Like a spectral form rising out of a cold mist, NASA’s Hubble and James Webb Space Telescopes have captured a hauntingly dynamic star-forming scene. It lies within the vast Carina Nebula, a diffuse star-forming region located about 7,500 light-years away from Earth. The small, select area both telescopes observed is nicknamed the Cat’s Head Nebula because of its resemblance to a cat sitting with its back toward the viewer. The “head” of the cat is turned to the right, revealing a glowing eye.

Though the Cat’s Head Nebula is a temporary scene that will eventually disperse as stars form and evolve over time, the region is packed with information. Hubble and Webb’s complementary views of the Cat’s Head Nebula are helping astronomers learn more about the elusive, chaotic, and complex process known as star formation. 

The distinctive “cat’s head” shape of the nebula was likely sculpted over time by the intense ultraviolet radiation and winds from massive stars in the Carina Nebula. As this stellar feedback erodes the surrounding gas and dust, denser material within the feline-shaped pillar resists erosion, at least for now.

Hubble’s visible-light view reveals an opaque, dark brown pillar of dust. The cat’s glowing red eye may indicate a young star that is still partially embedded in dust. A ridge of hazy yellow seems to follow the edge of the filament’s right side. This bright rim is consistent with gas illuminated and ionized by ultraviolet radiation from nearby massive stars, potentially driving a process known as photoevaporation.

The diffuse material surrounding the pillar glows blue and cyan above, shifting to yellow, orange, and red toward the bottom. Hubble’s filters capture light emitted by oxygen, hydrogen, and sulfur, along with starlight scattered by dust. These color variations reveal a complex mix of excited gas, dust, and stellar illumination.

Piercing Through Dust’s Darkness

Webb’s near- and mid-infrared images each offer different pieces of information to help create a more well-rounded understanding of the Cat’s Head Nebula. While the nebula’s overall structure is similar to the visible-light Hubble image, the filament becomes more transparent, and its complex surface structure becomes discernable in near-infrared light seen by Webb. On the cat’s left are ghostly wisps of dust and gas, delicate structures exposed to radiation from nearby massive stars.

Webb’s near-infrared view reveals a dense scattering of stars, shown in blue and yellow. Even in infrared light, some stars are still enshrouded in dust to various degrees. The cat’s eye remains conspicuous. The telescope’s high-resolution imagery even shows faint background galaxies, offering a partial view through our Milky Way galaxy and beyond.

In mid-infrared light, emission from warm dust and carbon-based molecules excited by starlight outlines intricate structures within the nebula. Changes in local conditions and compositions lead to variations in color and brightness. Delicate globules and strands to the pillar’s left are particularly evident in this mid-infrared view.

To the right of the pillar, a bright light source is shown as yellow in the mid-infrared image. Likely an infant star embedded in dust, it lies against reddish emission from surrounding material. A narrow filament appears to cross the source, although the image alone cannot establish whether the two are physically related.

The Hubble Space Telescope has been operating for more than three decades and continues to make ground-breaking discoveries that shape our fundamental understanding of the universe. Hubble is a project of international cooperation between NASA and ESA (European Space Agency). NASA’s Goddard Space Flight Center in Greenbelt, Maryland, manages the telescope and mission operations. Lockheed Martin Space also supports mission operations at Goddard. The Space Telescope Science Institute in Baltimore, which is operated by the Association of Universities for Research in Astronomy, conducts Hubble science operations for NASA.

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

A sweeping barred spiral galaxy marks the spot in this image, but the real treasure is the gravitational lens in the lower-right corner, where a distant background galaxy is being magnified and distorted by the gravity of a closer galaxy.

This observation is one of many gravitational lensing images taken by NASA’s Hubble Space Telescope in preparation for science with the new Nancy Grace Roman Space Telescope.

Gravitational lensing occurs when the mass of a foreground object – such as a galaxy – warps spacetime, causing light to bend, distort, and magnify as it passes around the object, similar to a giant lens in space. Lenses like this occur when a precise chance alignment takes place between the foreground and background galaxies, causing light from the background galaxy to curve around the foreground galaxy.

In this image, the gravitational lens features a foreground elliptical galaxy that is about 4.5 billion light-years away. That means the light we see from this galaxy now would have first started traveling toward us when our solar system was still forming. The background galaxy is about eight billion light-years away, almost twice as far. It appears as a pair of arcs, one large and very noticeable to the upper left of the foreground galaxy, the other a much smaller, flipped image of the same background galaxy to the lower right. This configuration is called an arc-counterarc pair.

The more massive the foreground galaxy is, the stronger the gravitational lens and the more significantly it bends light. By studying the distortion of the background galaxy, researchers can determine how much mass the foreground galaxy contains. This plays a huge role in the study of dark matter, the mysterious, invisible substance that makes up the majority of mass in the universe. The visible matter is not enough to account for the level of distortion in the background galaxy, which allows researchers to calculate both the mass of the foreground galaxy and how much dark matter it contains.

Almost all of the objects in this image are galaxies, except for a few scattered foreground stars. The barred spiral galaxy in this image – so called because its arms extend from a bar of stars in its center – is about the size of our own Milky Way galaxy, which astronomers think is a barred spiral as well. The tiny spiral to the left of the large spiral may be a satellite galaxy, similar to the Large and Small Magellanic Clouds that orbit the Milky Way.

Hubble views the cosmos primarily in visible and ultraviolet light with some infrared coverage, and Roman sees mainly infrared wavelengths and some visible light. Hubble can provide high-resolution views of individual objects, while Roman has a much larger field of view conducive to panoramas.

