The Hubble and James Webb space telescopes have teamed up to target some of the smallest, most distant objects in the solar system, discovering that the history of these tiny objects is more puzzling than we'd realized.

The two orbiting observatories collectively discovered 27 new Trans-Neptunian Objects, or TNOs, all less than 25 miles (40 kilometers) across, with the smallest being only 6 miles (10 kilometers) in diameter. As their name suggests, TNOs orbit the sun from far beyond Neptune. Some of them were born out there, at the dawn of the solar system, as small planetesimals unable to take the extra step to form planets.

Models of how these TNOs formed predicted that they should have been peppered with impacts that mixed up their surface material so that their composition, and therefore color, would be different than larger TNOs. Yet new observations, led by two PhD candidates, Anastasia Morgan of Northern Arizona University and Marielle Eduardo of the University of Victoria found the opposite – the little TNOs still look as pristine as the day they formed.

"You could imagine a scenario where getting knocked around and fragmented would change the surface composition, and then you would see a different surface color for tiny TNOs compared to their larger siblings," said Morgan, who led the color and composition analysis, in a statement. "So it's really fascinating to see that the smallest objects are somehow 'remembering' and preserving the history of how they were made."

TNOs native to the Kuiper Belt move in near-circular orbits around the sun and are level with the ecliptic plane, the imaginary flat 'disc' on which the planets and other objects orbit our star. They are said to be dynamically 'cold' because they haven't really budged since they formed.

Other TNOs, however, formed between the seventh and eighth planets, Uranus and Neptune, but before they could be assimilated into those worlds while those planets were growing, they were ejected by gravitational resonances into the region far beyond Neptune, collectively forming a 'Scattered Disk' of objects on highly elongated orbits significantly inclined to the plane of the solar system. Such TNOs are referred to as being dynamically 'hot'.

Yet even the 'hot' TNOs seem to have resisted any changes to their surface composition.

"These dynamically hot TNOs retain a signature of where they were born, even though they've been orbitally scrambled since then," said David Trilling of Northern Arizona University.

This leads to one of two surprising possibilities. Either there are far fewer impacts taking place far from the sun than astronomers thought, which doesn't match with what we think we know about the population density of objects out there, or the impacts and collisions do take place but for some reason do not tear up the surface of the small TNOs as much as we might expect.

Thanks to the James Webb Space Telescope's (JWST's) infrared vision, Marielle Eduardo was able to figure out the size distribution of the TNOs. When we look in visible light, how bright a TNO appears depends in part on how reflective its surface is, a property referred to as albedo. A larger body with a composition that isn't very reflective might appear fainter at the same distance as a smaller object covered in shiny ice.

However, at infrared wavelengths the brightness of an object is dependent mostly on its size, allowing accurate determinations of the diameters of the 27 TNOs. Surprisingly, there seem to be fewer of the very small TNOs than what models of their formation predict.

"It's very interesting that the process of planetesimal formation ends up producing the same distribution of sizes for both cold and hot populations, despite forming in different regions of the early solar system," said Eduardo. "The process seems to be insensitive to [planet-forming] disk conditions, producing similar planetesimal sizes whether the disk is hot or cold, and dense or fluffy."

These observations push Hubble's and JWST's abilities to the limit. The TNOs are incredibly faint, shining between magnitudes 24.1 and 29.3, described as being equivalent to seeing a swarm of fireflies on the moon from Earth. As such, it is the deepest survey yet into the relatively unknown realm beyond Neptune, just as you'd expect from these two powerful space telescopes getting together.

The research was published in The Astronomical Journal as two separate papers on Sept. 8, one on color and composition, the other on the size distribution of the TNOs.

Using the James Webb Space Telescope (JWST), astronomers have discovered that the ring system of a tiny solar system body is even more interesting than they knew.

The object in question is Chariklo, which orbits the sun between Saturn and Uranus, at around 17 times the distance between Earth and the sun. Despite only being around 155 miles (250 kilometers) wide, Chariklo, part of the Centaur family of asteroids, possesses two thick rings.

Though Saturn is the solar system body most famous for its rings, other planets also have ring systems, albeit less prominent. That includes Uranus, Neptune, and Jupiter. However, Chariklo and the even smaller body Chiron, show that even the most diminutive bodies can develop rings. Now, thanks to the incredible sensitivity of the JWST, scientists know that the rings of Chariklo are even stranger than their initial discovery in 2013 suggested.

The team, led by researchers from the Institute of Astrophysics of Andalusia (IAA-CSIC), began observing Chariklo with the JWST in Oct. 2022. They used a technique called stellar occultation, which measures the decrease in light from a star when an object passes in front of it.

"By comparing JWST observations with those obtained during other stellar occultations over the last decade, we discovered opposite changes in the two rings: while the inner ring shows significantly higher opacity, the outer ring shows lower opacity," team leader Pablo Santos-Sanz of the IAA-CSIC said in a statement.

The changing rings of the asteroid suggest that it experiences more complex physics than previously thought. This is important because scientists had previously believed that small bodies had relatively stable rings.

"Our results force us to rethink how they form, how they evolve, and what mechanisms maintain their stability," Santos-Sanz said. "The ability to detect these changes opens a new window for understanding the evolution of these systems and, possibly, that of other ring systems in the solar system."

The cause of these changes remains a mystery.

Another milestone for the JWST and Gaia

The research doesn't just represent an important step in our understanding of asteroids and solar system rings, but it is also an important milestone for the JWST.

"Achieving this required knowing with extraordinary precision the orbit of Chariklo, the position of the star, thanks to the European Space Agency’s Gaia mission, and the trajectory of JWST itself around the L2 Lagrange point, a region of space located about 1 million miles (1.5 million kilometers) beyond Earth, away from the sun," team member Yücel Kilic of the IAA-CSIC said. "The JWST follows an orbit around this region that requires periodic corrections through station-keeping maneuvers."

During the occultation the team used in their research, Chariklo was traveling at around 5,600 miles per hour (2.5 kilometers per second) relative to the JWST.

This is incredibly fast by Earth standards, but relatively slow for objects racing through the solar system. This low speed allowed the rings of Chariklo to be resolved in unprecedented detail. Astronomers currently rely on occultation to study Chariklo and its rings, as even the JWST isn't powerful enough to directly image this small and distant asteroid.

The team's research was published on Tuesday (Sept. 9) in the journal Science Advances.

Astronomers have witnessed a small, icy body that orbits the sun out beyond Jupiter transforming into a comet, providing a missing link between comets and inert bodies called centaurs.

The object in question is called 450P/LONEOS and is named after the Lowell Observatory survey that found it back in 2004. It is a centaur, which is a breed of inactive body that orbits the sun between Jupiter and Neptune. These objects are thought to have wandered in from the Kuiper Belt beyond Pluto, their paths perhaps perturbed by distant gravitational interactions with the gas giant planets, or even a nudge from a passing star.

Because a given centaur's orbit crosses the path of at least one of Jupiter, Saturn, Uranus and Neptune, a centaur's orbit is unstable over millions of years. Consequently, the giant planets can push them even closer to the sun or kick them out of the solar system entirely.

It has long been suspected that those pushed closer to the sun turn into what are called Jupiter-family comets, which are comets with orbital periods around the sun of less than 20 years and which are influenced by the gravity of Jupiter.

To date, no one has ever seen a centaur turn into a Jupiter-family comet. The orbital period of 450P is currently 22 years, so it isn't a Jupiter-family comet yet, but astronomers led by planetary scientist Charles Schambeau of the University of Central Florida have been observing the onset of comet-like behavior on the centaur. In particular, using the Gemini North telescope in Hawaii they have seen the formation of a cloud of gas and dust called a coma around the solid nucleus of 450P, with this coma brightening in the period between 2019 and 2024, when 450P arrived at perihelion (the closest point to the sun in its orbit).

Should 450P keep up this comet-like behavior and receive one more gravitational nudge from one of the giant planets, then it could finally become a Jupiter-family comet.

"Studying objects like 450P helps us connect different stages of small-body evolution," said Schambeau in a statement. "Centaurs are likely related to trans-Neptunian objects, and some will eventually become short-period comets. By studying their activity, surface properties and volatile [substances with low boiling or sublimation points such as water and carbon dioxide] composition, we can learn how comet nuclei change as they move inward through the solar system, how long they preserve primitive ices and what physical processes turn an otherwise quiet icy body into an active comet."

Using the James Webb Space Telescope (JWST), Schambeau's team analyzed 450P's coma, finding carbon dioxide gas and suggestions of particles of crystalline ice and dust.

Its transition from a centaur into a comet is thought to have resulted from 450P having a date with destiny. By tracking back its orbit to before its 2004 discovery, astronomers found that 450P had come within 2.9 million miles (4.6 million kilometers) of Saturn in 1992. That's pretty close on solar-system scales. The object's gravitational interaction with the ringed planet caused 450P's orbit to significantly shorten so that its perihelion is now at 5.4 astronomical units 506 million miles, or 813 million km), which is only slightly beyond the orbit of Jupiter at 5.2 astronomical units.

Its last perihelion was in August 2024 and, by getting closer to the sun, 450P received substantially more heat than it has in the past.

"That increased solar heating can warm the surface and the subsurface layers of the nucleus," said Schambeau. "As those layers heat up, volatile ices or trapped gases can be released, which can drag dust away from the surface and produce a coma."

The significance of the JWST's discovery of carbon dioxide gas in 450P's burgeoning coma, coupled with the complete absence of water vapor, tells us that it is carbon-dioxide driving the activity on 450P.

"At 450P's distance from the sun, the nucleus is too cold for normal water-ice sublimation to be the main activity source, so detecting carbon dioxide gives us an important clue about what is powering the coma," said Schambeau.

While there is no water vapor, JWST has picked up hints of solid particles of crystalline water-ice.

"The possible crystalline water-ice is also interesting because it suggests that some of the ice in the coma has experienced heating or physical processing, rather than remaining completely unchanged since formation," said Schambeau.

On pristine cometary bodies and Kuiper Belt objects, ice is usually in an amorphous state, meaning the frozen water molecules are not structured or arranged in any particular way, giving the ice a porous composition that allows it to trap pockets of gas. As 450P nears the sun, the extra warmth that it receives causes the amorphous ice to morph into crystalline ice that has a more regular structure. During the transformation the gases escape, dragging dust and ice particles off the surface with them. Therefore, the presence of crystalline ice is telling us that 450P is in the process of being thermally altered from its pristine state that quite possibly harkens back to the birth of the solar system 4.5 billion years ago.

Only a very small fraction of Centaurs have ever shown signs of activity, which makes 450P's recent perihelion a very important one to have studied because it is a rare example of an early stage in a centaur's transition into a comet.

"Centaurs are scientifically important because they are thought to be transitional objects that originated further out in the solar system and are slowly evolving toward becoming Jupiter-family comets," said Schambeau. "In that sense, they give us a way to study relatively primitive material from the outer solar system while it is beginning to respond to stronger solar heating."

The findings have been accepted for future publication in the Planetary Science Journal and is currently available on the arXiv pre-print archive.

NASA's next big space telescope has left Earth, but it's not ready to start observing the heavens just yet.

The Nancy Grace Roman Space Telescope launched yesterday (Aug. 30), riding a SpaceX Falcon Heavy rocket into the heavens. Astronomers are very excited about Roman, for it's expected to discover thousands of new exoplanets and shed light on mysterious dark energy and dark matter, among other accomplishments.

Such science work is a few months off, however. Here's a brief rundown of the next steps for the Roman team.

A long journey

The first order of business is getting Roman to its destination. The 42-foot-long (12.7 meters) scope isn't staying in Earth orbit; it's headed to the sun-Earth Lagrange Point 2 (L2), which lies about 930,000 miles (1.5 million kilometers) from our planet in the Marsward direction.

There are multiple reasons to target L2, which also hosts NASA's James Webb Space Telescope (JWST) and Europe's Euclid probe.

"At this special place in space," NASA officials wrote in a Roman explainer, "gravitational forces balance to keep objects in steady orbits with very little assistance."

"Roman's barrel-like shape will help block out unwanted light from the sun, Earth and moon, and the spacecraft’s distant location will help keep the instruments cool," they added. "The thermal stability of an observatory at L2 will provide a ten-fold improvement beyond Hubble in much of the data Roman will gather."

And don't worry about Roman and JWST bumping heads; though their cosmic addresses will be the same, they won't actually share space.

"Like Webb, Roman will trace out a large orbit around the actual L2 point — much larger than the moon's orbit around Earth — and the two will easily be kept far apart," NASA wrote in a different Roman piece.

It'll take Roman about 30 days to fly out to L2 and settle into its looping orbit there. A new round of work will then begin for the Roman team.

Checking Roman out

That work is "commissioning" — making sure that all of Roman's systems and subsystems are working properly, as is its science gear, which consists of the Wide Field Instrument (WFI) and the Coronagraph Instrument (CGI).

WFI "is a 300-megapixel infrared camera that will allow scientists to look very far back in time," NASA officials wrote in the explainer. "Seeing the universe in its early stages will help unravel how it has expanded throughout its history, which will hint at how it may continue to evolve."

CGI is a technology demonstration that will block the light of distant stars, allowing Roman to spot a wealth of previously unknown alien worlds.

"It will be far more powerful than any other coronagraph ever flown, seeing planets that are almost a billion times fainter than their host star," NASA officials wrote.

Roman should be ready to begin its science work in early 2027, according to the nonprofit Planetary Society. Its science life is slated to last five years, but astronomers are doubtless hoping for more. And there's precedent for such optimism; after all, NASA's Hubble Space Telescope is still going strong today, more than 36 years after its launch.

Hubble is a special case, given that astronauts repaired and upgraded it over the course of five servicing missions between 1993 and 2009. But other NASA space telescopes have far outlasted their warranties without such help. For example, the Chandra X-ray Observatory is operational in Earth orbit today, more than 25 years after its launch — and it has overcome budget issues along the way.

Using the James Webb Space Telescope (JWST), astronomers have studied 72 young, sun-like stars. As a result, they found that forming planets is a real race against time.

This is because the material that serves as the building blocks for planets is constantly escaping the swirling platters of gas and dust, or protoplanetary disks, that wrap around infant stars. Some types of planets may find their formation window closing sooner than others.

The team's research represents the most in-depth investigation yet into how matter escapes these protoplanetary disks and how this escape gives rise to different stages of planet formation around sun-like stars. All in all, the study helps paint a better picture of how and why our solar system took the shape it did around the infant sun around 4.6 billion years ago.

"Gas giants like Jupiter must assemble their massive atmospheres while the disk is still substantial enough to supply them, before winds and jets carry that raw material away into space," team leader Naman Bajaj from the University of Arizona said in a statement.

An ill wind blows around infant stars

The team conducted its research using data collected by the JWST’s Mid-Infrared Instrument (MIRI). The scientists tracked matter loss by following the movements of molecular hydrogen, one of the most common molecules in protoplanetary disks. Each of the stars involved in the investigation represented a different stage in the early life of a star system. That meant putting these snapshots together allowed the researchers to create a "movie" detailing the early life of a planetary system.

One of the most important findings of this approach is the mechanisms for material loss from protoplanetary disks seem to evolve and switch dominance as an infant star ages.

This is important because gas giants like Jupiter and Saturn have vast atmospheres. They thus require more raw material to form than smaller rocky worlds like Earth do. Understanding matter loss allows scientists to determine at what stages of protoplanetary disk evolution gas giants can form.

"What is exciting about this study is that we can now see, across a large sample of young systems, how the mechanisms that remove gas from planet-forming disks change with time," team member Uma Gorti from the SETI Institute said in the statement. "Disk dispersal sets a fundamental clock for planet formation: once the gas is gone, the opportunity to build gas-rich planets is essentially over."

The researchers found that early in the evolution of protoplanetary disks, powerful, magnetically driven jets and winds dominate mass loss. These jets and winds are powered by magnetic fields that weave through protoplanetary disks.

Later, as the disk thins and starlight can pass through it more easily, these winds and jets weaken, and magnetic processes are dominated by high-energy radiation from the infant star ionizing gas and blowing it into space. The latter process is called photoevaporation.

All this reveals there is no one single process responsible for stripping planet-forming material from around infant stars. The research also demonstrates the JWST is more than capable of studying the dispersal of gas and dust around individual infant stars.

The next step for the team is to discover just how much material these different mechanisms shift. The scientists could also look into the areas of the disks in which the mechanisms studied operate. Down the line, this will help develop a model to reveal just how rapidly planet-formation is shut off — and in which regions of a protoplanetary disk different types of planets are most likely to form.

The team's research was published on Tuesday (August 25) in The Astronomical Journal.

A trio of NASA space telescopes teamed up to capture a gorgeous new look at the glowing spiral galaxy NGC 4258 and its two anomalous extra arms.

What is it?

This image shows NGC 4258, also known as Messier 106, a spiral galaxy located some 24 million light-years away in the constellation Canes Venatici, the "Hunting Dogs." It is a fairly bright galaxy and can be viewed in the spring sky in the Northern Hemisphere with most telescopes.

Messier 106 is noteworthy for having two "anomalous" extra arms, the long curved regions of bright gases, dust and young stars that are characteristic of all spiral galaxies. But while most spiral galaxies have only a pair of arms, Messier 106 has two pairs. According to NASA, the extra set is composed of hot gases that are churned away from the galactic center by the supermassive black hole at the heart of NGC 4258.

Why is it incredible?

This image shows off the incredible teamwork that NASA's flagship orbital observatories can pull off. It combines X-ray observations from NASA's Chandra X-ray observatory (seen here in royal blue), optical light gathered by the Hubble Space Telescope (red, yellow and pale blue), and infrared light seen by the James Webb Space Telescope (bright orange).

By combining multiple types of light into one image, NASA is able to reveal the complete picture of what this energetic galaxy is made of.

The image also shows the incredible power of the black holes found at the centers of galaxies. "M106 helps show how supermassive black holes can create structural features that mimic star-bearing spiral arms, influencing a galaxy's evolution," NASA wrote in a statement accompanying the image.

This image was part of a NASA release of 16 new "galactic gems" captured by Chandra and other observatories.

Even if you aren't the kind of person who often looks up the latest space images, it's hard to navigate life (especially on the internet) without running into a few. Try choosing a new iPhone background and you'll have your pick of sharp, gray moon portraits. Watch an old "Star Trek" episode and you may not realize how many of those translucent nebulas outside the spaceship's windows were based on real, hard data.

When it comes to space, we're spoiled. Mind-bending objects light-years away from us have managed to become integrated into our everyday lives — and though we're still a ways away from understanding the true nature of the universe, we're also the closest we've ever been. It's in large part thanks to how impeccable our fleet of space telescopes is. In seconds, you can find a Hubble Space Telescope Deep Field with luminescent galaxies warped along the curvature of spacetime and James Webb Space Telescope images of strange hazy red objects from just after the dawn of time.

Moreover, what's tremendously exciting is this fleet is constantly growing. Indeed, very soon, a new space telescope will launch from NASA's Kennedy Space Center in Florida. It's called the Nancy Grace Roman Space Telescope, and it should be able to unlock a new level in the astronomy layer of our lives. It will show us new types of images, reveal new types of data and lead us in directions we may not yet know are possible.

What is Roman?

To put it succinctly, the Nancy Grace Roman Space Telescope is an approximately 42-foot-long (12.7-meter-long), cylindrical metal observatory scheduled to lift off from our planet on Aug. 30 aboard a SpaceX Falcon Heavy rocket.

Across a five-year-long mission (a 10-year-long one if everything goes well), Roman is meant to use two powerful instruments — the Wide-Field Instrument (WFI) and Coronagraph Instrument — to image huge swaths of the cosmos and tackle some crucial questions. It will help scientists probe the mysteries of dark matter and dark energy, directly image exoplanets near and far, witness an extensive amount of stars exploding in colossal supernovas and more.

But whether or not it's a fair thought, it's hard not to want to compare the specifications of this space telescope to some of the others that have brought the cosmos down into our daily lives. This is particularly true for two of the major players right now: the James Webb Space Telescope and the Hubble Space Telescope.

What can Roman do that these two cannot?

Roman vs. Hubble

To start, one of the biggest benefits of Roman over Hubble is its processing power.

By numbers, that means Hubble has managed to gather about 400 terabytes of data over its approximately 35 years of service so far. Roman is expected to be able to create 500 terabytes of data every single year.

"Its surveying capabilities are over 1,000 times faster than Hubble, and can chart 200 times more sky in a single image," NASA administrator Jared Isaacman said during a press conference about Roman in April. "What would take Hubble 2,000 years to process, Roman can do in a year — the images it captures will be so large there is not a screen in existence large enough to show them."

Roman's primary mirror is about 7.9 feet (2.4 meters) wide, which is actually the same as Hubble's. Primary mirrors are arguably the most important aspect of a space telescope, because it's how an observatory manages to gather light coming from the universe. Bigger mirrors can collect more light, which allows them to see dimmer or more distant objects. Interestingly, Roman's primary mirror is also about 80% lighter than Hubble's. Roman has a secondary mirror as well; it's just under 2 feet (0.5 meters) wide. Hubble's secondary mirror is very similar at exactly 12.2 inches (0.3 m) in width.

Yet even though Roman's mirrors are so comparable to Hubble's, because of Roman's processing power as well as the capabilities of its WFI, it will be able to image a far wider stretch of sky than Hubble can.

