Stunning new images from the NASA/ESA/CSA James Webb Space Telescope showcase two young stars, Tau 042021 (left) and Oph-163131 (right), encircled by planet-forming disks. This unique perspective provides invaluable insights into the formation of worlds similar to ours.
Composite images of protoplanetary disks Tau 042021 (left) and Oph 163131 (right). Image credits: NASA / ESA / CSA / Webb / Hubble / ALMA / ESO / NAOJ / NRAO / G. Duchêne / M. Villenave.
“Protoplanetary disks emerge around newly formed stars,” stated Webb astronomers.
“As gas clumps collapse within larger molecular clouds, a thick disk of unused gas and dust orbits the newborn star.”
“This dust gradually collides and coalesces, forming planetesimals that can develop into planets over time.”
“Some planetesimals that don’t evolve into full-fledged planets remain as asteroids or comets orbiting the star.”
“Gas not consumed in this process will eventually be expelled by the star’s radiation over millions of years, leading to the disappearance of the protoplanetary disk.”
“This phenomenon explains how our solar system formed, shaping the asteroids, comets, gas giants, and terrestrial planets we recognize today.”
By studying other protoplanetary disks from earlier epochs, we can enhance our understanding of how solar system formation occurs and how various planets throughout the galaxy came into being.
The captivating images of protoplanetary disks Tau 042021 and Oph 163131—designated as 2MASS J04202144+2813491 and 2MASS J16313124-2426281—were captured using Webb’s NIRCam and MIRI instruments.
Tau 042021 lies approximately 450 light-years away in the constellation Taurus, while Oph 163131 is about 480 light-years distant in the constellation Ophiuchus.
“What distinguishes these objects is the orientation of their disks towards Webb’s perspective,” the astronomers explained.
“This alignment blocks most of the bright light from the central young star, allowing the fine dust in the disk to be illuminated by reflected starlight, creating a nebula above and below the disk.”
“The resulting images resemble colorful floating tops in space, providing not only a breathtaking view but also critical data for understanding the organization of planet-forming disks.”
“The dust distribution within and surrounding the disk profoundly influences how and where planets form.”
Astronomers have utilized the Near Infrared Spectrometer (NIRSpec) on the NASA/ESA/CSA James Webb Space Telescope to analyze the atmosphere of TOI-5205b, an extrasolar gas giant orbiting a dim red dwarf star. These groundbreaking observations reveal that the atmosphere is surprisingly deficient in heavy elements, raising intriguing questions regarding the formation and evolution of such “forbidden” alien worlds.
The Jupiter-sized planet TOI-5205b has a surface temperature of 737 K and orbits at a distance of 0.02 astronomical units from its parent star, TOI-5205. Image credit: Sci.News.
TOI-5205b is a short-period gas giant with only 1.03 times the radius and 1.08 times the mass of Jupiter, completing its orbit in just 1.63 days.
Discovered in 2022, this planet orbits the TOI-5205, an M4-type star with approximately 39% of the Sun’s size and mass.
The system, also known as TIC 419411415, is located about 283 light-years away in the constellation Vorissa.
“Short-period Jupiter-mass planets are among the first exoplanets found around Sun-like main-sequence stars, yet their formation processes are still not fully understood,” explained Dr. Caleb Cañas from NASA’s Goddard Space Flight Center.
“The increasing number of short-period giant exoplanets around M dwarfs adds further complexity to gas giant planet formation theories.”
“These worlds are challenging to form through nuclear accretion due to the low disk masses and longer orbital time scales of M dwarfs, which hinder the efficient creation of massive planetary cores necessary for runaway gas accretion.”
“These planets exemplify an extreme formation regime for mid-to-late M-type dwarfs since the significant planet-to-star mass ratio demands a core mass exceeding the estimated dust mass of the protoplanetary disk.”
Astronomers used Webb’s NIRSpec to observe three separate transits of TOI-5205b.
To their surprise, they discovered that the concentration of heavy elements in the planet’s atmosphere, relative to hydrogen, is lower than found in the gas giants of our solar system, including Jupiter. Remarkably, it is even less metallic than its host star.
This finding sets TOI-5205b apart from all other studied giant planets.
Furthermore, the observations revealed the presence of methane and hydrogen sulfide in the planet’s atmosphere, corroborating previous findings.
To better understand their results, the researchers employed an advanced model of the planet’s interior, predicting that TOI-5205b’s overall composition is about 100 times richer in metals than its atmosphere.
“We observed a significantly lower metallicity than what models predicted for the planet’s bulk composition, based on measurements of its mass and radius,” noted Dr. Shubham Kanodia of Carnegie Science.
“This suggests that heavy elements migrated to the interior during formation, indicating that the interior and atmosphere are not currently mixing.”
“In essence, our findings imply that the planet’s atmosphere is notably carbon-rich and oxygen-poor.”
For more information on these findings, check out the latest publication in Astronomy Magazine.
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Caleb I. Cañas et al. 2026. GEMS JWST: TOI-5205b’s transmission spectroscopy reveals significant contamination of the star and a metal-poor atmosphere. A.J. 171, 260; doi: 10.3847/1538-3881/ae4976
By integrating infrared observations from the NASA/ESA/CSA James Webb Space Telescope with visible-light images from the NASA/ESA Hubble Space Telescope, astronomers have unveiled a stunning new perspective of Saturn, showcasing its atmospheric bands, storms, and brilliantly reflective rings.
Comparative images of Saturn in infrared (Webb, left) and visible light (Hubble, right). Image credits: NASA/ESA/CSA/STScI/A. Simon, NASA-GSFC/M. Wong, University of California/J. DePasquale, STScI.
A newly released image of Saturn emphasizes the dynamic features of the gas giant’s vibrant atmosphere.
Webb’s observations reveal a long-lived jet stream, referred to as a “ribbon wave,” traversing the northern mid-latitudes, influenced by atmospheric waves that are difficult to detect otherwise.
A small dot just below the jet stream indicates the remnants of the 2011-2012 “Spring Storm.”
Additionally, several storms scattered across Saturn’s southern hemisphere are evident in the Webb image.
The astronomers noted, “All these atmospheric formations are shaped by powerful winds and waves beneath the visible cloud layer, making Saturn an ideal natural laboratory for studying fluid dynamics under extreme conditions.”
“The iconic hexagonal jet stream at Saturn’s north pole, discovered by NASA’s Voyager spacecraft in 1981, displays some sharp edges that are also faintly visible in both images.”
“It continues to be one of the solar system’s most intriguing weather phenomena.”
“Its persistence over decades underscores the stability of particular atmospheric processes on giant planets.”
“These famous hexagons are likely to be observed in high resolution for the last time until the 2040s, when Arctic winters shift into 15 years of darkness.”
Recent Webb observations indicate that Saturn’s poles appear a distinct gray-green, emitting light at approximately 4.3 microns.
The researchers suggest, “This unique coloration might arise from a layer of high-altitude aerosol in Saturn’s atmosphere, scattering light differently in those latitudes.”
“Another possibility includes auroral activity, wherein charged particles interacting with the planet’s magnetic field produce a glowing luminescence near the poles.”
In Webb’s images, Saturn’s rings are notably bright due to their composition of highly reflective water ice.
The scientists explained, “Both images depict the ring’s surface illuminated by the sun; however, the Hubble image shows less illumination, creating a shadow beneath the planet.”
“Subtle features of the ring, like spokes and patterns in the B ring (the thick central region), exhibit differences between the two observatories.”
“The outermost ring, known as the F ring, appears thin and sharply defined in the Webb image, but glows only faintly in the Hubble image.”
“Saturn’s orbit around the sun, combined with Earth’s position in its annual path, dictates the varied angles from which we observe Saturn’s face and rings.”
“These observations from 2024, captured 14 weeks apart, indicate that Earth is moving away from northern summer and approaching the 2025 equinox.”
“As Saturn transitions into the southern spring and late southern summer of the 2030s, both Hubble and Webb will increasingly enhance their views of its hemisphere.”
NASA/ESA/CSA’s James Webb Space Telescope has meticulously scanned Jupiter’s circumference, documenting the mesmerizing aurora as it came into view. This dynamic spectacle arises from charged particles traveling along magnetic field lines and colliding with the planet’s ionosphere, creating a stunning glow. Utilizing Webb’s Near Infrared Spectrometer (NIRSpec), researchers captured an intriguing feature of Jupiter’s aurora, known as an auroral footprint. These bright luminescent patterns result from interactions between Jupiter’s Galilean moons—Io, Europa, Ganymede, and Callisto—and the surrounding cosmic environment. Planetary scientists leveraged NIRSpec data to analyze the physical characteristics of the auroral footprints of Jupiter’s innermost moons, Io and Europa, measuring local temperature and ionospheric density in near-infrared light. They uncovered a previously unseen low-temperature structure centered around Io’s bright spots, characterized by an exceptionally high density, likely caused by significant electron flow impacting the upper atmosphere.
Webb’s first spectral measurements of Io and Europa’s auroral footprints reveal unprecedented changes in physical characteristics linked to electron collisions in Jupiter’s atmosphere. Image credits: NASA / ESA / CSA / Webb / NIRCam / Jupiter ERS Team / Judy Schmidt / Katie L. Knowles, Northumbria University.
“Previously, these emissions were measured in ultraviolet and infrared wavelengths solely by their brightness,” stated lead author Dr. Katie Knowles, a student at Northumbria University.
“For the first time, we can describe the physical properties of an auroral footprint: the upper atmosphere’s temperature and ion density, which have never been documented before.”
Unlike Earth’s auroras, which primarily result from solar wind, Jupiter’s auroras are influenced by its four major Galilean moons, which generate their own “mini auroras.”
Jupiter’s immense magnetic field rotates every 10 hours, channeling charged particles. In contrast, its moons orbit much more slowly; for instance, Io takes approximately 42.5 hours to complete one orbit.
“The moons continuously interact with the planet’s magnetic field and plasma, driving high-energy particles down magnetic field lines into the atmosphere, forming auroral footprints that trace their orbits around Jupiter,” Knowles explained.
“Jupiter’s auroras are the most potent and persistent within the solar system.”
“Our observations with Webb offer an unprecedented glimpse into how Jupiter’s moons directly affect the upper atmosphere.”
During a 22-hour observation span in September 2023, Webb meticulously scanned around Jupiter’s edge, tracking auroras as they appeared.
Interestingly, they captured auroral footprints originating from Io and Europa, which did not exhibit the typical characteristics of Jupiter’s main auroras, which are generally hotter and denser.
Instead, researchers discovered a cold spot within Io’s auroral footprint that exhibited significantly lower temperatures and unusually high density compared to typical expectations.
Io is notably the most volcanically active celestial body in the solar system, ejecting approximately 1,000 kilograms of material into space every second, thus replenishing the dense plasma enveloping Jupiter.
This ejected material becomes ionized, forming a toroidal cloud around Jupiter known as the Ioplasma torus.
As Io moves through this complex environment, it generates powerful electrical currents that contribute to the brightest regions in Jupiter’s auroras.
The team found that these auroral footprints contained trihydrogen cation densities three times greater than those present in Jupiter’s primary auroras, with some localized areas experiencing density fluctuations of up to 45 times.
“We observed rapid fluctuations in both temperature and density within Io’s auroral footprint occurring within mere minutes,” Knowles noted.
“This indicates that the flow of high-energy electrons impacting Jupiter’s atmosphere is changing at an incredibly fast pace.”
The recorded temperature at the cold spot was only 538 degrees Celsius (265 degrees Fahrenheit), compared to 766 K (493 degrees Celsius or 919 degrees Fahrenheit) in the surrounding aurora.
This cold spot also contained three times the density of material found in Jupiter’s main aurora.
This discovery could have implications extending well beyond Jupiter, posing intriguing questions about other planetary systems.
Saturn’s moon Enceladus similarly generates auroral footprints on Earth, leading scientists to suspect that comparable phenomena may occur there too.
“This research opens up new avenues for studying not only Jupiter and its Galilean moons but also other giant planets and their satellite systems,” Knowles remarked.
“We are witnessing Jupiter’s atmosphere responding to its moons in real-time, providing insights into processes that may occur throughout our solar system and beyond.”
“This phenomenon was only observed in one of five snapshots, prompting questions: how frequently does this occur? Does it vary? How does it change under different conditions?”
The study is published in the journal Geophysical Research Letters.
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Katie L. Knowles et al. 2026. Short-term fluctuations in Jupiter’s moon footprint discovered by JWST. Geophysical Research Letters 53 (5): e2025GL118553; doi: 10.1029/2025GL118553
Astronomers utilizing the NASA/ESA/CSA James Webb Space Telescope have made a groundbreaking discovery: they have identified a nearby supernova, specifically a red supergiant star, that was obscured by a thick layer of dust and remained invisible to prior observatories.
This striking image combines observations from both the James Webb Space Telescope and Hubble, focusing on spiral galaxy NGC 1637. It captures the evolutionary stages of the red supergiant star and reveals its transformation following the supernova event SN 2025pht. Image credit: NASA/ESA/CSA/STScI/C. Kilpatrick, Northwestern/A. Suresh, Northwestern/J. DePasquale, STScI.
The supernova event, designated SN 2025pht, was first identified in NGC 1637 on June 29, 2025.
In response, astronomers dedicated substantial resources to investigating this supernova.
However, Northwestern University’s astronomer Charlie Kilpatrick and his team chose to explore archival data, analyzing pre-supernova images to determine which star exploded.
A 2024 image of NGC 1637 captured with Webb’s MIRI (Mid-Infrared Instrument) and NIRCam (Near-Infrared Camera) highlights a distinct red supergiant star positioned precisely where SN 2025pht is currently visible.
“We anticipated this moment, hoping for a supernova to occur in a galaxy that Webb was already monitoring,” stated Dr. Kilpatrick.
“By integrating the Hubble and Webb datasets, we unveiled the star’s complete characteristics for the first time.”
“This red supergiant represents the dustiest star we have ever observed transitioning into a supernova,” noted Aswin Suresh, a graduate student at Northwestern University.
This dust anomaly may help solve a persistent mystery in astronomy: the absence of certain red supergiant stars.
Astronomers expect that the most massive stars should explode as the brightest supernovae, making their identification in pre-explosion images straightforward. However, this has not been the case.
One possible explanation is that these massive, aging stars are often heavily surrounded by dust, rendering their light invisible.
Observations from Webb regarding SN 2025pht seem to support this hypothesis.
“I have advocated for this interpretation, but I didn’t expect the outcome to be as pronounced as in the case of SN 2025pht,” commented Dr. Kilpatrick.
“This might clarify the absence of these heavier supergiant stars, as they tend to be engulfed in more dust.”
The team also discovered that the dust enveloping the star is likely rich in carbon—an unexpected finding, as silicate-rich dust is typically anticipated in these environments.
They speculate that this carbon may have been released from the star’s core shortly before the explosion.
“Mid-infrared observations were crucial in identifying the specific type of dust present,” Suresh added.
For more in-depth details on this discovery, view the team’s research paper published in October 2025 in the Astrophysics Journal Letter.
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Charles D. Kilpatrick et al. 2025. Type II SN 2025pht of NGC 1637: Detection of a red supergiant star with carbon-rich circumstellar dust, marking the first acknowledgment of a supernova progenitor star via JWST. APJL 992, L10; doi: 10.3847/2041-8213/ae04de
For the first time, astronomers utilizing NASA/ESA/CSA’s James Webb Space Telescope have detected hydrogen sulfide gas in the atmospheres of three gas giant exoplanets orbiting the star HR 8799, located in the Pegasus constellation and approximately 30 million years old. This significant finding indicates that the sulfur originated from solid materials in the protoplanetary disk where the planets formed.