Images like this offer a glimpse of how Hubble and Roman will work together to build an even more comprehensive picture of the cosmos. This is just one of many gravitational lens images captured by Hubble. Astronomers will use them to analyze gravitational distortions to learn more about dark matter in the foreground galaxies and to lay the groundwork for future Roman observations.

Hubble can only view these gravitational lenses one at a time, while Roman’s wide view of the sky will provide a greater sample of these lenses. Astronomers are using Hubble’s sharp images to build a computer model to better analyze dark matter-induced distortions. This tool will help astronomers analyze Roman’s large images. Hubble will also follow up on interesting lenses Roman detects.

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Media Contact:

Claire Andreoli
NASA’s Goddard Space Flight Center, Greenbelt, MD
claire.andreoli@nasa.gov

Running complicated algorithms on quantum computing hardware is going to require the use of logical qubits, where collections of hardware qubits are linked together in ways that allow errors to be detected and corrected. In general, the more hardware qubits you dedicate to each logical qubit, the better the chances are of identifying errors. But, given that the hardware qubits are prone to errors, adding more of them also increases the probability that errors will occur. If the hardware error rate is too high, then growing the logical qubit will only make matters worse.

Fortunately, several companies have demonstrated hardware where the error rate is not too high. Several demonstrations show logical qubits are beyond the breakeven point, where adding more qubits improves performance. The problem is that the improvement isn't very dramatic. To lower error rates to levels we'll need to run complex algorithms, we'd have to add a completely impractical number of qubits to each logical qubit.

On Monday, Quantinuum announced that its current generation of hardware is capable of scaling well beyond the breakeven point. Each step up in the size of logical qubits improved some measures of their performance by a factor of over 10.

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This NASA Hubble Space Telescope image features the edge-on, intermediate spiral galaxy NGC 1827, located roughly 37 million light-years away in the constellation Columba, the Dove. Hubble captured the image as part of a survey looking at 260 satellite galaxies around 22 Milky Way-like host galaxies within a radius of about 32 million light-years from Earth. Hubble has already observed 111 of these satellite galaxies. The remaining galaxies will take an additional 149 Hubble orbits, one orbit for each galaxy, to observe.

The image, taken with Hubble’s Advanced Camera for Surveys, reveals bright-blue regions along the galaxy’s disk dotted with dark dust lanes where new stars are likely forming. A bright foreground star appears just to the left of the galaxy’s bright central bulge but is located between us and the galaxy. Its four diffraction spikes are the result of light bending around the internal supports that hold Hubble’s secondary mirror.

Low-mass galaxies like the ones in this Hubble observing program provide a way to test the predictions of cosmological models on small scales, which struggle to match observations. The data Hubble gathers will help us better understand and characterize the properties of low-mass galaxies in Milky Way-like systems, allowing researchers to refine cosmological models.

Media Contact:

Claire Andreoli
NASA’s Goddard Space Flight Center, Greenbelt, MD
claire.andreoli@nasa.gov

The Liberty Bell, with its famous crack, hasn't been rung in 180 years, but that hasn't stopped scientists from pondering what the bell might have sounded like when tolling. In honor of the nation's 250th anniversary, researchers at Penn State University have modeled its acoustic properties, drawing on data collected from one of the bell's replicas. The work was first presented at a meeting of the Acoustical Society of America in Philadelphia earlier this year, followed by an article in Physics Today.

Historians aren't sure exactly when the Liberty Bell acquired its distinctive crack, just that it occurred sometime between 1817 and 1846. An 1846 account in the Public Ledger described the ringing of the bell on February 23 that year and mentioned that the bell had developed a crack, which someone had attempted to fix by filing the sides down. But it didn't work: The February 23 ringing extended the crack even more, so much so that "the old Independence Bell ... now hangs in the great steeple irreparably cracked and forever dumb." Nobody has heard it ring since.

This wasn't the first time the bell had cracked; the rim cracked shortly after it arrived in Philadelphia in 1752, the first time the clapper struck while testing the sound. It was recast by two local foundry workers, John Pass and John Stow, not once but twice, because the first recast produced a sound that one bystander likened to coal scuttles banging together.

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Astronomers have used NASA’s Chandra X-ray Observatory to break down the cause of a remarkable formation of radio waves they have nicknamed the “Treble Clef” because its distinct shape strongly resembles the musical symbol.

The researchers discovered the Treble Clef is likely caused by an outburst from a supermassive black hole, followed by a collision of two galaxy clusters. A paper describing the findings, led by Andrea Botteon of the National Institute for Astrophysics, or INAF, in Italy, published Wednesday in the Astronomy & Astrophysics journal.

An explanation for the Treble Clef has been particularly difficult to find because the formation lies almost directly behind the plane of the Milky Way, meaning that stars, gas, and dust from our home galaxy largely block the view from Earth. However, by using telescopes that can peer through the intervening material, a team of researchers was able to identify what is responsible for this uncommon structure.

NASA’s Chandra and the German Extended RÖntgen Survey with an Imaging Telescope Array (eROSITA) X-ray telescope found diffuse, hot gas at the location of the Treble Clef, showing that a galaxy cluster hosts the object. The researchers also determined the galaxy cluster is, in fact, two clusters in the process of merging. Galaxy clusters are some of the largest structures in the universe, containing hundreds of individual galaxies and huge reservoirs of superheated gas.

This new composite image of the Treble Clef and its cluster shows the multimillion-degree gas detected in X-rays by Chandra and eROSITA in blue, with some of the Chandra data derived from a special technique the authors used to highlight important features in the Chandra data. Radio data shown in red from the LOw Frequency ARray (LOFAR), a large network of radio telescopes in Europe reveals the doppelganger of the musical notation. The final piece of the combined image comes from infrared data obtained by the United Kingdom Infrared Telescope, appearing mostly white.