Though Roman does have some visible light capabilities like Hubble, WFI specializes in infrared light — actually the kind of light the JWST works with, but we'll get to that telescope comparison shortly — so we should compare it to Hubble's infrared instrument. The WFI's field of view is about 100 times greater than the Hubble infrared instrument's field of view.

According to NASA, this view will allow Roman to measure light emanating from a billion galaxies and billions more cosmic phenomena over its years of service.

"Both observatories will perform spectroscopy," NASA explains, "which involves splitting light into individual colors to study patterns that reveal detailed information. But Roman's spectral studies will have lower resolution over a large area, while Hubble's has higher resolution over a small area."

This concept really sums up the difference between the two telescopes, and in fact foreshadows what we'll soon discuss about the JWST.

Roman vs. the JWST

The main similarity between the Roman Space Telescope and the JWST is those infrared light goggles.

Infrared light, unlike visible light, is invisible to human eyes. You can think of it more like a heat signature. Firefighters, for instance, use infrared trackers on burning buildings from the outside to see where the source of the fire might lie within. And when it comes to astronomy, infrared light is priceless — that's why the JWST's strong infrared capabilities give it an advantage over Hubble.

Infrared light's role in astronomy observations has to do with the way light moves throughout the universe. As light from a distant region of space moves toward us — through a continuously expanding universe, no less — those light wavelengths stretch out from tight, bluer ones into long, redder ones. Eventually, the wavelengths stretch out into the infrared region of the electromagnetic spectrum, which is the part of the spectrum we cannot see with our own eyes. Plus, any objects in our line of sight that are hidden behind dense clouds of interstellar dust or gas can only be seen via their infrared emissions.

What this means is that very, very distant objects as well as concealed objects in space are pretty much invisible to us, hiding in the infrared part of the spectrum. We therefore need infrared decoders, like the JWST's suite of tools or Hubble's infrared instrument, to reveal them.

The JWST has already made absolute strides in this regard, revealing to us peculiar objects from the early years of the universe, consistently breaking its own record while finding the most distant galaxies we've ever seen and revamping Hubble portraits like the spectacular Pillars of Creation with its infrared filter. It's even reintroduced us to our own solar system with crisp views of Neptune's frail, oft-forgotten rings and Saturn's big, bright ones.

When it comes to mirrors, the JWST's iconic golden primary mirror made of 18 hexagonal segments is a beautiful 21 feet and 4 inches (6.5 meters) across, which is much larger than Roman's. This means the JWST can collect tons more light than Roman can, which makes a lot of sense because it was built to see as deep into the ancient universe as possible.

But where the JWST lacks is, you guessed it, its field of view. This is on purpose. The whole point of JWST is to pierce into the universe with a highly narrow view in order to get great resolution on whatever it's looking at. Roman definitely won't be getting that same resolution, as its images will be shallower than the JWST's, but its WFI will see a region 50 times wider than what the JWST can see.

To be clear, there are indeed other survey telescopes that are able to image huge amounts of the sky at once, but Roman's version of doing this is expected to be with higher clarity. For example, the ground-based Rubin Observatory is revolutionary for the vast amounts of data it's able to collect while scanning a new section of the sky every 40 seconds. However, Rubin is on the ground. A space telescope sits above Earth's atmosphere, and therefore has less atmospheric interference to sift through. This makes the observations way better.

Okay, you've probably figured out the moral of the story at this point: Roman's reach is shallower than Hubble's and the JWST's, but extremely wide. So, what's the benefit of this enormity?

The promise of Roman

Imaging huge amounts of the universe in one go is of foremost importance because things in the universe happen simultaneously. A supernova on one end might be worth checking out, but a fleeting fast radio burst buzzing on the other end of the cosmos could be just as vital to study. Yet, with a narrow field of view, you'd have to select which target to zoom in on. And if you aren't sure which targets are even options, while perusing an ancient black hole with immense resolution you will most definitely miss an even older one that lurks 50 frames or so away.

With Roman, scientists won't have to be as selective about which parts of the sky they scan. Roman is designed to be able to capture the supernovas, fast radio bursts, black hole emissions and warped galaxy candidates all at once. For example, NASA explains how Roman will be able to spot colliding neutron stars — stellar corpses so dense a tablespoon of one is equal to the weight of Mount Everest — with its infrared view. The JWST would likely never even come across such an event due to its tunnel vision.

Of course, Roman won't be able to image these objects with as much depth as the JWST or Hubble — or several other telescopes for that matter, like maybe SPHEREx or Euclid — but it will be able to notice that these objects exist.

The next step would be to have one of those other telescopes follow up on the targets. You can think of Roman as creating the Google Maps of hotspot locations in the universe that the JWST, Hubble or another telescope may want to examine someday.

Big field of view means big science

Furthermore, capturing information from billions of objects in such a short period of time will enable specific kinds of research, such as the hunt for the truth about dark matter and dark energy. Despite collectively making up about 95% of the universe's contents, dark matter and dark energy aren't visible to us. However, we know dark energy exists because it appears to be applying a force that accelerates the expansion of our universe and we know dark matter exists because it seems to be the glue around galaxies that prevents them from falling apart like horses on a merry-go-round spinning too fast.

What this means is imaging tons of galaxies at once could allow scientists to have a better picture of how those interactions between the dark universe and our regular universe play out. Roman will also be able to create time-lapse "movies" of the universe in three dimensions and offer scientists the chance to see how other observations fit into that picture.

It would also be remiss not to mention what Roman's other instrument can do: the coronagraph. The telescope's coronagraph is actually one-of-a-kind. You can think of it like a special artificial eclipse that brings objects into view that would otherwise be obscured by bright starlight. No other space observatory in service right now has the ability to directly image exoplanets like Roman will be able to using that coronagraph. It would take an entire other article to explain the awesome complexities of this instrument — an article that you can definitely expect soon — but to go through the basics, this tool will block out the glare of distant stars and then measure the polarization of light around them in order to help scientists tease out exoplanets orbiting those stars.

According to NASA, Roman's coronagraph will be able to detect planets 100 million times fainter than their stars. That capability is about 100 to 1,000 times better than existing space-based coronagraphs. This will give scientists the opportunity to study planets beyond our solar system that are dimmer, colder, farther and more elusive than what we're currently able to see.

With all this in mind, there is an important concept to remember.

When the JWST first entered service in the year 2022, everyone (including me) started comparing it to Hubble and thinking of it as Hubble's upgrade. It's hard not to, especially when the images rolling out of a shiny new telescope are so utterly gorgeous. But "upgrade" couldn't be farther from reality. The JWST is just different. Impressive, sure, but different. The goal is for all of these telescopes to work together, each one giving us a new sheet of the universe to explore. Stack up all the sheets, and you'll get the full picture.

Roman will simply be offering us one breathtaking new sheet.

Sometimes, incredibly powerful space telescopes work together to accomplish amazing things. Recently, observations made by both the James Webb Space Telescope and Hubble were combined in a composite image that shows the incredible nature of the "Black Eye Galaxy," more formally known as Messier 64.

What is it?

The Black Eye Galaxy is a strange spiral galaxy located 17 million light-years from Earth, in the constellation Coma Berenices, a name that means "Berenice's Hair" in Latin.

Discovered in 1779, the Black Eye Galaxy is fairly isolated from other galaxies and is known for its hypnotizing "stare." This look is created by the galaxy's internal, swirling motion. However, unlike many other spiral galaxies, the gas in the outer reaches of this one rotates in the opposite direction to the gas and stars closer to its center, creating an especially unusual motion.

To capture this incredible composite view of the galaxy, astronomers combined near and mid-infrared wavelength observations made by JWST and ultraviolet, visible and near-infrared observations made by Hubble.

Why is it incredible?

As we look forward to observations from NASA's upcoming flagship space observer, the Nancy Grace Roman Space Telescope, this collaborative effort shows how such powerful instruments don't replace one another; rather, they bring different capabilities to the table and can complement each other.

And, while this new image is the result of a team effort of cutting edge-technology, the Black Eye Galaxy is also a favorite target for backyard astronomers because it can often be spotted in small telescopes.

The heart of the Milky Way may be more hospitable to water than astronomers thought.

Using the James Webb Space Telescope (JWST), researchers detected water and cosmic dust around an aging star only 0.55 light-years from Sagittarius A* (Sgr A*), the supermassive black hole at the center of our galaxy.

The new study suggests that water and dust can form and survive surprisingly close to a supermassive black hole, where intense radiation and other harsh conditions might otherwise be expected to destroy them. The team used Webb's Mid-Infrared Instrument (MIRI) to study IRS 3, an aging star located in the crowded environment surrounding Sgr A*, which has a mass of about 4 million suns, according to a statement from the European Space Agency (ESA).

"Galactic centres are among the most extreme environments, so understanding whether stars can continue enriching their surroundings there is an important question," Florian Peißker, lead author of the study from the University of Cologne in Germany, said in the statement. "With Webb, we can directly observe how stars behave under these conditions and see that dust production remains remarkably resilient."

IRS 3 — one of the brightest mid-infrared sources in the galactic center — is an asymptotic giant branch star, meaning it has reached a late stage of stellar evolution in which it sheds large amounts of gas and dust through powerful stellar winds. Such dying stars act as cosmic recycling centers, returning material to space that can eventually become incorporated into future generations of stars and planets.

But IRS 3 lives in a particularly unforgiving neighborhood. The center of the Milky Way is densely packed with stars and exposed to intense radiation, raising questions about whether molecules and newly produced dust can persist there.

However, Webb's observations suggest they can. By combining observations of IRS 3's spectrum with simulations of how its light travels through different models of the surrounding material, researchers reconstructed the structure of the star's envelope. They found a layered, shell-like distribution of silicate dust extending roughly 10,000 astronomical units from the star (one astronomical unit, or AU, is the average distance between Earth and the sun). Temperatures within the envelope fall from about 1,700 degrees Fahrenheit (927 degrees Celsius) near the star to around minus 280 F (minus 173 C) in its outer regions. Webb's observations also revealed clear evidence of water within the envelope — the first such detection for IRS 3.

"The detection of water is especially exciting because it shows that molecular material can survive in an environment dominated by intense radiation," Macarena Garcia Marin, co-author of the study and an ESA astronomer, said in the statement.

While the observations don't reveal how much water is present, the detection shows that water can survive in the harsh environment near the galactic center. Water and dust are important ingredients in the chemistry that accompanies star and planet formation, meaning material shed by aging stars such as IRS 3 could eventually contribute to future generations of stars and planets.

Finding water and dust near Sgr A* therefore suggests that aging stars can continue enriching their surroundings even in the harsh conditions near a supermassive black hole. The findings could help astronomers better understand how material is recycled in the centers of galaxies and the role evolved stars play in supplying those regions with fresh dust and molecules.

Their findings were published Aug. 11 in the journal Astronomy & Astrophysics.

The most distant 'black hole star' yet found, existing in the universe less than 660 million years after the Big Bang, has provided a vital clue as to the origin of the mysterious "little red dots" that populate the James Webb Space Telescope's images of the early universe.

The consensus seems to be that these bizarre objects, which were first discovered in 2022, are growing supermassive black holes entombed within huge clouds of gas that have spectrums similar to cool, red stars, such as red giants. Recently, astronomers have been finding that some of these objects are placed within the center of young galaxies whose light has been traveling for about 12 billion years, give or take a billion, to reach us. Given their distance and faintness, black hole stars' light is difficult to disentangle from the light of a surrounding galaxy, especially when we know there is likely a galaxy there that's too faint for the JWST to resolve.

However, a newly discovered black hole star, unearthed during a JWST program called the Mirage or Miracle (MoM) survey, is acting as a kind of a missing link.

"The Mirage or Miracle survey was designed specifically to target sources considered 'risky,' meaning they could either be amazing discoveries or just interlopers, such as some cold nearby stars that look like distant galaxies," Jorryt Matthee of the Institute of Science and Technology Austria and a co-investigator on the MoM survey said in a statement. In particular, the survey focuses on objects that look like they could be very high redshift galaxies (around a redshift of 10 or more, which equates to having existed about at least 13.1 billion years ago).

The black hole star found by the survey has been named MoM-BH*-1 and is the best example yet of a "naked" black hole star, meaning astronomers are fairly certain it exists in space on its own rather than inside a burgeoning galaxy. This means all of its light is generated by accretion onto the black hole at the center of the cloud. Though we cannot see this accretion because of the obscuring gas cloud, this light energizes the surrounding cloud from within, causing it to glow just as energy generated within the sun causes its outer layers to radiate.

"The spectrum we detected is our best evidence of a cloak of gas feeding an early forming black hole," Rohan Naidu of the University of Hawaii, who led the team who discovered MoM-BH*-1 and is co-leader of the MoM survey, said in the statement.

Intriguingly, MoM-BH*-1 lies close in space to a young galaxy at the same redshift, and estimates suggest that it will take another 100 million years for the black hole star to collide and merge with the galaxy. Naidu and Matthee's team modeled what the spectrum of the galaxy would look like after it has merged with MoM-BH*-1, and found that it would look very much like the little red dots already known to exist within galaxies.

"Considering the black hole star as a template for the black hole component of little red dots helps clarify many of the uncertainties about them," said Matthee. "If embedded in similar host galaxies, black hole stars like MoM-BH*-1 might well serve as the central engines of baby quasars."

In this way, MoM-BH*-1 provides strong evidence for the object at the heart of faint galaxies encompassing little red dots as being a black hole star. Recent observations of some little red dots at lower redshifts have shown the cloud of gas around the black hole begin to disintegrate, exposing the black hole and the X-rays produced by the accretion of gas onto it. These black holes appear to be growing fast, and the environments surrounding such active black holes become highly luminous, creating a quasar.

"Astronomers have never lacked imagination: since the discovery of quasars, there has been no dearth of theories to explain how these black holes grew so massive so fast," said Naidu. "Something spectacular must have happened in the early universe. Now with JWST, we can directly observe this era and see for ourselves which scenarios actually occur."

Learning of the birth of supermassive black holes and whether they predate the galaxies that surround them was one of the primary science goals of the JWST before it launched. In this it has been tremendously successful so far. Despite little red dots having only been discovered four years ago, research into them and black hole stars is accelerating, with new findings coming out now almost on a weekly basis.

"These are incredibly exciting times with nearly a thousand papers and preprints on little red dots in the past two to three years," said Matthee. "Far from a mirage, this might well be a cosmic miracle."

The findings were published on Aug. 13 in the journal Nature.

New evidence has come to light showing that the mysterious 'little red dots' discovered in the early universe by the James Webb Space Telescope could evolve into the active centers of fully formed galaxies.

"Everything created in the early universe must evolve into something around us," said George Rieke of the University of Arizona in a statement. "We have had little idea of what little red dots become, but these results finally show us how to find their progeny."

Discovered by the James Webb Space Telescope (JWST) almost as soon as it became operational in 2022, little red dots have been a perplexing cosmological mystery. As their name suggests, they appear small, red and surprisingly bright. They are mostly found at redshift values suggesting they existed between 13.2 and 12.2 billion years ago. To shine so brightly at such great distances would usually imply these objects are quasars — which are luminous nuclei of galaxies powered by active supermassive black holes — but the light coming from little red dots is more like that of bloated stars. It looks to be mostly in infrared with some ultraviolet, and none of the X-rays that one would expect from an active black hole chomping down on material.

As such, researchers have come up with the hypothesis that little red dots are "black hole stars," or vast clouds of gas heated from within by a concealed but growing supermassive black hole.

However, the population of little red dots drops off a cliff at redshifts equating to less than 12 billion years ago. Where did they all go? There are two options. Either they all died off, or they developed into objects more familiar to us.

One recent hypothesis is that little red dots turned into large globular clusters. And now, an alternative possibility has come along.

A team led by Pierluigi Rinaldi, who was at the University of Arizona's Steward Observatory when conducting this research but is now at the Space Telescope Science Institute (STScI) in Baltimore, think it has identified a descendent of a little red dot. It appears to be in the form of a distant galaxy, catalogued as WISEA J123635.56+621424.2, which is found at a redshift of 2, meaning that we see it as it was 10.5 billion years ago.

The galaxy displays neat spiral arms around a red core. Rinaldi's team have nicknamed it the Saguaro, after a species of cactus native to the Sonoran desert in the United States' south-west, thanks to the galaxy's arms and how its core resembles the red fruit produced by the cactus.

Saguaro's core has all the hallmarks of a little red dot. It shines bright in infrared as seen by JWST, and also emits in ultraviolet as detected by the Hubble Space Telescope. Yet, NASA's Chandra X-ray Observatory has also detected faint X-rays originating from Saguaro.

"What the X-ray observations show is that this galaxy has an active galactic nucleus, and a very obscured one at that," Carys Gilbert of the University of Cape Town in South Africa, who participated in the study alongside Rinaldi, said in the statement. "It's not only obscured but also X-ray weak. That kind of combination could explain the lack of X-ray emission that we see from all other little red dots. It fits the puzzle of little red dots nicely."

This is not the first time X-rays have been seen coming from a little red dot. Earlier this year it was reported that scattered X-rays were seen breaking through from a little red dot called 3DHST-AEGIS-12014, given credence to the hypothesis that little red dots are black hole stars, where the black hole gradually consumes the "star" from the inside out, eventually carving holes through which X-rays can escape. We see 3DHST-AEGIS-12014 as it was 11.8 billion years ago, meaning that Saguaro, which existed 1.3 billion years later, is a little bit further on in its development.

"Because the Saguaro is at lower redshift, we can see the very beautiful and bright host galaxy in high resolution and detail with Webb and Hubble," said Harvard's Zihao Wu, who was also part of Rinaldi's team.

Intrigued, Rinaldi's team simulated how Saguaro would appear to us if it existed a billion years after the big bang. Much of its galactic structure would either be less developed or simply just too faint to be seen at such distance. All that would be visible would be the nucleus, looking very much like all the other little red dots.

This implies that little red dots are not a unique population of their own, but are simply a phase in the development of galaxies with supermassive black holes. Our own Milky Way could have been a little red dot once upon a time.

Saguaro is a crucial link in the story of little red dots and how they connect with modern galaxies. While there is still much to learn, such as the beginning of their story and how they form, the middle and end of their story is now beginning to take shape.

The findings were reported on 29 July in The Astrophysical Journal.

In a nebula far, far away, colossal clouds of dust and gas tower amongst the stars.

What is it?

This spectacular new image from the James Webb Space Telescope showcases the brilliant majesty of the Carina Nebula, a giant cloud of dust and gas found 7,500 light-years away in the constellation Carina.

You may have seen the Carina Nebula before — in the first-ever image released from JWST, which has been dubbed "Cosmic Cliffs."

In this new image, captured by JWST's Near-Infrared Camera (NIRCam), you can see the nebula in a whole new light. This snapshot captures a specific feature that is being dubbed the "Treasure Chest," as it vaguely resembles a glowing coffer overflowing with stellar jewels.

This "Treasure Chest" contains a cluster of young stars, approximately 70 stars in total. While these might be young, growing stars, the most massive of the bunch is a whopping 19 times more massive than our sun.

Why is it incredible?

While JWST has looked at the Carina Nebula before, new observations can reveal completely new details and help scientists uncover new information about the nebula and the strange ways in which the universe works.

Right now, scientists think that the star cluster in the "Treasure Chest" is about 1.3 million years old. However, previous estimates thought the grouping could be just 100,000 years old. So, new observations by powerful telescopes like JWST can significantly change our understanding of the cosmos.

With each new observation or data point, the history and context of the universe around us could completely transform. And, as this star cluster grows over time, its stars will become more brilliant. They may therefore illuminate more of this star cluster, potentially revealing details and secrets of this "treasure" that scientists might never have predicted.

Paleontologists now know that many of the dinosaurs didn't disappear but instead evolved into modern birds, and new research suggests that "cosmic dinosaurs" observed by the James Webb Space Telescope (JWST) didn't go extinct either. Rather, they may have evolved into familiar sights in the modern universe: vast conglomerations of densely packed stars called "globular clusters."

Little Red Dots became quite the puzzle for astronomers in 2022, when the JWST began to routinely spot them in abundance around 600 million years after the Big Bang. That is because these objects seemingly disappear before the cosmos gets to around 2 billion years old.

Astronomers have proposed many different explanations for Little Red Dots, including the suggestion that they could be "black hole stars," or black holes wrapped in vast shrouds of dense gas and dust. This team theorizes that a forming globular cluster with a supermassive star, a hypothetical short-lived stellar body with between 1,000 and 10,000 times the mass of the sun, would also look a lot like a Little Red Dot at its heart.

"These may not be just a strange new JWST population with no connection to the universe around us today," team leader John Chisholm of the University of Texas Austin said in a statement. "Instead, Little Red Dots may persist past the early universe, evolving into something relatively familiar.

"Little Red Dots could be galaxies, they could involve black holes, or they could be something even more unexpected. Our work shows that forming globular clusters with supermassive stars should be part of that conversation."

An unfamiliar side to a familar sight

Globular clusters are generally seen in large galaxies and are densely packed with up to many millions of ancient stars. Our galaxy, the Milky Way, is host to at least 150 globular clusters, and though familiar, astronomers still aren't quite sure how they form.

"We usually see them [globular clusters] after billions of years of evolution, at a time when their massive stars are gone, their gas has been cleared out, and dynamical processes have changed their masses and structures," team member Danielle Berg of UT Austin said in the statement. "That makes it very hard to reconstruct the original conditions they formed in."

