaxy images. They are dynamical structures that actively redistribute gas within the disk. When interpreted as radial inflows, the inferred molecular gas transport rates are often comparable to the galaxies' star formation rates, of order tens of solar masses per year. Such flows could move gas inward to feed central star formation, contribute to the growth of bulges, and potentially supply material to central supermassive black holes.

The companion study examines where the cold gas and dust are actually located. Comparing the spatial distributions of CO emission, neutral carbon [C I], dust continuum, stars, and star formation across the same ten galaxies, it finds that molecular gas and dust are generally extended over the full galactic disk, with sizes broadly comparable to the stellar component. This stands in sharp contrast to merger-driven compact starburst galaxies at similar redshifts, where dust and star formation are typically concentrated in small central regions. The resolved measurements further show that both the molecular gas fraction and the gas depletion time remain broadly flat across the disk, out to approximately twice the stellar effective radius. “The depth of the NOEMA observations allows us to trace the cold-gas reservoirs that fueled galaxy growth during cosmic noon,” says Jianhang Chen. “We can now see, in unprecedented detail, how galaxies sustained star formation across their disks over billions of years.”

Taken together, the two studies present a coherent picture of how massive disk galaxies sustained their star formation during a crucial epoch in cosmic history. Gas was present across the full disk; star formation proceeded with broadly similar efficiency at different radii. Internal structures, like spiral arms and bars, provided an efficient mechanism for moving gas inward. The NOEMA3D observations thereby connect the large-scale gas reservoirs of galaxies to the internal dynamical processes that regulate their growth.

These results also highlight the power of combining NOEMA and JWST. NOEMA provides the cold-gas kinematics and molecular gas maps; JWST reveals the stellar structures that shape the gas motion. Only by combining both telescopes can the link between morphology and gas dynamics be directly observed.

The broader implication is significant. By z ~ 1–2, massive star-forming galaxies already possessed organized disks with spiral arms and bars capable of driving significant gas transport. These structures likely played an important role in keeping galaxies on the star-forming main sequence and in shaping the buildup of disks, bulges, and black holes over cosmic time. The findings challenge the long-held view that early galaxies were predominantly turbulent and merger-driven. Many were already mature, well-ordered systems — not unlike our own Milky Way, but younger and considerably more active.




Contacts:

Dr. Jean-Baptiste Jolly
Postdoc Infrared-Group
Tel:
+49 89 30000-3335
Email: jbjolly@mpe.mpg.de
Max-Planck-Institut für extraterrestrische Physik, Garching

Dr. Jianhang Chen
Postdoc Infrared-Group
Tel:
+49 89 30000-3374
Email: jhchen@mpe.mpg.de
Max-Planck-Institut für extraterrestrische Physik, Garching



Original Publication

1. Chen, J., L. Tacconi, R. Genzel, R. Neri, K. Schuster, N. Förster Schreiber, J.-B. Jolly et al.
NOEMA3D: Spatially resolved dust, CO, and [C I] in massive star-forming main sequence galaxies at cosmic noon
A & A


DOI

2. Jolly, J.-B., L.J. Tacconi, R. Genzel, R. Neri, K. Schuster, J. Chen et al.
NOEMA3D: Resolving radial gas flows in disk galaxies at z ∼ 1.1 − 1.6 with high-resolution CO observations
A & A


Source | DOI



Further Information

Series: Research Highlight

The series “Research Highlight” features a scientific highlight of MPE researchers.







September 22, 2014
With the official inauguration of the first of six planned NOEMA antennas on 22 September, the Max Planck Society and its partner institution IRAM are taking a crucial step towards one of the largest Franco-German projects in astronomy: the expansion of the Plateau de Bure observatory in the French Alps into the most powerful and most sensitive millimetre radio telescope in the northern hemisphere. The scientists are hoping that this state of the art observatory will provide answers to questions about our origins and the formation of the universe.




April 08, 2026
New observations and simulations by a team of researchers led by MPE reveal that a massive binary star near our Galaxy’s center is responsible for creating a series enigmatic gas clouds — compact gas clumps that help feed the supermassive black hole Sagittarius A*.


ALMA and VLA Reveal a Vast Reservoir of Star-Forming Fuel in a Galaxy Near Cosmic Dawn

Image of the galaxy REBELS-25, taken by the Atacama Large Millimeter/submillimeter Array (ALMA).
Credit: ALMA (ESO/NAOJ/NRAO)/L. Rowland et al.