The authors concluded that the Treble Clef likely formed in a two-stage process. First, an earlier outburst from a supermassive black hole in the galaxy cluster’s center drove clouds of charged particles and magnetic fields away at close to the speed of light. This led to a type of cosmic crescendo and initially produced bright radio waves that later faded as the particles lost energy. Next, the collision between the two clusters compressed or reenergized the cloud, which became brighter again in radio waves. Shock waves — similar to the sonic booms from supersonic jets — from the collision may have played a role in this reenergizing process.

To reveal evidence for the cluster collision in the Chandra data, the authors used a special technique that examined how much the cluster’s hot gas deviates from a symmetrical shape. Most of the hot gas is symmetrical and shaped approximately like an oval. The authors removed this symmetrical oval shape from the original X-ray image. The remaining X-ray emission in the residual image shows t is brightest on the left and right, and faintest in the center. The new composite image combines both the original X-ray and the residual X-ray images.

The brighter X-rays in the residual image, toward the left and right of the cluster’s center, imply that the collision between the two clusters likely occurred along the left-right direction as seen in the image. The researchers think the direct collision between the two clusters occurred a few hundred million years ago, and the clusters are now moving away from each other.

The resemblance to a treble clef is a case of pareidolia, the phenomenon when people see familiar shapes in random data, since there is no scientific connection to the musical notation.

NASA’s Marshall Space Flight Center in Huntsville, Alabama, manages the Chandra program. The Smithsonian Astrophysical Observatory’s Chandra X-ray Center controls science operations from Cambridge, Massachusetts, and flight operations from Burlington, Massachusetts.

To learn more about Chandra, visit:

https://nasa.gov/chandra

Visual Description

This release features a composite image of a remarkable radio wave formation that strongly resembles a treble clef musical symbol, hovering in the midst of two colliding galaxy clusters.

Here, galaxies in the galaxy clusters, plus foreground and background stars and galaxies, blanket the image with specks of light set against the blackness of space. At the center of the frame is a large, oval, blue-purple cloud with ragged edges. This is a multimillion-degree gas cloud in the two clusters detected in X-rays by Chandra and eROSITA, the Extended RÖntgen Survey with an Imaging Telescope Array.

In the middle of the purple field, tilting slightly to our left, is what appears to be a giant treble clef, loosely drawn with a neon pink marker. Like the musical notation for which it’s named, the formation has a strong vertical stroke with a continuous, fluid line swooping back and forth as it moves from top to bottom.

This radio wave formation appears to be the result of a two-stage process. First, charged particles and magnetic fields were driven from a supermassive black hole, producing bright radio waves. Those waves faded and lost energy over time, before being reenergized and compressed when the two galaxy clusters collided.

NASA’s SPHEREx (Spectro-Photometer for the History of the Universe, Epoch of Reionization, and Ices Explorer) space telescope is shedding light on brown dwarfs, celestial objects that blur the line between stars and exoplanets. New findings published in The Astrophysical Journal show that these dark and cloudy worlds have chemically rich atmospheres not unlike the giant planets in our own solar system. 

First discovered in the 1990s, brown dwarfs form from collapsing clouds of gas, like stars do, but they aren’t hefty enough to sustain hydrogen fusion in their cores. These dimly glowing balls of warm gas also share characteristics with Jupiter and Saturn. In contrast to most planets, however, brown dwarfs drift in darkness, ungoverned by a host star and heated entirely from within.

“They’re kind of goth,” said Zafar Rustamkulov, lead author of the new study and a scientist at IPAC, Caltech’s science and data center in Pasadena, California. “Unlike exoplanets, free-floating brown dwarfs are completely independent celestial objects that will fade into eternity alone. We’re still learning how complex they are.”

Only a few dozen of these “dark wanderers” have been studied in detail with space-based telescopes. Astronomers want to observe more of them in the wild because much of our understanding of their makeup, storminess, and evolution comes from theoretical models.

Enter NASA’s SPHEREx, an infrared space telescope launched in March 2025 and managed by the agency’s Jet Propulsion Laboratory in Southern California.

The study authors analyzed SPHEREx observations of 37 nearby brown dwarfs spanning the full brown dwarf temperature range, from about 4,000 to minus 10 degrees Fahrenheit (2,200 to minus 20 degrees Celsius). The telescope measures their brightness in 102 different colors, from the deepest red our eyes can see, to the invisible heat of infrared light, creating a spectrum. These spectra revealed to the study authors chemically rich atmospheres harboring water, carbon dioxide, carbon monoxide, and methane.

“We’re seeing the signatures of these molecules and how they change from object to object across the entire temperature regime,” said study coauthor J. Davy Kirkpatrick, a scientist at Caltech’s IPAC. “Our paper concentrated on just three dozen, but we have thousands more that we are in the process of analyzing. I really want to see what bounds the universe places on the variety of brown dwarfs.”

“From orbit, SPHEREx sees wavelengths of light that are basically impossible to see with telescopes on the ground because water in Earth’s atmosphere absorbs them,” Rustamkulov said. “We are picking up light from the deep, red clouds of brown dwarfs all over the sky.”

Sweet spot

Spotting brown dwarfs is something of a side project for SPHEREx. The space telescope takes about 3,600 unique images per day to stitch into maps of the entire sky. Knowing where hundreds of millions of galaxies are distributed across the cosmos will help scientists reconstruct what happened in the first billionth of a trillionth of a trillionth of a second after the big bang. As it scans the sky, the telescope also is searching for the chemical ingredients of life and finding interstellar ice that could one day seed oceans on distant worlds.