It is thought that the stars in globular clusters all formed at the same time in the early universe. However, at this time the cosmos should only have had hydrogen, helium and a smattering of heavier elements (which astronomers call "metals") available for star construction. Yet, many stars in globular clusters are strangely abundant in helium and metals like nitrogen, sodium and aluminum, while lacking the expected levels of carbon, oxygen and magnesium.

"This specific pattern indicates nuclear fusion at very high temperatures, much higher than in the cores of even massive normal stars," team member Mike Boylan-Kolchin of UT Austin said in the statement. "A supermassive star is precisely the kind of environment that could produce this combination."

Supermassive stars capable of generating this kind of heat would form in the dense environments of early globular clusters in which stellar collisions and mergers would be expected to occur over and over again. The resultant supermassive stars would be short-lived, lasting just around 1 million years (remember the sun is middle-aged at 4.6 billion years old) — but this would be sufficient time to forge the elements needed to explain the peculiar chemistry of globular clusters.

When these supermassive stars die in supernova explosions, the elements they forged would be blasted out to become the building blocks of the next generation of stars. This would provide the stars of modern globular clusters with their unusual chemical fingerprints.

"In our model, the supermassive star that helps make the object look like a Little Red Dot would live for only a short time," Chisholm continued. "Once that star dies, the object may no longer look like a Little Red Dot, even if the cluster itself survives billions of years."

Strange chemistry isn't the only thing linking early globular clusters with Little Red Dots, however. Not only does the team propose that the distribution of Little Red Dots in the early universe matches the distribution of modern globular clusters, but they also say models of Little Red Dot evolution show that their estimated masses could easily lead to the masses of globular clusters seen in the recent universe.

There is also the issue of timing. Little Red Dots appear around 600 million years after the Big Bang, and that is also the time that scientists estimate that globular clusters would have begun to form.

"There's no single smoking gun at this point that says Little Red Dots are globular clusters, but it would explain a lot of diverse and surprising observations," said Boylan-Kolchin.

This study is currently available to view as a pre-print on the paper repository arXiv.

Using the James Webb Space Telescope (JWST), astronomers have discovered the secrets of early galaxies that pumped the infant cosmos full of dust, which would become vital for the birth of new stars and the growth of galaxies.

However, while the JWST is powerful enough to see many of these early galaxies, it is still limited when it comes to delving into them in great detail. So, the team at the heart of this research worked around this by studying a much closer and more modern galaxy with many characteristics that resemble the universe's first galaxies.

In lieu of being able to study the processes that occurred in the early universe that allowed galaxies to be seeded with "metals, (the term astronomers use to describe elements heavier than hydrogen and helium), the researchers turned their attention to a dwarf galaxy just 4.6 million light-years away.

"Directly studying the galaxies that populated the early universe is still very difficult, which is why observing a nearby galaxy like Sextans A, which presents similar chemical conditions, offers us a precious opportunity to understand how the first generations of stars evolved and what role they played in transforming the interstellar medium," team leader Claudio Gavetti of the National Institute for Astrophysics (INAF) said in a statement.

How does Sextans A impersonate ancient galaxies?

The early universe was a pretty dull place in terms of chemistry. That is because it was dominated by the lightest element, hydrogen, with some helium and a tiny smattering of heavy elements, or metals. That means that the first generation of stars, so-called POP III stars, were correspondingly metal-poor.

During their lives, however, POP III stars fused hydrogen and helium in their cores to forge heavier elements. When these original stars reached the ends of their lives, they exploded in supernova explosions that dispersed these metals into the interstellar medium, the vast clouds of dust and gas between stars.

Eventually, dense and cool patches in these vast clouds collapsed under their own gravity, birthing the next generation of stars, POP II stars, which, thanks to the supernova deaths of their predecessors, were richer in metals.

Our own star, the sun, is classed as a POP I star, meaning it is even richer in metals than these second-generation stars. However, not all modern galaxies are so metal-rich; this is especially true for dwarf galaxies like Sextans A, even though it lies at the outer edge of our cosmic backyard, known as the "local group."

Sextans A is so metal-poor that it is estimated to contain only between 1% and 7% of the heavy elements found in the sun. That makes it a great proxy for the study of metal-poor early galaxies.

Using the JWST's NIRCam (Near-InfraRed Camera) and MIRI (Mid-Infrared Instrument) instruments, Gavetti and colleagues obtained high-resolution observations of Sextans A that allowed them to map the dwarf galaxy's entire population of stars during an evolutionary phase known as the "asymptotic red giant branch."

This phase occurs when stars larger than the sun exhaust helium in their cores, creating an inert carbon heart, but nuclear fusion continues in outer alternating helium- and hydrogen-burning layers. These stars "puff out" as a result of this and can undergo thousandfold increases in brightness.

The team's findings revealed that around 90% of the asymptotic red giant branch stars they studied were not surrounded by envelopes of dust. However, around 20 or so of these stars were embedded in thick dust shells. They also found that these "dust factories" formed between 2 billion and 3 billion years ago from stars with an initial mass about 1.5 times the mass of the sun.

This research is a leap forward in understanding which stars in the early universe were most likely to create the metal dust that would have enriched the next generations of stars. That means it helps paint a complete picture of how the universe as we see it today took shape.

The scientists behind this study say that this type of research would have been impossible before the launch of Webb.

"The JWST allows us to observe in unprecedented detail environments that until a few years ago were beyond our reach," team member Flavia Dell'Agli of the INAF. "The value of these data lies not only in the images, but in the ability to compare them with theoretical models and verify how correctly they describe the evolution of stars."

The team's research was published on Monday (July 20) in The Astrophysical Journal.

A young cluster of galaxies sparkles under a cosmic glow that's 4.4 billion years old. This peek into the past shows the stellar spectacle of a galaxy cluster still forming.

What is it?

The James Webb Space Telescope snapped this image of the galaxy cluster MACS J0553.4-3342 on July 3 using its near-infrared camera (NIRCam). The glorious, glimmering sight is actually a massive young galaxy cluster forming 4.4 billion years ago. A galaxy cluster is a grouping of galaxies held together by gravity. Galaxy clusters can contain hundreds or even thousands of galaxies and are the largest known structures in the entire universe that are held together in this way.

Why is it incredible?

Because light takes time to travel through space, and because the JWST can look incredibly far out into space, this telescope acts as a sort time machine.

This power isn't unique to the JWST, however. Other telescopes like the Hubble Space Telescope, for instance, have similarly peered back in time through the cosmos and revealed some incredible, ancient sights. However, the JWST's specialized instruments like NIRCam allow the telescope to pick up incredibly faint light from galaxies remarkably far away. This greatly stretches how far back in time we can see.

But the really incredible thing is, you can look back in time yourself — with only your eyes. While JWST can look exceptionally far out into space and can capture the very faint light of ancient galaxies, the light coming from the stars you can see with your bare eyes also had to travel over incredible stretches of time to reach you. Think about this: the light coming from a constellation you love may have traveled across millions of light-years to get to your eyes.

Separated by billions of miles and shaped by very different environments, Saturn's smoggy moon Titan and the dwarf planet Pluto have, on paper, little in common.

Titan is a geologically active world cloaked in an atmosphere denser than Earth's, its landscape shaped by seas of liquid methane and vast dunes built from organic particles that rain out of its skies. Pluto, by contrast, is a frigid outpost with a tenuous atmosphere hovering above an icy, frozen surface.

Yet, observations from the James Webb Space Telescope (JWST) have revealed these two disparate worlds share an identical, unexplained infrared signature on their surfaces — a sign that similar chemistry may be unfolding on both worlds despite their stark differences, scientists say.

Detailed in a new study, the feature appears at precisely the same infrared wavelength on both Titan and Pluto, indicating that it absorbs light identically on both worlds. The signal points to the presence of an unknown compound, or a family of related compounds, that scientists have yet to identify.

"It's rather mysterious," Bruno Bézard, a planetary scientist at the Paris Observatory who led the discovery, told Space.com. "We cannot say what it is."

Chasing the signal

Bézard first spotted the unexplained feature while analyzing Titan observations from November 2022, when JWST gathered infrared light leaking through the haze in very specific, narrow wavelength bands, allowing scientists to peer directly through the otherwise opaque atmosphere.

To make sense of this light, researchers rely on spectroscopy, a technique used to identify compounds by the specific wavelengths of light they absorb. Because every molecule leaves behind a unique spectral fingerprint that telescopes can detect, astronomers can routinely identify substances across the solar system and beyond, ranging from simple water ice to complex molecules.

But the newly detected feature neither matches any of the standard library spectra cataloged so far, nor does it appear to be a fluke of the hardware, the study notes. The exact same absorption feature was detected by two different JWST instruments — the Near-Infrared Spectrograph (NIRSpec) and the Mid-Infrared Instrument (MIRI) — ruling out the possibility of an instrumental artifact.

After failing to find a match with the cataloged spectral fingerprints of the simplest and most common planetary ices, Bézard wondered whether another world with similar atmospheric chemistry might hold a clue. He turned to his colleague Emmanuel Lellouch of the Paris Observatory, who had led a JWST program that had observed Pluto in May 2023.

"I asked him, 'Do you also have a signature [on Pluto] at this exact wavelength?'" Bézard recalled in the interview with Space.com. "So we looked, and we found that it is present there."

The ground truth

There is no evidence that the mystery molecule is a biosignature, Bézard said. Instead, it likely reflects the kind of prebiotic chemistry that has been operating in Titan's oxygen-free environment for more than 4 billion years.

One compelling possibility is that it belongs to a family of hydrocarbons known as allenes, which the study notes are essentially the only organic compounds known to exhibit strong absorption bands within the same 5-micron infrared range as the mystery signal.

But the allene family contains many complex variations for which complete spectra do not yet exist, Bézard said. Alternatively, the signature could belong to a known molecule whose spectral fingerprint has shifted, potentially because it is mixed with other planetary ices that have not yet been fully cataloged.

"We only have spectra for the simplest of them," Bézard said. "But it is possible that within this family you could find one or several compounds which are present together and make such an absorption feature."

Whatever the compound ultimately proves to be, he and his team believe it forms in the atmosphere through photochemical reactions before eventually "snowing" down onto the surface.

Despite their stark differences, both Titan and Pluto possess atmospheres dominated by nitrogen and methane. Scientists know from spacecraft observations and lab simulations that in the upper reaches of the planets' atmospheres, ultraviolet sunlight breaks these molecules apart, triggering a cascade of highly reactive chemical fragments. These fragments then reassemble into complex organic compounds, some of which condense and snow back down onto the surface below, which is where the JWST detected them.

A couple of different lines of evidence support this atmosphere-to-surface pipeline. First, the team analyzed how the signal behaved across Titan's disk. As the JWST scanned Titan from the center of its circular face toward its outer edge, or limb, the mysterious signal steadily weakened, the study notes.

"This is what you expect if it comes from the surface," said Bézard.

Because of the three-dimensional geometry of looking at a sphere, a signal coming from a flat surface will appear strongest at the center and grow fainter near the edge, where the angle of view through the atmosphere becomes longer and more obscured. This specific dimming trait was not shared by atmospheric carbon monoxide the team checked, which remained essentially unchanged from center to limb, Bézard said, which helped the team infer that this mystery molecule likely resides on the ground.

Pluto offered an independent line of evidence to back up this surface theory. Its near-vacuum atmosphere is physically too thin and sparse to generate an absorption feature of the observed depth, Bézard said, leaving the dwarf planet's solid surface as the only plausible source for the deep signature.

To further test their atmospheric-origin hypothesis, the team studied JWST observations of Jupiter's moon Ganymede. Because Ganymede lacks a nitrogen-methane atmosphere, it cannot run the same photochemical engine like Titan and Pluto do. Sure enough, the researchers found no trace of the mysterious feature, lending additional support to the theory that the compound is uniquely tied to the chemistry of nitrogen and methane skies.

Mapping Titan's surface

More clarity may arrive in the coming months. Researchers are currently analyzing newer JWST observations that provide a more complete view of Titan as it rotates. The data will allow the team to map the mysterious infrared signature across the moon's surface and determine whether it is associated with specific geologic features, such as Titan's vast organic-rich dune fields, which are continually replenished by a slow drizzle of complex particles produced in the atmosphere, Bézard said.

Further clues may have to wait for NASA's Dragonfly mission, a car-sized rotorcraft expected to launch in 2028 and arrive at Titan in the mid-2030s.

Although Dragonfly does not carry an infrared spectrometer to replicate JWST's light measurements, its onboard mass spectrometer will allow it to "taste" organic molecules across the various geologically interesting areas the spacecraft will fly to. By revealing which compounds are actually present on Titan's surface, the mission could give scientists a shortlist of candidates to replicate in laboratories back on Earth to see if they match the traits of the mystery molecule, Bézard said.

"It's always exciting when you discover something that was not seen before," Bézard said. "It's really the nicest part of our job."

The new study was accepted for publication in the journal Astronomy & Astrophysics.

July 2026 marks four years since NASA's James Webb Space Telescope (JWST) images were first revealed to the general public, marking a new era for astronomy. To celebrate this anniversary of the most powerful space telescope ever launched, NASA has released a stunning image of the strangely shaped galaxy called Centaurus A.

Located around 11 million light-years away, Centaurus A owes its unusual structure to a collision between two galaxies around 2 billion years ago. This merger provided the galaxy with an abundance of gas and dust, the raw material for intense star formation. It also supplied the supermassive black hole at the heart of this galaxy with an abundant supply of the same matter to feed upon and power a bright and violent central region, or active galactic nucleus (AGN), as that central area blasts out powerful, high-speed jets of plasma.

Though this galaxy is much closer to us than many of the early galaxies that the JWST has studied in its four years of operations, that doesn't mean it's any less useful. In fact, with its ultra-sensitive infrared vision, the JWST has been able to peer into the heart and inner workings of Centaurus A like no telescope that has gone before.

"No single telescope tells the whole story," Shawn Domagal-Goldman, division director of Astrophysics at NASA Headquarters in Washington, said in a statement. "Discoveries build over time, and new observatories expand on the foundations laid by earlier missions. The JWST represents the most powerful step forward yet, opening a window into wavelengths and details never before accessible.

"This allows astronomers to examine structures and processes that other telescopes could not see."

Building upon the legacy of Spitzer and Hubble

The key to the new view of Centaurus A that the JWST has been able to provide is the space telescope's powerful infrared vision. The thick dust that crowds the heart of this galaxy blocks visible light the Hubble Space Telescope previously relied on to study it. Infrared light is able to slip through these dense sheets of gas and dust.

The now-retired Spitzer Space Telescope had previously studied Centaurus A in infrared, but while it could resolve larger structures in the galaxy, it lacked the observational power to resolve individual stars and finer details.

However, even though the JWST has been able to use its MIRI (Mid-Infrared Instrument) and NIRCam (Near-Infrared Camera) to study Centaurus A like never before, there are still mysteries to be solved about this structure.

For example, in the MIRI image of Centaurus A, alongside the glowing stellar nurseries where new stars are born and spit gas and dust into their surroundings, there is a curious S-shaped feature. Scientists still don't know how this structure was formed and if the active black hole at the heart of Centaurus A played a role in its creation.

The JWST images of Centaurus A do reveal plenty about the role this galaxy's central black hole plays in carving out its morphology. For example, the JWST was able to see fast-moving ionized gas being shunted outwards by the black hole’s activity. The JWST data also revealed warmer molecular hydrogen in a warped and rotating disk near the heart of Centaurus A.

This data seems to show how a galaxy's central black hole can trigger bouts of intense star formation by condensing gas and dust, but also how these cosmic titans can stunt star birth and "kill" their host galaxies by purging the raw material needed for the star-formation process.

That means that thanks to the JWST, scientists are now building a more comprehensive cosmic history of Centaurus A, promising discoveries that can be applied to other galaxies to build a better picture of how the universe has evolved.

Here's to another four years of cosmic discoveries.

Mysterious "little red dots" discovered in the early universe by the James Webb Space Telescope could harbor buried black holes that fire high-energy cosmic "ghost particles" through the cosmos.

Neutrinos are referred to as ghost particles because as chargeless and near-massless particles, hundreds of trillions of them stream through your body every second at nearly the speed of light. Plus, the source of high-energy neutrinos frequently detected on Earth is something of a mystery.

And another cosmic mystery is the existence of the "little red dots," which are galaxies that have been discovered by the James Webb Space Telescope (JWST). Though common around 600 million years after the Big Bang, these dots seem to disappear before the universe gets to 2 billion years old. Some researchers have theorized that these curious small galaxies could harbor black holes that are buried in thick shrouds of cosmic dust. If that is the case, then the dots could be a major contributor of high-energy neutrinos, linking these two mysteries.

Neutrinos are produced when other particles, such as protons, collide with particles of light, or photons, or with different sorts of matter. This usually occurs in gas-dense environments, but the ghost-like characteristics of neutrinos mean they have little trouble escaping into the universe at large.

Usually, the events that create high-energy neutrinos also give rise to high-energy photons called gamma-rays. However, neutrinos are so abundant as the second most common particles in the cosmos that if all sources of neutrinos also created gamma-rays, the gamma-ray background of our universe should be much greater than it actually is.

That means some sources of high-energy neutrinos must be located in environments from which gamma-rays can't readily escape — and that's where the little red dots enter the picture. These curious objects display very little emission associated with galactic jets or other outflows. This led this team to assume that the lack of these emissions, which should come in the form of X-rays and radio waves, is because the black holes and associated jets in Little Red Dots are buried in dense halos of dust and gas.

"In the scenario we considered, abundant photons and dense gas are expected to exist around the central black hole in a little red dot, which may allow such collisions to occur efficiently," team leader Riku Kuze of Kyoto University said in a statement.

Kuze and colleagues estimated the contribution that the little red dots could add to the universe's neutrino background. This revealed that, should particle acceleration be occurring in the buried black holes within the dots, these environments could produce high-energy neutrinos to contribute a significant fraction of the high-energy neutrino background observed on Earth. This would be while also suppressing gamma-ray escape.

"Although it is difficult to observe the individual objects directly, we believe this study is significant because it is the first to demonstrate that, given their abundance, these little red galaxies could account for a part of the observed high-energy neutrinos," said Kuze.

Neutrinos come in more than one type, or flavor; thus, the next step for the team will be to determine the ratio of neutrino flavors generated by buried black holes in the little red dots and to determine if this matches cosmic abundances witnessed.

The team's research was published in the journal Physical Review D.

PASADENA, California — NASA's new alien-hunting telescope, the Habitable Worlds Observatory (HWO), will be serviceable out in space (and it will have gamma-ray detectors, to boot).

Do you remember seeing NASA's space shuttle astronauts working on the Hubble Space Telescope out in space? Well, it will likely be robots this time around, but NASA is planning for HWO to be serviceable, which means that they will need to figure out a way to work on, repair, and maintain the observatory while it operates roughly a million miles (1.5 million kilometers) away.

"HWO will have to be serviceable to some extent," NASA's astrophysics division director Shawn Domagal-Goldman told Space.com during a session at the American Astronomical Society's (AAS) 248th meeting in Pasadena, California.

From Hubble to HWO

The Habitable Worlds Observatory (HWO) is NASA's next planned flagship space telescope. But what separates it from previous space telescopes like Hubble or the James Webb Space Telescope (JWST) is its purpose: to look for and study rocky, Earth-like planets orbiting sun-like stars. In other words, to find planets that could hold life. The mission won't just hunt for aliens, but rather explore these habitable planets and their atmospheres, expanding our understanding of other worlds while also being used for a variety of astronomical purposes. And by making it serviceable, NASA will not just extend HWO's life, but it will also open the door for future technologies that can be used to enhance the observatory.

Hubble was a unique case. As the space telescope came about at roughly the same time as NASA's Space Shuttle program, and the telescope was designed to function in low-Earth orbit, it was a natural fit that astronauts go out to assemble, repair and maintain the observatory. "There were decisions made early on that the avionics would be modular in a way that astronauts could take the computer out and put a new computer in, or take a gyroscope out and put a new gyroscope in," former NASA astronaut and former NASA Chief Scientist John Grunsfeld, who today works independently as a consultant in the space industry, told Space.com.

However, HWO won't be so close to us. Instead, it will be located nearby L2, or the Sun-Earth Lagrange point 2, a point out in space roughly one million miles (1.5 million kilometers) away where the gravitational pull of the sun and Earth combine to keep objects in the same orbital period as Earth. This position, which is also home for the JWST, allows space telescopes to stay in sync with Earth, making communication easier. It also makes an astronaut mission quite difficult, if not nearly impossible with the technology we have today.

While the JWST was sent out to this distant vantage point without plans for servicing the telescope, HWO will "have to" be serviceable, according to Domagal-Goldman and further confirmed with NASA's press office. Servicing the observatory could look like anything from instrument swaps to regular maintenance or as-needed repairs, but it could also entail assembling the observatory itself. "If the telescope is too large to launch [fully assembled]," Domagal-Goldman added, it might need to be "assembled in space."

When the JWST went to L2, the mission team realized the problem with micrometeorites was a bit bigger than they anticipated. "We've learned that there's more micrometeorites and they're larger than we expected," said Grunsfeld, "and so you might be able to want to put a patch over a sunshield or a patch on a barrel to patch a hole — and, in principle, robotics could do that."