Artist’s rendering of the HR 8799 planetary system during its early evolutionary stages, featuring a gas and dust disk around planet HR 8799c (Dunlap Institute for Astronomy and Astrophysics/Media Farm).
HR 8799 lies about 129 light-years away from Earth and hosts a substantial debris disk alongside four super-Jupiter planets (HR 8799b, c, d, and e).
The smallest of these gas giants is five times the mass of Jupiter, while the largest exceeds ten times Jupiter’s mass.
These exoplanets reside far from their star, with the nearest planet being situated 15 times farther from its star than Earth is from the Sun.
Unlike many exoplanets discovered through indirect data analysis, the planets in the HR 8799 system can be directly observed using ground-based telescopes.
“HR 8799 is unique as the only imaged stellar system containing four gas giant planets, although other systems have one or two larger companion stars with formation processes yet to be understood,” explained Dr. Jean-Baptiste Ruffio, an astronomer at the University of California, San Diego.
Utilizing Webb’s unprecedented sensitivity, Dr. Ruffio and colleagues conducted detailed studies of the chemical compositions of the planets HR 8799c, d, and e.
Due to the faintness of these planets—approximately 10,000 times dimmer than their host star—the researchers developed innovative data analysis techniques to isolate weak signals in the Webb data.
“Prior studies of carbon and oxygen on these planets, conducted from Earth, could originate from ice, solids, or gas in the disk, making them unreliable indicators of solid material,” noted Dr. Jerry Xuan, a postdoctoral researcher at UCLA and Caltech.
“In contrast, sulfur is distinctive because, away from the star, these planets should harbor sulfur in solid form.”
“It’s impossible for these planets to accumulate sulfur in gaseous form.”
The identification of hydrogen sulfide indicates that sulfur was gathered in solid form from materials that existed in the disk surrounding the star during the planets’ formation. These solids were assimilated as the planet formed, and the intense heat of the young planet’s core and atmosphere caused them to vaporize into the sulfur gas present today.
Notably, the sulfur-to-hydrogen and carbon-to-oxygen-to-hydrogen ratios on these planets are significantly higher than those found in stars, hinting at a distinct planetary composition.
This puzzling consistency in the enrichment of heavy elements is also observed in Jupiter and Saturn.
“The uniform enhancement of carbon, oxygen, sulfur, and nitrogen in Jupiter is complex, but observing this in another star system suggests a universal trend in planet formation, where planets naturally integrate heavy elements in nearly equal proportions,” Dr. Xuan commented.
The findings could advance the search for Earth-like exoplanets.
“The techniques used here allow for the optical and spectral separation of planets from stars, enabling detailed studies of exoplanets located far from Earth,” Dr. Xuan stated.
“While currently limited to gas giants, as telescope technology and instruments improve, scientists aim to apply these methods to Earth-like planets.”
“Locating an Earth analog is the ultimate goal of exoplanet research; however, achieving this may take decades.”
“Nevertheless, within the next 20 to 30 years, we might obtain the first spectra of an Earth-like planet, allowing us to investigate biological markers such as oxygen and ozone in its atmosphere.”
J.B. Ruffio et al. “Jupiter-like homogeneous metal enrichment in a system of multiple giant exoplanets,” Nat Astron published online on February 9, 2026. doi: 10.1038/s41550-026-02783-z
NASA/ESA/CSA’s James Webb Space Telescope has made groundbreaking observations of a galaxy featuring gaseous “tentacles” within a galaxy cluster at a redshift of 1.156. This remarkable finding allows us to observe the universe as it was approximately 8.5 billion years ago.
This web image highlights the jellyfish galaxy COSMOS2020-635829, with dashed circles marking four out-of-plane sources in its tail. Image credit: Roberts et al., doi: 10.3847/1538-4357/ae3824.
“The jellyfish galaxy derives its name from the long, tentacle-like streams trailing behind it,” explained Dr. Ian Roberts of the University of Waterloo and his team.
“As it travels quickly through the hot, dense galaxy cluster, the gas within the cluster acts like a powerful wind, pushing the jellyfish galaxy’s gas backward and forming a visible trail.”
“This phenomenon is referred to as ram pressure stripping.”
The research team discovered a new jellyfish galaxy through deep-space data captured by the Webb Telescope.
Named COSMOS2020-635829, this galaxy resides in the COSMOS field, a well-explored area of the sky studied extensively by various telescopes.
“While sifting through vast amounts of data from this thoroughly investigated region, we aimed to uncover previously undocumented jellyfish galaxies,” Dr. Roberts noted.
“Early in our analysis, we stumbled upon a distant, uncharted jellyfish galaxy that piqued our interest.”
COSMOS2020-635829 exhibits a typical galactic disk coupled with bright blue nodes in its trajectory, indicative of very young stars.
The ages of these stars suggest they formed in gas trails stripped from their host galaxy, a behavior characteristic of jellyfish galaxies.
Insights from this study challenge established beliefs regarding the conditions in deep space during that era.
Scientists previously thought the galaxy cluster was still in formation and that ram pressure stripping was a rare occurrence.
Dr. Roberts and his co-authors identified three further discoveries that could reshape our understanding of the cosmos.
“The first discovery indicates that the cluster environment was already intense enough to strip galaxies away. Second, the cluster can significantly alter galaxy properties sooner than anticipated,” Roberts explained.
“Finally, these dynamics might play a crucial role in forming the populations of inactive galaxies we observe in today’s galaxy clusters.”
“These findings offer pivotal insight into the evolution of galaxies in the early universe.”
For more details on this discovery, check out the paper published in the Astrophysical Journal.
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Ian D. Roberts et al. 2026. JWST reveals candidate jellyfish galaxy at z = 1.156. APJ 998, 285; doi: 10.3847/1538-4357/ae3824
Astronomers have successfully mapped the vertical structure of Uranus’ ionosphere for the very first time, uncovering unexpected temperature peaks, a decline in ion density, and enigmatic dark regions influenced by the planet’s unique magnetic field. These groundbreaking findings, achieved through nearly a full day of observations using the NIRSpec instrument aboard NASA/ESA/CSA’s James Webb Space Telescope, confirm a decades-long cooling trend in Uranus’ upper atmosphere and offer an unprecedented look at how this ice giant interacts with its surrounding space differently than other celestial bodies in our solar system.
Tiranti et al. mapped the vertical structure of Uranus’s upper atmosphere, revealing variations in temperature and charged particles across different heights. Image credits: NASA / ESA / CSA / Webb / STScI / P. Tiranti / H. Melin / M. Zamani, ESA & Webb.
Uranus’s upper atmosphere remains one of the least understood components in our solar system, despite its critical role in elucidating the interactions between the giant planet and its space environment.
Astronomer Paola Tiranti from Northumbria University and her team dedicated nearly an entire day to observing Uranus with Webb’s NIRSpec instrument.
They successfully measured the vertical structure of the ionosphere, the electrically charged layer of the atmosphere where auroras occur.
“This is the first time we’ve been able to visualize Uranus’s upper atmosphere in three dimensions,” Tiranti remarked.
“Utilizing Webb’s sensitivity, we can investigate how energy migrates upward through the planet’s atmosphere, even observing the effects of polarized magnetic fields.”
Measurements revealed temperature peaks at approximately 3,000 to 4,000 km above the surface, while ion density peaked around 1,000 km, significantly weaker than previously modeled predictions.
Webb also identified two bright bands of auroral emission located near Uranus’s magnetic poles, along with an unexpected area of depleted emission and density, likely tied to the planet’s unusual magnetic field geometry.
These discoveries confirm a long-term cooling trend in Uranus’ upper atmosphere and highlight new structures shaped by its magnetic environment.
These findings offer critical benchmarks for future missions and enhance our comprehension of how giant planets—both within and beyond our solar system—maintain the energy balance in their upper atmospheres.
“Uranus’ magnetosphere is one of the most peculiar in the solar system,” Tiranti emphasized.
“Its tilt and offset from the planet’s rotational axis cause its auroras to be distributed in a complex fashion across the surface.”
“Webb has provided insights into how deeply these effects penetrate into the atmosphere.”
“By detailing Uranus’s vertical structure so thoroughly, Webb aids in our understanding of the energy balance of the ice giant.”
“This represents a significant step toward characterizing giant planets beyond our solar system.”
For further details, refer to the results published in the journal Geophysical Research Letters.
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Paola I. Tiranti et al. 2026. JWST uncovers the vertical structure of Uranus’ ionosphere. Geophysical Research Letters 53 (4): e2025GL119304; doi: 10.1029/2025GL119304
Astronomers utilizing the NASA/ESA/CSA James Webb Space Telescope have identified an extraordinary presence of small gas-phase hydrocarbons—such as benzene, triacetylene, diacetylene, acetylene, methane, and methyl radicals—within the concealed core of the ultra-bright infrared galaxy IRAS 07251-0248.
Hydrocarbons are influential in shaping the chemistry of the interstellar medium. However, definite observational constraints on their enrichment and relationship with carbonaceous particles and polycyclic aromatic hydrocarbons remain elusive. García Bernete et al. report Webb infrared observations of the Local Ultraluminous Infrared Galaxy (ULIRG) IRAS 07251-0248, revealing extragalactic detections of small gas-phase hydrocarbons. Image credit: García-Bernete et al., doi: 10.1038/s41550-025-02750-0.
The core of IRAS 07251-0248 (also known as 2MASS J07273756-0254540) is obscured by significant amounts of gas and dust.
This dense material absorbs most radiation emitted by the central supermassive black hole, complicating studies with traditional telescopes.
However, the infrared spectrum can penetrate this dust, providing unique insights about these regions and illuminating vital chemical processes in this heavily obscured core.
Dr. Ismael García Bernete and his team employed spectroscopic observations using Webb’s NIRSpec and MIRI instruments, covering wavelengths from 3 to 28 microns.
These observations reveal chemical signatures of gas-phase molecules alongside signatures from ice and dust particles.
These data empowered astronomers to characterize the abundance and temperature of various chemical species within the core of this concealed galaxy.
Remarkably, they discovered an exceptionally high abundance of small organic molecules such as benzene, methane, acetylene, diacetylene, and triacetylene—the first such detections outside our Milky Way, including the methyl radical.
Additionally, substantial amounts of solid molecular materials, including carbonaceous particles and water ice, were identified.
“We uncovered unexpected chemical complexity, showcasing abundances far exceeding current theoretical models,” stated Dr. García Bernete, an astronomer at the Astrobiology Center.
“This suggests a continuous source of carbon within these galactic nuclei, fueling this rich chemical network.”
“These molecules may serve as vital building blocks for complex organic chemistry, relevant to processes that pertain to life.”
Professor Dimitra Rigopoulou from the University of Oxford remarked, “Small organic molecules may not exist in living cells, yet they could play a pivotal role in prebiotic chemistry—a crucial step toward forming amino acids and nucleotides.”
These findings were published in a recent issue of Nature Astronomy.
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I. Garcia-Bernete et al. Abundant hydrocarbons within buried galactic nuclei with evidence of processing of carbonaceous particles and polycyclic aromatic hydrocarbons. Nat Astron, published online on February 8, 2026. doi: 10.1038/s41550-025-02750-0
New research led by Rohan Naidu from the Massachusetts Institute of Technology’s Kavli Institute for Astrophysics and Space Studies reveals that the galaxy MoM-z14 existed a mere 280 million years after the Big Bang.
This image depicts MoM-z14, a galaxy that emerged shortly after the Big Bang. Image credit: NASA/ESA/CSA/STScI/Rohan Naidu, MIT/Joseph DePasquale, STScI.
“Thanks to the Webb Space Telescope, humanity can now explore deeper into the universe than ever before, challenging our previous predictions,” stated Dr. Naidu.
Using Webb’s NIRSpec instrument, Dr. Naidu and colleagues confirmed that MoM-z14 possesses a cosmological redshift of 14.44. This indicates that for approximately 13.5 billion years—out of the universe’s estimated age of 13.8 billion years—the light has been elongated and “shifted” to red wavelengths as it travels through space.
Dr. Pascal Oesch from the University of Geneva emphasized, “While we can estimate a galaxy’s distance from images, it’s crucial to follow up with detailed spectroscopy to accurately understand what we are observing.”
MoM-z14 is part of an increasing number of unexpectedly bright galaxies in the early universe, outnumbering theoretical predictions before the Webb’s launch by 100 times.
“The disparity between theoretical models and observational data regarding the early universe is expanding, prompting intriguing questions for future exploration,” said Dr. Jacob Shen, a postdoctoral researcher at MIT.
One potential avenue for research lies in the oldest stars within the Milky Way, where a small number exhibit high nitrogen levels, mirroring some of Webb’s observations of early galaxies, including MoM-z14.
“We can examine ancient stars in our galaxy like fossils from the early universe, and thanks to Webb, we have direct insights into galaxies at that epoch, revealing shared features such as unusual nitrogen enrichment,” remarked Dr. Naidu.
Interestingly, MoM-z14 emerged only 280 million years post-Big Bang, a brief time span that shouldn’t have allowed for ample nitrogen production from stellar generations.
Researchers propose that the dense early universe environment might have facilitated the formation of supermassive stars, capable of producing more nitrogen than any stars observed nearby.
Additionally, MoM-z14 appears to be clearing the surrounding universe of the dense primordial hydrogen fog characteristic of early cosmic history.
The Webb was designed to chart this cleansing period known as reionization, where early stars broke through dense hydrogen gas and emitted enough high-energy light to reach us today.
MoM-z14 serves as a key clue in mapping the reionization timeline, a task previously unattainable before Webb unveiled this epoch of the universe.
“We require further information to understand the early universe better. More detailed observations from Webb and additional galaxies will help identify common features, and NASA’s next Nancy Grace Roman Space Telescope is expected to contribute significantly,” noted Yijia Li, a graduate student at Penn State.
“This is an exhilarating time as the Webb reveals the universe’s earliest epochs, showcasing the vastness of uncharted territory still to explore.”
Rohan P. Naidu et al. 2026. Cosmic Miracle: Confirmed in JWST, an extremely bright galaxy with zspec=14.44. Open Astrophysics Journal in press. arXiv: 2505.11263
Utilizing the ultra-sharp images from the NASA/ESA/CSA James Webb Space Telescope, astronomers have successfully crafted a highly detailed, wide-area mass map of the Universe. This groundbreaking map reveals the intricate interweaving of dark matter and ordinary matter, stretching from the filaments of galaxies to the dense clusters. Developed as part of the COSMOS-Web survey, this new map boasts more than double the resolution of previous efforts and delves deeper into the early universe’s evolution.
This web image shows about 800,000 galaxies, overlaid with a dark matter map in blue. Image credit: NASA / STScI / J. DePasquale / A. Pagan.
Dark matter constitutes roughly 85% of the universe’s total matter, yet it’s challenging to detect since it neither emits nor absorbs light, rendering it invisible to standard telescopes.
However, its gravitational influence alters the trajectory of light from far-off galaxies.
By examining subtle distortions in the shapes of numerous distant galaxies, scientists can ascertain how this unseen mass is distributed, irrespective of its nature.
When compared with known luminous structures, researchers can pinpoint the locations of dark matter.