This illustration traces the universe’s evolution from the Big Bang to the present day, highlighting REBELS-25, a very distant galaxy seen during the Epoch of Reionization 13 billion years ago. New deep observations with the NSF VLA and ALMA reveal that REBELS-25 already had an enormous reservoir of cool molecular gas—the direct fuel for star formation—when the universe was just 700 million years old.




Highlights
  • Astronomers used ALMA and the NSF Very Large Array (VLA) to detect molecular gas in REBELS-25, a massive star-forming galaxy observed just 700 million years after the Big Bang.
  • The observations reveal a reservoir of roughly 100 billion solar masses of cool gas — the raw fuel for star formation — in one of the earliest and most distant galaxies ever studied in this way.
  • The VLA achieved the most distant detection to date of a key molecular gas tracer, while ALMA provided a detailed picture of the galaxy’s star-forming environment.



Astronomers have directly detected a vast reservoir of cool molecular gas in REBELS-25, a massive star-forming galaxy seen just 700 million years after the Big Bang. The discovery, made using the NSF Very Large Array (VLA) and the Atacama Large Millimeter/submillimeter Array (ALMA), provides a rare direct measurement of the star-forming fuel available to a galaxy in the early universe.

REBELS-25 is observed at a cosmic distance so vast that its light has been stretched – or redshifted – by the expansion of the universe to a redshift of z = 7.31. Astronomers see the galaxy as it was roughly 13 billion years ago, during the Epoch of Reionization — the period when the first stars and galaxies were transforming the young universe, just 5% of its current age.

Galaxies grow by turning gas into stars, and molecular gas is the primary raw material for that process. Until now, astronomers had strong indirect evidence that some early, massive galaxies contained large gas supplies, but directly detecting this material at such early cosmic times has been extremely difficult.

The team, led by Karin Cescon of Leiden University, used deep VLA observations to search for faint radio emission from carbon monoxide, or CO, a molecule commonly used to trace molecular gas. The VLA detected a low-energy CO transition that traces relatively cool gas – the most distant detection of this kind ever reported, and the first in a star-forming galaxy this early in cosmic history.

“Our results show galaxies just 700 million years after the Big Bang already contained large reservoirs of cold gas available for star formation,” said Karin Cescon, PhD student at Leiden University and lead author. “With these deep NSF VLA observations, we were able to overcome the observational challenges posed by the cosmic microwave background.”

That background – the ancient glow of radiation left over from the early universe – makes these observations especially challenging. At high redshift, it is warmer and brighter than it is today, like trying to spot a faint light against an increasingly bright sky. By accounting for this effect, the team derived a molecular gas mass of roughly 100 billion solar masses, a figure independently supported by modeling of both the CO and dust emission.

ALMA played a crucial role in completing the picture. Its observations detected higher-energy carbon monoxide emission and provided measurements of dust and ionized carbon, together revealing the gas’s physical conditions and confirming that the CO emission lines up spatially with other star-formation tracers. The results confirm that REBELS-25 is strongly gas-dominated, with a reservoir large enough to sustain vigorous star formation. They also suggest that ionized carbon emission, one of ALMA’s most powerful tools for studying early galaxies, remains a viable – if imperfect – tracer of molecular gas at these distances.

“This NSF VLA detection is an exciting sneak peek of what’s to come with the ngVLA,” noted Karin’s PhD advisor, Professor Jacqueline Hodge. “The ngVLA will allow us to find and study cool gas in many more young galaxies, including those at even earlier times. This will be crucial for understanding how the first galaxies formed and grew.”

The discovery helps explain how some early galaxies grew so large, so fast. The direct confirmation of such a massive gas reservoir – assembled when the universe was still in its infancy – places REBELS-25 among the most informative laboratories for studying how galaxies built up their ordinary matter, formed stars, and enriched the chemical content of their interstellar medium during the first billion years of cosmic history.}

Together, ALMA and current and future radio facilities are opening a new window onto the fuel supply of the earliest galaxies. Expanding the sample of galaxies with these kinds of measurements at z>7 will be essential for understanding how efficiently the first galaxies formed stars – and ultimately, how the universe came to look the way it does today.