For years, brown dwarfs have been spotted by other observatories, including NASA’s James Webb Space Telescope and retired Spitzer Space Telescope. But thanks to its spectral coverage, SPHEREx is now imaging thousands of them for the first time in a fruitful region of the electromagnetic spectrum that spans deep red and infrared wavelengths of light.

At those wavelengths, molecules carve out distinct absorption patterns in the light shining out to space. The patterns change as brown dwarfs grow older and colder. Some of the brown dwarfs observed by SPHEREx are in a dynamic stage of life when their exotic clouds thin out, giving way to methane-rich atmospheres.

“The state-of-the-art models are capturing the general chemical trend, but when it comes to these cloudy transitions, the models are struggling to match the data,” said Rustamkulov. “No two brown dwarfs are alike. Even at the same temperature, their spectra look quite distinct.”

“The findings are a call to action to explore even more of these dark worlds,” said Kirkpatrick. “This journey has turned many of us into accidental meteorologists. We know how hard it is to predict weather on our own planet, and we realize it’s going to be just as challenging to explain the phenomena we see in these bizarre, cold objects.”

More about SPHEREx

The mission is managed by JPL for NASA’s Astrophysics Division within the Science Mission Directorate in Washington. The telescope and the spacecraft bus were built by BAE Systems. The science analysis of the SPHEREx data is being conducted by a team of scientists at 13 institutions across the United States and in South Korea and Taiwan, led by Jamie Bock, principal investigator, who is based at Caltech with a joint JPL appointment, and by JPL’s Olivier Doré, the project scientist. Data is processed and archived at IPAC at Caltech in Pasadena. Caltech manages JPL for NASA. The SPHEREx dataset is freely available to scientists and the public.

For more information about the SPHEREx mission visit:

https://science.nasa.gov/mission/spherex/

-end-

Media Contact

Calla Cofield
Jet Propulsion Laboratory, Pasadena, Calif.
626-808-2469
calla.e.cofield@jpl.nasa.gov

Written by Sally Younger

2026-069

First discovered in 2007, fast radio bursts are enigmatic, millisecond-long flashes of radio emission from the distant universe. Their origin remains uncertain, particularly since most are seen once and never again. Astronomers using NASA’s James Webb Space Telescope have pinpointed the host galaxy of the most distant fast radio burst (FRB) seen to date. Their finding has implications for what kind of energetic event creates these bursts.

“What makes fast radio bursts interesting is that we don’t know what generates them. We have theories for what objects produce them, but we don’t have conclusive proof,” said Manisha Caleb of the University of Sydney, lead author on the study published Thursday in the journal Science.

The MeerTRAP team used the MeerKAT telescope to detect the burst on March 4, 2024, leading to its designation as FRB 20240304B. The radio data from this burst suggested that it was extremely distant, possibly the most distant one seen to date. To confirm that distance, though, astronomers would need to study its host galaxy. Although they knew the location of the FRB very precisely, the world’s largest ground-based telescopes could not see any galaxy at that spot in the sky. As a result, the team turned to the Webb telescope.

Image: FRB 20240304B (NIRCam Image)

Webb’s NIRCam (Near-Infrared Camera) instrument detected a galaxy in the right location, and its NIRSpec (Near-Infrared Spectrograph) instrument provided a precise measurement of the galaxy’s redshift: 2.148, corresponding to a time just 3 billion years after the big bang. The vast majority of FRBs detected to date occurred billions of years later in cosmic history.

The team discovered that the host galaxy of FRB 20240304B was not typical of other galaxies with FRBs. Most FRB galaxies are massive star-forming galaxies, but the galaxy they found was 1,000 times less massive than they expected. 

“We thought it would be a big, nicely formed galaxy with lots of stars, and instead it was a little dwarf galaxy, although it was actively forming stars,” said Caleb. 

“The host sticks out in the whole galaxy sample that we have. And it definitely was not what we were expecting,” said Ben Stappers of the University of Manchester, United Kingdom, a co-author on the paper. “This combination of using the MeerTRAP project on the MeerKAT telescope to discover and localize these distant bursts and Webb to study their hosts is very exciting.”

The galaxy existed at the height of “cosmic noon” – a period in the history of the universe when star formation was at its peak. The galaxy’s rate of star formation suggested that the majority of its stars may have formed within just 30 million years.

This has important implications for the origin of fast radio bursts. One theory suggests that FRBs may originate from the merger of two neutron stars. However, the process of orbiting neutron stars gradually approaching closer and closer until they collide is expected to take billions of years. As a result, FRBs would be expected to be associated with older galaxies containing more evolved stellar populations.

A second theory proposes that an FRB can originate from a single, young, highly magnetic neutron star known as a magnetar through a mechanism like starquakes. In that case, once a massive star explodes as a supernova and leaves behind a magnetar, an FRB might occur relatively quickly with no large time delay. As a result, FRBs would also be expected to be found in younger galaxies like the host of FRB 20240304B.

“Our work suggests that it’s very unlikely that this FRB was produced by a merger,” said Caleb.

“Our results further show the amazing capability of Webb where we can push boundaries beyond what was previously possible,” said co-author Themiya Nanayakkara of the University of Sydney, Australia.

In addition to being a record-holder, the new FRB enabled the team to learn more about the billions of light-years of apparently empty space between the burst and Earth.

“A fast radio burst is almost like a cosmic flashlight. It lights up everything along the path. It carries an imprint of everything that it travels through, so you can use it to trace the ‘cosmic web’ – the otherwise invisible matter and structures that it encounters along the way,” said co-author J. Xavier Prochaska of the University of California, Santa Cruz.

The team found the imprint of two cosmic structures on the FRB’s signal – one previously unknown galaxy cluster at a redshift of 0.3 (about 3.5 billion light-years from Earth), and the nearby Virgo Cluster, which is located about 54 million light-years from Earth.