Previous mass maps generated using the NASA/ESA Hubble Space Telescope and other observatories suffered from limited resolution, sensitivity, and area coverage, restricting their views to only the largest cosmic structures.
Dr. Diana Scognamiglio from NASA’s Jet Propulsion Laboratory and her team harnessed Webb’s imaging capabilities to analyze the shapes of approximately 250,000 galaxies, reconstructing the most detailed mass map of a contiguous universe region to date.
“This is the most extensive dark matter map produced in conjunction with Webb, boasting clarity unmatched by any prior dark matter maps from other observatories,” stated Dr. Scognamiglio.
“Previously, we only glimpsed blurred images of dark matter.”
“With Webb’s extraordinary resolution, we can now observe the universe’s invisible framework in unprecedented detail.”
This new map uncovers substantial galaxy clusters along with intricate networks of dark filamentary bridges and low-mass galaxies, too faint or too distant to be spotted by conventional telescopes.
These formations align with major cosmological models, suggesting that galaxies emerge at dense points between the dark matter filaments spreading throughout the universe.
Dr. Gavin Leroy, an astronomer at Durham University, remarked: “By illustrating dark matter with unparalleled precision, our map demonstrates how the unseen elements of the universe shaped visible matter, facilitating the creation of galaxies, stars, and ultimately, life itself.”
“This map highlights the crucial role of dark matter, the universe’s true architect, which gradually organizes the structures we observe through our telescopes.”
Professor Richard Massey of Durham University added, “Wherever normal matter exists in the universe today, dark matter is also present.”
“Every second, billions of dark matter particles pass through your body. They are harmless and continue on their paths unnoticed.”
“However, the entire cloud of dark matter surrounding the Milky Way possesses enough gravity to keep our galaxy intact. Without dark matter, the Milky Way would disintegrate.”
For more information, refer to the published results in this week’s edition of Nature Astronomy.
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D. Scognamiglio et al. Ultra-high resolution map of (dark) matter. Nat Astron published online on January 26, 2026. doi: 10.1038/s41550-025-02763-9
Webb astronomers have unveiled a breathtaking image captured by the NASA/ESA/CSA James Webb Space Telescope, showcasing MACS J1149.5+2223 (MACS J1149), a cosmic collection of hundreds of galaxies situated about 5 billion light-years from Earth in the constellation Leo. The latest images not only highlight the cluster’s brilliant galaxies but also illustrate how their immense gravitational forces uniquely affect the fabric of space-time.
The stunning image of the galaxy cluster MACS J1149.5+2223. Image credits: NASA / ESA / CSA / Webb / C. Willott, National Research Council Canada / R. Tripodi, INAF-Astronomical Observatory of Rome.
The latest Webb image of MACS J1149 dramatically showcases light from background galaxies, which is bent and magnified in a remarkable phenomenon known as gravitational lensing. This creates elongated arcs and distorted shapes, revealing the mass of both clusters.
“The immense gravity of this galaxy cluster does more than hold the galaxies adrift in the universe,” the Webb astronomers explained in a statement.
“As light from galaxies beyond the cluster travels toward our telescope over billions of years, its trajectory through space-time is warped by the gravitational forces of the intervening galaxies.”
This gravitational lensing effect is evident throughout the image of MACS J1149, with galaxies appearing stretched into narrow streaks and others morphing into unusual shapes. A prime example of gravitational lensing can be seen near the image’s center, just below the prominent white galaxy.
In this area, a galaxy with spiral arms has been transformed into a shape resembling a pink jellyfish. This peculiar galaxy once harbored the farthest single star ever identified and a supernova that appeared four times simultaneously.
“This program employs Webb’s advanced instruments to explore the evolution of low-mass galaxies in the early Universe, shedding light on their star formation, dust content, and chemical makeup,” the astronomers stated.
The data collected will also assist researchers in studying the epoch of reionization, when the first stars and galaxies illuminated the universe, mapping mass distributions in galaxy clusters, and understanding how star formation diminishes within cluster environments.
Astronomers utilizing NASA’s James Webb Space Telescope have captured the most detailed infrared images of the Circus Galaxy’s core, making it one of the closest known active galaxies to the Milky Way. Webb’s observations indicate that much of the hot dust surrounding supermassive black holes in galaxies is being drawn into the black holes themselves, contrary to previous models that suggested powerful outward streams.
The Hubble image showcases the Circinus Galaxy, a spiral galaxy located approximately 13 million light-years away in the southern constellation Circinus. A close-up from Webb reveals the core’s glow in infrared light, highlighting the intricate features obscured by dust. Image credits: NASA / ESA / CSA / Webb / Hubble / Enrique Lopez-Rodriguez, University of South Carolina / Deepashri Thatte, STScI / Alyssa Pagan, NOIRLab / CTIO at STScI / NSF.
The Circus Galaxy, also known as ESO 97-G13 or LEDA 50779, is situated about 13 million light-years from Earth, nestled south of the constellation Circinus. This galaxy has fascinated astronomers due to its center being enveloped in a dense cloud of gas and dust.
Traditional ground-based telescopes have faced challenges in isolating regions near the central black hole, where matter spirals inwards and emanates intense infrared light. However, Webb’s state-of-the-art technology enabled Dr. Julien Girard and his team at the Space Telescope Science Institute to pierce through this dust veil with extraordinary clarity.
This remarkable breakthrough was achieved by employing Webb’s Near-Infrared Imager and Slitless Spectrometer (NIRISS) in a specialized high-contrast mode known as aperture masking interferometry.
This innovative technique transforms the instrument into a compact interferometer, merging light captured through various small apertures to generate precise interference patterns.
By examining these patterns, astronomers were able to reconstruct a finely detailed image of the Circus Galaxy’s central engine, revealing that the majority of infrared radiation originates from the donut-shaped torus of dust encircling the black hole, rather than from materials being ejected outward.
Dr. Girard remarked, “This is the first instance where Webb’s high-contrast mode has been employed to observe an extragalactic source.” He expressed hope that their findings will inspire fellow astronomers to leverage aperture masking interferometry to study faint but relatively small, dusty structures surrounding bright objects.
The supermassive black hole remains active, continuously consuming surrounding matter. Gas and dust conglomerate in a torus around the black hole, forming a rotating accretion disk as material spirals inward. This disk generates heat through friction, releasing light across diverse wavelengths, including infrared.
New data from Webb indicate that most of the infrared emissions near the center of the Circus Galaxy stem from the innermost region of this dusty torus, challenging previous assumptions that outflow dominated emissions.
This pioneering technique lays the groundwork for more profound investigations of black holes in other galaxies. By applying Webb’s high-contrast imaging to subsequent targets, researchers aim to establish a broader catalog of emission patterns, which could ascertain whether the behavior observed in the Circus Galaxy is typical among active galactic nuclei or a distinct case.
Their discoveries not only present a clearer perspective on the feeding mechanisms of black holes but also underscore the escalating power of interferometry in space-based astronomy.
More observations are forthcoming, as Webb continues to redefine what can be observed from the most concealed regions of the universe.
Dr. Enrique López Rodríguez, an astronomer at the University of South Carolina, noted, “We will likely require a statistical sample of a dozen or two dozen black holes to comprehend how the mass of the accretion disk and its outflow correlate with the black hole’s power.”
For further details, refer to the results published in today’s edition of Nature Communications.
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E. Lopez Rodriguez et al. 2026. JWST interferometry imaging reveals a dusty torus obscuring the Circinus Galaxy’s supermassive black hole. Nat Commun 17, 42; doi: 10.1038/s41467-025-66010-5
PSR J2322-2650b, an enigmatic Jupiter-mass exoplanet orbiting the millisecond pulsar PSR J2322-2650, exhibits an unusual atmosphere primarily composed of helium and carbon, presenting a new phenomenon never observed before.
Artist’s concept of PSR J2322-2650b. Image credit: NASA/ESA/CSA/Ralf Crawford, STScI.
“This discovery was completely unexpected,” stated Dr. Peter Gao, an astronomer at the Carnegie Earth and Planetary Institute.
“After analyzing the data, our immediate reaction was, ‘What on Earth is this?’ It contradicted all our expectations.”
“This system is fascinating because we can see the planet lit by its star, yet the star itself is invisible,” explained Dr. Maya Bereznay, a candidate at Stanford University.
“This allows us to capture exceptionally clear spectra, enabling us to study the system in a much more detailed way than we typically do with other exoplanets.”
“This planet orbits a truly unique star—it’s as massive as the sun but as compact as a city,” remarked Dr. Michael Chan from the University of Chicago.
“This represents a new kind of planetary atmosphere never before observed. Instead of the typical molecules like water, methane, and carbon dioxide, we detected carbon molecules, particularly C.3 and C2.”
Molecular carbon is exceedingly rare; at temperatures exceeding 2,000 degrees Celsius, carbon typically bonds with other atoms in the atmosphere.
Out of around 150 planets studied both within and beyond our solar system, none have showcased detectable molecular carbon.
“Did this form as a typical planet? Certainly not, due to its starkly different composition,” Dr. Zhang stated.
“Could it have been created by stripping the outer layers of a star, like what happens in a conventional black widow system? Likely not, as nuclear processes do not yield pure carbon.”
“Envisioning how this drastically carbon-rich composition came to be is quite challenging. All known formation theories seem to be excluded.”
The authors suggest an intriguing phenomenon that might occur in such a unique atmosphere.
“As the companion star cools, the carbon and oxygen mixture within begins to crystallize,” explained Roger Romani, an astronomer at Stanford University and the Kavli Institute for Particle Astrophysics and Cosmology.
“What we observed was pure carbon crystals rising to the surface and blending with the helium.”
“Yet, there must be a mechanism to prevent the oxygen and nitrogen from mixing in. This is where the mystery deepens.”
“However, it’s intriguing not to have all the answers. I’m eager to uncover more about the peculiarities of this atmosphere. Solving these enigmas will be remarkable.”
For more information, refer to the paper published in Astrophysics Journal Letter.
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michael chan et al. 2025. The carbon-rich atmosphere of a windy pulsar planet. APJL 995, L64; doi: 10.3847/2041-8213/ae157c
Recent findings from the NASA/ESA/CSA James Webb Space Telescope indicate that TOI-561b is enveloped by a dense gas blanket above its global magma ocean.
This artist’s concept illustrates TOI-561b and its stars. Image credit: NASA/ESA/CSA/Ralf Crawford, STScI.
TOI-561 is a luminous star located 280.5 light-years away in the constellation Sextant.
This star is approximately 10 billion years old and has about 80% of the Sun’s mass and size.
It is also known as TYC 243-1528-1 and belongs to a rare category of stars known as the galaxy’s thick disk stars.
TOI-561 hosts at least three exoplanets (TOI-561b, c, and d) and is among the oldest and most metal-poor planetary systems discovered in the Milky Way.
The inner planet, TOI-561b, is classified as a super-Earth with an orbital period of just 0.44 days.
Its mass and radius are 3.2 and 1.45 times that of Earth, with a density of 5.5 g/cm³, consistent with its rocky composition.
“What distinguishes this planet is its notably low density,” remarked Dr. Johanna Teske, an astronomer at the Carnegie Institution for Science.
“It is not significantly bloated, yet it is less dense than would be expected for an Earth-like composition.”
One potential reason for the low density, astronomers suggest, is that it may possess a relatively small iron core and a mantle composed of less dense rock compared to Earth’s.
“TOI-561b is exceptional among ultrashort-period planets as it orbits a substantially older (twice the age of the Sun), iron-poor star within the thick disk region of the Milky Way,” Teske added.
“It likely formed under a vastly different chemical environment than the planets in our solar system.”
Researchers also posit that TOI-561b is encircled by a thick atmosphere, possibly giving it an apparent size larger than its actual one.
Although small planets subjected to intense stellar radiation for billions of years are not anticipated to possess atmospheres, some are exhibiting characteristics beyond mere rocky surfaces or lava.
To investigate the possibility of TOI-561b having an atmosphere, they employed: Webb’s NIRSpec (near infrared spectrometer). This device measures the planet’s daytime temperature through near-infrared brightness.
The technique tracks the decrease in brightness of the star-planet system as the planet transits behind its star, similar to methods used for detecting atmospheres of rocky worlds like the TRAPPIST-1 system.
If TOI-561b were devoid of an atmosphere and comprised entirely of bare rock, daytime temperatures would approach 2,700 degrees Celsius (4,900 degrees Fahrenheit).
However, NIRSpec observations indicate that the planet’s dayside temperature is closer to 1,800 degrees Celsius (3,200 degrees Fahrenheit), indicating it remains extremely hot, but considerably cooler than anticipated.
Emission spectra captured by Webb in May 2024 illustrate the brightness of different wavelengths of near-infrared radiation emitted by the exoplanet TOI-561b. Image credits: NASA / ESA / CSA / Ralf Crawford, STScI / Johanna Teske, Carnegie Institute for Science, Earth and Planets / Anjali Piette, University of Birmingham / Tim Lichtenberg, Groningen / Nicole Wallack, Carnegie Institute for Science, Earth and Planets.
To interpret these findings, the researchers evaluated multiple scenarios.
A magma ocean could redistribute some heat; however, without an atmosphere, the night side is likely solid, limiting heat transfer from the day side.
There may be a thin layer of rock vapor above the magma ocean’s surface, but this alone could cause less significant cooling than observed.
Dr. Anjali Piette, an astronomer at the University of Birmingham, stated, “We truly require a thick atmosphere rich in volatiles to account for all observations.”
“Strong winds could transport heat to the night side while cooling the day side.”
“Gases such as water vapor absorb some wavelengths of near-infrared radiation emitted from the planet’s surface before reaching the atmosphere.”
“Bright silicate clouds might also reflect starlight and cool the atmosphere.”
Although Webb’s findings provide compelling evidence of an atmosphere, the question persists: How can such a small planet exposed to intense radiation maintain an atmosphere, especially one of such significance? Some gas is likely escaping into space, but possibly at a lower rate than expected.
“We believe there is a balance between the magma ocean and the atmosphere,” said Tim Lichtenberg, an astronomer at the University of Groningen.
“As gases escape from the Earth to form the atmosphere, the magma ocean simultaneously reabsorbs them.”
“To account for these observations, this planet would need to be far richer in volatile materials than Earth. It resembles a wet lava ball.”
Findings from this study will be published in today’s Astrophysics Journal Letter.
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Johanna K. Teske et al. 2025. A dense volatile atmosphere over the ultra-hot super-earth TOI-561b. APJL 995, L39; doi: 10.3847/2041-8213/ae0a4c
Astronomers utilizing the NASA/ESA/CSA James Webb Space Telescope have identified a supernova explosion linked to gamma-ray burst event GRB 250314A at a redshift of 7.3, occurring when the universe was merely 730 million years old. The previous record-holder for supernovae was observed when the universe reached 1.8 billion years. This discovery is detailed in two papers published in the journal Astronomy and Astrophysics.
Webb identified the origin of the blinding flashes known as gamma-ray bursts. This particular gamma-ray burst exploded when the universe was merely 730 million years old. Image credit: NASA / ESA / CSA / STScI / A. Levan, IMAPP / A. Pagan, STScI.
“Only Mr. Webb has directly demonstrated that this light is from a collapsing massive star,” stated Dr. Andrew Levan, an astronomer at Radboud University and the University of Warwick, and lead author of one of the papers.
“This observation suggests that we can utilize Webb to detect individual stars from a time when the universe was just 5% of its current age.”