Additional Information

This research is presented in “Direct detection of cool molecular gas in a star-forming galaxy at z = 7.31,” by K. Cescon et al., published in Monthly Notices of the Royal Astronomical Society.

The Atacama Large Millimeter/submillimeter Array (ALMA) data used in this study include observations from project 2021.1.01495.S. The VLA observations are available under project 21A-335.

This article is based on the original press release by the U.S. National Science Foundation National Radio Astronomy Observatory (NRAO), an ALMA partner on behalf of North America.

The Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is a partnership of the European Southern Observatory (ESO), the U.S. National Science Foundation (NSF) and the National Institutes of Natural Sciences (NINS) of Japan in cooperation with the Republic of Chile. ALMA is funded by ESO on behalf of its Member States, by NSF in cooperation with the National Research Council of Canada (NRC) and the National Science and Technology Council (NSTC) in Taiwan and by NINS in cooperation with the Academia Sinica (AS) in Taiwan and the Korea Astronomy and Space Science Institute (KASI).

ALMA construction and operations are led by ESO on behalf of its Member States; by the National Radio Astronomy Observatory (NRAO), managed by Associated Universities, Inc. (AUI), on behalf of North America; and by the National Astronomical Observatory of Japan (NAOJ) on behalf of East Asia. The Joint ALMA Observatory (JAO) provides the unified leadership and management of the construction, commissioning and operation of ALMA.



Contacts:

Nicolás Lira
Education and Public Outreach Officer
Joint ALMA Observatory, Santiago - Chile
Phone: +56 2 2467 6519
Cel:
+56 9 9445 7726
Email: nicolas.lira@alma.cl

Jill Malusky
Public Information Officer
NRAO
Phone
: +1 304-456-2236
Email: jmalusky@nrao.edu

Bárbara Ferreira
ESO Media Manager
Garching bei München, Germany
Phone:
 +49 89 3200 6670
Email: press@eso.org

Seiichiro Naito
NAOJ EPO Lead
Email:
naito.seiichiro@nao.ac.jp


Wednesday, June 17, 2026

'Crisis averted' as experts confirm universe's expansion IS accelerating

Studying Type Ia supernovae – violent, luminous white dwarf star explosions – led to the Nobel Prize-winning discovery that the universe's expansion is accelerating. This image combines data from four space telescopes to create a multi-wavelength view of all that remains of RCW 86, the oldest documented example of a supernova. Credit: X-ray: NASA/CXC/SAO & ESA; Infared: NASA/JPL-Caltech/B. Williams (NCSU)
Licence type: Attribution (CC BY 4.0)



Our universe's expansion is still accelerating despite recent claims suggesting otherwise, an international team of astrophysicists say.

They refuted a study published last year claiming the growth of the universe is slowing and insist there is no flaw in the widely-accepted theory that a mysterious force known as dark energy is driving the expanding cosmos.

The researchers, who include two Nobel Laureates and represent institutions worldwide, say the debate that followed last November’s revelations was the result of a scientific misunderstanding rather than a cosmic grenade threatening to blow apart everything we know about the universe.

Their paper has been published today in Monthly Notices of the Royal Astronomical Society.

It is a direct rebuttal of a study by a team of South Korean researchers that made the erroneous claim the universe's expansion may have entered a deceleration phase, caused by the influence of dark energy – which acts as a kind of anti-gravity – weakening over time.

"The previous and well accepted measurements were, in fact, fine and our current understanding of the fate of the universe remains robust," said lead author Dr Phil Wiseman, from the University of Southampton.

"Thankfully we have averted this crisis, but the mystery about why the rate of expansion of the universe is still accelerating remains.

"By proving our measurements are correct, we can get back to trying to understand what this dark energy actually is, rather than wondering if it exists at all."

The international team of researchers involved in the new study included Professor Adam Riess and Professor Brian Schmidt, who won the 2011 Nobel Prize in Physics alongside Professor Saul Perlmutter.

The trio studied Type Ia supernovae – violent, luminous white dwarf star explosions – and determined that more distant objects appeared to move faster, leading to their conclusion that the universe's expansion was accelerating.

This has been the globally-accepted theory ever since, although last year's research by the South Korean team threatened to upset the apple cart. It claimed that, as the universe aged, these supernovae had different maximum brightnesses, tricking astronomers into thinking the cosmos was accelerating when it was in fact slowing.