Image: Farthest Fast Radio Burst Host Galaxy Spectrum

In the future, the team is excited about the potential to discover more distant FRBs. They estimate that the MeerKAT telescope may be able to detect and localize several FRBs per year at a redshift greater than 1.0, meaning they existed more than halfway back to the start of the universe. As other new radio telescope facilities and instruments come online, that discovery pace may grow. The Webb telescope will be essential for characterizing those distant host galaxies.

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

To learn more about Webb, visit:

https://science.nasa.gov/webb

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Read more: Hubble Tracks Down Fast Radio Bursts to Galaxies’ Spiral Arms

Watch: Visualization of a Magnetar Generating a Radio Burst

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NASA has taken the next step in the process of developing a new all-glass telescope for the LISA (Laser Interferometer Space Antenna) mission, a space observatory designed to detect ripples in space-time called gravitational waves.

L3Harris Technologies will design, assemble, and integrate the new telescope for NASA. Called the Engineering Test Unit, this contribution represents a final step toward the future production of flight hardware. 

Led by ESA (European Space Agency), the LISA mission is slated for launch in the mid-2030s. As a collaborative partner, NASA is contributing the telescopes, other critical hardware, and engineering and scientific support as part of its mission to better understand how the universe works.

The LISA mission will deploy a trio of satellites into an Earth-following orbit, creating a vast triangular array stretching 1.6 million miles (2.5 million kilometers) on each side. Each satellite will include two telescopes that will use infrared laser beams to simultaneously transmit and receive signals between adjacent spacecraft. Through these telescopes, the spacecraft will measure miniscule changes in their relative distances, the signals of passing gravitational waves.  

“These changes are tiny, smaller than the width of a helium atom, but through them LISA will reveal a sea of low-frequency gravitational waves that we cannot currently detect through facilities on Earth,” said Ira Thorpe, the NASA project scientist for the mission at the agency’s Goddard Space Flight Center in Greenbelt, Maryland. “The LISA mission will be able to detect mergers of monster black holes billions of light-years away, map compact pairs of white dwarfs, neutron stars, and stellar-mass black holes in our own cosmic backyard, and perhaps provide new insights into gravity itself.”    

Each telescope will be entirely made of an amber-colored ceramic-glass composite called Zerodur, which is widely used in high-precision applications because it resists changes in shape across a wide range of temperatures. In 2024, L3Harris delivered a prototype telescope to NASA that served as an engineering development unit for this next step.

“We’ve put the prototype through rigorous testing, and we’re bringing everything we’ve learned into this new telescope,” said Ritva Keski-Kuha, lead for the LISA Telescope program at NASA Goddard. “This will be our last pre-flight unit and our first optical telescope delivery to ESA.” Earlier this year, in June, the team delivered a structural model of the telescope made from metal instead of glass.

Gravitational waves were predicted by Albert Einstein’s 1916 general theory of relativity and first detected by ground-based observatories in 2015. The waves form whenever massive objects accelerate, such as two stars in orbit around each other. They flow across space-time, moving at the speed of light, and are unaffected by objects they encounter along the way. These properties make them a valuable tool for probing the cosmos.

Each of the three LISA spacecraft contains a free-floating gold-platinum cube called a proof mass. The spacecraft will fly around the cube and manage its environment so the cube falls through space only under the influence of gravity. In 2016, ESA’s LISA Pathfinder mission showed that it was possible to reduce non-gravitational forces on the proof masses to the level needed for gravitational wave detection.

Additional NASA contributions include the laser system, devices to manage the buildup of electric charge on the proof masses, data analysis for identifying and characterizing individual gravitational wave sources, and additional scientific and engineering expertise.

To learn more about the LISA mission, visit:

https://nasa.gov/lisa

A cauldron of cosmic creation is being revealed in a new image from NASA’s James Webb Space Telescope. Webb has unveiled numerous stars formerly hidden by clouds of dust in a stellar nursery known as NGC 7129, which resides about 3,300 light-years from Earth.

Stars, the engines of elemental creation, have life cycles that begin with their birth in molecular clouds – cold, dense regions of dust and gas. Because of these dusty cocoons, young stars are often impossible to view by many telescopes, particularly those incapable of capturing infrared light. Webb, however, has a high degree of infrared sensitivity, allowing astronomers to peer through that dust and study the beginning of the star life cycle.

Image: NGC 7129 (NIRCam Image)

The stars from this cluster are in different stages of their development, as the more massive stars form and evolve the fastest. The most massive (and the most mature) is the region’s luminous central star, LkH(alpha) 234 (pronounced Lick-H-alpha). This star, which sports the image’s most prominent diffraction pattern, is a pre-main-sequence star weighing around 5 to 8 times the mass of our Sun. Pre-main-sequence stars like these have mostly finished gathering mass and are contracting under the force of gravity, causing their temperatures to rise. In time, this star will fuse its own hydrogen like our Sun. 

The cavity to its left, which appears in gold and spans about 3.5 light-years, is the largest demonstration of the central star’s impact. Outflows from an earlier stage of the star’s life cycle carve into the dense molecular cloud of hydrogen. Both the outflows and the star’s light energize the gas, causing it to glow. While much of this hydrogen gas is blown away, a large amount is also compressed, creating the conditions for even more stars to form. 

Interactive: The Colorful Clouds of NGC 7129

A few of these stars are visible within the cavity. Several of them are also pre-main-sequence and emit stellar winds. The nearby bow shocks, the curved compressed gas that appears near the stars, are created as those winds push into the energetic gas and create their own, smaller cavities. 