NASA has yet to confirm details about exactly how they plan to service the new observatory, which makes sense as the design of HWO itself is still in flux. But with L2 being so far away, it's logical to assume that it will need to be supported robotically, instead of with astronauts working out in space like with Hubble. We don't know what these future space telescope robot mechanics might look like, but they will have to be very capable to work on such a powerful observatory all the way out at L2.

"This will be by far the most challenging observatory that we've ever built," Grunsfeld said. "It's just remarkable that we are so bold as to think we can do it, and to be really close to showing that we can … so since we're just getting started, this is the time to have the discussion about should it be serviceable or not."

Science is the driving force

In addition to extending HWO's longevity by building it in a way that will allow it to be repaired out in space, making the observatory serviceable will also stretch its science capabilities in ways we can't yet imagine. If we look at Hubble's history, its instruments have been swapped out for newer, better versions over time that have not just allowed the telescope to continue functioning, it has allowed the telescope to evolve with changing technologies. From Hubble's gyroscopes to the Wide-Field Camera 3 swapped out in 2009, the telescope has benefitted from many technological upgrades. With servicing capabilities, the same could be true for HWO.

HWO is still fairly early in its development, and many years from launch (estimated for the 2040s). But NASA is laying the groundwork for this mission with the upcoming flagship mission the Nancy Grace Roman Space Telescope. This mission carries with it a technology demonstration called the Roman Coronagraph Instrument. Essentially an "exoplanet camera," this instrument will block the glare of far-off stars, getting a direct look at the planets in their orbit. Roman will provide a proving ground for this next-gen coronagraph technology. But even if HWO launches with an advanced version of this coronagraph five , 10 or even 15 years following launch there could be even better planet-spotting technology available.

"I'm sure we will be highly motivated if we see a little rocky planet around a nearby star that kind of looks like Earth," Grunsfeld said, "we're going to be highly motivated to send a higher resolution spectrograph, or some different type of detector … up there as fast as we can. So that's the primary driver of servicing, is to be able to put in new scientific instruments."

By making HWO serviceable, NASA will enable the use of future technologies without having to launch entirely new space telescopes to support them. This is a cost-effective method, but it might also enable the deployment of future technologies that might otherwise not have a place to operate out in space.

"Imagine 20 years from now, or 25 years from now, that there'll be a robust space industry doing servicing, such that we could have a commercial servicer deliver new scientific instruments to habitable worlds," Grunsfeld said. They would simply "slide the old ones out, [and slide] the new ones in."

Speaking of future technologies, this decision to make HWO serviceable wasn't all that NASA revealed at AAS. Domagal-Goldman also shared that HWO will be equipped with Gamma-ray detectors. The specific details of these detectors and what they will be used for is also to-be-determined, but with HWO being serviceable, these detectors could continue to evolve with the observatory over time, enabling future astronomy that we can't even imagine today.

On July 4, the United States of America celebrates its 250th birthday, marking the anniversary of the Declaration of Independence and becoming a sovereign nation.

Today, this relatively young country leads the way in our understanding of the universe. It's where many major players in space science, like NASA, the California Institute of Technology (Caltech), the Massachusetts Institute of Technology (MIT), and Northwestern University, to name just a few.

And to celebrate 250 years of the U.S. as an independent nation, Space.com takes you on a journey through some common misunderstandings of the universe through the years and the roles American scientists played in clearing up that cosmic confusion.

By 1776, Sir Isaac Newton's laws of motion had been around for about 89 years since the publication of Philosophiæ Naturalis Principia Mathematica (Mathematical Principles of Natural Philosophy) in 1687. Five of the solar system planets had been discovered by the Ancient Greeks long before the birth of the U.S. Also, after a long struggle and many attempts to stifle this knowledge, humans were made aware that the Earth orbits the sun rather than the other way around, with the final nail in this coffin of misunderstanding laid by Polish astronomer Nicolaus Copernicus in 1543 and Galileo Galilei in 1610, receiving an extra hammer blow from Newton in 1687.

Galileo had also delivered us to the understanding that not only was Earth's place in the solar system unique, but it wasn't even the only planet to possess moons, with the moons of Jupiter, Io, Europa, Ganymede and Callisto discovered in 1610.

Clearly, by the time the U.S. was born we were already beginning to understand the universe and our place within it, but some major misunderstandings still persisted. One of the largest of these surrounded the nature of the sun itself.

The sun as a burning lump of coal

America was formed during the "steam age," a period of industrialization that lasted from 1770 to 1914. This revolution was driven by coal, powering locomotives, ships, and factories, changing the shape of industry, transportation, and manufacturing. At this time, coal was the densest and most powerful fuel source known to humanity, so it is perhaps little wonder that many early scientists theorized the sun was actually a tremendously massive lump of burning coal.

Then, one of the oldest and most prominent scientific periodicals in the world, the U.S.-based Scientific American, wrote a 1863 article that first began the pushback against the sun as a burning lump of coal.

"If the sun were composed of coal, it would last at the present rate only 5,000 years. The sun, in all probability, is not a burning, but an incandescent, body. Its light is rather that of a glowing molten metal than that of a burning furnace. But it is impossible that the sun should constantly be giving out heat, without either losing heat or being supplied with new fuel," the Scientific American article stated. "Assuming that the heat of the sun has been kept up by meteoric bodies falling into it, it is possible from the mass of the solar system to determine approximately the period during which the sun has shone. The limits lie between 100 millions and 400 millions of years."

Though this estimate was still miles out, we now understand that the sun is around 4.6 billion years old; this development came at a time of a geological revolution that was uncovering evidence that our planet was much older than theological estimates of just a few thousand years.

Around 57 years later in 1920, British scientist Arthur Eddington first suggested stars like the sun are actually powered by the nuclear fusion of hydrogen to helium. The idea was published by Eddington in his 1926 book, "The Internal Constitution of the Stars." Twelve years after this, nuclear physicist Hans Bethe formulated the first explanation of this nuclear fusion process, detailing the proton-proton chain reaction and the Carbon-Nitrogen-Oxygen (CNO) cycle.

The idea of the sun as a burning lump of coal finally burnt out 162 years after the formation of the U.S., a chain reaction kick-started by an American publication.

Ether or…?

During the infancy of the U.S. in the 1800s, scientists understood that light is a wave. Applying this to what they knew of other waves, it was logical to presume that light also needed a medium through which it could propagate. This medium would have to be ubiquitous and possess some unique properties to allow light to propagate through it at the speed of light.

Thus, it was proposed that space was filled with a medium called the luminiferous ether, with luminiferous meaning "light-bearing." The fact that this would have to be an invisible and infinite material that doesn't interact with physical objects made the existence of the luminiferous ether highly controversial.

We now know this medium doesn't exist, and that is thanks to two American physicists, Albert A. Michelson and Edward W. Morley, who in 1887 delivered the most important null result in the history of science: disproving the existence of the luminiferous ether.

Should the luminiferous ether exist, then scientists reasoned that as the Earth orbits the sun at around 66,000 miles per hour (106,216 kilometers per hour), our planet should be moving through the ether, which had been deemed to be stationary. That meant Earth must be moving with respect to the stationary ether. And if the ether is the medium through which light waves ripple, this should mean the speed of light differs ever so slightly in the direction Earth is traveling.

Conducted in Cleveland, Ohio, the Michelson–Morley experiment used a piece of kit called a Michelson–Morley interferometer to test differences in speed for a wave of light traveling perpendicular to Earth and one traveling parallel to Earth. Michelson and Morley had expected to observe an interference pattern caused by the differing travel times of the light waves.

That is what happens when light of the same wavelength arrives at a detector at ever so slightly different times, meaning the peaks and troughs of the waves no longer perfectly align. However, to the surprise of the American physicists, no interference was detected. This meant no difference in the travel speed of light, essentially disproving the existence of the ether.

The negation of the luminiferous ether was of vital importance as it opened the door to Albert Einstein's theory of special relativity in 1905 and general relativity in 1915, the latter of which revised our understanding of gravity and led to our knowledge of black holes and gravitational waves well before the experimental observation of such objects.

Other galaxies!

Though scientists realized Earth isn't in the center of the solar system before the birth of the U.S., there was another glaring misconception. It was believed that the Milky Way, first proposed in Immanuel Kant's "Island Universe" theory in 1755, still occupied a unique position in the universe — with the existence of other galaxies a hotly debated topic. The solar system itself was also thought to be at the center of the Milky Way.

In 1785, astronomer William Herschel set about mapping our galaxy, correctly determining the disk-like shape of the Milky Way but incorrectly placing the solar system at its heart. This picture changed in 1918, when American astronomer Harlow Shapley determined that dense groups of stars called globular clusters are centered on a distant core in the direction of the Sagittarius constellation. This placed the solar system off-center in the galaxy. Today we've expanded upon this, moving our planetary system 27,000 light-years away from the Galactic Center and onto one of our galaxy's spiral arms.

It was five years later, in 1923, that the uniqueness of the Milky Way was shattered. Using the 100-inch (2.5-meter) Hooker telescope at the Mount Wilson Observatory, American astronomer Edwin Hubble imaged the Andromeda nebula (Messier 31) and determined that it was at least a million light-years away. Though we now know this distance is closer to 2.5 million light-years, it was still enough to place M31 outside the boundary of the Milky Way.

The fact that the Andromeda nebula is actually the Andromeda galaxy, a distant and separate galaxy from our own, was announced to the public via The New York Times in Nov. 1924. We were no longer alone galactically — but Hubble wasn't done.

The universe is not static

Another assumption at this time was that the universe was static, something supported by Einstein in 1917. However, in 1929, Hubble discovered that the light from distant galaxies was being redshifted. In other words, the wavelengths of light emanating from these sources were being stretched as those wavelengths traveled toward us. This indicated that these galaxies are moving away from us. Convinced of this, Einstein abandoned his model of the static universe.

American scientists weren't done revising our entire picture of the cosmos, however. In 1998, U.S. researchers like Saul Perlmutter, Adam Riess, and Robert Kirshner were part of two international teams of researchers that discovered that not only is the universe expanding, but this expansion is actually speeding up.

Dark energy was introduced as the mysterious force driving this accelerating expansion. It remains today one of the most pressing mysteries of the cosmos.

Possibly by the time the U.S. celebrates its 300th birthday, the mystery of dark matter will have been solved along with other cosmic puzzles such as the nature of dark matter. If this is the case, it is highly likely that U.S. projects like the Hubble Space Telescope, the James Webb Space Telescope, and the upcoming Nancy Grace Roman Space Telescope will put American innovators and scientists at the forefront of these developments, just as their predecessors have been for the last 250 years.

Using the James Webb Space Telescope, astronomers have spotted a massive and densely packed galaxy cluster at "cosmic noon." The fact that this cluster is so highly evolved could change theories of cosmic evolution, as it seems to exist before such structures were thought to be possible.

Designated XLSSC 122 and first seen in 2014, the cluster immediately stood out to the team in James Webb Space Telescope (JWST) data because, being so large and concentrated, it resembled the galactic clusters found much closer to our own galaxy. However, this cluster is seen as it was around 10.4 billion years, just around 3.4 billion years after the Big Bang, a time when such structures were theorized to have only just begun to assemble.

Even more excitingly, XLSSC 122 is acting as a gravitational lens and is aligned with even more distant galaxies, amplifying their light and making them easier to study.

"When we got those first images back from JWST, we said, 'wow, look at this, there's strong lensing coming from this cluster!' XLSSC 122 has now set the record for the most distant galaxy cluster displaying strong lensing, which is a valuable tool for astronomers," team leader Kyle Finner of the California Institute of Technology said in a statement.

What is gravitational lensing and why is it so useful?

Gravitational lensing was first predicted by Albert Einstein in his 1915 theory of gravity, known as general relativity. General relativity says that objects with mass cause the fabric of space and time to warp. Think of this as being akin to placing a bowling ball on a stretched rubber sheet. Gravity arises from this curvature.

The greater the mass of the object, the more extreme the curvature and thus the greater the gravitational influence of that object.

But there is another consequence. Light normally travels in a straight line, but spacetime is the track that it follows. If spacetime is curved, then the path of light is also curved. The closer that light travels to an object of great mass, the more its path swerves.

That means when an object of great mass, in this case XLSSC 122, comes between Earth and a more distant light source, light from that background source arrives at our telescopes at different times based on the path it took around the intermediate object. This amplifies light from the background source and has been used by the JWST team to great effect in the study of ancient galaxies.

When the Hubble Space Telescope previously studied XLSSC 122, it wasn't able to capture images that showed it was a strong gravitational lens; it took the tremendous observing power of the JWST to determine this.

The strong lensing of this early galaxy cluster could also help unravel the mystery of dark matter. Effectively invisible because it doesn't interact with light, dark matter does interact with gravity. Plus, because it outweighs the "ordinary matter" that makes up stars, planets, moons, and gas clouds in galaxies by a ratio of five to one, dark matter makes the largest contribution to the lensing effect of galaxies and galactic clusters like XLSSC 122.

This means that gravitational lensing can be used to study the distribution of otherwise invisible dark matter in galaxy clusters, which is a vital element of galactic evolution, as it is thought that galaxies and galaxy clusters gather along vast filaments of dark matter. The hunt is now on for more lensing clusters like XLSSC 122, and if they are found so early in the universe's history, a major revision of cosmology may be on the cards.

"Strong lensing is a way to measure the dark matter without actually seeing the dark matter. It gives us a sensitive probe of our cosmological models,” said Finner. "It's still early in the JWST era, and if we can start to get data on tens or hundreds of these types of objects at this stage in the universe, then we can really start putting our cosmological models to the test."

The team's results were presented on June 17, 2026, at the 248th meeting of the American Astronomical Society. The research is available as a paper published in The Astrophysical Journal Letters.

An intense demolition derby of at least six galaxies smashing into one another has been found lurking in the early universe by the James Webb Space Telescope. This merger is also expected to fuel the growth of a supermassive black hole and trigger the formation of what will eventually become one of the most massive galaxies in the cosmos.

"What makes this special is that we can follow both the build-up of a giant galaxy and the growth of the black hole at its center," Huub Röttgering, an astronomer at the Netherlands' Leiden Observatory, said in a statement.

The discovery came after a tip-off from radio astronomers who had noticed emissions that seemed to be coming from an undiscovered active black hole. When the James Webb Space Telescope (JWST) looked closer, it found a surprise.

"We didn't find a single galaxy, but an entire complex of at least six galaxies," said Aayush Saxena of the University of Oxford.

These six galaxies sit at a redshift of 4.0, which equates to a time about 12 billion years ago, just 1.8 billion years after the Big Bang.

Through the vision of the JWST's Near-Infrared Camera the six galaxies appear fuzzy, reminiscent of a faraway version of Stephan's Quintet, which is a collection of five galaxies, four of which form a compact group that are on course to merge to become a giant elliptical galaxy.

Similarly, the six galaxies spotted by the JWST, and collectively termed TGSSJ1530+1049, will undergo a series of rapid mergers to become what is known as a 'brightest cluster galaxy,' which is an enormous elliptical galaxy of the kind found at the center of galaxy clusters.

"We call structures like this protoclusters: the precursors of the vast collections of galaxies we see today," said Leiden's Roderik Overzier. "These are places where matter came together very early on. We think we are seeing a rare moment when several massive galaxies still exist separately, but are already in the process of forming one much larger galaxy."

Already a supermassive black hole has formed at the heart of this galactic maelstrom, and radio observations with the European VLBI (very long Baseline Interferometer) Network and the U.K.'s e-MERLIN (enhanced Multi-Element Remotely Linked Interferometer Network) at a resolution on the scale of a 100 milliarcseconds have identified radio lobes and hotspots typical of an active black hole's jet interacting with the gas surrounding it.

"Using a network of connected radio telescopes, we were able to produce a very sharp image of TGSSJ1530+1049," said Krisztina Gabányi of Eötvös Loránd University in Budapest, Hungary. "The radio emission is produced as material falls into the black hole, while some of it is expelled again at high speed."

The jet doesn't seem to extend as far as all the galaxies in TGSSJ1530+1049 yet, implying that the black hole is still fairly young.

The six galaxies of TGSSJ1530+1049 span a volume only a few tens of thousands of light-years across, which is smaller than our Milky Way galaxy — and yet, they pack in a humungous amount of stars, equivalent to hundreds of billions of solar masses and a star-formation rate somewhere between 70–163 solar masses per year. That's a frenetic pace compared to the Milky Way, which produces much less than ten solar masses per year.

TGSSJ1530+1049 is one of the densest collections of heavyweight galaxies found in the early universe so far, and is giving exciting clues as to how the most massive galaxies, clusters and black holes in the universe formed.

The JWST observations are reported in The Open Journal of Astrophysics, while the radio measurements are described in a paper in Astronomy & Astrophysics.

NASA's James Webb Space Telescope is finding clues that are leading scientists closer to understanding the origins of the interstellar comet 3I/ATLAS.

What is it?

Comet 3I/ATLAS captured the world's attention when it was discovered nearly a year ago on July 1, 2025. The comet was first spotted by the Asteroid Terrestrial-impact Last Alert System (ATLAS), and is only the third interstellar object every discovered.

The comet swooped through our solar system, passing by Earth at a far (and safe) distance on its tour of our cosmic neighborhood. It is on a long trajectory that will take it out of our solar system, never to return.

In observations from the James Webb Space Telescope, scientists were able to look in the direction the comet as it began moving away from the sun in December of last year. While in close proximity to our star, the sun's heat warmed the comet, making it extra bright and easy to observe.

With this view, astronomers were able to calculate some of the ratios of the chemicals present in the comet. This further highlighted that the object is from out of our solar system, as they found ratios of carbon and heavy hydrogen not found in comets in our solar system.

Researchers described their results in a new paper published June 22 in the journal Nature.

Why is it incredible?

Being only the third interstellar object ever found, people were excited about 3I/ATLAS. They were so excited, in fact, that conspiracies about the object sprouted up quickly. Due to it being from outside of our solar system, some claimed that the comet could be some sort of alien spaceship, similar to the initial suspicions about the interstellar object 'Oumuamua found years earlier.

But with new information coming in from space telescopes, and astronomers eager to understand this object better, these clues are leading us closer and closer to the true origins of this strange comet.

A huge, shining bauble of stars called Terzan 5 could be a clump of our galaxy's central bulge that hasn't been smoothed out into the mix, and has instead survived as a fossil relic leftover from the birth of the Milky Way galaxy.

"Terzan 5 may provide direct evidence that can help explain how bulges formed in galaxies throughout the universe," said Barbara Lanzoni of the University of Bologna in a statement. Lanzoni is a member of a team of astronomers, led by Bologna colleagues Giorgia Zullo and Francesco Ferraro, who tackled Terzan 5 with the James Webb Space Telescope (JWST).

Terzan 5 is a globular cluster — a huge sphere of stars with a total mass two million times greater than our sun's and a total luminosity 800,000 times greater. The problem is, Terzan 5 lies about 18,800 light-years away in the bulge of the Milky Way galaxy. This means dense lanes of intervening galactic dust block our view, significantly dimming Terzan 5's apparent brightness. That's why it wasn't discovered until 1968 by the Turkish–French–Armenian astronomer Agop Terzan.

Globular clusters tend to be ancient. They also tend to have formed all their stars in one giant burst. As such, all their stars should be the same age, 12 to 13 billion years old. Yet, a select few globular clusters show evidence of having more than one generation of stars. These include Omega Centauri, NGC 2808 and NGC 1783 in the Milky Way galaxy, as well as NGC 411 in the Small Magellanic Cloud and NGC 1696 in the Large Magellanic Cloud. Several explanations have been put forward, including the possibility that they are the core remnants of dwarf galaxies that have been stripped of most of their stars by gravitational tidal forces emanating from the Milky Way. Or perhaps these clusters were simply massive enough to retain some molecular gas for future stellar generations.

When the Hubble Space Telescope took a look at Terzan 5 in 2009 and then again in 2016, it found that it too was among the ranks of weird globular clusters with two generations of stars, dating back 12.5 and 4.7 billion years. However, because it is behind so much galactic dust, not even Hubble has the clearest of views.

The JWST, however, does. Its near-infrared vision can see through the dust.

"Webb's new near-infrared observations, cross-referenced with Hubble's archival observations, have given us a much clearer picture of the history of Terzan 5," said study leader Giorgia Zullo, who is a Ph.D. student at Bologna.

The JWST detected two further generations of stars, one generation born 3.8 billion years ago and another 2.5 billion years ago. Four generations of stars is hard to explain for any globular cluster, which is why the team think that Terzan 5 could be something more primordial: a leftover building block of the Milky Way's bulge that was never quite assimilated by our galaxy.

"For some reason, this peculiar clump of stars formed separately from the bulge and was not destroyed as the bulge itself formed," said Ferraro. "Terzan 5 is what we now call a bulge fossil fragment because it resembles the primordial clumps that contributed to the formation of the bulge."

Disk galaxies sport two main components: a relatively narrow disk formed from spiral arms, and a bulbous core called the bulge. Galactic bulges tend to be the oldest parts of galaxies, forming billions of years before the disks, at least in the Milky Way's case. The JWST is seeing this process occurring in the early universe, revealing clumpy, young galaxies, but given the great expanse of space and time that JWST is looking across, the observations of the building blocks that go into making these galaxies are still not totally clear. With Terzan 5, we could be looking at one of the building blocks of the Milky Way's bulge relatively close-up, and it could provide new insights into the birth of our galaxy.