But the University of Southampton-led researchers found an error in how the age of these stars was estimated. They say the previous findings incorrectly assumed the age of a galaxy was the same as the age of the star that exploded.

The experts also said the South Korean paper failed to account for the mass of host galaxies, a standard correction used in modern cosmology to prove accuracy.

Professor Riess added: "Extraordinary claims require especially careful testing.

"What we find is that when we calibrate these supernovae, accounting for different host environments and populations, the evidence for cosmic acceleration remains remarkably consistent."

Professor Mark Sullivan, also from the University of Southampton, said challenging accepted theories and observations was fundamental to science.

"This is how progress is made. Although this idea did not turn out to be correct, it has opened up new ways of thinking about how supernovae explode and how we can measure dark energy more accurately," he added.

Fellow co-author Dr Brodie Popovic agreed. "We've recently been really focused on astrophysics of the explosions and how they impact cosmology," he said.

"This was a good opportunity to go back and go over all of our assumptions – it turns out, yes, we do understand this stuff and we're accounting for it in our cosmology measurement."




Media contacts:

Sam Tonkin
Royal Astronomical Society
Mob: +44 (0)7802 877 700
Email:
press@ras.ac.uk

James Haigh
University of Southampton
Mob: +44 (0)7584 368684
Email:
J.haigh@soton.ac.uk

Science contacts:

Dr Phil Wiseman
University of Southampton
Email:
P.S.Wiseman@soton.ac.uk

Dr Brodie Popovic
University of Southampton
Email:
B.A.Popovic@soton.ac.uk



Images & video

Supernova

Caption: Studying Type Ia supernovae – violent, luminous white dwarf star explosions – led to the Nobel Prize-winning discovery that the universe's expansion is accelerating. This image combines data from four space telescopes to create a multi-wavelength view of all that remains of RCW 86, the oldest documented example of a supernova. Credit: X-ray: NASA/CXC/SAO & ESA; Infared: NASA/JPL-Caltech/B. Williams (NCSU)

Type Ia supernova animation

Caption: This animation shows the explosion of a Type Ia supernova, where the white dwarf's gravity steals material away from a nearby stellar companion until it can no longer sustain its own weight and blows up. Credit: NASA/JPL-Caltech



Further information

The paper '
Still Accelerating: Type Ia supernova cosmology is robust to host galaxy age evolution' by Wiseman et al. has been published in >Monthly Notices of the Royal Astronomical Society. DOI: 10.1093/mnras/stag797.



Notes for editors

About the Royal Astronomical Society

The Royal Astronomical Society (RAS), founded in 1820, encourages and promotes the study of astronomy, solar-system science, geophysics and closely related branches of science.

The RAS organises scientific meetings, publishes international research journals, recognises outstanding achievements by the award of medals and prizes, maintains an extensive library, supports education through grants and outreach activities and represents UK astronomy nationally and internationally. Its more than 4,000 members (Fellows), a third based overseas, include scientific researchers in universities, observatories and laboratories as well as historians of astronomy and others.

The RAS accepts papers for its journals based on the principle of successful peer review, following which experts on the Editorial Boards accept the papers for publication. The Society issues press releases based on a similar principle, but the organisations and scientists concerned have overall responsibility for their content.

Keep up with the RAS on Instagram, Bluesky, LinkedIn, Facebook and YouTube.

Download the RAS Supermassive podcast

Submitted by Sam Tonkin on Thu, 11/06/2026 - 00:01


NASA Webb, Hubble Reveal History of Relic of Milky Way’s Formation

New observations from Webb combined with multiple observations from Hubble prove that Terzan 5 is a self-contained, self-enriching stellar system that contains up to four distinct star populations. It orbits within our Milky Way galaxy’s central bulge.Credit Image: NASA, ESA, CSA, STScI, Giorgia Zullo (University of Bologna), Francesco Ferraro (University of Bologna); Image Processing: Alyssa Pagan (STScI)