Together, the central and embedded stars also create the sharp ridge seen at the top of the golden cavity. Their light generates a hot environment that pushes against the colder and denser molecular gas outside the cavity, and creates a boundary known as a photodissociation region. In this region, the molecules of hydrogen break down into atoms. By influencing the temperature and chemistry of the region, this collection of stars offers insight into how these molecular clouds will gradually erode over millions of years. 

The region to the right of the central star narrates a different, but equally chaotic tale. This clumpy matter represented in red hides much younger objects than those on the left: protostars. The protostar stage is earlier than the pre-main-sequence stage and occurs after molecular clouds of gas and dust initially compress and fragment.

As the protostars accumulate matter and increase their mass, they eject outflows of superheated material. These outflows interact with the dense, gray, translucent matter the protostars are wrapped within, creating shocks that cause a textured appearance. The red glow is also the result of the interaction. Multiple outflows from multiple stars overlap from our point of view, leading to the scene’s chaotic look. 

Image: NGC 7129 Side-by-Side (Spitzer and Webb Image)

More of these protostellar outflows can be seen at the upper left of the image, near a blue-colored nebula. The center of this blue region hosts a protostar surrounded by a donut-shaped disk of material. This disk casts a shadow against the surrounding nebula, reminiscent of a similar structure known as the “Bat Shadow” that was observed by NASA’s Hubble Space Telescope. 

Webb’s high spatial resolution reveals many rich structures in the region’s gas, building on research done previously by NASA’s retired Spitzer Space Telescope. Astronomers will continue to use this Webb data to study how the stars and protostars in this region influence the surrounding gas and dust.

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

To learn more about Webb, visit:

https://science.nasa.gov/webb

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The following sections contain links to download this article’s images and videos in all available resolutions followed by related information links, media contacts, and if available, research paper and Spanish translation links.

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Read more: Webb’s Star Formation Discoveries

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Diligent sleuthing by astronomers has broken open a cold case in the data archive of NASA’s Hubble Space Telescope. In a study published Monday in Nature Astronomy, researchers report uncovering a surprising chemical clue that indicates the white dwarf star HS 0209+0832 may host a second-generation planet. 

A white dwarf is the remnant core of a low-mass star that has burned through all its nuclear fuel and lost its outer envelope of gas and dust to space. A second-generation planet is a world that forms around the stellar remnant from its cast-off material. 

“Rather than the white dwarf stage being a kind of epilogue to the story of a star and its planets, this research points to the systems we are familiar with only being the first chapter of a potentially much longer tale, with some new characters showing up. That’s a really exciting prospect to pursue,” said Jamie Williams, astronomer and lead author, a doctoral candidate at the University of Warwick in the United Kingdom.

Earth and the other planets in our solar system are first-generation planets, which form from material left over from a star’s birth. 

“What Hubble is showing us in this white dwarf system is something we haven’t seen before: a high abundance of the element niobium, the signature of which I was unfamiliar with when I first found it in the archival data,” Williams said.

When Hubble first observed the star in 1999, the data contained roughly 100 chemical features that could not be identified. Williams went back to those records armed with an updated chemical database and found that niobium matched many of the mystery features.

Williams explained that, while niobium is found in our solar system and has multiple uses on Earth, including in jewelry and medical imaging devices, the amount Hubble found in the HS 0209+0832 system points to a planet forming not from a star’s birth, but from the material ejected as it dies. 

“Niobium and other elements heavier than iron are astronomically special because, unlike many common elements, they are not formed in the cores of stars by thermonuclear fusion,” said Nicholas Stone, a theoretical astrophysicist at the University of Wisconsin – Madison and member of the research team. “Instead, these heavy elements can only be synthesized in the exotic conditions that briefly emerge inside dying stars. The presence of niobium is a signpost of these ‘death’ throes, and the expulsion of the dying star’s innards into space.” 

Once the star ejected this chemically enriched material, the team theorizes that some of it coalesced into a gas giant planet. The remainder of the ejecta dispersed long ago, but the planet remains.

“When Jamie asked me about niobium in relation to this study I was truly gobsmacked, as that element had not been reported in any other white dwarf analyzed to date. Once we realized it was there, everything fell into place,” said astronomer and study co-author Boris Gaensicke, also at the University of Warwick.

The research team confirmed the Hubble observations with data from NASA’s retired FUSE (Far Ultraviolet Spectroscopic Explorer) mission, which also showed strong signatures of niobium in the HS 0209+0832 system. 

NASA’s TESS (Transiting Exoplanet Survey Satellite) also observed the white dwarf for four months, allowing it to detect periodic brightness variations that indicate that a planet orbits at a distance of about 3.7 million miles (6 million kilometers), much closer than Mercury orbits the Sun. 

The research team estimates the candidate planet is a gas giant about the size of Jupiter that is rapidly losing atmosphere. Because the white dwarf star is relatively new, it is still very hot and likely blasting this planet with energy that is stripping its outer material. This could result in the planet having a comet-like tail of material that would form a disk around the white dwarf star and fall back on to its surface, leading to Hubble detecting the niobium when studying the star. Despite this mass loss, Williams said that the planet is likely not a temporary blip on the cosmic radar. 

“If the second-generation planet is there, I think it is likely to survive. Eventually the white dwarf will cool and then maintain a consistent temperature, with the planet in its stable habitable zone for millions of years,” Williams said.

Williams added that there is still a lot of work to do to understand these types of systems — how second-generation planets form, how common or rare they are, and how they evolve in orbit around a “dead” star. He’ll use Hubble to explore these questions for the next several years, hoping to build up substantial data and statistics about these new types of celestial bodies.