Terzan 5 is probably not the only bulge fossil fragment either. As well as those other aforementioned globular clusters, some of which might be fossil fragments and others might be the cores of dwarf galaxies, the globular cluster Liller 1 close to the center of our galaxy shares many of Terzan 5's properties, including its high abundance of heavy elements produced by multiple generations of stars that have died either in supernova explosions.

The team are now looking to chase up another 40 or 50 globular clusters in the bulge to see if they could also be bulge fossil fragments, or whether they are just regular globular clusters.

The findings were presented at the 248th meeting of the American Astronomical Society in Pasadena, California which took place between June 14 and June 18. A paper describing the JWST observations has also been published in the journal Astronomy & Astrophysics.

The image of the day for Monday (June 22) shows the star-forming clouds of Orion A in stunning detail.

Released as the James Webb Space Telescope (JWST) Picture of the Month, the image further demonstrates the impact the $10 billion space telescope has had on our view of the cosmos since it began operations in July 2022.

What is Orion A?

Located around 1,300 light-years from Earth and situated to the south of Orion's Belt in the night sky, Orion A is one of the largest and closest molecular clouds to our planet. Shaped like a filament, this structure of gas and dust is around 290 light-years long.

Part of the Orion molecular cloud complex, Orion A is a packed stellar nursery. Over the last few million years alone, it is estimated that Orion A has given birth to around 3,000 stellar objects.

The molecular cloud is also host to many young protostars surrounded by platters of gas and dust called protoplanetary disks, which, as the name suggests, will form planets. Thus, studying regions like Orion A could be key to understanding how the solar system came to be around 4.6 billion years ago.

Using the James Webb Space Telescope, astronomers have discovered that the well-known "Pink Planet" harbors a salty surprise and an exotic atmospheric chemistry. The discovery marks an advancement in the study of cold objects beyond the solar system.

Initially discovered in 2013, GJ504b orbits a sun-like star located around 57 light-years from Earth. With a mass around 25 times that of Jupiter, this Pink Planet may not be a planet at all despite its moniker. It may instead be a brown dwarf, a failed star that formed like a star but was unable to gather enough mass to achieve the nuclear fusion of hydrogen to helium in its core. Thus, astronomers refer to it as a "planetary-mass companion," which means a planet-size object orbiting a parent star.

GJ504b remains one of the coldest planetary-mass companions discovered using ground-based telescopes, with a temperature of around 550 degrees Fahrenheit (290 degrees Celsius). Although, that still makes it hot enough to bake bread. Now, James Webb Space Telescope (JWST) data reveals it has a key ingredient for bread making too: salt located in its atmospheric clouds, unlike anything astronomers have seen before.

"The Pink Planet is the coldest companion ever discovered using ground-based instruments," team leader Aneesh Baburaj of Northwestern University said in a statement. "Many teams all around the world performed follow-up observations to study its light, but it was too faint for ground-based instruments. That made it a perfect target for JWST.

"When we finally obtained its spectrum, it immediately looked interesting. But once we started digging deeper into the data, we realized it was not like anything we have analyzed before."

The Pink Planet is cold and old

The team studied this planetary companion by measuring its faint electromagnetic radiation emissions and filtering out the bright glare of its parent star.

They found the relative coolness of the Pink Planet is a result of the planet's age. Both gas giant planets and brown dwarfs are born blisteringly hot but cool off as they get older. This new research estimated that GJ504b is between 2.5 billion and 4 billion years old.

Breaking down light from the Pink Planet into individual wavelengths, the team was also able to determine its chemical composition. This is possible because elements absorb and emit light at characteristic wavelengths, meaning they leave "fingerprints" on light passing through their atmospheres.

"In the past, other astronomers observed the companion for an entire night with some of the biggest telescopes in the world to obtain a spectrum," Baburaj said. "And they could not see the object. With JWST, our entire observation took around two hours, and we were successful."

The JWST data revealed a rich cocktail of chemicals in the atmosphere of the Pink Planet that included water, carbon dioxide, methane, and ammonia. However, these observations didn't match modeling of the planetary companion's atmosphere until the team factored in something completely unexpected: clouds of salt deep in the atmosphere.

"We ran simulations with clouds, and the results aligned with what we know about cold planets," Baburaj said. "We tried three different types of clouds, and salt clouds fit best. When we accounted for salt clouds, it subdued the signature of molecules hidden deeper in the companion’s atmosphere. Then, the results became physically possible.

"This is the first time we've found that salt clouds are critical to explaining the spectrum of an object. It's a good reminder to account for clouds in our models."

Though this mystery may be solved, there are still questions surrounding GJ504b that will only be solved with further investigation. The Pink Planet seems to be unusually rich in elements heavier than hydrogen and helium, which astronomers call metals. This means the team still can't pin down the origin of the Pink Planet; did it form like a planet, or like a star?

That means they aren't quite ready to determine if GJ504b is a gas giant planet or a brown dwarf... or should that be Pink Dwarf?

The team's research was published on Thursday (June 18) in The Astronomical Journal.

Astronomers using the James Webb Space Telescope may be close to solving the mystery of "little red dots" in the early universe. The team has studied one of these strange objects, designated GLIMPSE-17775, finding evidence it is a black hole star — a ravenously feeding, growing supermassive black hole cocooned in a dense cloud of partially ionised gas.

Little red dots first started to turn up when the James Webb Space Telescope (JWST) began sending data back to Earth in the summer of 2022. They were said by some scientists to have "broken cosmology" because they appear in large numbers around 600 million years after the Big Bang, but they appear to disappear before the universe reaches 2 billion years old. Several explanations for little red dots have been proposed, but one that has emerged as a frontrunner is the concept of black hole stars. If black hole stars exist, the little red dot disappearance would be the result of their intense, short-lived growth spurts that cause them to burn out — or, because the growing supermassive black holes at their centers eventually clear away the dense gas and dust obscuring them, changing their appearance as they evolve into more typical active galaxies.

The problem is, however, that astronomers have been unable to gather observational evidence that little red dots are indeed black hole stars. That was until the JWST imaged little red dot GLIMPSE-17775, seen as it was just 1.8 billion years after the Big Bang, while making observations of the gravitational lens galaxy cluster Abell S1063. This data represents the deepest spectrum of light from a little red dot collected to date and, according to this team, contains multiple lines of evidence pointing to a black hole star.

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

Solving the little red dot puzzle with a hand from Einstein

The JWST caught a glimpse of GLIMPSE-17775 while searching for the first generation of stars in our universe, somewhat confusingly called "Population III" stars. The telescope searched for these particular stars in the galaxies that comprise galaxy cluster Abell S1063.

Separately, Abell S1063 is a gravitational lens, meaning its massive gravitational influence actually curves the fabric of space and time (united as a single, four-dimensional entity called spacetime). This, in turn, means an object "behind" the galaxy cluster that's emitting light toward our vantage point would have its light path curved in tandem with the spacetime curve. This can create a magnifying effect.

The concept of gravitational lensing was first predicted by Albert Einstein in his theory of general relativity, and it's how scientists were able to observe GLIMPSE-17775 — essentially turning 30 hours of observing time into just about 80.

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

The team identified several lines of evidence in the JWST observations that indicate "little red dot" GLIMPSE-17775 is indeed a black hole star. This includes emissions from elements that don't conform with what would be expected in a rotating gas cloud. The emission lines instead indicate the scattering of electrons, which is expected when a source of radiation is enshrouded by a vast and dense cocoon of gas. Also indicative of a dense shroud of gas were signs of fluorescence and helium-absorbing radiation.

The team also saw spectral lines from iron, which the team dubbed an "iron forest." That is something expected as a result of the high-energy output of a rapidly feeding supermassive black hole: a black hole star.If little red dots are rapidly accreting supermassive black holes shrouded by dense gas envelopes, this would explain why these mystery objects are so faint in X-rays, as these cocoons should absorb this high-energy radiation.

There is something missing from observations of GLIMPSE-17775, however.

Little red dots usually have a strong characteristic dip in the spectra of light they emit, what's known as a "Balmer Break." The team thinks this feature is weaker for this little red dot than others because GLIMPSE-17775 is surrounded by a massive host galaxy. The team's data therefore fits as a missing piece of the puzzle of little red dots, slotting in nicely with our understanding of the evolution of the universe.

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

The team's research was published on Wednesday (June 10) in The Astrophysical Journal.

Using the James Webb Space Telescope (JWST), astronomers have "weighed" a sleeping giant — a dormant supermassive black hole located a staggering 10 billion light-years away. That makes this black hole the most distant supermassive black hole scientists have ever measured the mass of.

The supermassive black hole is located at the heart of the galaxy MRG-M0138, which is seen as it was when the universe was just around 4 billion years old — and we now know, thanks to the James Webb Space Telescope (JWST), that it weighs an incredible 6 billion times the mass of the sun.

Supermassive black holes can be very conspicuous when actively feeding and therefore surrounded by a wealth of matter in a region called an active galactic nuclei (AGN). Because of the black hole's immense gravitational forces, an AGN glows very brightly. However, because black holes are surrounded by a light-trapping boundary called an event horizon, dormant black holes with larders that aren't quite so well stocked are far more elusive. They're practically invisible. Still, even these black holes have gravitational influences that can impact more than the swirling platters of gas and dust — that influence can also affect the motion of stars orbiting the black holes. And those stars are indeed visible.

To detect and measure the mass of this supermassive black hole, the team behind this research used the JWST to track the motion of stars at the heart of MRG-M0138. This star-tracking trick has been used in the past to weigh dormant black holes much closer to Earth — for example, the 4.3-million-solar-mass supermassive black hole at the heart of our own galaxy, Sagittarius A* (Sgr A*). However, Sgr A* and its attendant stars are just 26,000 light-years away, and the most distant black hole this technique, called stellar dynamics, had been used to weigh was located just 700 million light-years away. At about 15 times that previous record-holding distance, this new research is the first time it has been successfully employed to measure the mass of such a distant sleeping giant.

"Determining how stars collectively move within the core of this distant galaxy has allowed us to measure the mass of its otherwise undetectable supermassive black hole," team leader and University College of London scientist Richard Ellis said in a statement. "By demonstrating the feasibility of such a technique for galaxies in the early universe, we can now undertake a more complete census of how black holes develop over time and infer their role in shaping galaxy evolution."

However, determining the motion of the stars at the heart of MRG-M0138 was anything but straightforward. It required a natural cosmic phenomenon known as gravitational lensing, which emerged from Albert Einstein's magnum opus theory of gravity, known as general relativity.

What is gravitational lensing?

General relativity predicts that objects with mass create an actual curvature in the fabric of spacetime, the four-dimensional unification of the three dimensions of space and the one dimension of time. Gravity emerges from this curvature, and because the larger the mass, the greater the curvature, the larger the mass of an object, the stronger its gravity.

Gravitational lensing occurs when a massive object such as a galaxy or a cluster of galaxies sits between a more distant foreground object and Earth. As light from a background source passes the curvature of space caused by the massive foreground object, or gravitational lens, its usually straight path becomes curved.

The closer to the gravitational lens light passes, the more its path is diverted, and that means that light from the same object reaches our telescopes at different times. This can magnify the object and, in extreme cases, can make the same object appear multiple times at different positions in the same image.

The gravitational lensing effect of a galaxy between MRG-M0138 and Earth refocused the light from that distant galaxy, magnifying it by 30 times, allowing Ellis and colleagues to intricately reconstruct the internal details of MRG-M0138.

"By combining JWST data with gravitational lensing, we could peer inside the black hole’s sphere of influence, where its gravity boosts the speeds of stars," Andrew Newman of Carnegie Science in Pasadena, California, said. "This is one of the best techniques we have to weigh a black hole, so we were excited to extend it to a much earlier period in cosmic history."

In addition to investigating this dormant black hole, the team also determined that MRG-M0138 itself is dormant, meaning it is no longer forming new stars. This is likely the result of the supermassive black hole undergoing a ravenous feeding frenzy earlier in its history when it would have appeared as a blazing quasar at the heart of an AGN. The energy released during this phase would have pushed gas and dust away from both the black hole, ending its feeding phase, and from MRG-M0138 itself. This would deplete the galaxy of the raw material for star formation, thus quenching its stellar birth rate.

This means that with these observations, and with more JWST dormant supermassive black hole data, scientists can better understand the relationship between galaxy growth and supermassive black hole growth, as well as the role these cosmic titans play in cutting off star formation in their host galaxies.

The team's research was published on Thursday (June 4) in Science.

On May 22 at Heft Gallery in New York City, "Redshift" transformed a gallery space into an existential experience for an intimate audience. The immersive audiovisual performance, created by artist Ashley Zelinskie and DJ/Producer illich Mujica, blended live electronic music, custom-coded visuals, NASA-inspired imagery and spoken-word narration into a cosmic ride through light and sound themselves.

The sold-out event opened with a listening session of NASA's Golden Record — the message launched aboard the interstellar Voyager probe in 1977 to offer a slice of Earth to any intelligent life that might encounter it. Played through the "Volumes" listening system designed by Joe Doucet, the opening moments set the tone for a performance rooted in science, art and wonder.

Drawing heavily from imagery captured by the James Webb Space Telescope, Zelinskie's visuals, projected on a wall of the gallery, shifted through wavelengths of light to simulate the astronomical phenomenon of redshift — the stretching of light across space and time. Mujica's live audio performance moved alongside the stunning visualizations, weaving together ambient electronica, psychedelic rock, and NASA-inspired spoken word samples to deliver a psychedelic event that was meditative and hypnotic at times.

In the conversation below, Zelinskie, Mujica and gallery owner Adam Berninger talk about how "Redshift" came to life, the Webb imagery behind the visuals, the inclusion of Pink Floyd's "Is There Anybody Out There?," and more.

Space.com: How did you decide which part of NASA's historic Golden Record would open the experience?

Adam Berninger: ​The evening began with a listening session from NASA's Golden Record, the sounds of Earth encoded on a disc and launched into deep space in 1977 aboard Voyager. A message from us to whatever might be out there. We listened to the opening greeting from the United Nations followed by a selection of music.

The record was played on the Volumes listening system designed by Joe Docet, conceived as spatial listening instruments rather than conventional audio speakers. They're installed as the centerpiece of our "Transmissions" initiative, created to bring together important musical experiences with a range of systems-based fine artworks at our LES gallery, Heft. These events run from May 15 - June 12th.

Space.com: "Redshift" was shaped by both astronomy and sound design. How did the concept evolve between the two of you?

Ashley Zelinskie: Once Illich and I decided we wanted to collaborate on a Transmission, we met in my studio to come up with our concept. We liked the way sound and light are both waves (sometimes). Redshift occurs when light gets older, the waves stretch out and become longer or more red. This is similar to the Doppler effect with sound. During my time working alongside the Webb Telescope team, which is an infrared telescope for this very reason, I became familiar with this phenomenon. Our concept for "Redshift" ended up being "light in service of sound and sound in service of light."

We started our performance in the ultraviolet light spectrum and slowly shifted toward red. The music also shifted from long-wave, experimental sounds to higher BPM (Beats Per Minute) and more complete scores of music — short light waves, long sound waves / long light waves, short sound waves. The cross back and forth was important to us.

Space.com: The James Webb Space Telescope (JWST) imagery throughout the performance was stunning. Which observations resonated most with you artistically, and why were they chosen?

Ashley Zelinskie: I am always drawn back to the first images. They will forever be my favorite. They made such a huge impact on my artistic practice because I watched the telescope be built and launched, and then had the honor of being at Goddard when the first images were released. They were the core inspiration for my exhibition Unfolding the Universe: First Light in 2021 at Onassis ONX Studio.

I made several visuals based on the cosmic cliffs of the Carina Nebula. One of my calmer visuals was the slow orbit and collision of Stephan's Quintet and for the end of the performance I had the pulsing beat of rings of stardust exploding from the Southern Ring Nebula.

I used a few new JWST images as well, including the MIRI (Mid-Infrared Instrument) image of galaxy M77. Every visual had a background of stars trained off a LoRA of Webb deep fields. I used a few AI tools to create the visuals as well as wrote the VJ software used in the performance.

Space.com: Redshift blended live DJ performance, immersive sound design and custom visuals seamlessly. What tools and techniques powered the experience?

illich Mujica: I DJ'ed and mixed the audio spontaneously during performance time using curated playlists of my 25 year catalogue of DJ'ing. I was chopping, looping, time-stretching, adding FX and blending 4 channels of audio via Traktor Pro 4; choosing from my library of ambient and electronica (old and contemporary), Psychedelic & Indie Rock and samples from space-related podcasts and films.

On the hardware side of things I used a portable Traktor Z1 DJ mixer and sound card + an AKAI Pro MIDI keyboard to MIDI control and navigate my whole laptop DJ rig. While I use the mini MIDI keyboard to produce music while I travel, this time it functioned fully as a DJ controller. Both of our machines were MIDI-linked via Ethernet cable connection.

Space.com: A memorable moment of the night was the inclusion of Pink Floyd's "Is There Anybody Out There?" What drew you to that particular piece?

illich Mujica: That was my choice, and it was an in-the performance moment. I was frantically browsing through my psychedelic rock playlist before the music went to silence, hoping to find spacey/space-related songs. I was actually looking for David Bowie's "Space Oddity" at first and then I remembered about Pink Floyd's "Is there Anybody Out There?".

This isn't one of their most famous songs, it actually works as a bridge song in the album "The Wall" between "Hey You" (a well-known song of theirs), and "Nobody Home" on Volume 2 of that album. The themes of Pink Floyd's concept album "The Wall" revolve around aspects of alienation, trauma and self-isolation.

When I first heard "Is there anybody out there?" in my teenage years, I understood it as an inner monologue of the mind; that monologue of detachment someone could have when grappling with issues of mental health; but over time, after many years, for me, the theme of this song as I hear it, morphed into the age-old question of "is there life in other planets?".

I love playing this on listening sessions and felt the sonic ethereal and more-abstract qualities of it was a better fit than Bowie's song for the nature of our Redshift performance; specially as I knew I was about to mix in a sample from a podcast interview with the crew of the Artemis II expedition where one of the astronauts talks about whether or not there is life (or someone) out there.

Space.com: The spoken-word samples and narration added a cinematic layer to the performance. Can you talk about the voices and stories woven into the show?

illich Mujica: As I mentioned, it was a selection of samples I dug exclusively for the performance. On one hand I sampled a question a kid asked the crew of the Artemis II in the NY Times' podcast The Daily. The question was "is there life out there?" and one of the answers one of the crew members shared just blew my mind:

"If you look at the closest neighboring galaxy which is Andromeda - let's say there's another amazing civilization there with the most amazing telescope, looking at Earth right now while we are chatting - what do they see? - They see us a couple of thousand years ago, so … we are not here. That's our closest neighboring galaxy so it gives you an idea of how hard it is to look for life in the universe..."

This concept also tied in with the spirit of Redshift and light as a measurement of time. The opening sample is also from "The Daily," in the same interview they used the kid singing about going to the moon as their intro.

For "The Daily," the sample was about space travel — for me it was about that, but most importantly, we were about to travel into a sonic journey with Joe Doucet's "Volumes" sound art/sound system!

The other sample used is my friend Tory Stolper, whose spoken word poem is part of our song "Surya Rising." I was able to not only play my original song on this amazing sound system but also feature a never-before-played sample from her voice note messages, where she was unsure about the creative process of the song from her perspective, as a prelude to our song about to be mixed in.

It's one of my most famous songs (with her), and I knew my crowd and fans were waiting for this one to drop on the amazing sound system. It was a treat for them, but it also fit the cosmic nature of the performance.

"Surya Rising" (Surya = sun in San script) was a song I wrote about sunrises at Burning Man. It speaks to the feelings this cinematic sunrise evokes in the desert as we find ourselves on this amazing planet.

You can listen to the entire mind-bending performance on SoundCloud. Explore Ashley's artwork on her website, and dive into illich's musical journey here.

The James Webb Space Telescope (JWST) has made a weather forecast for the exoplanet WASP-94Ab, a world with clouds of sand in the morning that gradually give way to a clear sky at sunset.

It is the first time that the daily cycle of weather has been observed on a hot Jupiter exoplanet. Furthermore, the clear evening sky has provided astronomers with an unobscured view of WASP-94Ab's atmospheric composition, finding it to be closer to that of our own Jupiter than previous inaccurate measurements had suggested.

WASP-94Ab is located about 690 light-years from Earth and orbits one of two stars in a wide binary system. The planet is a gas giant 1.7 times larger than Jupiter and orbits its star every four days at a distance of 5.1 million miles (8.2 million kilometers) — close enough to be hotter than over 2,200 degrees Fahrenheit (1,200 degrees Celsius). Hence, we call such worlds "hot Jupiters."

Previous attempts to get a handle on the composition of hot Jupiters has been stymied by the fact that they are often very cloudy, which obscures much of the atmosphere. Unlike Earth's clouds of water vapor, a hot Jupiter's clouds are made of vaporized metals and rock, like giant flying sandstorms. In the case of WASP-94Ab, the clouds are composed of vaporized magnesium silicate.

"I've been looking at exoplanets for 20 years and general cloudiness has been a thorn in our side," David Sing of Johns Hopkins University said in a statement. "We've known for quite a while that clouds are pervasive on hot Jupiter planets, which is annoying because it's like trying to look at the planet through a foggy window."