Whereas gamma-ray bursts typically last from seconds to minutes, supernovae rapidly brighten over several weeks before slowly dimming.
In contrast, the supernova linked to GRB 250314A took months to brighten.
Because this explosion occurred so early in the universe’s history, its light continued to evolve as the universe expanded over billions of years.
As the light stretches, the duration for events to unfold also lengthens.
Webb’s observations were intentionally made three and a half months after the closure of the GRB 250314A event, as it was expected that the supernova would be at its brightest at this time.
“Webb provided the rapid and sensitive follow-up we so desperately needed,” remarked Dr. Benjamin Schneider, an astronomer at the Marseille Institute of Astrophysics.
Gamma-ray bursts are exceedingly rare. Bursts lasting only a few seconds may originate from the collision of two neutron stars or a neutron star and a black hole.
Longer bursts, like this one, which lasted around 10 seconds, are often linked to the explosions of massive stars.
On March 14, 2025, the SVOM mission—a joint Franco-Chinese telescope launched in 2024 designed to spot fleeting events—will detect gamma-ray bursts from extremely distant sources.
Within an hour and a half, NASA’s Neil Gehrels Swift Observatory had pinpointed the X-ray source in the sky, facilitating follow-up observations to measure the distance of the web.
Eleven hours later, Nordic optical telescopes revealed the afterglow of the infrared gamma-ray burst, indicating that gamma rays may correspond to very distant objects.
Four hours later, ESO’s Very Large Telescope estimated that the object existed 730 million years after the Big Bang.
“Only a handful of gamma-ray bursts have been identified in the first billion years of the universe and merely a few in the last 50 years,” Levan noted.
“This remarkable event is exceedingly rare and thrilling.”
As this is the oldest and most distant supernova ever identified, researchers compared it to nearby modern supernovae, finding surprising similarities.
Why? Little is still understood about the early billion years of the universe.
Early stars likely lacked heavy elements, were massive, and had brief lifespans.
They also existed during the reionization era, when intergalactic gas was almost opaque to high-energy light.
“Dr. Webb has demonstrated that this supernova resembles modern supernovae very closely,” stated Professor Nial Tanvir from the University of Leicester.
“Webb’s findings indicate that this distant galaxy is akin to other galaxies of the same epoch,” commented Dr. Emeric Le Floch, an astronomer at CEA Paris-Saclay.
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AJ Levan et al. 2025. JWST reveals a supernova following a gamma-ray burst at z ≃ 7.3. A&A 704, L8; doi: 10.1051/0004-6361/202556581
B. Cordier et al. 2025. SVOM GRB 250314A at z ≃ 7.3: Exploding star in the reionization era. A&A 704, L7; doi: 10.1051/0004-6361/202556580
By utilizing highly precise spectroscopic observations from the Near Infrared Imager and Slitless Spectrometer (NIRISS) on board the NASA/ESA/CSA James Webb Space Telescope, astronomers have identified helium gas escaping from WASP-107b, a super-Neptunian exoplanet located in the Virgo constellation, approximately 212 light-years away.
Artist’s impression of exoplanet WASP-107b. Image credit: University of Geneva / NCCR PlanetS / Thibaut Roger.
WASP-107 is an active K-type main-sequence star situated roughly 212 light-years away in the Virgo constellation.
Discovered in 2017, WASP-107b is among the least dense known exoplanets, categorized by astrophysicists as a “superpuff” or “cotton candy” planet.
This exoplanet has an orbit significantly closer to its star than Earth is to the Sun, completing its orbit every 5.7 days.
While this planet features the coldest atmosphere recorded for an exoplanet, at 500 degrees Celsius (932 degrees Fahrenheit), it remains much hotter than Earth.
This elevated temperature results from tidal heating linked to its slightly elliptical orbit, which may help explain how WASP-107b can expand without invoking extreme formation theories.
“A planet’s atmosphere can sometimes dissipate into space,” explained Yann Carteret, an astronomer at the University of Geneva, alongside colleagues.
“On Earth, we lose just over 3 kg of matter (primarily hydrogen) every second.”
“This phenomenon, known as atmospheric escape, is especially significant for astronomers studying exoplanets in close proximity to their stars. Such planets experience intense heating, making them particularly vulnerable to this effect.”
With data from Webb’s NIRISS instrument, astronomers observed a substantial flow of helium within WASP-107b’s exosphere.
This helium cloud partially obscures the star’s light even before the planet transits in front of the star.
“Our atmospheric escape model indicates a helium flow both in front of and behind the planet, extending nearly 10 times the planet’s radius in the direction of its orbit,” Carteret stated.
Alongside helium, astronomers confirmed the existence of water and various trace chemicals (including carbon monoxide, carbon dioxide, and ammonia) in WASP-107b’s atmosphere.
These findings provide essential insights for piecing together the history of their formation and migration.
The research suggests that the planet initially formed at a greater distance from its current orbit before drifting closer to its star, which may account for the thickening of its atmosphere and gas loss.
“Atmospheric escape on Earth is too weak to have a significant impact on our planet,” noted Vincent Boullier, an astronomer at the University of Geneva.
“However, it could explain the absence of water on Venus, which is nearby.”
“Thus, understanding the mechanisms involved in this process is crucial, as it could erode the atmospheres of certain rocky exoplanets.”
Details of these findings were published in the journal Nature Astronomy.
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V. Krishnamurthy et al. Continuum helium absorption from both the leading and trailing atmospheric tails of WASP-107b. Nat Astron, published online on December 1, 2025. doi: 10.1038/s41550-025-02710-8
By utilizing data from the NASA/ESA/CSA James Webb Space Telescope along with ESO’s Very Large Telescope (VLT), two separate teams of astronomers have captured mid-infrared images of a system featuring four intricate spirals of dust encircling a pair of aging Wolf-Rayet stars located in a system known as Apep (2XMM J160050.7-514245).
Webb’s mid-infrared images reveal four coiled dust shells surrounding two Wolf-Rayet stars known as Apep. Image credits: NASA / ESA / CSA / STScI / California Institute of Technology Yeahuo Han / Macquarie University Ryan White / Alyssa Pagan, STScI.
Wolf-Rayet stars represent a rare class of massive binary stars where the universe’s earliest carbon is formed.
There are estimated to be only around 1,000 of these stars in the Milky Way galaxy, which contains hundreds of billions of stars in total.
Among the multiple Wolf-Rayet binaries observed so far, the Apep system stands out as the sole example of having two such Wolf-Rayet stars within our galaxy.
In a recent study, astronomer Ryan White from Macquarie University and his team set out to refine the orbital characteristics of the Wolf-Rayet stars in the Apep system.
They integrated precise ring position measurements from the Webb images with the shell’s expansion rate obtained over eight years of VLT observations.
“This is a unique system with a very extended orbital period,” White mentioned.
“The next longest orbit for a dusty Wolf-Rayet binary is roughly 30 years, while most orbits tend to span between 2 and 10 years.”
One of the team’s papers was published concurrently in the Astrophysical Journal alongside another study led by astronomer Yinuo Han from the California Institute of Technology.
“Observing the new Webb data felt like stepping into a dark room and flipping on a light switch. Everything became visible,” Dr. Han remarked.
“Dust is abundant throughout the Webb image, and telescope observations indicate that much of it is fragmenting into repeating and predictable structures.”
Webb’s observations yielded unprecedented images. It produced a clear mid-infrared image revealing a system of four swirling spirals of dust, each expanding in a consistent pattern. Ground-based telescopes had only identified one shell prior to Webb’s discoveries.
By merging Webb imagery with several years of VLT data, they refined the orbital frequency of the star pairs to every 190 years.
Within this remarkably lengthy orbit, the star approaches closely for 25 years, enabling dust formation.
Additionally, Webb’s observations confirmed the existence of three stars that are gravitationally bound to each other in this system.
The dust expelled by the two Wolf-Rayet stars is being cleaved by a third star, a massive supergiant, which creates holes in the dust cloud emanating from its expansive orbit.
“Dr. Webb has provided us with the ‘smoking gun’ evidence to confirm that a third star is gravitationally linked to this system,” Dr. Han noted.
Researchers were aware of this third star since VLT observed its brightest inner shell in 2018, but Webb’s findings helped refine the geometric model and reinforced the connection.
“We unraveled several mysteries with Webb,” Dr. Han added.
“The lingering mystery remains the precise distance from Earth to the star, which will necessitate further observations.”
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Ryan MT White et al. 2025. Snake eating its own tail: Dust destruction of the Apep impact wind nebula. APJ 994, 121; doi: 10.3847/1538-4357/adfbe1
Han Yinuo et al. 2025. JWST reveals the formation and evolution of dust in APEP, a binary star with colliding winds. APJ 994, 122; doi: 10.3847/1538-4357/ae12e5
Utilizing the Near Infrared Camera (NIRCam) aboard the NASA/ESA/CSA James Webb Space Telescope, astronomers have obtained fresh images of the Red Spider Nebula, a prominent planetary nebula located in the constellation Sagittarius.
This web image showcases the Red Spider Nebula. Image credit: NASA/ESA/CSA/Webb/JH Kastner, Rochester Institute of Technology.
The Red Spider Nebula was identified by American astronomer and physicist Edward Charles Pickering on July 15, 1882.
This astronomical object is located roughly 12,420 light-years away from Earth in the constellation Sagittarius.
Commonly referred to as NGC 6537, ESO 590-1, and IRAS 18021-1950, it has an approximate radius of 3.6 light-years.
“Planetary nebulae, like the Red Spider Nebula, form when average stars, such as our Sun, reach the conclusion of their life cycles,” Webb astronomers noted in a statement.
“As these stars expand into cool red giants, they shed their outer layers, propelling them into space and revealing their hot white cores.”
“Ultraviolet radiation from the central star ionizes the ejected material, causing it to emit light.”
“The planetary nebula stage of a star’s lifecycle is both spectacular and brief, lasting only tens of thousands of years.”
“This Webb image displays the central star of the Red Spider Nebula, which shines slightly brighter than the dusty gas web surrounding it.”
In optical images from telescopes such as Hubble, the stars appear faintly blue.
However, in the NIRCam image, it appears red. Webb’s sensitive near-infrared capabilities have unveiled the hot dust enveloping the central star.
“This hot dust likely orbits the central star in a disk-like formation,” the astronomers explained.
“Even though only one star is visible at the nebula’s center, a concealed companion star may exist there.”
“Such a stellar companion could account for the nebula’s shape, including its distinctive narrow waist and broad jets.”
“This hourglass configuration is also observed in other planetary nebulae, like the Butterfly Nebula, which Webb has also recently studied.”
“Webb’s fresh perspective on the Red Spider Nebula reveals, for the first time, the complete extent of the nebula’s extended lobes that resemble the spider’s ‘legs,'” researchers stated.
“These lobes, depicted in blue, are traced by light emitted from H.2, a molecule consisting of two hydrogen atoms bonded together.”
“These lobes, which are visible across NIRCam’s field of view, are shown to be closed, bubble-like structures, each stretching about three light-years.”
“Gas streaming from the core of the nebula has inflated these massive bubbles over countless years.”
“New observations from Webb indicate that gas is also actively being ejected from the nebula’s center.”
“A protracted purple ‘S’ shape at the nebula’s center follows light from ionized iron atoms.”
“This feature illustrates where a fast-moving jet has emerged near the nebula’s central star, colliding with previously ejected material and shaping the nebula’s undulating structure that we observe today.”
Astronomers utilizing the NASA/ESA/CSA James Webb Space Telescope have identified phosphine (PH)3 in the atmosphere of the brown dwarf Wolf 1130c, part of the triple system 1130ABC.
Schematic diagram of the Wolf 1130ABC triple system, featuring red dwarf star Wolf 1130a (left), compact white dwarf companion 1130b (center), and distant brown dwarf Wolf 1130c (right); each component scaled according to its relative size. Image credit: Adam Burgasser.
Wolf 1130ABC is located approximately 54 light years away in the constellation Cygnus.
The system is also known for LHS 482, Gliese 781, and Ross 1069b. It consists of three components: the Cool Red Star Wolf 1130a, the massive white dwarf Wolf 1130b, and the brown dwarf Wolf 1130c.
Initially discovered in 2013, Wolf 1130c orbits the closely bound systems of Wolf 1130a and Wolf 1130b on a wide trajectory.
“The astronomical initiative known as the Ancient Arcana concentrates on ancient, metal-rich brown dwarfs to enhance our understanding of atmospheric chemistry,” stated Adam Burgasser, a professor at the University of California, San Diego.
“Identifying phosphine was one of our primary objectives.”
Phosphine naturally emerges in the hydrogen-dominated atmospheres of gas giants like Jupiter and Saturn.
This has led scientists to theorize that phosphine should exist in the atmospheres of exoplanetary gas giants as well.
Nevertheless, previous Webb observations often failed to detect phosphines, pointing to an incomplete understanding of phosphorus chemistry.
“Before Webb, the expectation was that phosphine would be plentiful in planetary and brown dwarf atmospheres, according to theoretical models based on the turbulent mixing in these environments.”
Wolf 1130c is of particular interest to brown dwarf astronomers due to its lower concentration of “metals” (elements beyond hydrogen and helium) compared to the Sun.
In contrast to other brown dwarfs, the team successfully detected phosphines in the infrared spectral data collected by Webb from Wolf 1130c.
To accurately interpret their findings, researchers needed to ascertain the abundance of this gas within the atmosphere of Wolf 1130c.
“We employed a modeling approach called atmospheric recovery to quantify the molecular constituents of Wolf 1130c,” explained Dr. Irene Gonzalez from San Francisco State University.
“This technique leverages Webb’s data to validate the expected presence of various molecular gas species in the atmosphere.”
“It’s akin to reverse-engineering a delicious cookie when a chef remains committed to a recipe.”
“Typically, phosphorus may bond with other molecules, such as phosphorus trioxide,” remarked Dr. Baylor.
“In the metal-poor atmosphere of Wolf 1130c, insufficient oxygen prevents phosphorus from forming this way, allowing it to arise from phosphine-rich hydrogen.”
Alternatively, the phosphine could have been synthesized locally within the Wolf 1130ABC system, particularly from the white dwarf Wolf 1130b.
“The white dwarf represents the remnant shell of a star that has completed hydrogen fusion,” Professor Burgasser explained.
“These stars are incredibly dense and can accumulate material on their surfaces, potentially spurring runaway nuclear reactions.”
While astronomers have not observed such phenomena in the Wolf 1130ABC system in recent history, nova events usually cycle every thousands to tens of thousands of years.
This system has been recognized for just a century, and earlier invisible explosions may have contributed to a legacy of phosphorus contamination.
Gaining insights into why this particular brown dwarf exhibits a distinct signature of phosphine could shed new light on phosphorus synthesis in the Milky Way and atmospheric chemistry on exoplanets.
“If we aim to use this molecule in the quest for life in terrestrial worlds outside our solar system, understanding the atmospheric phosphine chemistry of brown dwarfs becomes crucial,” Professor Burgasser commented.
This study will be published in the journal Science.
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Adam J. Burgasser et al. Observation of unexpected phosphines in the atmosphere of the cold brown dwarf. Science. Released online on October 2, 2025. doi:10.1126/science.adu0401
Astronomers utilizing the NASA/ESA/CSA James Webb Space Telescope have found evidence of energy deposition in the upper atmosphere of the nearby brown dwarf SIMP J013656.5+093347.3 caused by auroras.
Artist’s impression of aurora and brown dwarf SIMP-0136. Image credit: Evert Nasedkin.