“I think this research is an important example of the fact that scientific discovery is not a straight path,” Gaensicke said. “It often needs that magical moment when people discuss big questions on their minds and realize that together they can find unexpected answers.”

The Hubble Space Telescope has been operating for more than three decades and continues to make ground-breaking discoveries that shape our fundamental understanding of the universe. Hubble is a project of international cooperation between NASA and ESA (European Space Agency). NASA’s Goddard Space Flight Center in Greenbelt, Maryland, manages the telescope and mission operations. Lockheed Martin Space also supports mission operations at Goddard. The Space Telescope Science Institute in Baltimore, which is operated by the Association of Universities for Research in Astronomy, conducts Hubble science operations for NASA.

In the early history of our solar system, scientists theorize that a Mars-sized object called Theia smashed into the infant Earth, vaporizing massive amounts of rock and blasting it into space. Some of that material coalesced into the Moon, where NASA’s Artemis program is returning humans, preparing for Mars, and shaping the future of space exploration.

That long-ago, violent collision reshaped our home planet. Astronomers have used NASA’s James Webb Space Telescope to examine a class of young stellar systems that show signs of similar upheavals, providing clues to the amount of energy in their collisions. The results offer insights into the composition and evolution of these chaotic systems.

The team’s findings published Thursday in The Astrophysical Journal.

Image: Extreme Debris Disk (Artist’s Concept)

The environment surrounding a star changes as it ages, beginning with a juvenile, gas-rich protoplanetary disk where forming planets can reside, before evolving to a gas-poor debris disk. During its mission lifetime, NASA’s retired Spitzer Space Telescope examined the debris disk stage and discovered a subclass termed extreme debris disks. These systems harbor unusually large amounts of warm dust close to the star, in the region comparable to where rocky planets orbit in our solar system. A team of astronomers led by Kate Su of the Space Science Institute in Boulder, Colorado investigated these intriguing objects with Webb.

Contrary to theoretical predictions, which suggest we should observe many extreme debris disks, observations indicate that these environments are rare. Scientists estimate roughly only 1% of young stars show observable signatures of this phase based on the data collected so far, including possibly our own solar system during its formation. Despite their rarity, the team was able to compile a sample of 21 extreme debris disks, including five from Spitzer’s archival data and 16 from Webb, with 12 newly observed disks and follow-up observations on four of Spitzer’s.

“This is the first time we have gathered enough systems to truly understand this subclass that we call extreme debris disks,” said Su, lead author of the paper. “Before Webb, we had limited information. We knew that they are weird and very different from the typical cold debris disks that we know, like Vega and Fomalhaut. Now that we have more data, we can pin down what these disks represent for planet formation and evolution.”

The team confirmed that extreme debris disks share three key properties: smaller dust grains than those in protoplanetary or classic debris disks, a high concentration of warm dust, and irregular brightness variations, all revealed by mid-infrared spectra from Webb and Spitzer.

To determine the driving factor for these qualities, the team studied the mineralogical makeup of the disks. They found that their sample could be categorized into silica-rich and silica-poor disks. Volcanic glass like obsidian is one example of silica-rich material found on Earth, whereas the silica-poor mineral forsterite appears as green sand grains on some beaches in Hawaii. An extreme debris disk’s category relays information on the type of collisions producing the impact debris and may help account for its variability in infrared brightness.

“To just see their mid-infrared emission and beautiful spectral features with Webb, which allowed us to identify their compositions, was the most exciting thing for me,” said Agnes Kospal of Konkoly Observatory in Budapest, Hungary, and a coauthor of the study. “We have no other way to study these planetary embryos directly because they are too small.”

Of their sample, about one-third is silica-rich, suggesting these disks are produced by high-energy impacts between Mars-sized bodies where a significant portion of the material is vaporized. The remaining two-thirds of their sample is silica-poor, indicating that the collisions are occurring on smaller scales, like grazing, between Moon-sized objects. Silica-rich disks are found only around stars younger than 300 million years, while silica-poor disks persist across a broad range of ages and often show greater brightness variability. The team proposes that this variability is driven by the rapid evolution of fresh debris through orbital changes and additional impacts.

Their findings can be applied to our own solar system, which may have experienced more than one extreme debris disk phase.

“How rocky planets formed and giant planets evolved are part of the broader story of the solar system’s formation. It’s all one story,” said Su. “Our work on extreme debris disks helps us bring together the big picture of what we currently understand.”

Image: Composition of Extreme Debris Disks Across Time

Simulations suggest that terrestrial planets, such as Earth, should form within the first few hundred million years of a solar system’s formation. This period fits with the ages of silica-rich extreme debris disks observed so far and aligns with the estimation that Earth and the Moon formed around 100 million years after the Sun formed, with the Moon likely being the result of a collision between Earth and a Mars-sized object.

As for whether our Sun underwent a silica-poor extreme disk phase, if older silica-poor disks and their random intervals of infrared brightness do reflect orbital instability, this would be broadly consistent with the Late Heavy Bombardment hypothesis for our solar system. In that scenario, the gas giant planets migrated significant distances, gravitationally disrupting the orbits of smaller bodies and triggering catastrophic collisions that generated the short-lived, dust-rich phases observed in extreme debris disks.

“Of course, there’s many things we still don’t know about these disks,” said Attila Moor of Konkoly Observatory, a coauthor of the study. “We expect no silica-rich systems among older extreme debris disks. We only have three disks in our sample that fit that age criteria, so it’ll be nice to observe more of these systems to confirm our hypothesis.”

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

To learn more about Webb, visit:

https://science.nasa.gov/webb

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A commercial mission to boost NASA’s Neil Gehrels Swift Observatory concluded without raising the spacecraft’s orbit, but the agency and industry vendor Katalyst Space have gained valuable experience that will benefit future in-space servicing programs.