Yhis image of bulge fossil fragment Terzan 5 was captured by the James Webb and Hubble space telescopes. Webb’s data are from its NIRCam (Near-Infrared Camera) and Hubble’s from its Advanced Camera for Surveys (ACS). The image shows a scale bar, compass arrows, and color key for reference. The scale bar is labeled in light-years along the bottom, which is the distance that light travels in one Earth-year. (It takes two years for light to travel a distance equal to the length of the scale bar.) One light-year is equal to about 5.88 trillion miles or 9.46 trillion kilometers. The north and east compass arrows show the orientation of the image on the sky. Note that the relations hip between north and east on the sky (as seen from below) is flipped relative to direction arrows on a map of the ground (as seen from above). This image shows visible and near-infrared wavelengths of light that have been translated into visible-light colors. The color key shows which NIRCam and ACS filters were used when collecting the light. The color of each filter name is the visible-light color used to represent the infrared light that passes through that filter. Credit Image: NASA, ESA, CSA, STScI, Giorgia Zullo (University of Bologna), Francesco Ferraro (University of Bologna); Image Processing: Alyssa Pagan (STScI)

Zoom in to Terzan 5, a star cluster that lies within the crowded central region of our Milky Way galaxy known as the bulge. The scene starts with a ground-based image of our Milky Way bulge and zooms in on and circles Terzan 5, ending with the composite image of the star system from the James Webb and Hubble Space Telescopes. The Milky Way is shaped like a giant fried egg. The yolk in the middle is the galactic bulge, a crowded region packed with ancient stars of various masses and brightnesses. It’s also home to a number of globular star clusters that formed early in our galaxy’s history, which typically have only one ancient star population. In contrast, Terzan 5 was recently reclassified as a bulge fossil fragment because it has four generations of stars and has maintained its separate identity. Credit Video: NASA, ESA, CSA, Alyssa Pagan (STScI); Acknowledgment: ESO, Pan-STARRS, DSS2, Akira Fujii



Researchers using two of humanity’s most powerful observatories — NASA’s James Webb and Hubble Space Telescopes — have definitively shown that Terzan 5 is not a globular star cluster as it was once classified, offering new insight into how galaxies like our own form and evolve over time. A globular star cluster typically has only one ancient star population. New data not only confirms the existence of two distinct populations of stars in Terzan 5, but also provides evidence for two more recent rounds of star formation. Although located within the crowded bulge of our Milky Way, our galaxy’s central, spherical region of older stars, Terzan 5 was massive enough to maintain its separate identity while lighter weight systems spread out and mixed to form the bulge billions of years ago. It’s like a lump in an otherwise well-mixed cake batter.

“Webb’s new near-infrared observations, cross-referenced with Hubble’s archival observations, have given us a much clearer picture of the history of Terzan 5,” said Giorgia Zullo, who led the research and is a PhD student at the University of Bologna in Italy.

These results were presented at a press conference Tuesday at the 248th meeting of the American Astronomical Society in Pasadena, and were published in Astronomy & Astrophysics.

Four generations of stars

Discovered in 1968 by astronomer Azop Terzan, Terzan 5 resembles a globular cluster in many ways. However, in 2009 this system was discovered to harbor two distinct populations of stars. In 2016 Hubble provided the first estimate of their ages, showing that one formed roughly 12 billion years ago — as the Milky Way itself was assembling — and the other about 5 billion years ago, just before Earth started forming. This pointed to a more complex history than a typical globular cluster.

Studying Terzan 5 is complicated by its location in a region of our galaxy crowded with stars and heavily obscured by dust. This is where Webb stepped in. Its infrared view allowed the research team to peer through the dust and catalog many more stars, and fainter stars, than previous work. By measuring star colors and brightnesses, astronomers can classify them into populations of different ages and chemistries.

Webb was able to measure these key properties for every star within the field of view in the sky — both stars within Terzan 5 and unrelated foreground stars. To isolate the stars of Terzan 5, the team relied on the power and longevity of Hubble. The 12-year separation allowed the team to measure very small movements of individual stars, known as proper motions, to determine which stars belong to Terzan 5 and which are part of the Milky Way bulge.

By combining data from both Webb and Hubble, the researchers found strong evidence for two more stellar populations, one that formed 3.8 billion years ago and another only 2.5 billion years ago. They also were able to determine the ages of the previously known stellar populations with unprecedented precision, finding that they formed 12.5 billion and 4.7 billion years ago.

With the previously known two generations of stars, astronomers could not rule out the possibility that Terzan 5 interacted with another object, like a globular cluster or a giant molecular cloud, becoming enriched with new gas and dust that set off a second round of star formation. With four stellar generations, those explanations are ruled out.