But are hot Jupiters cloudy all of the time? Astronomers led by Sing put this to the test by watching WASP-94Ab with the James Webb Space Telescope (JWST) as the planet transited, or crossed the face of, its star from the spacecraft's point of view. Using a technique called transit spectroscopy, the astronomers were able to watch as the light from the star was filtered through the atmospheric gases and clouds on the leading and trailing limbs of WASP-94Ab as it transited. Some of this light is blocked by gases in the atmosphere, and the wavelengths at which that light is absorbed gives away the identity of those gases.

Sing's team saw that on the leading edge, where it was considered "morning" with air flowing from the nightside to the dayside, there were plenty of magnesium silicate clouds. However, on the trailing edge where it was "evening" with air flowing back to the nightside, the clouds had disappeared, leaving an unencumbered view of the hydrogen-dominated atmosphere. Previous Hubble Space Telescope observations had not been able to split the absorption effects of the leading and trailing limbs, so it seemed as though WASP-94Ab had hundreds of times more oxygen and carbon than Jupiter does. Given what we know about how gas giants form, this seemed improbable.

However, by detecting the cloudless sky of the trailing edge the JWST was able to get a more accurate reading by removing the effect of the clouds, finding that oxygen and carbon were only five times more abundant than on our Jupiter.

So WASP-94Ab seems like a fairly ordinary gas giant planet after all, but why are the clouds clearing? According to Sing and his colleagues there are two possibilities. WASP-94Ab is tidally locked, meaning that it always shows the same face to its star, so it has one hemisphere of permanent daylight and one hemisphere of permanent darkness. Strong winds at the terminator between day and night could be blowing the magnesium silicate high into the atmosphere, where it forms clouds over the nightside. Winds then blow these clouds around to the dayside, where they gradually descend deeper into the planet where they can no longer be seen, only to be dredged back up when the magnesium silicate circulates back around to the nightside.

The alternative is that the magnesium silicate clouds are like morning fog on Earth, steadily dissipating over the course of the day in 2,200-degree-Fahrenheit heat.

"Not only have we been able to clear the view, but we can finally pin down what the clouds are made out of and how they’re condensing and evaporating as they move around the planet," said Sing.

He and his team then used the JWST to follow up on another eight hot Jupiters, finding a similar cycle of clouds on two of them, WASP-17b, which is a large but very low density world with a bloated atmosphere and orbiting backwards around its star, and WASP-39b, which is another low density world with an atmosphere unusually rich in water vapor as well as carbon and sulfur dioxide.

The next step is to expand the search for cloudy weather on exoplanets by looking at a greater variety of worlds, including one gas giant that is on a highly eccentric orbit that takes it from its star’s habitable zone to much closer in and then back out again. The dramatic changes in heating could drive all manner of powerful weather systems that could be visible to the JWST.

The clouds on WASP-94Ab, WASP-17b and WASP-39b were reported on May 21 in the journal Science.

Is this a galaxy or a movie poster for a sci-fi smash hit?

A new image captured by NASA's James Webb Space Telescope shows the galaxy Messier 77 (M77) in stunning new detail with beams of glowing light shining outward. And the secret behind its incredible glow? A black hole.

What is it?

The galaxy M77, nicknamed the Squid Galaxy, takes center stage in this striking new image snapped by NASA's James Webb Space Telescope. The galaxy's heart shines brightly in the image, with gleaming rays of light radiating from its center while gas and dust swirls around.

M77 is a barred spiral galaxy located about 47 million light-years from Earth and can be found in the night sky in the constellation Cetus. The galaxy is visible to skywatchers, with a magnitude of 9.6, you can typically spot it with the help of a small telescope.

Interestingly, while this object is a Messier galaxy, meaning it was catalogued by astronomer Charles Messier, it was actually discovered by another French astronomer named Pierre Méchain who told Messier of his discovery.

Why is it incredible?

The secret behind this ethereal glow is actually a black hole. Scientists think that at the heart of most galaxies lies a black hole, and in M77, its central black hole's intense gravity is pulling gas inward. This movement causes the gas to heat up, releasing radiation and glowing tremendously as we can see in this snapshot, according to a statement from NASA.

In addition to the glow, the image stands out because of the incredible rays of light shining from its center. But these lines of light aren't caused by the gravitational pull of a black hole, instead they are actually an optical effect caused by the telescope, according to the statement.

Whatever the reason behind its appearance, one thing is certain: this galaxy is truly breathtaking in this new image.

Using the James Webb Space Telescope, astronomers have mapped the "cosmic web" of galaxies — the largest structure in the universe — with unprecedented detail.

This is the largest James Webb Space Telescope (JWST) survey conducted to date, and is known as COSMOS-Web. It traces a network of galaxies back to when the universe was about 1 billion years old.

The cosmic web is the term scientists use to describe a skeleton-like framework of filaments and sheets of dark matter and gas along which galaxies gathered and evolved over time, which is punctuated by nearly empty voids. Thus, the cosmic web forms the architecture of the universe — it's a singular, intricate, far-reaching structure that traps galaxies and galactic clusters like flies strung along the sticky silk web of a greedy spider.

The results obtained by the COSMOS-Web team further demonstrate the power of the JWST to refine and redefine our view of the universe since the $10 billion space telescope began beaming data back to Earth in the summer of 2022.

"JWST has completely changed our view of the universe, and COSMOS-Web was designed from the start to give us the wide, deep view we need to see the cosmic web," leader of this research, Hossein Hatamnia of the University of California, Riverside (UCR), said in a statement. "For the first time, we can study the evolution of galaxies in cluster and filamentary structures across cosmic time, all the way from when the universe was a billion years old up to the nearby universe."

By the "nearby universe," Hatamnia means up to a distance of around 1 billion light-years. The solar system is estimated to be around 2 light-years wide, giving you an idea of just how far astronomers consider our cosmic backyard to extend. COSMOS-Web extends this by another 13 or so billion light-years.

That kind of depth of view is the only way astronomers can get a true picture of the cosmic web.

The large-scale structure delivered by COSMOS-Web provides a wealth of information greater than that provided by earlier maps of the same region of sky captured by the Hubble Space Telescope. Team member and UCR scientist Bahram Mobasher explained that comparing Hubble and JWST shows that many cosmic structures had been "smoothed over" in data from the JWST's space telescope predecessor.

"The jump in depth and resolution is truly significant, and we can now see the cosmic web at a time when the universe was only a few hundred million years old, an era that was essentially out of reach before JWST," Mobasher said. "What used to look like a single structure now resolves into many, and details that were smoothed away before are now clearly visible."

The impressive leap in detail provided by the JWST and COSMOS-Web is the result of the unification of two of this powerful new space telescope's key strengths.

"The telescope detects many more faint galaxies in the same patch of sky, and the distances to those galaxies are measured far more precisely," Hatamnia said. "Each galaxy can therefore be placed into the correct slice of cosmic time, sharpening the map's resolution."

The team's research was published on May 6 in The Astrophysical Journal.

The Whirlpool Galaxy sprawls across the cosmos in this striking new snapshot from NASA's James Webb Space Telescope (JWST).

The galaxy, formally known as M51 (Messier 51), stretches out its spiral arms, glowing brightly in the darkness of space. While the galaxy's many limbs have been spotted before by the Hubble Space Telescope and even amateur astronomers, this image captures a uniquely striking view of its galactic beauty.

What is it?

The Whirlpool Galaxy was captured in this image by JWST's Near-Infrared Camera (NIRCam), according to a statement. This is JWST's primary instrument for seeing the universe in near-infrared light, which is a range of the electromagnetic wavelengths just out of our eyes' reach.

By seeing in near-infrared, NIRCam was able to capture this incredible view of part of the Whirlpool Galaxy. Located in the constellation Canes Vanatici, the spiral galaxy is made up of long swirls of gas and dust speckled with stars.

Beyond being just a beautiful cosmic sight, the formations of dust and gas that comprise this galaxy are actually a star-forming region. Here, gases like hydrogen and dust are compressed, condensing into new stars.

Why is it incredible?

This image shows only a section of the incredibly expansive spiral galaxy. The galaxy's red and orange spiral arms bending outward can measure tens or even hundreds of light-years across.

The full galaxy measures an incredible 76,900 light-years across. While this is an enormous size for any object or region, our own Milky Way galaxy measures over 100,000 light-years in diameter. But size and distances get fairly massive when we're talking on a cosmic scale. The Whirlpool Galaxy is a whopping 31 million light-years away from our own, but it's still considered one of our closer neighbors.

Something that has made the Whirlpool Galaxy beloved is its visibility. With an apparent magnitude of +8.4, skywatchers and amateur astronomers using small telescopes or even just binoculars are able to spot the galaxy and its spiral shape.

Astronomers have captured an extraordinary new look at the hidden birthplaces of star clusters, uncovering fresh clues about how galaxies evolve — and how young planets may be shaped by their stellar environments.

Using observations from the James Webb Space Telescope (JWST) and the Hubble Space Telescope, astronomers studied nearly 9,000 young star clusters across four nearby galaxies: Messier 51, Messier 83, NGC 628 and NGC 4449. The newly released images reveal glowing clouds of gas and dust where thousands of stars are actively forming, while also highlighting the JWST's growing ability to uncover hidden galactic structure. Brilliant knots of newborn stars, dark rivers of dust and glowing cavities carved by stellar winds combine to create a vivid portrait of galaxies in constant motion.

While the JWST's infrared vision allowed scientists to peer through thick cosmic dust, Hubble traced older, fully exposed clusters in visible light. Together, the observations allow researchers to study star clusters from their earliest, dust-shrouded stages to fully emerged stellar groups, according to a statement from NASA.

"This work brings together researchers simulating star formation and those working with observations, as well as groups researching planet formation," Alex Pedrini, lead author of the study from Stockholm University and the Oskar Klein Centre in Sweden, said in the statement. "Using Webb, we can look into the cradles of star clusters and connect planet formation to the cycle of star formation and stellar feedback."

By developing simulations that account for stellar dynamics in emerging star clusters, researchers discovered the universe's largest star clusters break free from their birth clouds much faster than expected, dramatically altering their surroundings in the process. The team found that the most massive clusters cleared away their natal gas clouds in about five million years, while smaller clusters took up to eight million years to emerge — a relatively small difference that could influence how star formation unfolds within galaxies over time.

"Simulations of star formation and stellar feedback have struggled to reproduce how star clusters form and emerge from their natal clouds," said Angela Adamo, co-author of the study and Principal Investigator of the FEAST (Feedback in Emerging Extragalactic Star Clusters) program, which collected the observations used in the research as part of a broader effort to investigate how newly formed stars shape the galaxies around them. "These results give us important new constraints on that process."

Once freed from their birth material, these giant clusters unleash intense ultraviolet radiation and stellar winds that heat and disperse nearby gas — a process known as stellar feedback. Because cold gas is the raw material needed to form new stars, stellar feedback can effectively regulate future star formation inside galaxies.

The findings could also reshape scientists' understanding of planet formation. Young planetary systems developing around stars inside these clusters may become exposed to harsh ultraviolet radiation earlier than expected. That radiation can erode the disks of gas and dust surrounding newborn stars, potentially limiting how large planets are able to grow, according to the statement.

Their findings were published May 6 in the journal Nature Astronomy.

Astronomers using the James Webb Space Telescope have, for the first time, directly analyzed the surface of a planet beyond our solar system,

The James Webb Space Telescope's (JWST) exoplanet subject, LHS 3844 b, is a so-called "super-Earth" about 30% larger than our planet and located nearly 50 light-years away. Unlike most exoplanet studies, which focus on atmospheres, astronomers analyzed heat emitted from this planet's surface.

The findings reveal a dark, airless world that may resemble Mercury. Scientists say this kind of direct interpretation of a distant planet's geology marks "the next step in unveiling their nature."

"Thanks to the amazing sensitivity of JWST, we can detect light coming directly from the surface of this distant rocky planet," Laura Kreidberg of the Max Planck Institute for Astronomy in Germany, who served as the principal investigator of the JWST observations, said in a statement. "We see a dark, hot, barren rock, devoid of any atmosphere."

Discovered in 2019, LHS 3844 b orbits a cool red dwarf star in just 11 hours and is tidally locked, meaning one side constantly faces the star while the other remains in darkness. The dayside reaches temperatures of about 1,340 degrees Fahrenheit (725 degrees Celsius), the scientists say.

In 2023 and 2024, Kreidberg and her team observed three secondary eclipses, when the planet moved behind its star. Using the JWST's Mid-Infrared Instrument (MIRI), they measured the infrared light emitted from the planet's intensely hot dayside and used it to study its surface.

By comparing the signal with known rocks and minerals from Earth, the moon and Mars, the team ruled out an Earth-like crust rich in silica and granite. Such crusts typically form through water-driven geological processes and plate tectonics, which recycle rock and allow lighter minerals to rise to the surface, the study notes.

Instead, the data point to a surface dominated by basalt, a dark volcanic rock rich in iron and magnesium commonly found on the moon and Mercury, the researchers say.

"This planet likely only contains little water," study lead author Sebastian Zieba of the Center for Astrophysics, Harvard & Smithsonian in Massachusetts said in the statement.

One possible explanation, the researchers say, is that LHS 3844 b has a relatively young surface shaped by recent volcanic activity, where fresh lava has not yet been broken down by micrometeorite impacts. However, such activity is known to release gases such as carbon dioxide or sulfur dioxide, which were not detected by MIRI, the study notes.

"If present on LHS 3844 b in reasonable amounts, MIRI should have detected it," the statement read. "Still, it found nothing."

Alternatively, the planet may be covered in a thick layer of dark, fine-grained material formed over long periods by radiation and meteorite impacts, similar to the moon or Mercury. Without an atmosphere, the surface would be especially vulnerable to this process, known as space weathering, which gradually breaks down and darkens rock.

"This alternative relies on longer periods of geological inactivity, thereby requiring conditions opposite to the first scenario," the statement read.

Follow-up JWST observations are planned to further refine the planet’s surface properties and determine whether it is solid rock or loose, weathered material, the study notes.

"We are confident the same technique will allow us to clarify the nature of LHS 3844 b's crust and, in the future, other rocky exoplanets," Kreidberg said in the same statement.

A study about these results was published Monday (May 4) in the journal Nature Astronomy,

In its infancy, the universe had a bit of an identity crisis.

For the first few hundred million years, the vast cosmic gas between galaxies was primarily a chilly, dense affair. But then, it seemed to wake up, deciding to get all warm and fuzzy.

This strange shift in the cosmos’ early disposition is a crucial clue to how the very first galaxies burst into being, shaping everything we see today. The early universe, a mere whisper after the Big Bang, just a few hundred million years old — that's when the first stars and galaxies were starting to flicker on, like fairy lights across a cosmic dark.

The fuel for all this grand production: gigantic clouds of gas, mostly hydrogen. Astronomers have always suspected these baby galaxies were busy, but new glimpses from the James Webb Space Telescope are showing them to be even brighter and larger than our wildest dreams. They're like finding teenagers sitting in a kindergarten class, way ahead of their expected development.

This cosmic precociousness means our existing models of how galaxies form might need a serious tune-up. We thought we had a pretty good handle on how gas falls into dark matter halos, cools down, and then ignites into stars. But the JWST data suggests a much more aggressive, faster-paced star-making frenzy in those early days. The question becomes: How did these young galaxies manage such a booming business so quickly?

To untangle this mystery, Umberto Maio from the INAF-Italian National Institute of Astrophysics and the Institute for Fundamental Physics of the Universe, working with Céline Péroux at the European Southern Observatory, decided to dive into the virtual cosmos. They created incredibly detailed computer simulations, a sort of cosmic time machine called ColdSIM, to rewind the clock and watch how gas behaved in the first billion years after the Big Bang. Their goal was to make predictions about the early universe’s baryon budget — that's the accounting sheet for all the "normal" matter, the stuff stars and planets are made of, and where it ended up.

What they found was a universe in flux. Before a pivotal moment called the epoch of reionization — when the universe finally became transparent to ultraviolet light — the gas was indeed mostly cold. It was the perfect, dense environment for star formation. But as star formation really picked up, and that intense ultraviolet light started zipping around, things changed. The simulations showed that the gas quickly shifted, becoming dominated by a warm, less dense phase. It’s like the universe went from a quiet, cool morning to a bustling, sun-drenched afternoon, with all that energy from new stars and radiation heating things up.

This wasn't just a minor temperature change. It fundamentally altered the rhythm of galaxy evolution. The team's clever simulations traced the journey of various types of gas, carefully avoiding the usual shortcuts in models that can often lead to fuzzy answers. They found some eye-opening things about how these infant galaxies put themselves together.

For starters, the stellar return fraction was surprisingly low. This is the amount of material that stars eject back into the surrounding gas when they die, essentially recycling fuel for the next generation of stars. In the early universe, it seems, stars were less efficient at this recycling. Lower quantities of old stellar material returned to the gas, meaning that new stars largely formed from fresh, pristine gas constantly falling in from the cosmic web. It's a bit like a construction site that keeps getting new materials delivered rather than reusing much from demolished buildings.

But even with less recycling, these galaxies were burning through their gas at an astonishing rate. Maio and Péroux discovered that the depletion times — the time it would take for a galaxy to convert all its gas into stars at its current rate — were incredibly short. Much shorter than we see in galaxies today. This means that early galaxies were true star-forming machines, gobbling up gas and spitting out stars with a furious intensity. It paints a picture of baby galaxies throwing one heck of a tantrum, furiously making stars with every available bit of gas.

So, why does any of this matter? Because it rewrites a part of our cosmic origin story. Our initial predictions for these early galaxies, based on observations of later, more mature galaxies, simply weren't capturing this dynamic, rapidly evolving picture. It turns out that you can't just take what you know about middle-aged galaxies and apply it to their energetic youth. The physical processes, from gas dynamics to stellar feedback, are just too different when the universe itself is so young and compact.

Of course, this cosmic detective story is far from over. Numerical simulations are powerful, but they’re always battling with the sheer complexity of the universe. Modeling everything from the intricate, multi-phase structure of gas to the powerful winds blown out by massive stars and black holes is a huge challenge. There are still big uncertainties, like the exact initial mass function of stars (how many big stars versus small stars are born) and the precise amount of "metals" needed to kickstart cooling. Our models still have plenty of room to grow.

But the good news is, we’re armed with ever more powerful tools. The James Webb Space Telescope is out there, giving us sharper and sharper images of these distant, ancient galaxies. And coming down the pipeline are next-generation radio telescopes, like the Square Kilometer Array (SKA), which will let us peer even deeper into the cold gas reservoirs of these early galaxies. These new eyes on the sky will give us the crucial real-world data needed to test these new theoretical predictions, helping us refine our models and paint an even clearer picture of the universe's chaotic, yet beautiful, beginnings.

The journey to understand how the universe built itself, one galaxy at a time, is still unfolding before us.

AI image processing has sped up analysis of data from NASA's James Webb Space Telescope from years to mere days or less, ushering in an avalanche of ground-breaking discoveries that may otherwise never have been made.

And now, the technology will be used to enhance the quality of images taken by the Chile-based Vera C. Rubin Observatory, the newest astronomy power house, to make them appear as sharp as if they have been taken from space.

The Vera C. Rubin Observatory, named after the American astronomer who discovered one of the key pieces of evidence for the existence of dark matter, sits atop the 8,770-feet (2,673 meters ) Cerro Pachón in the Chilean Andes. The telescope began operations last year. It scans the entire sky every three nights, aiming to create a 10-year timelapse of the motions of objects in the sky.

Its position in Chile's Atacama Desert, the most parched region on the planet, allows the observatory to benefit from a dry atmosphere and a year-round clear sky. Still, Rubin's observations suffer from significant distortions, as light from distant celestial objects must pass through Earth's atmosphere before it hits the telescope's detectors.

A new AI algorithm developed by researchers from the University of California, Santa Cruz (UCSC) will now attempt to remove this distortion and increase the resolution of the images to make them look as if they have been taken from space.

"Ground-based telescopes suffer from blurring owing to atmospheric turbulence as the light comes through," Brant Robertson, a professor of astronomy and astrophysics at UCSC, whose team developed the new AI model, told Space.com. "We spend a lot of money on high-performance technology to remove that atmospheric distortion, but we can also train AI machine learning models to take out some of that blurring."

The researchers trained the generative model, called Neo, using images taken by the Subaru Telescope in Japan and snaps of the same sections of the sky captured by the Hubble Space Telescope. The task for the model was to learn how to fill the details missing in the images taken from Earth. The results were impressive. The researchers said in a paper that the Neo model "improves the accuracy of measured morphological parameters by factors of 2-10."

In practice, that means an increased resolution that reveals a vast quantity of individual stars and precise shapes of galaxies where before one would find only vague smudges.

"The model improves the spatial quality of that data and recovers, in a statistical sense, the properties of galaxies that you see in these images as if they were seen by a telescope in space," Robertson said.

The technology, he added, super-charges discovery and enables the scientific community to maximize the scientific return on money invested into cutting-edge astronomical telescopes. The Vera C. Rubin Observatory in Chile, fitted with a 27.6-foot (8.4 m) mirror, cost $800 million to build. That, however, is still only a fraction of the cost of space-based telescopes such as Hubble and James Webb, both of which cost billions to build and operate.

"We spend a lot of money, huge amounts of resources, on astronomical observatories, and we would like to leverage that investment by the public and by the community to get everything that we can out of the data," said Robertson.