“From the beginning, this was a high-risk, high-reward mission,” said Shawn Domagal-Goldman, Astrophysics Division director at NASA Headquarters in Washington. “Without intervention, Swift was going to re-enter the atmosphere by year’s end. And while we’ll be sad to see Swift’s mission come to a close, we knew this boost effort would be valuable to the agency on multiple levels — advancing U.S. spacecraft servicing technology, challenging us to meet unprecedented mission timelines, and testing how we operate satellites to extend their time in low Earth orbit. We’re very proud of how quickly this team got so far, and we’re capturing lessons learned to ensure we’re ready to go even farther.”

Swift, which launched in November 2004, was designed to study gamma-ray bursts, the most powerful explosions in the cosmos.

Over the last two decades, the observatory has revolutionized our understanding of how the universe works, from studying comets and asteroids in our own solar system and various types of cosmic explosions to flares from black holes in distant galaxies.

All spacecraft in low Earth orbit experience drag from our planet’s atmosphere. If they don’t have propulsion systems, this drag gradually reduces their altitudes. A period of increased solar activity magnified this effect on Swift.

After deciding to investigate the potential for a boost attempt, NASA had only a few months to issue a call for proposals through its Center of Excellence for Collaborative Innovation and fund design concept studies through the agency’s Small Business Innovation Research program.

In September 2025, NASA contracted Katalyst, based in Flagstaff, Arizona, to attempt the mission. The company had around one year to design, build, test, and launch a satellite that would then meet, grab, and lift Swift.

The LINK spacecraft took off from Kwajalein Atoll in the Republic of the Marshall Islands in July aboard a Northrop Grumman Pegasus XL rocket. Katalyst selected the Pegasus as the best launch option for reaching the observatory on the mission’s condensed timeline, based on the mission’s orbital and programmatic needs.

After successfully reaching space and performing initial spacecraft checkouts, LINK began experiencing intermittent communications losses and developed issues with its orientation control.

Following a period of around-the-clock troubleshooting from both teams, NASA and Katalyst agreed to scale back the mission. LINK would no longer attempt to grab or boost Swift but instead attempt to perform a series of technology demonstrations that would advance the capabilities of the U.S. commercial servicing industry.

These included exercising the spacecraft’s xenon-powered propulsion system and three robotic arms, which were designed to provide flexibility regarding where LINK could safely grapple Swift. NASA formally concluded the agency’s involvement in LINK’s mission on Sept. 3. The spacecraft re-entered the atmosphere on Sept. 25.

“LINK was built to take on a problem that did not have an easy solution,” said Ghonhee Lee, CEO of Katalyst Space. “This was an ambitious mission on an aggressive timeline. While we did not accomplish every objective we set out to achieve, in less than a year we went from mission concept to launching and operating the first commercial space robot. This is a foundation we can build on.”

Science missions like Swift take years to develop and then operate in orbit for decades. For the Swift boost, however, the most important factor was the timeline. All decision-making and risk acceptance hinged on predictions showing the observatory sinking to the point of no return — an altitude of around 185 miles (300 kilometers) — in fall 2026. As such, the boost mission required a new form of agile project management for NASA.

Swift team members in SSMO (Space Science Mission Operations) at NASA’s Goddard Space Flight Center in Greenbelt, Maryland, worked with Katalyst to develop milestones and approval processes that gave the mission the best chance of success while being flexible enough to move quickly toward launch.

Both groups received valuable input and feedback from NASA’s Engineering and Safety Center when tackling questions and issues that arose during integration and testing.

“Katalyst was committed to leveraging NASA’s deep experience to give themselves the best possible chance of successfully achieving the unprecedented challenge we gave them,” said Russell Carpenter, project manager in SSMO at NASA Goddard “Missions like these, where public-private teams work tenaciously to overcome obstacles, are an inspiration to the world, reminding us that striving for the near impossible brings out what is exceptional in all of us.”

While teams at NASA and Katalyst were racing to get LINK ready on the ground, flight controllers in Swift’s Mission Operations Center, located at Penn State in University Park in Pennsylvania, were trying to keep Swift above the critical altitude for as long as possible. Below it, any boost attempt would become increasingly difficult.

During normal operations, the Penn State team sends a plan to Swift that tells the observatory which cosmic objects and events to observe each day.

In December 2025, however, the controllers started swapping around 25% of these science targets for points on the sky that would minimize drag when Swift was trained on them. By February, the team had switched over to this approach entirely.

“Even though Swift was not executing pointed science observations from mid-February to late August, we nonetheless continued Penn State’s history of innovative space research and operations, pioneering new methods to minimize drag experienced by the spacecraft,” said John Nousek, the mission director and professor of astronomy and astrophysics in the university’s Eberly College of Science. “These changes bought valuable time for the boost mission and can be carried forward for future NASA missions.”

The team also couldn’t point too close to Earth, the Moon, or the Sun, since the brightness of all three could overheat and damage the observatory’s instruments. Pointing Swift in the most streamlined position also tilted it too close to the atmosphere, where particles could collide with the telescopes and affect future observations. The team struck a balance that managed to maintain Swift’s altitude above the critical threshold for several months.

“We’re grateful to all our collaborators for the incredible amount of time and dedication they’ve put into the boost mission,” said S. Bradley Cenko, Swift’s principal investigator at NASA Goddard. “When Neil Gehrels, Swift’s namesake, designed the observatory, nothing like it had ever launched. He would have celebrated that this boost effort was part of Swift’s legacy, that it allowed NASA to try something new and daring even though the outcome wasn’t guaranteed. That’s how we explore the universe — as a team, learning from each other, constantly pushing forward.”