SIMP J013656.5+093347.3 (commonly referred to as SIMP-0136) is a low-mass brown dwarf located 20 light years away in the Pisces constellation, approximately 6.12 light years from Earth.
As part of the Carina-near Stellar Association, this celestial object is estimated to be around 200 million years old.
The mass of SIMP-0136 is roughly estimated to fall between 12.7 and 17.8 times that of Jupiter.
With a spectral type of T2.5 and a temperature nearing 1,100 K, it exhibits many atmospheric properties similar to those of directly imaged exoplanets, such as HR 8799B and AF Lep b.
“Our observations have illuminated the activity of the robust aurora of SIMP-0136, which warms its atmosphere, much like the auroras on Earth and the powerful auroras found on Jupiter.”
“These measurements represent some of the most precise assessments of the atmospheres of extreme objects to this date, with direct measurements of atmospheric changes occurring for the first time.”
“Furthermore, with temperatures exceeding 1,500 degrees Celsius, SIMP-0136 will display mild heat waves this summer.”
“Our specific observations indicated that we could precisely record temperature variations of less than 5 degrees Celsius.”
“These temperature fluctuations were linked to minor alterations in the chemical makeup of this free-floating planet, hinting at storms akin to the Great Red Spot on Jupiter.
Another unexpected finding was the constancy of cloud variability in SIMP-0136.
Changes in cloud coverage might typically lead to atmospheric changes, similar to the variability observed with patches of clouds and clear skies on Earth.
However, astronomers discovered that cloud coverage remains stable across the surface of SIMP-0136.
At SIMP-0136’s temperatures, these clouds are distinct from Earth’s, primarily composed of silicate grains reminiscent of beach sand.
“Different wavelengths of light are associated with various atmospheric features,” stated Dr. Nasedkin.
“Similar to observing color changes on Earth’s surface, the color variations of SIMP-0136 are driven by alterations in atmospheric properties.”
“Utilizing advanced models enables us to deduce atmospheric temperature, chemical composition, and cloud positioning.”
“This work is thrilling as it showcases that by leveraging cutting-edge modeling techniques on Webb’s advanced datasets, we can understand the processes driving global weather throughout our solar system.”
“Understanding these meteorological processes is crucial as we continue discovering and characterizing exoplanets in the future.”
“Currently, such spectroscopic variability observations are limited to isolated brown dwarfs, but large telescopes and future studies, along with the eventual establishment of a habitable world observatory, will allow us to explore the atmospheric dynamics of exoplanets ranging from gas giants like Jupiter to rocky planets.”
The team’s survey results will be published in the journal Astronomy and Astrophysics.
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E. Nasedkin et al. 2025. JWST Weather Report: Investigating temperature variations, aurora heating, and stable cloud coverage on SIMP-0136. A&A 702, A1; doi: 10.1051/0004-6361/202555370
Astronomers utilizing the NASA/ESA/CSA James Webb Space Telescope have identified a carbon-rich disk encircling CT Cha B, a massive exoplanet located approximately 620 light years from Earth in the Chamaeleon constellation. This discovery offers the first direct insights into the chemical and physical characteristics of the gas giant and the materials that might contribute to its potential lunar system.
Artistic rendering of dust and gas discs surrounding a young exoplanet CT Cha b. Image credits: NASA/ESA/CSA/STSCI/G. CUGNO, University of Zurich & NCCR Planets/S. Grant, Carnegie Institution for Science/J. Olmsted, Stsci/L. Hustak, Stsci.
CT CHA, also referred to as PDS 44 and TIC 454259409, is merely 2 million years old and continues to accumulate materials for its formation.
However, the disks identified by Webb are independent of the larger accretion disks surrounding the central star.
“We can observe signs of disks around companion celestial bodies and explore their chemistry for the first time,” remarks Dr. Sierra Grant, an astronomer at the Carnegie Institution for Science.
“We are not merely observing the moon’s formation; we are witnessing the planet’s formation as well.”
“We are investigating the materials involved in forming planets and moons,” added Dr. Gabriele Kuno, an astronomer from the University of Zurich and the National Center for Capacity for Research Planets.
An initial examination of Webb’s archived data revealed evidence of molecules in the surrounding disk, prompting deeper analysis of the data.
The planet’s faint signal is obscured by the glare of its host star, requiring astronomers to utilize high-contrast techniques to separate the star’s light from that of the planet.
“We detected molecules in the planet’s vicinity, indicating there was something significant to delve into within the data, which took us a year of dedicated effort. It truly required a lot of patience,” Dr. Grant stated.
Ultimately, researchers identified seven carbon-containing molecules within the disk, including acetylene (C2H2) and benzene (C6H6).
This carbon-rich chemistry contrasts sharply with that found in the disks around the host star, where water was detected alongside carbon.
The disparity between the two disks suggests rapid chemical evolution occurring within just 2 million years.
“We aim to better understand how our solar system formed its moons. This necessitates examining other systems that are still in the process of development. We are striving to comprehend all the underlying mechanisms,” Dr. Cugno explained.
“What do these moons resemble? What are their components? What physical processes are in action, and what are the associated timescales?”
“Webb is capturing the narrative of moon formation, enabling us to explore these questions observationally for the very first time.”
The survey results were published today in the Astrophysical Journal Letters.
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Gabriele Cugno & Sierra L. Grant. 2025. A carbon-rich disk surrounding the planetary mass ally. ApJL 991, L46; doi: 10.3847/2041-8213/ae0290
Positioned at the core of the Milky Way galaxy, Sagittarius B2 is an immense molecular cloud of gas and dust, boasting around 3 million times the mass of the sun.
The Sagittarius B2 molecular cloud, where stars, gases, and cosmic dust shimmer in near-infrared light, as captured by Webb’s Nircam instruments. Image credits: NASA/ESA/CSA/STSCI/A. GINSBURG, University of Florida/N. Budaiyev, University of Florida/T. Yu, University of Florida/A. Pagan, STSCI.
The distance from Earth to Sagittarius B2 is roughly 27,000 light years, while it sits just 390 light years from the center of the Milky Way.
This is the largest and most active star-forming cloud within our galaxy, accounting for half of the stars birthed in the central region, even though it comprises merely 10% of the material required for star formation in that area.
“Sagittarius B2 is situated just hundreds of light years away from the supermassive black hole located at the galaxy’s center, right at the heart of star formation.”
“Webb’s infrared observations can penetrate some of the dense clouds present, uncovering young stars alongside the warm dust enveloping them.”
“Examining Webb’s findings aids in unraveling the long-standing enigma surrounding the star formation process and why Sagittarius B2 generates stars at a rate surpassing other galaxy centers.”
“Interestingly, one of the most striking elements of Webb’s imagery of Sagittarius B2 is the regions that remain dark.”
“These seemingly vacant areas of space are so tightly packed with gas and dust that even Webb cannot detect them.”
“These dense clouds are the progenitors of future stars and are too young to emit light themselves.”
Webb’s Miri (medium-infrared device) displays the Sagittarius B2 region in medium-red light, revealing bright warm dust. Image credits: NASA/ESA/CSA/STSCI/A. GINSBURG, University of Florida/N. Budaiyev, University of Florida/T. Yu, University of Florida/A. Pagan, STSCI.
With the high resolution and sensitivity of Webb’s Miri (mid-infrared device), this area has been uncovered in remarkable detail, showcasing luminous cosmic dust heated by a massive, young star.
The red area labeled Sagittarius B2 North (located to the right in these Webb images) is among the most molecularly abundant regions known, yet astronomers have never observed it with such clarity before.
The differentiation lies in the longer wavelengths produced, even within the infrared spectrum, and the contrast between images from Webb’s Miri and Nircam (near-infrared camera) makes it evident.
“The luminous gas and dust emerge dramatically in mid-red light, though everything except for the brightest stars vanishes from sight,” the astronomer noted.
“In contrast to Miri, vibrant stars take center stage in Webb’s Nircam images.”
“Further investigations into these stars will yield insights into their masses and ages, aiding astronomers in comprehending the intricacies of star formation within this dense, dynamic galactic core.”
“Has this activity persisted for millions of years? Or has an unknown process triggered it recently?”
“We anticipate that Webb will illuminate the reasons behind the disproportionate star formation centered around galaxies.”
“While there are ample gaseous components in this area, overall productivity is not on par with that of Sagittarius B2.”
“Sagittarius B2 contains only 10% of the galaxy-centric gas but is responsible for 50% of the stars.”
Astronomers utilizing the NASA/ESA James Webb Space Telescope have identified a series of dark, bead-like star formations within Saturn’s ionosphere and stratosphere.
Detection of near-infrared emissions in Saturn’s ionosphere (left) reveals dark bead-like features embedded in bright auroras. In the stratosphere (right), below 500 km, an asymmetric star pattern extends toward the equator. Image credit: NASA/ESA/CSA/WEBB/STALLARD et al.
“This was the first opportunity for me to make such detailed near-infrared observations of Saturn’s aurora and upper atmosphere,” said the researcher.
“We anticipated seeing emissions across various levels.”
“Instead, we observed intricate patterns of beads and stars, which might be interconnected despite their considerable height separation and could relate to the iconic hexagon within Saturn’s clouds.”
“These features were entirely unforeseen and remain unexplained.”
The research team concentrated on detecting infrared emissions from charged molecular hydrogen, which plays a significant role in Saturn’s atmospheric dynamics, offering valuable insights into the chemical and physical processes at work.
Using Webb’s near-infrared spectrograph, scientists observed H3+ ions at an altitude of 600 km, 1,100 km above Saturn’s nominal surface, alongside lower stratospheric methane molecules.
Within the ionosphere’s electrically charged plasma, a series of dark bead-like features intermingled within bright aurora halos were detected.
These structures maintained stability for several hours but seemed to drift slowly over time.
In the stratosphere of Saturn, researchers identified asymmetric star-shaped features, dropping approximately 500 km.
This remarkable formation extended from Saturn’s North Pole down toward the equator.
Only four of the star’s six arms were visible, with two mysteriously absent, resulting in a biased pattern.
“Studying Saturn’s atmosphere has always posed challenges due to the faint emissions from that region,” remarked Professor Stallard.
“Webb’s remarkable sensitivity transforms our capacity to observe these atmospheric layers, unveiling a wholly different structural configuration than previously noted.”
The authors meticulously mapped the precise locations of features, overlaying data for the same Saturn area, discovering that the arms of the star seem to emanate from a point just above the hexagonal structure at the Stormcloud level.
This implies that the mechanisms driving the pattern could influence structures penetrating through Saturn’s atmosphere.
“We believe the dark beads arise from the intricate interactions between Saturn’s magnetosphere and its dynamic atmosphere, potentially providing new insights into the energy exchanges that fuel Saturn’s auroras,” stated Professor Stallard.
“The asymmetric star formations suggest previously unknown atmospheric processes functioning within Saturn’s stratosphere and are likely connected to the hexagonal storm pattern observed deeper in Saturn’s atmosphere.”
“Interestingly, the dark beads in the ionosphere seem to align with the arms of the strongest stars in the stratosphere, though it’s unclear whether this connection is genuine or merely coincidental.”
Both phenomena may have significant implications for our comprehension of atmospheric dynamics within the gas giant, although further investigation is needed to elucidate their underlying causes.
The team aspires for additional time to conduct follow-up observations of Saturn using Webb to explore further features.
As planets align approximately every 15 years, the structure can undergo dramatic changes as Saturn’s orientation shifts toward the Sun, moving the Northern Hemisphere into autumn.
“The necessity for follow-up Webb observations during this pivotal phase of Saturn’s seasonal transition is evident, as neither atmospheric layer can be examined using ground-based telescopes.” Paper published in the journal Geophysical Research Book.
Tom S. Stallard et al. 2025. JWST/NIRSPEC detects the complex structures of Saturn’s ionosphere and stratosphere. Geophysical Research Book 52 (17): E2025GL116491; doi: 10.1029/2025GL116491
Tom S. Stallard et al. 2025. Transformational observations of the ionosphere of the giant planet with JWST. EPSC Abstract 18: EPSC-DPS2025-817; doi: 10.5194/epsc-dps2025-1438
Astronomers are making strides in exploring the TRAPPIST-1 system with the NASA/ESA/CSA James Webb Space Telescope, showcasing its remarkable capability to glean detailed data about the exoplanet atmospheres and effectively utilize this information. The initial findings stem from Webb’s observation of TRAPPIST-1e. Although the first four observations by Webb are not adequate to fully assess the atmosphere, scientists are using the data to refine the possibilities for these planets, including the presence of oceans similar to those on Earth and a methane-rich environment akin to Saturn’s moon Titan. Meanwhile, additional innovative observations from Webb are ongoing, revealing the unique characteristics of TRAPPIST-1e.
The Earth-sized Exoplanet TRAPPIST-1E is illustrated in the bottom right as it eclipses the flare host star in this artist’s representation of the TRAPPIST-1 system. Image credits: NASA/ESA/CSA/STSCI/JOSEPH OLMSTED, STSCI.
TRAPPIST-1 is a cool dwarf star located in the Aquarius constellation, approximately 38.8 light-years away.
The stars are only slightly larger than Jupiter and possess a mere 8% of the solar mass. They rotate rapidly and emit UV energy flares.
TRAPPIST-1 harbors seven transiting planets designated TRAPPIST-1b, c, d, e, f, g, and h.
All these planets are comparable in size to Earth and Venus, or slightly smaller, with remarkably short orbital periods: 1.51, 2.42, 4.04, 6.06, 9.21, 12.35, and 20 days, respectively.
It is possible that they could be tidally locked, meaning the same side is always facing the host star, resulting in a perpetual day and night side for each TRAPPIST-1 planet.
Among the seven planets, TRAPPIST-1E is of particular interest if it possesses an atmosphere, as its surface water is situated at a theoretically viable distance from the star.
The Space Telescope Science Institute and colleague Dr. Néstor Espinoza aimed the Webb’s NIRSpec (near-infrared spectrometer) instrument at TRAPPIST-1e during its transits in front of the star.
As starlight filters through the planet’s atmosphere, it can be partially absorbed, revealing the specific chemicals present by the resulting dips in the light spectrum that reaches Webb.
As more transits are analyzed, the clarity regarding the atmospheric composition improves.
With only four transits analyzed thus far, numerous possibilities remain open for TRAPPIST-1E, though researchers speculate that it lacks a significant primary atmosphere.
Given TRAPPIST-1’s active nature and frequent flares, it’s not unexpected that the potential hydrogen-helium atmosphere of the planet could have been stripped away by stellar radiation.
However, many planets, like Earth, develop a denser secondary atmosphere after losing their initial one.
TRAPPIST-1E may not have the capacity for this and could potentially lack a secondary atmosphere.
“We have devised a novel method to analyze Webb’s data to assess the potential atmosphere and surface conditions of TRAPPIST-1E,” said the scientist.
It appears unlikely that TRAPPIST-1e’s atmosphere is largely composed of carbon dioxide, reminiscent of Venus’s thick atmosphere or Mars’s thinner one.
Nonetheless, astronomers should be cautious, as there are no direct parallels to our solar system.
“Because TRAPPIST-1 is significantly different from our Sun, the surrounding planetary systems also exhibit notable differences, posing challenges to both observational and theoretical frameworks,” remarked Dr. Nicole Lewis of Cornell University.
“If TRAPPIST-1E has liquid water, it would require a greenhouse effect. This effect incorporates various gases, especially carbon dioxide, which help stabilize the atmosphere and maintain a warm environment on the planet.”