The Neo model is a Conditional Generative Adversarial Network, a collaboration of two neural networks, frequently used for AI image generation. In the case of Neo, the first network generates improved images from the captured photographs; the other evaluates their quality.

The model is based on an earlier technology Robertson's team developed to speed up processing of images from Webb. The $10 billion astronomical powerhouse produces such vast quantities of data that it's impossible to keep on top of it using just visual assessment by human astronomers. AI algorithms, like the one developed by Robertson and his colleagues, accomplish what would have taken humans years, in mere days.

"We're being inundated with such an amount of data that it's very difficult to keep up with," said Robertson. "Our standard approaches to analyzing these images are just really not sufficient."

The algorithm, running on NVIDIA's GPU-powered supercomputers, has made some of the most jaw-dropping discoveries in the Webb era, including spotting complex galaxies in the earliest universe, which astronomers did not expect.

"The model analyzes every pixel and distinguishes whether it's part of the sky or a part of an object," said Robertson. "And if it's an object, is it a part of a disk galaxy or a spheroid galaxy or a part of a star?"

Robertson added that the algorithm is not replacing astronomers. Rather, it helps them make discoveries faster, and also detect patterns that they might overlook.

"AI is not going to be pure or complete, but of course, neither are humans and traditional methodologies. They all have different strengths and benefits," he said.

The astronomers are making the processed images available to other teams and the public to explore.

The paper describing the Leo model, which will help improve the resolution of images from the Vera Rubin Observatory, has been accepted for publication in the Astrophysical Journal.

GREENBELT, Md. — On Tuesday (April 21) here at NASA's Goddard Space Flight Center, I watched as scientists stood proudly around a metal contraption with towering orange solar panels and a sparkling silver base. Gleaming right before me in a sterile white clean room stood the Nancy Grace Roman Space Telescope — at last, complete.

"I very much hope, and in fact, expect, that the most exciting science from Roman is going to be the things that we didn't expect, that we couldn't predict, but that will set the new deep questions for future missions to address," Julie McEnery, senior project scientist of Roman said during a press conference on Tuesday.

Named for NASA's first chief of astronomy and the first woman to hold an executive position at the agency, this space telescope should turn out to be yet another valuable tool in our species' hunt to understand the true nature of the universe. It'll stand among the ranks of our other powerful robotic eyes on the sky — famed instruments like the James Webb Space Telescope (JWST), SPHEREx, the Euclid Space Telescope and even the aged but always impressive Hubble. Except, as is the case with each of those landmark observatories, this new one has its own specialty. We'll get into some of those specs soon.

Above all, now projected to launch in September 2026 — eight months ahead of schedule, and under budget — the Nancy Grace Roman Space Telescope (or "Roman" for short) has the potential to show us pockets of the cosmos we've yet to touch.

According to NASA, Roman's primary mirror measures about 7.9 feet (2.4 meters) wide, which is similar to Hubble's. However, Roman has the ability to take images that capture a patch of the sky at least 100 times larger than Hubble can.

"Its surveying capabilities are over 1,000 times faster than Hubble, and can chart 200 times more sky in a single image," NASA administrator Jared Isaacman said during the conference. "What would take Hubble 2,000 years to process, Roman can do in a year — the images it captures will be so large there is not a screen in existence large enough to show them."

To put that into context, over its approximately 35 years of service so far, Hubble has gathered about 400 terabytes of data; once fully operational at its workstation in space, Roman should be able to create 500 terabytes of data per year.

As for what this data could hold, well, the possibilities are pretty endless. That's typically the gold standard for a telescope; as scientists like to say, we're always hoping to answer questions we never even thought to ask.

Cosmic and panoramic

Roman is specifically calibrated to capture images of the universe in visible and near-infrared light. Different telescopes view the universe in different light wavelengths. The JWST, for instance, specializes in infrared observations, while Hubble's powers allow it to see some infrared but mostly visible and ultraviolet light.

Diversifying in this way is important, because you can think of a patch of sky as having various layers. As an example, many extremely distant objects can be seen only in infrared light — which consists of super-long wavelengths that aren't visible to the human eye — so you need an infrared telescope to decode that layer. But there are also visible-light objects in the same patch of sky that need to be studied in greater detail, for which you need a telescope that behaves like an ultrapowerful human eye. And so on.

A few things set Roman apart, including that quick data-processing speed we discussed earlier.

Compared to the JWST, Roman's images — taken with its aptly named Wide Field Instrument (WFI) — will be 50 times wider but more shallow, because Roman doesn't need to access the deep universe the way the JWST does. As we discussed, it can't see infrared like the JWST can and therefore would be wasted in looking too far back.

More specifically, WFI is composed of a 300-megapixel visible-to-near-infrared imaging camera and slitless spectrometer (a special tool that allows scientists to capture light dispersion of objects in a field of view). But there is something uniquely special about that shallow, panoramic view.

It means scientists don't have to be as picky about which patch of sky they're looking at. They can just survey and hope to find a cool lead to zoom in on. This offers Roman the ability to catch events that transpire very quickly, such as fast radio bursts, and increases the chances that scientists can witness remarkable supernovas, colliding neutron stars and other easy-to-miss phenomena right as they happen.

"So we're going to see thousands of supernovae, and some of these are going to be further away than any supernovae we've ever seen before," Dominic Benford, program scientist for the Nancy Grace Roman Telescope told Space.com. "We'll trace the history of the universe through exploding stars."

There is also the hope that Roman helps us unravel one of the greatest mysteries of our universe — the details of its dark side.

The dark and faint universe

Despite years upon years of searching for an answer, scientists still don't know what exactly dark matter and dark energy are. All we know so far for sure is that our universe's normal matter does not appear to be enough to prevent galaxies from falling apart like horses on a merry-go-round that isn't nailed together properly, and that the universe is also accelerating in its continuous expansion far faster than seems normal. The former is explained by a substance called "dark matter" picking up where normal matter leaves off, and the latter is explained by "dark energy" driving that expansion.

These two substances collectively constitute 95% of the universe yet have never been detected with certainty. It's absolutely bizarre, if I may say.

Of course, with that kind of track record, it can't be known for sure whether Roman will suddenly reveal what the dark universe actually is — but if all goes to plan, we can expect it to bring us quite a bit closer.

Thanks to that lovely wide field of view, Roman will be able to rapidly image tons of galaxies to generate detailed, 3D vistas of the cosmos. It will therefore be able to show us things like the dynamics of different galaxies and track the universe's expansion — the two main ways we investigate dark matter and dark energy.

"We'll also study how the universe itself has expanded over time. And these are the keys to unlocking the fundamental nature of dark matter, dark energy, the fabric of the universe itself," McEnery said.

And that's not to mention what the Roman's other special instrument suite can do for science. For example, it has a coronagraph, a tool that can block the glare of distant suns and help the mission directly image exoplanets. In fact, NASA says this telescope's coronagraph can detect planets 100 million times fainter than their stars. That capability is about 100 to 1,000 times better than existing space-based coronagraphs, the agency explains in an overview.

"The Roman Coronagraph will be capable of directly imaging reflected starlight from a planet akin to Jupiter in size, temperature, and distance from its parent star," that overview states.

Road to launch

Now that Roman is complete, the next phase of its journey can soon commence. That'll include being shipped to the launch site, NASA's Kennedy Space Center in Florida, and undergoing any necessary launch-related testing.

A hefty amount of prelaunch testing has already been conducted on Roman so far, including the poor observatory being blasted with extreme sounds, being shaken up to an extreme degree, being exposed to extreme heat and extreme cold — and way more (all just as extreme). Sounds rough, but the point is to make sure Roman will be able to handle the rigors of launch and the most extreme environment we know of: space.

"Most of the stuff that's left are the final checkouts, and the final wrap-ups," Jeremy S. Perkins, Observatory Integration and Test Scientist for Roman, told Space.com "There is lots of blanket close-outs and making sure that we've put all the sensors on and taken off the ones that were there for testing."

As for launch procedures, once all aspects of testing are squared away, NASA has chosen a SpaceX Falcon Heavy rocket to carry this treasure to space. There have been 11 Falcon Heavy launches to date, with a 100% success rate for the 230-foot-tall (70-meter-tall) vehicle.

Once in space, after separating from that rocket, Roman will head to a stable point about a million miles away from Earth called Lagrange Point 2, or L2. This is a popular spot for our space explorers to end up because it allows them to remain shielded from the sun's heat while still orbiting in such a way that mission control can communicate with them easily.

Hopefully the JWST, Euclid and the rest of the L2 crew welcome Roman with open arms (solar panels?).

Correction 4/21: Julie McEnery's name has been updated to reflect the correct spelling.

Using the James Webb Space Telescope (JWST), astronomers have investigated an alien planet that could help define the line dividing planets and stars.

The curious exoplanet is 29 Cygni b, a gas giant with around 15 times the mass of Jupiter that lies 133 light-years away from Earth.

Most planets are thought to form via a "bottom-up" process that sees tiny clumps of rock and ice coming together to gradually grow a world. However, bottom-up processes struggle to account for the formation of planets with as much mass as 29 Cygni b.

Such giants are thought to form instead via a top-down process — the direct collapse of dense patches of gas and dust in the protoplanetary disks that swirl around infant stars. That's the same way that stars themselves form, from dense patches in much larger clouds of interstellar gas and dust.

Now, JWST has collected multiple lines of evidence that suggest there is a way that huge planets such as 29 Cygni b could form via bottom-up processes, just like their more diminutive counterparts.

29 Cygni b sits on the dividing line of formation processes. Though its large mass suggests a top-down process, its wide orbit — an average distance from its star of 1.5 billion miles (2.4 billion kilometers), similar to that of Uranus in our own solar system — hints at a bottom-up formation mechanism.

The team directly imaged 29 Cygni b using JWST's Near-Infrared Camera (NIRCam), as part of a program that will image four exoplanets, all of which orbit their stars within around 9.3 billion miles (15 billion km) and have masses between one and 15 times that of Jupiter. The planets are all also relatively young and are still hot from their formation, with temperatures ranging from 990 to 1,830 degrees Fahrenheit (530 to 1,000 degrees Celsius), meaning they should all have similar atmospheric chemistry, too.

The researchers hunted for light being absorbed by carbon dioxide and carbon monoxide, which allowed them to measure the proportions of elements heavier than helium, which astronomers call "metals," in 29 Cygni b's atmosphere.

This revealed that, not only is the exoplanet around 150 times richer in metals than Earth, but it is also much more metal-rich than its parent star. This indicates that, as it was forming, the gas giant gathered a wealth of metal-enriched clumps of material from its natal protoplanetary disk.

The team also determined that the orientation of 29 Cygni b's orbit is aligned with the rotation of its parent star, which indicates it did indeed form within a protoplanetary disk.

As the program continues to investigate similar planets, it will discover if other such worlds also greedily grabbed metal-rich matter during their formation. This could finally help scientists understand how the most massive planets in the Milky Way were born, be it like stars or like smaller planets.

The team's research was published on Tuesday (April 14) in the Astrophysical Journal Letters.

Astronomers have used the James Webb Space Telescope to study the star-forming region called W51, revealing "hidden" stars that were invisible to other telescopes.

The investigation has resulted in some absolutely stunning images that show the lanes of gas and dust illuminated by these young stars in unprecedented detail.

The team behind these observations was able to use the $10 billion space telescope to determine that the stars in W51 began to form within the last million years. If this makes these stellar infants sound ancient, consider that our middle-aged star, the sun, is around 4.6 billion years old.

This is far from the first time that astronomers have captured images of W51, but the JWST observations reveal these young stars like never before.

That is because these still-growing stellar infants are shrouded in natal blankets of gas and dust that readily block and absorb light, preventing most telescopes from seeing them. But infrared light is able to slip through these clouds, and that is the type of electromagnetic radiation that the JWST uses to observe the cosmos.

"With optical and ground-based infrared telescopes, we can't see through the dust to see the young stars," team member and University of Florida researcher Adam Ginsburg said in a statement accompanying the images. "Now we can."

Aside from their considerable aesthetic value, the images are of great scientific interest too. They could help researchers determine how massive stars like those that populate W51 form. The formation mechanism of high-mass stars is much less well understood than that of low-mass stellar bodies.

"Because of James Webb, we can see those hidden, young massive stars forming in this star-forming region," team member Taehwa Yoo of the University of Florida said. "By looking at them, we can study their formation mechanisms."

With the massive leap in quality of the JWST, the team was able to discover hitherto unseen structures in W51. This included shockwaves rippling out from infant stars, giant bubbles of gas, and dark filaments of dust.

"They are not the first photos of this region, but they are the best. They're so much better that they essentially are brand new photos," Ginsburg said. "Every time we look at these images, we learn something new and unexpected."

Stunning new views of Saturn offer the most detailed portrait yet of the ringed planet, showcasing the combined power of NASA's most advanced space telescopes.

Using observations from the James Webb Space Telescope (JWST) and the Hubble Space Telescope, astronomers have created the most comprehensive look at Saturn to date, blending infrared, visible and ultraviolet light into a single, richly layered image, according to a statement from NASA.

"Together, scientists can effectively 'slice' through Saturn's atmosphere at multiple altitudes, like peeling back the layers of an onion," NASA officials said in the statement. "Each telescope tells a different part of Saturn's story, and the observations together help researchers understand how Saturn's atmosphere works as a connected three-dimensional system."

Each space telescope brings a distinct perspective. Hubble captures crisp, long-term visible-light views of Saturn's cloud bands and atmospheric changes, while the JWST peers deeper into the planet's atmosphere in infrared, revealing heat patterns and structures hidden beneath the upper cloud layers.

The Hubble data, captured in August 2024 as part of the long-running Outer Planet Atmospheres Legacy (OPAL) program, was followed about 14 weeks later by Webb observations taken through Director's Discretionary Time, showing Saturn shifting from northern summer toward its 2025 equinox. Saturn's long seasonal cycles — each lasting about seven Earth years — also provide important context for interpreting changes in the planet's atmosphere and rings over time.

Together, the observations present Saturn as a layered and dynamic world. Hubble's visible-light view shows the planet's softly banded atmosphere, while Webb's infrared observations reveal additional structure, including deeper atmospheric layers, a meandering jet stream in the northern mid-latitudes, possible auroral activity, and several storms scattered across the southern hemisphere.

The combined data highlights how Saturn's appearance changes across different wavelengths, offering a more complete view of its atmosphere, according to the NASA statement.

The images also provide complementary views of Saturn's rings. In Hubble's data, the rings, made of water ice, appear bright in reflected sunlight, with clearly defined structure. In Webb's infrared view, the rings shine even more prominently, standing out against the darker background of space and revealing additional detail in the ring system.

Subtle differences between the telescopes' views also reveal ring features like spokes and structure in the thick central region, as well as differing perspectives of the outer ring, which appears thin and sharply defined in Webb's image but only faintly visible in Hubble's, according to the statement.

Seasonal context adds further value to the observations. Hubble's OPAL program has been tracking changes in the outer planets for more than a decade, providing a long-term record of Saturn's atmosphere. The new Webb observations build on that dataset, offering a broader, multiwavelength perspective as the planet continues its progression toward its next equinox.

The new dataset underscores the power of combining multiple observatories. By integrating Webb's infrared sensitivity with Hubble's long-standing visible-light record, scientists can construct a far more complete picture of planetary behavior than either telescope could achieve alone.

As both observatories continue their missions, researchers plan to build on these observations, tracking Saturn's evolving atmosphere, monitoring storm systems and refining models of its complex climate. With this new composite view, Saturn isn't just a distant gas giant — it's a dynamic world whose hidden layers are finally coming into focus.

An exoplanet so light that it would float on water, were there an ocean large enough, is continuing to frustrate astronomers by concealing its closest secrets with a layer of haze thicker than any ever seen on a planet before.

The haze is so thick that not even the vision of the James Webb Space Telescope (JWST) can penetrate it, leaving the mystery of how this ultra-low density world and its sibling planets all formed unsolved for now.

"These ultra-low density planets are rare and they defy conventional understanding of how gas giants form," said Jessica Libby-Roberts of the University of Tampa in Florida in a statement. "And if explaining how one formed wasn't difficult enough, this system has three!"

Kepler-51d is a member of a four-planet system orbiting a young Sun-like star 2,615 light years away. They were discovered by NASA's Kepler Space Telescope, which observed the planets transiting their star. From the amount of the star's light blocked during the transits, astronomers deduced the size of the worlds, and from transit timing variations — the way each planet's gravity pulls and pushes on the other planets, varying exactly when they are seen to transit — their masses were measured. Planets 51b, c and d have 7.1, 9 and 9.7 times the radius of Earth, respectively, making them about the same size as Saturn.

However, planets b, c and d have masses only 3.7, 5.6 and 5.6 times greater than Earth's, respectively. Saturn, on the other hand, has a mass 95 times more than Earth. So, these worlds are a similar size to Saturn, but much (much) less massive. (The fourth planet in the system, e, was only discovered in 2024 and its mass and radius are yet to be measured to any degree of accuracy.)

It is remarkable that the densities of planets 51b, c and d have more in common with cotton candy (or candy floss as we call it in the U.K.!) than with the planets we are more familiar with.

As such, Kepler-51d and its fellow ultra-low density worlds are completely alien to the planets in our own solar system. Take the gas giants Jupiter or Saturn, for example, which have large, dense and well-defined cores that on their own are ten times more massive than Earth. These cores formed first and then their gravitational pull attracted masses of gas from the planet-forming disk that encircled the Sun 4.5 billion years ago.

In contrast, the ultra-low density worlds of Kepler-51 "have tiny cores and huge atmospheres giving them a density akin to cotton candy," said Libby-Roberts. It is not clear how these small cores could have accreted relatively large amounts of gas.

So in search of answers, when Libby-Roberts was at Penn State University she led a team in 2020 to observe the Kepler-51 system spectroscopically using the Hubble Space Telescope's Wide-Field Camera 3. The purpose was to look for signs of the chemical composition of the atmosphere around the planets, which could provide clues as to how far from their star these worlds formed, and how they subsequently came to be so tenuous. Given their low density, they are undoubtedly rich in hydrogen and helium, the two lightest and most common elements in the universe, but the various trace gases present in their atmosphere could tell us more about their origin.

Yet Hubble found no sign of any chemistry, leading Libby-Roberts and her colleagues to suspect that there could be a featureless haze swamping the atmosphere of the planets.

Now, Libby-Roberts has returned to the Kepler-51 system, using the JWST's Near Infrared Spectrometer (NIRSpec) to try and probe harder into the atmosphere of Kepler-51d in the hope of detecting its chemical composition.

They aimed to accomplish this via transit spectroscopy. When Kepler-51d transits its star, some of its star's light filters through the planet's atmosphere. Any molecules present can absorb certain wavelengths of the star's light, which should show up in the star's spectrum as absorption lines.

"A star's light is filtered through the atmosphere of the planet before it reaches our telescopes," said Libby-Roberts. "If we look across a range of wavelengths, across a spectrum, we get a sort of fingerprint of the planet's atmosphere that reveals its composition."

Yet the spectrum still showed no signs of the chemistry of 51d's atmosphere, meaning that the haze that is present must be the thickest ever encountered on an exoplanet if even NIRSpec, operating at longer wavelengths than Hubble, cannot see through it.

"It seems very similar to the haze we see on Saturn's largest moon Titan, which has hydrocarbons like methane, but at a much larger scale," said co-researcher Suvrath Mahadevan at Penn State. "Kepler-51d seems to have a huge amount of haze, almost the radius of Earth."

There are currently no planet-formation models that can explain how such low density worlds can form, particularly so close to their star — if 51b, c and d were transported to our solar system they would all be packed into a region well inside the orbit of Venus.

"It's possible that [51d] formed further away and moved inward, but we are still left with a ton of questions about how this planet — and the other planets in this system — formed," said Libby-Roberts. "What is it about this system that created these three really oddball planets, a combination of extremes that we haven't seen anywhere else?"

It is possible that we are seeing these planets in a transitory phase. The system is half a billion years old, so young compared to our 4.5-billion-year-old solar system. Being young, the Kepler-51 star is still quite active and its stellar wind will be stripping away the outer gases of the ultra-low density planets. Perhaps if we came back in a billion years' time, much of each planets' gas will have been whittled away leaving behind a small core.

Some answers could still be forthcoming. A separate team is performing NIRSpec observations of Kepler-51b to try and find evidence of the composition of its atmosphere. They might instead find that it is also covered in haze, but if they are successful, then the clues those observations provide might also apply to 51c and d.

Then measurements of Kepler-51d are reported in the 16 March issue of The Astronomical Journal.

The James Webb Space Telescope has helped scientists determine that asteroid 2024 YR4, which previously had a 4.3% chance of crashing into our moon, will not impact our lunar companion at all. Instead, it will instead safely cruise past the moon at an altitude of 13,200 miles (21,200 kilometers).

When asteroid 2024 YR4 was discovered on Dec. 27, 2024 by the NASA-funded Asteroid Terrestrial-impact Last Alert System (ATLAS), it was for a short time the most dangerous asteroid ever discovered. With a diameter of about 197 feet (60 meters) there was originally a non-zero chance that it could impact Earth on Dec. 22, 2032. An asteroid of this size could destroy a city, or if it struck the ocean, produce a catastrophic tsunami that would endanger multiple coastal regions.