Measurements of the stellar composition of Terzan 5 populations made at the W. M. Keck Observatory and European Southern Observatory’s Very Large Telescope also point toward very distinct populations. “Along with the ages of these populations, the cluster preserves a fossil record of progressive enrichment of heavy elements by supernovae,” said co-author R. Michael Rich, a research astronomer at the University of California, Los Angeles. Terzan 5 formed multiple generations of stars because it was able to retain the necessary raw materials. There is evidence of powerful supernova explosions in Terzan 5 that forged heavier elements that were swept up by subsequent generations of stars. In lighter weight systems, the force of the explosions themselves could have ejected the resulting elements as well as sweeping out leftover gas and dust. The progenitor of Terzan 5 had enough mass to retain those stars’ ejections, allowing new generations of stars to form over billions of years.

‘Bulge fossil fragment’

The results show that Terzan 5 is most likely the remnant of a much more massive stellar system that initially formed 12.5 billion years ago. Terzan 5 is extraordinary because it survived — and never merged or fully “mixed in” with the Milky Way’s bulge. “For some reason, this peculiar clump of stars formed separately from the bulge and was not destroyed as the bulge itself formed,” said Francesco R. Ferraro, a professor at the University of Bologna and principal investigator of the Webb observations. “Terzan 5 is what we now call a bulge fossil fragment because it resembles the primordial clumps that contributed to the formation of the bulge.”

To date, there’s one other known cosmic object like Terzan 5. Liller 1 was the second to be reclassified from a globular star cluster to a bulge fossil fragment. It also contains multiple generations of stars. There may be more objects like it. Between 40 to 50 additional globular clusters that orbit within the bulge will be examined by Ferraro’s team to determine if their stellar populations are all the same, like globular clusters, or have several generations, like bulge fossil fragments.




Details:

Last Updated: Jun 16, 2026
Location:
NASA Goddard Space Flight Center

Contact Media:

Laura Betz
NASA’s Goddard Space Flight Center
Greenbelt, Maryland

laura.e.betz@nasa.gov

Christine Pulliam
Space Telescope Science Institute
Baltimore, Maryland


Claire Blome
Space Telescope Science Institute
Baltimore, Maryland



Tuesday, June 16, 2026

NASA Webb Finds Strongest Evidence Yet for ‘Black Hole Stars’

While the primary purpose of NASA’s James Webb Space Telescope’s observations of galaxy cluster Abell S1063 was to look for a certain population of stars, scientists obtained a detailed spectrum of GLIMPSE-17775 from the dataset. This little red dot is located behind Abell S1063. Credit Image: NASA, ESA, CSA, Vasily Kokorev (UT Austin); Image Processing: Alyssa Pagan (STScI)

NASA’s James Webb Space Telescope captured the deepest spectrum to date of a little red dot. More than 40 spectral lines have been discerned from the data, many of which independently support the theory that GLIMPSE-17775 is a black hole enshrouded by a hot, dense gas cocoon. Credit Illustration: NASA, ESA, CSA, Vasily Kokorev (UT Austin); Designer: Leah Hustak (STScI)



The complex puzzle known as little red dots has become more complete since their initial discovery by NASA’s James Webb Space Telescope in 2022. Now a particular little red dot’s spectrum is helping connect many of the pieces.

A team of astronomers led by Vasily Kokorev at the University of Texas at Austin identified the lucky dot in question: GLIMPSE-17775. By carefully analyzing the dot’s spectrum captured by Webb — the deepest spectrum to date of a little red dot — the research team has identified multiple lines of evidence, all of which support the interpretation that GLIMPSE-17775 is a supermassive black hole enveloped in a dense cocoon of partially ionized gas, a model referred to as the BH* (black hole star) scenario. A paper describing the results was published today in The Astrophysical Journal.

“I think part of the scientific community is converging on a singular picture — that little red dots can be explained by black hole star models. But none of the previous little red dots have all of the pieces of evidence in the same place,” said Kokorev, lead author of the study. “With GLIMPSE-17775 we can test these models because of how deep and amazing this source’s spectrum is.”

Connecting puzzle pieces

Soon after Webb first began science operations, it discovered a new, mysterious type of object in the very early universe – abundant red objects that emerged about 600 million years after the big bang. Scientists have explored multiple explanations for these little red dots, including the black hole star scenario.