“A minimal greenhouse effect is beneficial, and measurements do not exclude the presence of carbon dioxide necessary to preserve water on the surface.”
The team’s analysis suggests that water could exist as global oceans or be distributed in smaller, ice-encased regions at midday.
This is due to the size of the TRAPPIST-1 planets and their orbital sizes, all of which are thought to be tidally locked, with one side perpetually facing the star and the other shrouded in darkness.
“They’re remarkable,” stated Dr. Anna Glidden, an astronomer at the Kavli Institute for Astrophysics and Space Research at MIT.
“This is an astounding measurement of starlight around an Earth-sized planet located 40 light-years away, providing insights into potential life there if conditions permit.”
“It’s thrilling to be part of this new era of exploration.”
Néstor Espinoza et al. 2025. JWST-TST Dreams: NIRSpec/Prism transmission spectroscopy of the planet TRAPPIST-1e. ApJL 990, L52; doi: 10.3847/2041-8213/adf42e
Anna Glidden et al. 2025. JWST-TST Dreams: Secondary atmosphere constraints of the habitable zone planet TRAPPIST-1e. ApJL 990, L53; doi: 10.3847/2041-8213/adf62e
Astronomers utilizing the NASA/ESA/CSA James Webb Space Telescope have discovered evidence of gaseous methane on the remote dwarf planet Macemeiki. This finding is detailed in a paper published in the Astrophysics Journal Letter. This discovery challenges the conventional perception of Makemake as a stable, frozen entity. Following Pltune, where gas presence was confirmed, it is now only the second Transneptune object to display this characteristic.
Protopapa et al. Methane gas was detected with Makemake using Webb observations (white). A sharp radiation peak near 3.3 microns reveals methane in the gas phase on the surface of Makemake. The continuum model (CYAN) is overlaid for comparison. An observable spectrum above the continuum indicates a gas emission peak. Image credit: S. Protopapa/I. Wong/SWRI/STSCI/NASA/ESA/CSA/WEBB.
Makemake, also referred to as FY9 and (136472), was identified in 2005 by a team of astronomers at the California Institute of Technology, led by Mike Brown.
This planet of War is situated in a region beyond Neptune, home to a small solar system.
Its radius measures approximately 715 km (444 miles), making it a dimmer and slightly smaller body than Pluto.
It takes around 305 Earth years for this dwarf planet to complete one orbit around the Sun.
Previously observed stellar occultations indicated that Makemake likely lacked a significant global atmosphere, although thin atmospheres could not be completely dismissed.
Meanwhile, infrared observations suggested mysterious thermal anomalies and peculiar characteristics of its methane ice, hinting at the possibility of local hotspots and potential outgassing on its surface.
“Makemake is one of the largest and brightest icy worlds in the outer solar system, with its surface predominantly comprised of frozen methane,” stated Dr. Sylvia Protopapa, an astronomer at the Southwest Institute.
“Webb has revealed that methane is also present in the gas phase above the surface, making Makemake an even more intriguing subject of study.”
“This indicates that Makemake is not an inert remnant of the outer solar system; rather, it is a dynamic body where methane ice is actively evolving.”
The detected methane spectral emission is interpreted as solar absorbing fluorescence, which occurs when sunlight is re-emitted after being absorbed by methane molecules.
The research team posited that this could either indicate a tenuous atmosphere in equilibrium with surface ice, akin to Pluto, or more transient activities such as comet-like sublimation or cryovolcanic processes.
Both scenarios are plausible and align with current data, given the signal-to-noise ratios and limited spectral resolution.
“The inclination to connect Makemake’s various spectra with thermal anomalies is compelling, but identifying mechanisms that enable volatile activities remains essential to interpreting these observations cohesively.”
“Future Webb observations at higher spectral resolutions will aid in determining whether methane originates from thin atmospheres or outgassing processes like plumes.”
“This discovery opens up the possibility that Makemake has a very thin atmosphere supported by methane sublimation,” noted Dr. Emmanuel Lelouch, an astronomer at the Paris Observatory.
“Our best model estimates a surface pressure around 40 K (minus 233 degrees Celsius) and about 10 picobars, which is a hundred billion times less than Earth’s atmospheric pressure, indicating a dilute surface pressure about ten billion times that of Pluto.”
“If this hypothesis is validated, Makemake will join a select group of outer solar system bodies where surface mass exchanges are still actively occurring today.”
“Another scenario proposes that methane is being expelled in plume-like eruptions,” Dr. Protopapa added.
“In this case, our model indicates that methane may be released at a rate of several hundred kilograms per second, comparable to the intense water plumes seen on Enceladus, Saturn’s moon, and significantly larger than the faint steam observed on Ceres.”
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Silvia Protopapa et al. 2025. JWST detection of hydrocarbon ice and methane gas on Makemake. apjl in press; Arxiv: 2509.06772
Thanks to the NASA/ESA/CSA James Webb Space Telescope, astronomers have made significant progress in understanding the connection between the raw materials of rocky planets. This cosmic material—crystalline silicate dust and polycyclic aromatic hydrocarbons—was analyzed in the core of the remarkable bipolar planetary nebula known as the Butterfly Nebula.
Hubble and Webb/Alma images of Butterfly Nebula. Image credits: NASA/ESA/CSA/Webb/Hubble/Alma/Matsuura et al. , doi: 10.1093/mnras/staf1194.
The Butterfly Nebula, also referred to as NGC 6302, is among the most extensively studied planetary nebulae.
This nebula is situated approximately 2,417 light years away from Earth, in the constellation Scorpio.
Its distinctive butterfly shape has expanded over two light years, roughly half the distance from the Sun to Proxima Centauri.
The object exhibits extreme bipolarity, complex morphology, and features very high excitation gases, high molecular weight, and crystalline silicates.
“The planetary nebula is one of the most stunning and elusive phenomena in the cosmic landscape,” stated Mikako, an astronomer from Cardiff University, along with Matsui Ko and her colleague.
“These nebulae form when stars with masses between 0.8 and 8 times that of the Sun shed most of their mass at the end of their lifecycle.”
“The nebula phases on planets are transient, lasting only about 20,000 years.”
“Despite their name, planetary nebulae have no connection to planets. The confusion arose centuries ago, when astronomers noted that these nebulae appeared round, resembling planets.”
“Although many planetary nebulae are not round, their titles often reflect misleading names, and the Butterfly Nebula is a prime illustration of the extraordinary shapes these nebulae can assume.”
“As a bipolar nebula, the Butterfly Nebula has two lobes extending in opposite directions, forming what resembles butterfly ‘wings’,” they continued.
“The dark band of dusty gas acts as the ‘body’ of the butterfly. This band is actually a donut-shaped torus that conceals the central star of the nebula.”
“Dusty donuts may indeed contribute to the insect-like shape of the nebula by hindering gas from escaping outward from the star uniformly.”
New images from Webb’s Mid-Infrared Instrument (MIRI) offer a close-up view of the center of the Butterfly Nebula and its dusty torus, revealing its complex structure like never before.
Astronomers have detected nearly 200 spectral lines, each providing insights into the nebula’s atoms and molecules.
These lines uncover nested interconnected structures tracked by various species.
Researchers have also pinpointed the central star in the Butterfly Nebula, which heats a previously undetected dust cloud surrounding it, causing it to emit bright light at mid-infrared wavelengths.
The star boasts a temperature of 220,000 Kelvin, making it one of the hottest known central stars in the galaxy’s planetary nebulae.
This image takes viewers diving deep into the heart of the Butterfly Nebula, as seen by Webb. Image credit: NASA/ESA/CSA/WEBB/M. MATSUURA/ALMA/ESO/NAOJ/NRAO/N. HIRANO/M. ZAMANI.
“This incredible, radiant engine is responsible for the stunning brilliance of the nebula, yet its full effect is moderated by the dense band of thin gas, the torus, that surrounds it,” the author noted.
“New data from Webb reveals that the torus comprises crystalline silicates such as quartz and irregularly shaped dust particles.”
“Dust grains measure about one millionth of a meter, typical for space dust.”
“Beyond the torus, emissions from various atoms and molecules form multilayer structures.”
“Ions needing the highest energy to form cluster near the center, while those requiring less energy are positioned farther away from the central star.”
“Iron and nickel are particularly noteworthy, following jets that erupt outward from the star in opposite directions.”
In an intriguing finding, the team also identified light emitted by carbon-based molecules known as polycyclic aromatic hydrocarbons (PAHs).
“These molecules have a flat, ring-like configuration, reminiscent of honeycomb shapes found in beehives,” said the astronomer.
“On Earth, PAHs are often present in smoke from campfires, vehicle exhausts, or burnt toast.”
“Given their location, these PAHs likely form when the winds from the central star push against the surrounding gas.”
“This discovery marks the first evidence of PAH formation in oxygen-rich planetary nebulae, offering a glimpse into the processes behind their formation.”
Survey results were published this week in the Monthly Notices of the Royal Astronomical Society.
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Mikako Matsumura et al. 2025. JWST/MIRI view of Planetary Nebula NGC 6302 – I. UV irradiated torus and hot bubbles cause PAH formation. mnras 542(2):1287-1307; doi:10.1093/mnras/staf1194
Astronomers utilizing the NASA/ESA/CSA James Webb Space Telescope have identified a previously uncharted small moon, provisionally named S/2025 U 1. This discovery, made from a series of images taken on February 2, 2025, brings Uranus’s total number of moons to 29.
This Webb/nircam image illustrates S/2025 U1 along with 13 of the other 28 identified moons. Image credits: NASA/ESA/CSA/STSCI/M. El Moutamid, SWRI/M. Hedman, University of Idaho.
Situated in the outer solar system, Uranus is the seventh planet from the Sun.
This cyan ice giant, often referred to as a “lateral planet” due to its extreme axial tilt, has a thick atmosphere composed of hydrogen, helium, and methane.
The 28 moons of Uranus include five major ones: Titania, Oberon, Ambriel, Ariel, and Miranda, discovered between 1787 and 1948.
Known as “The Literary Moons,” the moons of Uranus are named after characters from the works of Shakespeare and Alexander Pope.
Astronomers estimate that Uranus’s larger moons are approximately equal parts water ice and silicate rock.
“As part of Webb’s Guest Observer program, we discovered a previously unknown satellite of the ice giant,” explained Dr. Maryame El Moutamid, a researcher at the Southwest Research Institute.
“This object is the smallest ever detected and was observed during a set of 10 long exposures captured by Webb’s near-infrared camera (NIRCAM).”
The moon, provisionally designated S/2025 U1, resides at the end of Uranus’s inner ring.
Estimated to have a diameter of only 10 km (6 miles), its reflectance (albedo) is presumed to be similar to that of other small Uranian satellites.
It is located approximately 56,250 km (35,000 miles) away from the Earth’s equatorial plane, positioned between the orbits of Ophelia and Bianca.
Ophelia has a diameter of about 43 km (13 miles), while Bianca is elongated, measuring 64 x 46 km (40 x 29 miles).
“While it’s a small moon, its discovery is significant. This is something that even NASA’s Voyager 2 spacecraft missed during its flybys nearly 40 years ago,” Dr. El Moutamid remarked.
S/2025 U1 becomes the 14th member of a complex system of small moons, circling inward among the larger moons, including Miranda, Ariel, Umbriel, Titania, and Oberon.
“Unlike other planets, Uranus possesses a remarkable number of small inner moons. The intricate interactions with its ring system indicate a chaotic history that merges the ring and lunar systems,” Dr. El Moutamid noted.
“Furthermore, this new moon’s small size and unexpected nature may lead to the discovery of even more complexities.”
Astronomers captured a new high-resolution image of the planetary nebula NGC 6072 using two instruments on board the NASA/ESA/CSA James Webb Space Telescope.
This Webb/Nircam image depicts NGC 6072, a planetary nebula located about 4,048 light years away in the constellation of Scorpius. Photo credits: NASA/ESA/CSA/STSCI.
NGC 6072 is situated approximately 1,241 parsecs (4,048 light years) away from the southern constellations of Scorpius.
Also known by designations such as ESO 389-15, HEN 2-148, and IRAS 16097-3606, this nebula has a dynamic age of about 10,000 years.
It was first discovered by British astronomer John Herschel on June 7, 1837.
“Since their discovery in the 1700s, astronomers have learned that planetary nebulae, the expanding shells of luminous gases expelled by dying stars, can take on various shapes and forms,” noted Webb astronomers.
“While most planetary nebulae are circular, elliptical, or bipolar, the new Webb image of NGC 6072 reveals a more complex structure.”
Images captured by Webb’s Nircam (near-infrared camera) suggest that NGC 6072 displays a multipolar configuration.
“This indicates there are multiple oval lobes being ejected from the center in various directions,” the astronomers explained.
“These outflows compress the surrounding gas into a disk-like structure.”
“This suggests the presence of at least two stars at the center of this nebula.”
“In particular, a companion star appears to be interacting with an aging star, drawing in some of its outer gas and dust layers.”
The central area of the nebula glows due to hot stars, reflected in the light blue hue characteristic of near-infrared light.
The dark orange regions, composed of gas and dust, create pockets and voids appearing dark blue.
This material likely forms when dense molecules shield themselves from the intense radiation emitted by the central star.
There may also be a temporal aspect; for thousands of years, rapid winds from the main star could have been blowing away the surrounding material as it loses mass.
This web/milli image highlights the planetary nebula NGC 6072. Image credits: NASA/ESA/CSA/STSCI.
The long wavelengths captured by Webb’s Miri (mid-infrared instrument) emphasize the dust, unveiling a star that astronomers believe resides at the center of the nebula.
“The image appears as a small pink dot,” remarked the researchers.
“The mid-infrared wavelengths also reveal a concentric ring expanding outward from the central region.
“This might indicate the presence of a secondary star at the heart of the nebula, obscured from direct observation.”
“This secondary star orbits the primary star, creating rings of material that spiral outward as the original star sheds mass over time.”
“The red regions captured by Nircam and the blue areas highlighted by Miri track cool molecular gases (likely molecular hydrogen), while the central region tracks hot ionized gases.”
To celebrate the remarkable advancements in science during the third year, astronomers have utilized the NASA/ESA/CSA James Webb Space Telescope to capture images of the Cat’s Paw Nebula.
This web image depicts the Cat’s Paw Nebula, a significant star-forming region located 5,500 light years from the constellation Scorpio. Image credits: NASA/ESA/CSA/STSCI.
The Cat’s Paw Nebula resides in the southern constellation of Scorpio and is approximately 5,500 light years from Earth.
First identified in 1837 by British astronomer John Herschel, this dynamic star-forming region spans an estimated 80 to 90 light years.
Also known as NGC 6334 or the Bear Claw Nebula, it is one of the most vibrant stellar nurseries in the night sky, producing thousands of young, hot stars that emit light not visible from our perspective.
Recent images captured by Webb’s NIRCam instrument reveal structural details and functionalities previously unseen.
“Massive young stars are actively interacting with nearby gas and dust, and their bright stellar light produces a luminous, hazy glow, represented in blue,” Webb astronomers stated.
“This scenario illustrates a transient period where a destructive young star plays a significant role in the broader narrative of the region, characterized by relatively short lifespans and high luminosity.”
“Due to the dynamic activities of these massive stars, the local star formation process will eventually come to a halt.”
“We begin with a central area identified as the ‘opera house’ because of its hierarchical circulatory structure,” they noted.