However, it was quickly found that 2024 YR4 would miss the Earth — but it remained unclear whether it'd hit the moon instead. Specifically, there was a 4.3% chance that it could strike the moon on Dec .22, 2032 instead. The uncertainty was the result of 2024 YR4's orbit around the sun not being known as precisely as needed in order to decide for sure whether it would hit the moon or miss it.

Astronomers thought they would have to wait until 2028 to get the next chance to observe 2024 YR4 and refine its orbit before getting some clear answers, but researchers at the Johns Hopkins University Applied Physics Laboratory (JHUAPL) realized that there would be a chance for the James Webb Space Telescope (JWST) to observe 2024 YR4 between Feb. 18 and Feb. 26 this year.

During that week, the asteroid was moving against a faint field of stars whose positions have been precisely measured by the European Space Agency's Gaia mission. By tracking the object's motion against those stars, the James Webb Space Telescope (JWST) was able to refine its orbit to high precision. It wasn't an easy measurement; the field of view of its Near-Infrared Camera is just 2.2 square arcminutes, and the asteroid is one of the faintest targets the JWST has ever observed.

The scientists at JHUAPL worked with the space telescope’s engineers, alongside the European Space Agency's Near-Earth Object Coordination Centre and NASA's Center for Near-Earth Object Studies, to aim the telescope precisely.

The new measurements mean that astronomers have now ruled out a collision with the moon. Instead, 2024 YR4 will pass 13,200 miles above the lunar surface — still a very close encounter, but posing no danger.

Had the impact happened on the near side of the moon, it would have provided scientists with their first up-close view of a large impact, and provided a stunning sight for observers on Earth, resulting in a brilliant flash and a new crater about 0.62 miles (1 kilometer) across. The energy imparted would have been equivalent to 6 million tons of TNT, or basically a large nuclear detonation. Ejecta thrown up by the impact would mostly have rained back down onto the surface of the moon, but millions of pounds of debris would have still escaped the lunar gravity and fallen towards Earth instead, possibly creating a unique meteor shower lasting a few days. The debris would also have been a hazard to satellites in orbit around the Earth, and, as some of the debris could linger in Earth orbital space for years, that hazard would have been long-lasting.

However, now that we know 2024 YR4 will miss its target, we'll just have to wait for the next asteroid to worry about, and remain ever vigilant for any that may threaten Earth.

The James Webb Space Telescope (JWST) has captured a truly spectacular view of the spiral galaxy NGC 5134, revealing glowing dust clouds, newborn stars and the ongoing cycle of stellar life and death.

Located about 65 million light-years away in the constellation Virgo, the galaxy may seem distant, but in cosmic terms, it's relatively close. This proximity allows the James Webb Space Telescope (JWST) to resolve remarkable details in the tightly wound spiral arms of the galaxy.

What is it?

NGC 5134 is a spiral galaxy, a type of galaxy characterized by a bright central core surrounded by sweeping arms filled with stars, gas and dust. These arms act as cosmic nurseries where new stars are constantly forming.

This dramatic image combines observations from two of the JWST's powerful instruments: the mid-infrared instrument (MIRI) and the near-infrared instrument (NIRCam). MIRI detects mid-infrared light emitted by warm dust, revealing strands and clumps of gas scattered throughout the galaxy. NIRCam captures shorter-wavelength infrared light that highlights the stars and star clusters embedded deep within the spiral arms.

Why is it amazing?

The glowing dust clouds visible throughout the galaxy are the raw material for new stars. As gravity pulls this gas together, new stars ignite — gradually using up all the galaxy's star-forming fuel. When stars die, they return some of that material back into space. Massive stars explode into supernovas, scattering elements across hundreds of light-years, while smaller stars like our sun shed their outer layers as they expand into red giants.

By studying galaxies like NGC 5134 in infrared light, astronomers can trace this ongoing cycle of stellar birth, evolution and recycling, helping scientists understand how galaxies grow and change over billions of years.

The James Webb Space Telescope's latest imagery is its most "cerebral" yet, capturing a dying star's nebula that looks uncannily like a brain inside a transparent skull.

Located about 5,000 light-years away in the constellation of Vela, the Sails, the nebula is officially called PMR 1. It is named after the astronomers who discovered it — Parker, Morgan and Russell — while conducting a survey with the 1.2-meter U.K. Schmidt Telescope at the Australian Astronomical Observatory in the late 1990s. When the Spitzer Space Telescope observed PMR 1 in infrared light in 2013, the nebula's appearance led to its unofficial nickname of the "Exposed Cranium Nebula."

Now the James Webb Space Telescope (JWST) has taken a new look at PMR-1 with both its Near-Infrared Camera (NIRCam) and its Mid-Infrared Instrument (MIRI). Their unprecedented resolution reveals greater detail in the inner gases that form the "brain" and which are surrounded by a thinner shell of mostly hydrogen gas that forms the "cranium."

That outer shell is thought to have been expelled from the star at the center of the nebula first, and that shell has cooled down considerably compared to the complex mix of various ionized gases within the interior that were emitted later.

A curious split down the middle of the nebula looks like it is dividing the brain into left and right lobes. This split could have been blown by polar jets from the dying star. This hypothesis is supported in the MIRI image where the ionized gas can be seen spewing out through the hydrogen envelope at the top of the picture. If the split was produced by a jet, it gives some indication as to the orientation of the star relative to the nebula.

The big question though is the nature of the central, dying star. When it was discovered in the 1990s, the nebula's emission features looked like they belonged to a Wolf–Rayet star, which is one of the more extreme breeds of massive star. Wolf–Rayet stars are so unstable that they shed mass at a tremendous rate, blown away by a wind of radiation many times more powerful than the sun's solar wind. This expelled matter then forms a Wolf–Rayet nebula before the star itself eventually explodes as a supernova.

However, the presence of a Wolf–Rayet star inside PMR 1, or indeed inside its cousin PMR 2 that was discovered at the same time, has yet to be confirmed.

This leaves the door ajar for the possibility that the Exposed Cranium is actually just an ordinary planetary nebula produced by a less massive sun-like star that has expanded into its red giant phase and is now casting adrift its outer envelope to eventually leave behind its inert core in the form of a white dwarf.

Using the James Webb Space Telescope and the Atacama Large Millimeter/sub-millimeter Array , astronomers have investigated 70 dusty, star-forming galaxies at the very edge of the universe. These galaxies, seen as they were less than 1 billion years after the Big Bang, could change everything we know about cosmic evolution.

It seems these galaxies were already rich in "metals," the term astronomers use to describe elements heavier than hydrogen and helium, despite existing before current models predict the current generation of stars could have forged and distributed those heavy elements.

"Dusty galaxies are massive galaxies with large amounts of metals and cosmic dust," team leader Jorge Zavala of the University of Massachusetts Amherst said in a statement. "And these galaxies are very old, which means stars were being formed in the early universe, earlier than our current models predict."

The research into these galaxies began when Zavala and colleagues used the Atacama Large Millimeter/sub-millimeter Array (ALMA), an array of 66 radio antennas located in the Atacama Desert region of northern Chile, to identify a population of 400 bright and dusty galaxies.

Further investigation with the James Webb Space Telescope (JWST) whittled these galaxies down to 70 faint dusty galaxy candidates on the very edge of the cosmos, the majority of which had never been seen before. Combining JWST and ALMA observations, the researchers then confirmed these galaxies had formed as long ago as 500 million years after the Big Bang.

That not only suggests that our story of cosmic history needs revision, but it also connects these galaxies to two other families of strange galaxies. These are extremely bright, star-birthing galaxies discovered in the early universe by the JWST and older galaxies that have "died" and are no longer forming stars.

"It's as if we now have snapshots of the lifecycle of these rare galaxies," Zavala said. "The ultrabright ones are young galaxies, the quiescent ones are in their old age, and the ones we found are young adults."

More research will be needed to link these three populations of galaxies. However, if they are connected, then it is clear that something is missing from our understanding of galactic evolution, and the development of stars must begin earlier in the cosmos than currently theorized.

The team's results were published on Tuesday (Feb. 17) in The Astrophysical Journal Letters.

Scientists have long suspected that active supermassive black holes can kill their own host galaxies, but new research suggests these cosmic titans are more like serial killers that can extend their murderous rampage across many light-years and destroy neighboring galaxies, too.

For scientists, "death" for a galaxy means the curtailing of star formation. Supermassive black holes are known to cause this when they are actively feeding, as they heat their larder of gas and dust, provoking that matter content to emit powerful radiation. This radiation either pushes away gas, the building blocks of stars — thereby starving the galaxies and black holes themselves — or simply heats that gas and prevents it from cooling enough to collapse and birth a stellar body. Both outcomes can slow or even stop star formation.

"Traditionally, people have thought that because galaxies are so far apart, they evolve largely on their own," team leader Yongda Zhu of the University of Arizona said in a statement. "But we found that a very active, supermassive black hole in one galaxy can affect other galaxies across millions of light-years, suggesting that galaxy evolution may be more of a group effort."

Zhu and colleagues point out that this influence suggests the existence of a "galactic ecosystem" akin to the linked ecosystems of Earth in which changes in one region can deeply impact conditions in another.

"An active supermassive black hole is like a hungry predator dominating the ecosystem," he said. "Simply put, it swallows up matter and influences how stars in nearby galaxies grow."

There goes the neighborhood!

Though supermassive black holes with masses of millions or even billions of times that of the sun are thought to dwell at the hearts of all large galaxies, not all of these objects are cosmic killers. For instance, Sagittarius A* (Sgr A*) at the heart of the Milky Way may once have quenched star formation in our galaxy, but today it is quiet, existing on a diet equivalent to a human eating one grain of rice every million years.

Active supermassive black holes greedily feast on matter from a surrounding swirling cloud called an accretion disk. Their immense gravity generates tidal forces in this accretion disk that cause intense friction, resulting in high temperatures that cause this region to brightly glow across the electromagnetic spectrum. This turbulent region, an Active Galactic Nucleus (AGN), can be seen from across the cosmos as a phenomenon known as a "quasar," often outshining the combined light of every star in its host galaxy.

Not all of the matter in an accretion disk is channeled to the black hole, however. Some matter is channeled to the poles of the supermassive black hole from where it is blasted out as parallel twin jets travelling at near light-speeds. These jets can stretch out far beyond the limits of the galaxy that hosts the active supermassive black hole.

It is little wonder, given the intense radiation of the accretion disk and the violent outflows represented by these twin jets, that active supermassive black holes have a powerful influence over the evolution of their host galaxies.

Since the James Webb Space Telescope (JWST) began investigating the cosmos, a curious pattern has emerged regarding quasars. The more massive and powerful these active supermassive black holes are, the less they seem to be surrounded by neighboring galaxies. That's curious because large galaxies are usually found clustered together, not in isolation.

"We were puzzled," Zhu explained. "Was the expensive JWST broken?" he added with a laugh. "Then we realized the galaxies might actually be there, but difficult to detect because their very recent star formation was suppressed."

Zhu and colleagues began to suspect that bright quasars may not just be dampening star formation in their own galactic backyards; they may be disturbing the neighbors, too.

To investigate the possibility of active supermassive black holes killing star formation in neighboring galaxies, the team set about studying one of the brightest quasars ever seen, J0100+2802. This quasar existed when the universe was less than 1 billion years old, and its central engine is a supermassive black hole with around 12 billion times the mass of the sun.

Using the JWST, the scientists hunted for traces of ionized oxygen in the galaxies around J0100+2802, which is a sign of recent star formation. They found this tracer of star birth was much scarcer in galaxies within a million light-years of the powerful quasar than in galaxies outside that radius. That hints at squashed star formation in these proximate galaxies.

"Black holes are known to 'eat' a lot of stuff, but during the active eating process and in their luminous quasar form, they also emit very strong radiation. The intense heat and radiation split the molecular hydrogen that makes up vast, interstellar gas clouds, quenching its potential to accumulate and turn into new stars," Zhu said. "For the first time, we have evidence that this radiation impacts the universe on an intergalactic scale.

"Quasars don't just suppress stars in their host galaxies, but also in nearby galaxies within a radius of at least a million light-years."

The team now intends to look for this effect in other so-called quasar fields to develop a clearer picture of how supermassive black holes influence their cosmic neighborhoods.

"Understanding how galaxies influenced one another in the early universe helps us better understand how our own galaxy came to be," Zhu said. "Now we realize that supermassive black holes may have played a much larger role in galaxy evolution than we once thought — acting as cosmic predators, influencing the growth of stars in nearby galaxies during the early universe."

The team's results were published on Dec. 3, 2025 in The Astrophysical Journal Letters.

An international team of researchers has uncovered new insights into the upper atmosphere of Uranus, where ions swirling above the ice giant planet's clouds meet the magnetic field surrounding the world.

"Uranus's magnetosphere is one of the strangest in the solar system," Paola Tiranti, a researcher at Northumbria University in the U.K., said in a statement. "It's tilted and offset from the planet's rotation axis, which means its auroras sweep across the surface in complex ways."

Using the Near-Infrared Spectrograph (NIRSpec) instrument aboard the James Webb Space Telescope (JWST), the team studied Uranus as it rotated. The researchers observed how temperature and charged particles "vary with height across the planet," according to the statement; the resulting data could help scientists understand more about how energy behaves in ice giants' upper layers.

"By revealing Uranus's vertical structure in such detail, Webb is helping us understand the energy balance of the ice giants," Tiranti said. "This is a crucial step towards characterizing giant planets beyond our solar system."

The JWST continues to provide unprecedented detail on comic phenomena located millions, even billions, of miles away from us. With such detailed data available, scientists are still able to make new discoveries about the planets in our solar system. The telescope has previously had its sights set on Uranus too, even discovering a new moon of the planet in 2025.

"This is the first time we've been able to see Uranus's upper atmosphere in three dimensions," said Paola. "With Webb's sensitivity, we can trace how energy moves upward through the planet's atmosphere and even see the influence of its lopsided magnetic field."

Voyager 2 provided our first close-up data and images of Uranus way back in 1986. The flyby helped scientists figure out that Uranus is very cold compared to its neighboring planets — in fact, around then is when we found out Uranus is our solar system's coldest planet.

"Webb's data confirm that Uranus's upper atmosphere is still cooling, extending a trend that began in the early 1990s," said Paola. "The team measured an average temperature of around 426 kelvins (about 150 degrees Celsius), lower than values recorded by ground-based telescopes or previous spacecraft."

The research was published on Feb. 19 in the journal Geophysical Research Letters.

Using the James Webb Space Telescope (JWST), astronomers have captured a stunning image of a "cosmic jellyfish." This aquatic-creature-like galaxy, designated COSMOS2020-635829, was seen as it existed 8.5 billion years ago, or around 5.3 billion years after the Big Bang. Astronomers say it could paint a more detailed picture of the evolution of galaxies at a crucial period in the adolescent universe.

COSMOS2020-635829 is an example of a jellyfish galaxy, a class of galaxies that get their moniker from the fact that they possess trailing tendrils of gas that resemble the flexible, stinging appendages of their oceanic namesakes. For jellyfish galaxies, these trails are created as they 'swim' through their galaxy cluster homes against the flow of strong winds that push on them, forcing out gas, a process called "ram-stripping."

The team discovered COSMOS2020-635829 while examining data collected by the JWST from a patch of sky over Earth called the Cosmic Evolution Survey Deep field, or the COSMOS field. This region is favored by astronomers for the study of distant and ancient galaxies because it lies away from the plane of the Milky Way and is clear of bright objects that would serve as obstructions.

"We were looking through a large amount of data from this well-studied region in the sky with the hopes of spotting jellyfish galaxies that haven’t been studied before," team member Ian Roberts of the Waterloo Centre for Astrophysics in the Faculty of Science in the UK, said in a statement. "Early on in our search of the JWST data, we spotted a distant, undocumented jellyfish galaxy that sparked immediate interest."

The JWST image of COSMOS2020-635829 shows a galactic disk that appears relatively normal, not dissimilar from our own modern-day galaxy, barring the distinct gas trails. Bright blue "knots" can be seen in these tendrils that represent groupings of young stars. Similar features can be seen in the Hubble Space Telescope image of a similar jellyfish galaxy, seen above.

The youth of these stellar bodies implies that they were born outside the main galactic disk of COSMOS2020-635829 within these tendrils of ram-stripped gas. While this phenomenon is expected of jellyfish galaxies, the image of COSMOS2020-635829 has delivered at least one surprise. Previously, researchers had thought that still-forming galaxy clusters that existed 8.5 billion years or so ago would not commonly produce the pressure that leads to ram-stripping.

"The first is that cluster environments were already harsh enough to strip galaxies, and the second is that galaxy clusters may strongly alter galaxy properties earlier than expected," Roberts explained. "Another is that all the challenges listed might have played a part in building the large population of dead galaxies we see in galaxy clusters today. This data provides us with rare insight into how galaxies were transformed in the early universe."

The team now intends to continue studying COSMOS2020-635829 with the JWST, hoping to solve further mysteries regarding this and other jellyfish galaxies.

The team's results were published on Tuesday (Feb. 17) in The Astrophysical Journal.

Editor's Note (02/19/26): The article was updated to reflect the fact that the featured image was captured by the Hubble Space Telescope

Woven through the universe are forces, often unseen, that dictate its grand design. For example, at the very heart of nearly every galaxy, we find a supermassive black hole. This isn't just some cosmic void — it's a powerful engine.

Even in its quieter moments, this engine profoundly shapes its surroundings. We call black holes with this kind of behavior Low-Luminosity Active Galactic Nuclei, or LLAGN. Picture galactic engines, just idling. They're running, doing their thing, but at a much slower pace. Still, they influence entire galaxies. The quest for scientists? Deciphering the unique infrared language these galactic nuclei speak.

A new paper provides comprehensive emission line measurements from James Webb Space Telescope (JWST) nuclear spectra for seven LLAGN as well as the active galaxy Centaurus A. This research acts like a cosmic linguist, analyzing subtle spectral signatures to give us unprecedented insight into how these powerful, yet often hidden, forces influence star birth, sculpt galactic gas and orchestrate the evolution of galaxies.

To listen to these quiet galactic whispers, scientists need the right tools. The James Webb Space Telescope is perfectly suited.

JWST sees in the infrared, light with wavelengths longer than what our eyes see. This is absolutely crucial. Gas and dust swirling around a black hole block visible light, but infrared light can punch right through. When gas gets energized by the black hole, its atoms get excited. The atoms then settle back down, releasing light at very specific colors — what we call emission lines. These are like a fingerprint for the gas, telling us what it is made of, how hot it is, and even how fast it moves. This energy often comes from the ionizing continuum, a powerful, high-energy flashlight from the black hole that strips electrons from atoms. These are the critical clues astronomers collect, piecing together the story of what happens near these massive black holes.

The celestial language spoken by LLAGN offers significant insights into how these quiet giants operate. JWST observations reveal how these black holes, even with less power, eject material and energize gas, influencing star birth and galactic evolution. These are known as kinetic feedback processes.

The black hole also actively pushes and stirs the galactic gas and dust. It is not a passive bystander. This can clear out regions, stopping new stars from forming, or sometimes compress gas, triggering a burst of star formation. It's a complex dance these quiet engines perform regularly. A striking discovery is that these galaxies with LLAGN have unusually warm molecular hydrogen gas. Excitation temperatures are systematically higher than in other galaxies. This suggests that even an idling black hole can really heat its surroundings.

The team also measured the "full width at half maximum," or FWHM, of these emission lines. FWHM tells us how wide a light spike is. A wider spike means the gas moves around a lot, or it is very hot. These FWHM measurements provide crucial data on the chaotic motions and conditions within the gas, showing just how much activity there really is.

Understanding these cosmic architects helps us grasp how galaxies evolve. Historically, astronomers assumed the supermassive black holes in LLAGN were largely inert. Just kind of ... there. They thought the objects weren't much, their power having sunk to the background. But this work shows that even these quiet engines have a profound impact on their galactic homes. The fact that they can eject material, energize gas and create unusually warm molecular hydrogen means they are active players. They influence new star formation and dictate how galactic gas moves around.

These LLAGN influence the cosmos, even when they are not roaring at full power.

This research is just one piece of a much larger puzzle. It opens up new questions about how common this warm molecular hydrogen is. It also prompts scientists to consider what other subtle effects these quiet black holes might have. The universe holds many mysteries, and scientists, with instruments like JWST, are quickly learning to speak its many languages. The quest for understanding these architects of the cosmos, it continues. Always.

Our journey through the infrared whispers of LLAGN reveals a universe far more interconnected and dynamic than we often imagine. The supermassive black holes at the heart of galaxies, even when seemingly dormant, exert a powerful, quiet influence. This latest research, powered by the vision of JWST, provides detailed measurements that paint a clearer picture of their ionizing continuum and kinetic feedback processes.

We have learned these cosmic engines actively sculpt their surroundings, impacting star formation and galactic evolution. The discovery of unusually warm molecular hydrogen in these LLAGN is a testament to the unexpected complexity hiding in plain sight. It is a reminder that the universe always has more to teach us.

With every new emission line we decipher, we get a little closer to understanding the grand cosmic story. The work of scientists, using advanced tools, is made up of these small, significant steps. They are pushing the boundaries of human knowledge, one quiet whisper at a time. And we will keep listening, because there is a whole lot more to hear.

The study is currently viewable on the pre-print paper repository arXiv.