A set of fortunate circumstances brought about this new, elaborate spectrum of a little red dot. The little red dot that would come to be known as GLIMPSE-17775 was fortunately included in Webb’s imaging and spectroscopy efforts for a project that sought to look for Population III stars and faint galaxies in galaxy cluster Abell S1063. This little red dot is more distant than the galaxy cluster and magnified by gravitational lensing. (GLIMPSE-17775 has a cosmological redshift of 3.5, meaning it existed about 1.8 billion years after the big bang.)

While Webb provided a 30-hour spectrum of the little red dot, the effect of gravitational lensing made it equivalent to 80 hours of telescope time. This combination of Webb’s infrared sensitivity and nature’s own “magnifying glass” amplified the amount of detail that could be gleaned from GLIMPSE-17775. The result was more than 40 spectral lines from this small, red source, which is the most detailed little red dot spectrum to date.

“When we saw the spectrum for the first time, it was like having all the pieces of a puzzle scattered on the floor,” said Kokorev. “We picked up each piece of the puzzle, measured the lines, and started combining the different pieces into a mosaic. Maybe a few pieces looked like nothing at first, but then a couple of them came together, and we realized that there was something there.”

The spectroscopic data collected by Webb contains multiple lines of evidence that support the interpretation that little red dot GLIMPSE-17775 is a black hole star: a rapidly accreting, or growing, black hole enveloped in a dense gas cocoon, which is reprocessing the light emitted from near the black hole and producing the features seen in the spectrum.

Lines of evidence

Among the 40-plus lines that the team detected in GLIMPSE-17775’s spectrum were various independent indicators that all align with the BH* scenario. For example, the team found that many of the spectral lines, such as hydrogen, oxygen, and helium, do not fit a simple model of a rotating gas cloud. Instead, the best fit model includes a broadening effect known as electron scattering, a telltale sign that a dense, layered gas cocoon is enshrouding this source.

The strength and ratios of certain lines to each other, most notably the 16 iron lines that compose what the team has dubbed an “iron forest” and certain oxygen lines, require a high-energy source to produce them, like a rapidly accreting black hole. Additionally, astronomers noted the fluorescence and absorption of helium in the spectrum, both of which individually suggest that there is a dense medium enveloping a powerful source.

The BH* scenario not only fits GLIMPSE-17775; it also accounts for why most little red dots are faint in X-rays, since any such emission is likely absorbed by the dense gas cocoon.

One missing element of the GLIMPSE-17775 puzzle piece is the part of the spectrum that would reveal what’s known as a Balmer break, or a strong dip in the emitted light that’s a signature characteristic of little red dots. To build a more comprehensive understanding of this little red dot, the team incorporated ancillary data from two observing programs that used NASA’s Hubble Space Telescope: the Frontier Fields and BUFFALO (Beyond Ultra-deep Frontier Fields And Legacy Observations) programs.

The Webb and Hubble data together help explain why the Balmer break is weaker than what typically is found in other little red dots: A giant host galaxy is surrounding GLIMPSE-17775. Although a little red dot’s host galaxy is not something that has been usually seen at such scale before, it isn’t inconsistent with the dense gas cocoon model. The black hole star model of little red dots attributes excess blue light to stars in the host galaxy.

When Webb first discovered little red dots, some researchers thought these objects had “broken cosmology,” unsure how galaxies could have grown so big so quickly in the early universe to account for all this light coming from their stars. However, the team believes the GLIMPSE-17775 puzzle piece fits nicely in the existing framework of the universe’s evolutionary history, because black hole masses don’t need to be as high in order to explain the broad emission lines.

“Everything fits, nothing is broken, and I think that makes the puzzle that is our universe even better,” said Kokorev. “Looking ahead, I’m eager to dive deeper and learn about what is powering the central engines of little red dots. While we think it’s a black hole, there are some other interesting theories being proposed, which is exciting. Maybe in a year or two, we’ll have the final answer to what powers these sources.”

The James Webb Space Telescope is the world’s premier space science observatory. Webb is solving mysteries in our solar system, looking beyond to distant worlds around other stars, and probing the mysterious structures and origins of our universe and our place in it. Webb is an international program led by NASA with its partners, ESA (European Space Agency) and CSA (Canadian Space Agency).