“The principal sources of the blue glow in this area are likely positioned towards the bottom, obscured by dense brown dust, interspersed with light from bright, yellowish stars or nearby sources.”
“Beneath the orange-brown dust lies a bright yellow star displaying distinct diffraction spikes.”
“This giant star is sculpting its surrounding environment but has not managed to push gas and dust away sufficiently nor create a compact shell of surrounding material.”
“Take note of smaller regions, such as the tuning fork-shaped area adjacent to the opera house, which contains fewer stars.”
“These seemingly vacant zones are still in the process of forming stars, indicating the presence of dense filaments of dust that obscure the light of background stars.”
At the center of the image, small, fiery red masses can be seen scattered within the brown dust.
“These glowing red sources highlight areas where large-scale star formation is occurring, albeit in a less visible manner,” the researchers explained.
“Some of the blue-white stars, particularly in the lower left area, appear more sharply resolved than others.”
“This sharper appearance is attributed to the material between the star and the telescope being diffused by the star’s radiation.”
Near the bottom of this area is a compact dust filament.
“These small dust aggregates have managed to survive the intense radiation, indicating they are dense enough to give rise to protostars.”
The small yellow section on the right marks the location of a massive star still in its formative stages, managing to shine through the intervening material.
Numerous small yellow stars are scattered across the scene, displaying distinct diffraction spikes.
“The bright blue-white stars prominently feature in the foreground of this web image, with some possibly being part of the larger Cat’s Paw Nebula region.”
A particularly striking feature of this web image is the bright red-orange oval shape located in the top right corner.
The low concentration of background stars indicates it is a dense area where the star-forming process has only recently commenced.
Several visible stars are distributed throughout the region, contributing to the illumination of central materials.
Some of the developing stars have left behind traces of their existence, such as the shock wave visible in the lower left area.
Astronomers utilized the mid-infrared instrument (Miri) on the NASA/ESA/CSA James Webb Space Telescope to capture breathtaking infrared images of the heart of Messier 82, an edge-on starburst galaxy located approximately 12 million light-years away.
This Webb/Miri image highlights the central region of the Starburst Galaxy Messier 82. Image credits: NASA/ESA/CSA/Webb/A. Bolatto.
Messier 82 is positioned higher in the Northern Spring Sky, situated within the Ursa Major constellation’s direction.
The galaxy was first identified by German astronomer Johann Erard Bord in 1774 and is estimated to be around 40,000 light-years old.
Messier 82 is also referred to as the Cigar Galaxy due to its elongated oval shape, a result of the tilt of its stellar disk relative to our perspective.
Known for its exceptional rate of star formation, galaxies like Messier 82 generate stars ten times faster than our Milky Way.
“Though smaller than the Milky Way, Messier 82 is five times as luminous and creates stars at a rate 10 times greater,” the Webb astronomers noted.
“Classified as a Starburst Galaxy, Messier 82 is particularly active in its center, producing new stars at an accelerated pace compared to other galaxies of its size.”
In visible light images, the central region’s intense activity is concealed by a thick veil of dust clouds, but Webb’s infrared capabilities allow it to penetrate this obscuring layer and unveil the hidden dynamism.
“The reason for the star formation surge in Messier 82 likely lies with its gravitational interactions with the neighboring Spiral Galaxy Messier 81,” the astronomers remarked.
“These interactions directed gas towards the center of Messier 82 millions of years ago.”
“This influx of gas supplied essential materials for new star formation, resulting in Messier 82’s distinct structure! The galaxy boasts over 100 superstar clusters.”
“Superstar clusters are larger and more luminous than normal star clusters, each containing approximately 100,000 stars.”
Earlier Webb images of Messier 82, utilizing data from the telescope’s near-infrared camera (Nircam), were made public in 2024.
These images concentrated on the galaxy’s core, where individual clusters of young stars contrasted with gas clumps and tendrils.
The latest images from Webb’s Miri instruments provide an astonishing, almost starless view of Messier 82.
“Instead, these images highlight warm dust and a complex cloud of sooted organic molecules known as polycyclic aromatic hydrocarbons (PAHs),” the researchers explained.
“Emissions from PAH molecules trace the expansive runoff of the galaxy, propelled by intense radiation and winds from the hot young stars within the central superstar cluster.”
“Superstar clusters are responsible for Messier 82’s powerful galactic winds, which may signal the conclusion of the galaxy’s Starburst period. These winds, transforming into massive waves in intergalactic space, carry the cool gas necessary for further star formation.”
Modern disk galaxies frequently display distinct thin and thick disks. The mechanisms driving the formation of these two discs and the timeline of their emergence are still unanswered questions. To investigate these issues, astronomers examined various epochs (statistical samples of 111 edge-on disk galaxies dating back up to 11 billion years, or approximately 2.8 billion years post-Big Bang) utilizing archived data from the NASA/ESA/CSA James Webb Space Telescope.
Webb/nircam composite images of a quarter of the team’s samples were sorted by increasing redshift. Image credit: Tsukui et al., doi: 10.1093/mnras/staf604.
Present-day disk galaxies often comprise extensive, star-rich outer disks alongside thin, star-like disks.
For instance, the thick discs of the Milky Way reach approximately 3,000 light-years in height, while the thin discs are roughly 1,000 light-years thick.
But what mechanisms lead to the formation of this dual disk structure?
“The thickness of high redshift discs, or unique measurements from the early universe, serve as benchmarks for theoretical research that can only be conducted using Webb,” states Takagi, an astronomer at the Australian National University.
“Typically, older, thicker disk stars are dim, while the younger, thinner disk stars dominate the galaxy.”
“However, Webb’s exceptional resolution allows us to observe and highlight faint older stars, enabling us to distinguish between two disk structures in a galaxy and measure their thickness separately.”
Through an analysis of 111 edge-on targets over cosmological time, astronomers studied both single-disc and double-disc galaxies.
The findings indicate that galaxies initially form a thick disk, which is followed by the formation of a thin disk.
The timing of this process is contingent on the galaxy’s mass: high-mass, single-disk galaxies transitioned to two-disk structures around 8 billion years ago.
In contrast, a thin disk emerged about 4 billion years ago within low-mass, single-disk galaxies.
“This is the first time we’ve resolved a thin star disk at such a high redshift,” remarked Dr. Emily Wysnioski from the Australian National University.
“The novelty becomes evident when observing the onset of thin star disks.”
“It was astonishing to witness a thin star disk from 8 billion years ago, and even further back.”
To elucidate the transition from a single thick disk to a dual-disk structure, as well as the timing differences between high-mass and low-mass galaxies, researchers expanded their investigation beyond the initial edge-on-galaxy samples. They examined data showing the movement of gases from large millimeter/sub-millimeter arrays (ALMAs) in Atacama and ground surveys.
By considering the movement of the galaxy’s gas disks, they found their results aligned with the “turbulent gas disk” scenario.
In this framework, the turbulent gas disks of the early universe catalyze intense star formation, leading to the creation of thick star disks.
As stars form, they stabilize the gas disks, diminishing turbulence and consequently resulting in thinner disks.
Larger galaxies can convert gas into stars more efficiently and thus calm down more quickly than their lower-mass counterparts, leading to the formation of the earlier thin disk.
“This study delineates structural differences between thin and thick discs, but we aim to explore further,” Dr. Tsukui mentioned.
“We look to incorporate the types of information typically acquired from nearby galaxies, such as stellar movement, age, and metallicity.”
“By doing so, we can bridge insights from both nearby and distant galaxies, enhancing our understanding of disk formation.”
Survey results were published in Monthly Notices of the Royal Astronomical Society.
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Takagi Tsukui et al. 2025. The emergence of thin and thick discs of galaxies across the history of the universe. mnras 540(4): 3493-3522; doi: 10.1093/mnras/staf604
Astronomers utilize the exceptional sensitivity of the Mid-infrared instrument (Miri) on the NASA/ESA/CSA James Webb Space Telescope to investigate exoplanets within the three-ring debris disks surrounding the 6.4 million-year-old star TWA 7.
This Webb/Miri image shows the exoplanet TWA 7b, comparable in mass to Saturn. Image credits: NASA/ESA/CSA/WEBB/AM LAGRANGE/M. ZAMANI, ESA & WEBB.
Debris disks, comprised of dust and rocky materials, can exist around both young and evolved stars, but they are more luminous and detectable around younger celestial bodies.
These disks are often identified by their visible rings and gaps, which are believed to be shaped by planets that form within them.
The star TWA 7 is a low-mass (0.46 solar mass) M-type star situated approximately 111 light-years away in the constellation of Antlia.
Also referred to as Ce Antilae or Tyc 7190-2111-1, it is part of the TW Hydra Association.
The nearly edge-on three-ring fragmented disks make TWA 7 an optimal target for Webb’s highly sensitive mid-infrared observations.
“Our observations indicate a strong candidate for the planet that influences the structure of the TWA 7 debris disk, located precisely where we anticipated finding a planet of this mass,” states Dr. En Marie Lagrange, an astronomer at the Observatoire de Paris-PSL.
On June 21, 2024, Dr. Lagrange and colleagues employed a coronagraph with Webb’s Miri instrument to effectively suppress the bright glare of the host star, uncovering faint nearby objects.
This method, known as high contrast imaging, enables astronomers to directly observe planets that would otherwise be obscured by the overwhelming light of their host stars.
After eliminating residual starlight through advanced image processing, a faint infrared source was detected near TWA 7, distinguishable from background galaxies or other solar system objects.
This source is located within one of the three dust rings previously identified around TWA 7 by earlier ground-based investigations.
Its brightness, color, distance from the star, and position within the ring align with theoretical expectations for a young, cold Saturn-mass planet that shapes the surrounding debris disks.
“They are also the most popular and highly skilled professionals,” remarked Dr. Matilde Marin, an astronomer at Johns Hopkins University and the Institute for Space Telescope Science.
The team’s preliminary analysis suggests that the object known as TWA 7B has a mass approximately 0.3 times that of Jupiter (about 100 times that of Earth) and may be a young, cold exoplanet with a temperature of 320 K (around 47°C).
Its positioning (approximately 52 AU from the star) corresponds with a gap in the disk, indicating a dynamic interaction between the planet and its surroundings.
Once corroborated, this discovery marks the first direct link between a planet and the structure of debris, offering initial observational insights into the Trojan disk.
“These findings underscore Webb’s capability to probe previously unobservable low-mass planets orbiting nearby stars,” the astronomer commented.
“Ongoing and future observations will seek to more accurately characterize candidates, investigate the state of their atmospheres, and enhance our understanding of planet formation in young systems and the evolution of disks.”
“This preliminary result represents an exciting new frontier where Webb sheds light on the discovery and characterization of exoplanets.”
These findings are detailed in a publication in the journal Nature.
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Lagrange et al. Evidence of sub-Jovian planets within the young TWA 7 disk. Nature Published online on June 25th, 2025. doi:10.1038/s41586-025-09150-4
Astronomers utilizing the NASA/ESA/CSA James Webb Space Telescope have discovered a silicate cloud in the atmosphere of the exoplanet YSES-1C and a disk in the evasion facility surrounding the planet YSES-1B.
Artist rendering of the YSES-1 system, featuring a central sun-like star, YSES-1B with its dusty evasive disc (right), and YSES-1C’s atmospheric silicate clouds. Image credit: Ellis Bogut.
YSES-1 is a solar-type star located approximately 309 light-years away in the constellation of Masca.
Also referred to as TYC 8998-760-1 or 2mass J13251211-6456207, this star is roughly equivalent in mass to our Sun but is only 16.7 million years old.
The system comprises two planets, YSES-1B and YSES-1C.
These planets orbit their parent star at distances of 160 and 320 AU, making them more distant from their star than Jupiter and Saturn are from the Sun.
YSES-1B and C could exhibit redder hues compared to other exoplanets (or brown dwarfs), indicating distinct atmospheric properties.
While the system has been observed with various telescopes before the Webb, comprehensive observations were not achievable prior to the Webb program.
“Directly imaged exoplanets are the only types we can truly photograph,” stated Dr. Ebert Nazkin, a postdoctoral researcher at Trinity College Dublin.
“Typically, these exoplanets are younger, hotter from their formative layers, and astronomers observe this heat in the thermal infrared spectrum.”
Utilizing Webb’s spectroscopic capabilities, Dr. Nasedkin and his team obtained detailed spectra of the planets YSES-1B and YSES-1C.
These observations include the first direct detection of atmospheric silicate clouds on YSES-1C, validating prior hypotheses regarding its atmospheric structure.
These silicate clouds likely contain iron, which might contribute to rainfall on the planet.
Astronomers estimate that the cloud particles are less than 0.1 μm in size.
“Upon observing a smaller, more distant companion identified as YSES-1C, I detected a silicate cloud signature in the mid-infrared,” Dr. Nasedkin remarked.
“Composed primarily of sand-like particles, this represents the strongest silicate absorption feature documented in an exoplanet.”
“We believe this is connected to the planet’s youth. Younger planets tend to have slightly larger radii, and this expanded atmosphere enables clouds to absorb more light emitted by the planet.”
“We were able to employ detailed modeling to uncover the chemical makeup of these clouds as well as the size and shape of the cloud particles.”
The team also identified silicate disks surrounding YSES-1B, marking a rare observation of a substellar companion exoplanet.
This finding suggests that YSES-1B may be a relatively recently formed planet.
The discoveries enhance our understanding of the early stages of planetary formation and atmospheric development.
“The planets within the YSES-1 system are so widely separated that current formation theories cannot explain them. The discovery of distinct silicate clouds around YSES-1C and additional findings of small, hot, dusty materials around YSES-1B introduces further mystery and complexity regarding how planets form and evolve.”
The team’s results will be featured in the journal Nature this week.
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kkw hoch et al. Silicate cloud and evasive agent disks in the YSES-1 exoplanet system. Nature Published online on June 10th, 2025. doi:10.1038/s41586-025-09174-w
With the aid of the NICAM (Near-infrared camera), astronomers aboard the NASA/ESA/CSA James Webb Space Telescope have captured new images of the Sombrero Galaxy.
The new Webb/Nircam image reveals the prominent bulge of the Sombrero Galaxy, which consists of a dense cluster of stars at the galaxy’s center, while dust on the outer rim obscures some starlight. Image credits: NASA/ESA/CSA/STSCI.
The Sombrero Galaxy is situated approximately 28 million light years away in the Virgo constellation.
Also referred to as Messier 104, M104, or NGC 4594, this galaxy was discovered by the French astronomer Pierre Méchain on May 11, 1781.
It has a diameter of 49,000 light years, which is nearly twice that of our Milky Way galaxy.
The Sombrero Galaxy displays features typical of both spiral and elliptical galaxies.
It features a spiral arm and a prominently illuminated central bulge that resembles two hybrid forms.
Viewed edge-on, the Sombrero Galaxy sits at a six-degree angle south of its plane, with the dark dust lane creating a striking visual.
“Researching galaxies like the Sombrero through various wavelengths, including near-infrared with Webb, as well as data from the NASA/ESA Hubble Space Telescope, assists us in understanding the formation and evolution of this intricate system and its constituent materials,” said an astronomer.
“Unlike Hubble’s visible light images, the dust disk is not detectable in Nircam’s new near-infrared imagery.”
“This is because the longer wavelengths of infrared radiation emitted by stars penetrate dust more effectively, resulting in less obstruction of stellar light.”
“In mid-infrared images, the dust actually emits light.”
“Research indicates that the smooth surface and subtle glow of the galaxy hint at a turbulent history,” the astronomer noted.
“Anomalies discovered over the years suggest that this galaxy may have been involved in a violent merger with at least one other galaxy.”
“Spectroscopic analyses reveal unexpected variances among the stars in these globular clusters.”
“Stars that form under similar conditions and from the same materials typically share similar chemical ‘fingerprints,’ such as the same abundance of elements like oxygen or neon.”
“However, the apparent variations among stars in this galaxy’s globular clusters are notably significant.”
“The merging of various galaxies over billions of years can explain these discrepancies.”
“Further evidence supporting the merger hypothesis is seen in the distorted look of the galaxy’s inner disk.”
“While our observations categorize it as edge-on, it actually gives the impression of being at quite an angle,” they added.
“Seen from six degrees off the galaxy’s equator, our viewpoint allows us to glimpse it slightly from above, rather than straight on.”
“From this vantage point, the inner disk appears tilted inward, resembling a funnel rather than a flat plane.”
“Nircam’s advanced resolution reveals parts of the galaxy that look red, indicating the presence of red giants—cooler stars that shine brightly due to their larger surface areas.”
“These red giants are also visible in mid-infrared, but the smaller blue stars in the near-infrared become indistinguishable at longer wavelengths.”
“Additionally, Nircam’s images capture a variety of galaxies in differing shapes and colors scattered across the backdrop of space.”
This color diversity offers astronomers insights into characteristics such as their distances from Earth.
Astronomers leveraging the NASA/ESA/CSA James Webb Space Telescope have identified water, carbon monoxide, and methane in the atmosphere of WASP-121B, as well as in Earth’s nightside atmosphere. This marks the first detection of silicon monoxide in any planetary atmosphere, including those within our solar system and beyond.
This artistic impression illustrates the phase during which WASP-121B collects most of its gas, inferred from recent findings. Image credit: T. Muller, MPIA & HDA.
WASP-121B is approximately 1.87 times larger and 1.18 times more massive than Jupiter.
First discovered in 2016, it completes an orbit around its host star, the F6-type WASP-121 (TYC 7630-352-1), in just 1.3 days, as observed by the WASP-SOUTH SURVEY.
The WASP-121 system is situated about 881 light years away in the constellation of Puppis.
Characterized as an Ultra Hot Jupiter, WASP-121B orbits its parent star in a mere 1.3 days, being so close that the star’s gravitational pull begins to physically disrupt it.
Estimates suggest that the temperatures on the planet’s eternal daytime side exceed 3,000 degrees Celsius, while the nightside cools down to around 1,500 degrees Celsius.
“The discovery of silicon monoxide in the atmosphere of WASP-121B is revolutionary, marking the first definitive identification of this molecule in any planetary atmosphere,” stated Dr. Anjali Piette, an astronomer at the University of Birmingham.
“The composition of the nightside atmosphere of WASP-121B indicates vertical mixing: the transport of gases from deeper atmospheric layers to the peak observed in infrared light.”
“We were surprised to find methane on the nightside given the extreme temperatures of this planet.”
Measurements of carbon-to-hydrogen, oxygen-to-hydrogen, silicon-to-hydrogen, and oxygen-to-oxygen ratios in the atmosphere suggest that during its formation, WASP-121B’s atmosphere was enriched by inner rocky materials enhanced by erosion-resistant bombardment.
“They’re outstanding,” remarked Dr. Thomas Evans Soma, an astronomer at Newcastle University.
In their research, astronomers employed a method known as phase curve observation, which entails tracking a planet’s orbit around its star and analyzing variations in its brightness.
These observations reveal details about both the daytime and nighttime hemispheres, along with their chemical makeups.
“The successful detection of these elements and characterization of WASP-121B’s atmosphere with Webb showcases the telescope’s capabilities and sets a precedent for future exploratory research,” Dr. Piette remarked.
Study published today in the journal Nature Astronomy.
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TM Evans-Soma et al. Ultra-Stellar C/O ratio in the atmosphere of SIO and giant exoplanet WASP-121. Nature Astronomy Published online on June 2, 2025. doi:10.1038/s41550-025-02513-x
Astronomers utilizing the NASA/ESA/CSA James Webb Space Telescope have captured incredible new images of the Galaxy Cluster Abell S1063.
This Webb image illustrates the colossal galaxy cluster Abell S1063. Image credits: NASA/ESA/CSA/Webb/H. Atek & M. Zamani, ESA & Webb/R. Endley.
Abell S1063 is a significant cluster of galaxies located about 4.5 billion light years away in the constellation Grus.
This cluster houses approximately 100 million solar masses, including 51 confirmed galaxies, with potentially over 400 more yet to be identified.
The enormous mass of Abell S1063 bends and magnifies light from galaxies located behind it, an effect known as gravitational lensing.
“Upon closer examination, this dense grouping of massive galaxies is encircled by glowing light streaks, and these warped arcs are the essence of our interest: faint galaxies from the distant past of the universe.”
“Abell S1063 was previously explored by the Frontier Fields program using the NASA/ESA Hubble Space Telescope.”
“It possesses a remarkable gravitational lens. The immense size of these galaxy clusters causes light from the distant galaxies positioned behind them to curve around them, forming the distorted arcs visible here.”
“Similar to a glass lens, it directs light from these remote galaxies.”
“The resulting image, while distorted, is bright and magnified, making it possible for observation and study.”
“This was Hubble’s objective — to investigate the early universe using galaxy clusters as a magnifying glass.”
“The image reveals an astonishing array of structures around Abell S1063, showcasing distorted background galaxies at various distances, along with numerous faint galaxies and previously unseen features,” the researchers noted.
“This image is classified as a deep field. It focuses on a single segment of the sky for an extended period, gathering as much light as possible to detect the faintest distant galaxies that aren’t visible in standard images.”
“It comprises nine distinct snapshots of different near-infrared wavelengths, totaling approximately 120 hours of observation time, enhanced by the gravitational lensing effect. This marks Webb’s deepest observation of a single target to date.”
“Thus, directing such observational capability at a large gravitational lens, like Abell S1063, could uncover some of the earliest galaxies formed in the early universe.”
Water ice plays a crucial role in the formation of giant planets and can also be delivered by comets to fully developed rocky planets. Utilizing data from the Near-infrared spectrometer (NIRSPEC), which is part of the NASA/ESA/CSA James Webb Space Telescope, astronomers have identified crystallized ice on a dusty fragment disk surrounding HD 181327.
Artist impression of a debris disk around the sun-like star HD 181327. Image credits: NASA/ESA/CSA/STSCI/RALF CRAWFORD, STSCI.
HD 181327 is a young main sequence star located approximately 169 light years away in the constellation Pictor.
Also referred to as TYC 8765-638-1 and WISE J192258.97-543217.8, the star is about 23 million years old and roughly 30% larger than the Sun.
Astronomer Chen Zai and a team at Johns Hopkins University utilized Webb’s NIRSPEC instrument to study HD 181327.
“The HD 181327 system is highly dynamic,” Dr. Xie noted.
“There are ongoing collisions occurring within the debris disk.”
“When these icy bodies collide, they release tiny particles of dusty water ice, which are ideally sized for Webb to detect.”
Webb’s observations reveal a significant gap between the star and its surrounding debris disk, indicating a considerable area devoid of dust.
Moreover, the structure of the fragment disk is reminiscent of the Kuiper Belt within our Solar System, where we find dwarf planets, comets, and various icy and rocky bodies that may also collide.
Billions of years ago, the Kuiper Belt in our own Solar System could have resembled the HD 181327 debris disk.
“Webb clearly detected crystallized water ice not only present in the debris disk but also in places like Saturn’s rings and the icy bodies of the Kuiper Belt,” Dr. Xie stated.
The water ice is not uniformly distributed across the HD 181327 system.
The majority is found in the coldest and most distant regions from the star.
“The area beyond the debris disk contains over 20% water ice,” Dr. Xie explained.
Near the center of the debris disk, Webb detected approximately 8% water ice.
In this region, frozen water particles may form slightly faster than they are destroyed.
Closest to the star, Webb’s detection was minimal.
Ultraviolet radiation from the star can evaporate the nearby water ice deposits.
It is also possible that the interiors contain rocky bodies, referred to as planets, which are “confined” such that their frozen water remains undetectable by Webb.
“The presence of ice facilitates planetary formation,” said Dr. Xie.
“Icy materials can ultimately contribute to the delivery of resources to terrestrial planets that may form over hundreds of millions of years in such systems.”
Survey results were published in the May 14, 2025 issue of the journal Nature.
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C. Xie et al. 2025. Water ice on debris disks around HD181327. Nature 641, 608-611; doi:10.1038/s41586-025-08920-4
Jovian auroras shine hundreds of times brighter than those visible from Earth, according to a team of astronomers led by Dr. Jonathan Nichols at the University of Leicester.
These observations of Jupiter’s aurora were captured on December 25, 2023 by Webb’s near-infrared camera (NIRCAM). Image credit: NASA / ESA / CSA / STSCI / RICARDO HUESO, UPV / IMKE DE PATER, UC BERKELEY / THIERRY FOUCHET, OBSERVATORY OF PARIS / LE FLETCHER, JOSEPH DEPASQUALE, STSCI/J. NICHOLS, UNIVERSITY OF LEICESTER/M. ZAMANI, ESA & WEBB.
When high-energy particles enter the planet’s atmosphere near its magnetic poles, they collide with gas atoms, creating the auroras.
Jupiter’s auroras are not only massive in scale but also exhibit energy levels hundreds of times greater than those seen on Earth.
These auroras are primarily triggered by solar storms, where charged particles entering the atmosphere excite gas particles, resulting in vibrant red, green, and purple hues.
Additionally, Jupiter has a unique source of auroral activity—its strong magnetic field captures charged particles from its surroundings.
This includes not only those from the solar wind but also particles ejected from the volcanic moon Io.
The eruptions from Io’s volcanoes release particles that escape both the moon’s and Jupiter’s gravitational pull.
Solar storms also discharge vast amounts of charged particles towards Jupiter.
Jupiter’s immense magnetic fields accelerate these charged particles to extraordinary speeds.
When these high-velocity particles collide with the planet’s atmosphere, they excite the gas and produce radiant displays.
Thanks to the advanced capabilities of the NASA/ESA/CSA James Webb Space Telescope, new insights into Jovian auroras can be gained.
The telescope’s sensitivity enables astronomers to use faster shutter speeds to capture the rapidly evolving features of the auroras.
This latest data was collected using Webb’s near-infrared camera (NIRCAM) on Christmas Day 2023.
“What a Christmas gift; it truly astonished me!” exclaimed Dr. Nichols.
“We aimed to observe how quickly the aurora transformed, hoping to see beautiful fluctuations within about an hour.”
“Instead, we witnessed the entire aurora region illuminating the sky in a spectacular display.
Astronomers noted fluctuations in the effects caused by trihydrogen ions, known as H.3+, which varied more than previously assumed.
These observations help scientists unravel how Jupiter’s upper atmosphere undergoes heating and cooling.
Additionally, several unknown phenomena were identified in the data.
“What made these observations particularly intriguing was that the NASA/ESA Hubble Space Telescope was capturing images simultaneously in ultraviolet light,” Dr. Nichols commented.
“Strangely, the brightest light observed by Webb seemed to have no corresponding feature in Hubble’s images. This left me puzzled.”
“To produce the brightness observed in both Webb and Hubble, we would require an improbable mix of a substantial quantity of very low-energy particles impacting the atmosphere.
study Published in the journal Nature Communications.
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JD Nichols et al. 2025. The dynamic infrared aurora of Jupiter. Nature Communications 16, 3907; doi:10.1038/s41467-025-58984-z
Subneptin is a type of exoplanet characterized by high birth discharge thrombosis and lacks analogs within our solar system. Significantly smaller than gas giants, and typically cooler than Hot Jupiter exoplanets, these worlds were notably challenging to study before the launch of the NASA/ESA/CSA James Webb Space Telescope. Many subneptins are obscured by thick clouds and hazards, hindering our ability to analyze their atmospheric structures. Utilizing the Webb, astronomers have obtained the transmission spectrum of subneptin TOI-421B, unveiling its atmospheric chemical signatures.
TOI-421 is a solar-type star located approximately 245 light years away in the constellation of Repas.
Commonly known as BD-14 1137, this star is around 10 billion years old and hosts at least two giant exoplanets.
The inner planet, TOI-421B, is a subneptin with a radius of 2.65 times that of Earth and boasts a high equilibrium temperature of 647 degrees Celsius (1,197 degrees Fahrenheit).
“Prior to Webb, scientists had scant information regarding subneptins,” stated University of Maryland astronomer Brian Davenport and his team.
“These planets are several times larger than Earth, yet still much smaller than gas giants, usually cooler than hot Jupiters, and significantly harder to observe than their larger gas analogs.”
“A crucial finding before Webb was that many Neptune-like atmospheres exhibited flat or featureless transmission spectra.”
“This indicates that when scientists scrutinized the spectrum of planets transiting in front of a host star, they only observed flatline spectra, missing the details of the spectrum (chemical fingerprints revealing atmospheric composition).”
“Based on these flatline spectra observations, it was concluded that certain subneptins are extremely obscured, potentially due to clouds or haze.”
“Why did we focus on planet TOI-421B? Because we hypothesized it might be an exception,” said Eliza Kempton, an astronomer at the University of Maryland.
“This hypothesis stemmed from previous data suggesting that planets within specific temperature ranges were less likely to be shrouded in haze or clouds.”
“The temperature threshold is around 577 degrees (1,070 degrees Fahrenheit); beneath this, it was assumed that complex photochemical reactions occur between sunlight and methane gas, leading to haze.”
TOI-421B, with a temperature of approximately 727 degrees Celsius (1,340 degrees Fahrenheit), is significantly above this threshold.
The transmission spectra of subneptune TOI-421B uncover the presence of water and potential indications of sulfur dioxide and carbon monoxide, without signs of carbon dioxide or methane. Image credits: NASA/ESA/CSA/Joseph Olmsted, STSCI.
Without the interference of haze or clouds, astronomers anticipated observing a clear atmosphere.
“We identified spectral features attributable to various gases, which empowered us to ascertain the atmospheric composition,” explained Davenport.
“In many previously studied subneptins, although I inferred that their atmospheres contained specific gases, they remained obscured by haze.”
Researchers have identified atmospheric water vapor along with tentative signatures of carbon monoxide and sulfur dioxide.
However, they did not find molecules such as methane and carbon dioxide.
From the gathered data, they speculate a substantial amount of hydrogen constitutes the atmosphere.
This prevalence of lightweight hydrogen was an unexpected revelation for scientists.
“We recently came to grips with the notion that one of the initial subneptins observed by Webb has a significant molecular atmosphere.
“This implies that TOI-421B may have formed and evolved differently compared to other cooler subneptins.”
“The hydrogen-rich atmosphere is intriguing, as it resembles the composition of its host star TOI-421B.”
“By incorporating the same gases that formed the host star into the planet’s atmosphere, and cooling them, one could replicate the same gas combination.”
“This process aligns more closely with the giant planets of our solar system, differing from previously observed subneptins through Webb.”
The team’s research paper was published this week in the Astrophysical Journal Letters.
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Brian Davenport et al. 2025. TOI-421B: High-temperature Neptune with a low average molecular weight atmosphere, haze-free. apjl 984, L44; doi: 10.3847/2041-8213/ADCD76
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