Details:

Last Updated: Jun 10, 2026

Location:
NASA Goddard Space Flight Center

Contact Media:

Laura Betz
NASA’s Goddard Space Flight Center
Greenbelt, Maryland

laura.e.betz@nasa.gov

Abigail Major
Space Telescope Science Institute
Baltimore, Maryland


Christine Pulliam
Space Telescope Science Institute
Baltimore, Maryland




Monday, June 15, 2026

Webb unveils young stars across every stage of formation

An area inside a star-forming molecular cloud. The background is covered with layers of gas and dust in blue, green and yellowish colours. Thicker clumps of cold dust, dark brown to black, block out light completely. Stars lie among and atop the clouds, from small orange ones to large white or blue ones. Waves and streams of glowing whitish gas are created by jets from protostars colliding with the surrounding material. Credit: ESA/Webb, NASA & CSA, T. Megeath, M. Zamani (ESA/Webb) - Acknowledgement: M. H. Özsaraç



For this NASA/ESA/CSA James Webb Space Telescope Picture of the Month we return to the constellation Orion (the Hunter), a location familiar to Webb. This area of the sky is replete with star-forming clouds that make up a complex hundreds of light-years across. We find ourselves in the giant molecular cloud Orion A, of which the familiar Orion Nebula (also known as M42) is just a part; Webb has taken both close-up and wide-angle looks at M42 before.

The target of these observations, however, requires us to look behind the Orion Nebula. Behind the stars, gas and dust of M42 is a long, massive filament of cold gas and dust called (somewhat confusingly) the Orion Molecular Clouds, which is divided into four parts, OMC-1 through OMC-4. OMC-1 sits immediately behind M42, to the north are OMC-2 and OMC-3, and OMC-4 lies to the south.

This image shows just a small, northern portion of OMC-2, located 1280 light-years from Earth and a little north of the Orion Nebula. Every stage of star formation — from the youngest stellar embryos, to protoplanetary discs, to newly-minted pre-main sequence stars — is contained within just this scene, which stretches 150 light-years across. The intense star-forming activity has produced an impressive display of billowing outflows and sparkling stars atop swirling layers of gas and dark, obscuring clouds.

Molecular clouds such as OMC-2 are vast clumps of gas much more dense than the rest of interstellar space. This density allows complex molecules to form, protected from the radiation given off by other stars, and it means that gravity can cause the cloud to collapse and form stars. The earliest stage of this process is a protostar - a growing star that is being fed gas from the surrounding cloud through a spinning disc of gas. As gas falls onto the protostar, it heats up, powering the glow of the protostar. The immense amount of energy acquired during this process is unleashed in fierce jets of gas from the poles of the star, frequently seen as twin glowing outflows that mark the location of a protostar.

The abundance of protostars forming here in OMC-2 has created many spectacular outflows, large and small. Jets emitted from the young stars form high-speed shockwaves that sweep through the dense material around them; where the shockwaves are impacting the gas, it heats up and glows brightly, creating sharp ridges. Zoom in to observe the fine details in these shockwaves, as well as spot the smaller outflows from younger protostars. See if you can spot the location of hidden protostars, still so deeply obscured by their dusty cradles that they can’t be seen directly, by following outflows! Compare these very young protostars to the most evolved examples: the large, bright stars which have cleared away the clouds that surrounded them and now illuminate OMC-2.

Webb’s Near-Infrared Camera (NIRCam) was used to capture this view of OMC-2. The thick gas and dust in and around the Orion Nebula blocks any light coming from OMC-2 at visible wavelengths, and the clouds in OMC-2 itself obscure the protostars that astronomers really want to find. Only in the infrared do we see these protostars begin to shine out from their cocoons of dust. In many places, the cold dust is so dense that it absorbs all or almost all light, creating dark globules. Orange, brown and some of the red colours mark warmer dust that absorbs some light and emits some of its own. The yellow to green gradient is largely emission from polycyclic aromatic hydrocarbons (PAHs), while light from stars and protostars scattered by dust grains is seen here primarily as blue and cyan hazes. Gas heated by the outflows creates the detailed, glowing red ridges.

The data was collected in observing programme #5804, which aims to study the star formation in OMC-2 and its immediate neighbour, OMC-3. Since these molecular clouds are so near to Earth, they are excellent laboratories to learn about the earliest stages of stellar evolution. Astronomers will use the data from Webb to investigate how the many outflows affect star formation in the two regions, how the ultraviolet emission from the young stars impacts chemistry in the circumstellar discs which one day will form planets, and how gas and dust accretes onto the tens of protostars in the region.




Links