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It has been a busy month for astronomy. In the midst of an eclipse season bookended by the total solar eclipse on August 12th and the deep partial lunar eclipse coming right up this week on August 28th, an outbound comet hanging high in the dawn sky just refuses to die: 220P/McNaught.

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?

The multiple-image effect seen in this Hubble picture is produced by a process called gravitational lensing, a quirk of warped spacetime in which the gravitational field of a massive object bends and amplifies light from a background object. (Image credit: ESA, NASA, K. Sharon (Tel Aviv University) and E. Ofek (Caltech))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.

On the left, the Roman Space Telescope. On the right, Hubble. (Image credit: NASA’s Goddard Space Flight Center)

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.

NASA's Nancy Grace Roman Space Telescope is encapsulated in the payload fairing of its SpaceX Falcon Heavy rocket. (Image credit: SpaceX)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.

The JWST's view of Neptune and its rings. The world looks so small when seen this way. (Image credit: ESA/NASA)

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.

A view of the James Webb Space Telescope's giant mirror. (Image credit: NASA)

The Roman Space Telescope's mirror. (Image credit: NASA/Sydney Rohde)

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?

Simulated views of what a section of space would look like from the Rubin Observatory and the Roman Space Telescope. Because it has to peer through Earth’s atmosphere, Rubin’s images won’t always be sharp enough to distinguish multiple, close sources as separate objects. (Image credit: J. Chiang (SLAC), C. Hirata (OSU), and NASA’s Goddard Space Flight Center)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.

A side by side view of the Hubble Telescope's view of the Pillars creation and the JWST's. (Image credit: NASA, ESA, CSA, STScI, Hubble Heritage Project (STScI, AURA), Joseph DePasquale (STScI), Anton M. Koekemoer (STScI), Alyssa Pagan (STScI))

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.

A request for information from the Department of Health and Human Services seeks public input as to how vaccines are categorized

Both of the deceased were unvaccinated against measles. The deaths are the first fatalities caused by the preventable disease in the state of Pennsylvania in 35 years

4 Min Read Galactic Gems Glisten in New Gallery From NASA’s Chandra

Galaxies are like cosmic gems, each with characteristics including size and shape that make them distinct. A new gallery released today from NASA’s Chandra X-ray Observatory and other telescopes displays a collection of galactic images that showcase this variety.

Astronomers put galaxies into three main categories: spirals like our own Milky Way with arms emanating from their cores, ellipticals that are older and likely the results of mergers, and irregulars that can encompass a wide range of galactic phenomena.

This gallery displays a collection of 16 galactic images from Chandra and other telescopes. Astronomers put galaxies into three main categories: spirals like our own Milky Way, ellipticals that are older and likely the results of mergers, and irregulars that can encompass a wide range of galactic phenomena. All types are represented in this collection. Each galactic image contains X-ray data from Chandra combined with data from telescopes such as NASA’s Webb, Hubble, IXPE, Swift, and NuSTAR, and others both in space and on the ground.Credit: NASA/CXC/SAO

See full gallery

Just as gems reveal the history of Earth through how they were forged over billions of years, these galactic gems are a way to study Earth’s place in our home galaxy of the Milky Way. By looking outward to other galaxies, we learn more about our own – including clues to its past and future.

There are 16 new images in this galactic gallery. Each one contains X-ray data from Chandra that has been collected across Chandra’s decades in space. This high-energy data has been combined with data from telescopes such as NASA’s James Webb and Hubble Space Telescopes, IXPE (Imaging X-ray Polarimetry Explorer), Neil Gehrels Swift Observatory, NuSTAR (Nuclear Spectroscopic Telescope Array), and others both on the ground and in space.

NGC 1672A barred spiral galaxy featuring a prominent central bar or bridge of stars that channels gas toward its core. Chandra X-rays (purple) highlight growing black holes along the bar and core, merged with Hubble optical light (white, yellow and soft blue) and JWST infrared dust filaments (red). Studying barred spirals in action can help reveal how gas in our own Milky Way, which is also a barred spiral, feeds its central black hole and forms new stars.X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI/Hubble Heritage Team; Infrared: NASA/ESA/CSA/STScI/J. Lee and T. Williams; Image Processing: NASA/CXC/SAO/L. Frattare, J. Major, K. Arcand II Zw 096A chaotic, dust-shrouded system of merging galaxies forming stars at a furious rate. Chandra X-ray data (magenta) pinpoint powerful black hole activity and hot gas, while Hubble optical (blue and white) and Webb infrared (red and grey) data illuminate vast stellar nurseries hidden behind interstellar dust. Systems like II Zw 096 show us how powerful galaxy collisions shaped the early universe.X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI; Infrared: NASA/ESA/CSA/STScI; Image Processing: NASA/CXC/SAO/L. Frattare and J. Major M33A nearby, face-on spiral galaxy whose clear spiral arms offer an unhindered view of its stellar engine. X-ray data from Chandra (purple) highlights point sources like neutron stars and stellar-mass black holes pulling material off companion stars (systems called X-ray binaries), while optical data from the Very Large Telescope’s MUSE instrument (pink and grey) maps glowing pockets of hydrogen gas. Ultraviolet data from NASA’s Swift telescope (blue) reveals populations of young, massive stars sizzling across the spiral arms. M33’s proximity to us allows astronomers to audit individual high-energy objects and map how stellar feedback affects a galaxy’s ecosystem.X-ray: NASA/CXC/SAO; Optical: ESO/VLT; UV: NASA/Swift; Image Processing: NASA/CXC/SAO/L. Frattare NGC 4258A spiral galaxy famous for having two extra, “anomalous” spiral arms composed of hot gas. Chandra’s X-rays (royal blue) show superheated shockwaves created by central black hole jets, combined with optical light from Hubble (red, yellow and pale blue) and infrared dust filaments from Webb (bright orange). M106 helps show how supermassive black holes can create structural features that mimic star-bearing spiral arms, influencing a galaxy’s evolution.X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI; Infrared: NASA/ESA/CSA/STScI; Image Processing: NASA/CXC/SAO/L. Frattare NGC 1569A compact dwarf irregular galaxy undergoing a violent, compact burst of star formation. Chandra and XMM-Newton observations (blue and purple) reveal massive bubbles of million-degree gas inflated by stellar winds, set against a backdrop of optical light (magenta, orange and white) imaged by Adam Block. Dwarf starburst galaxies can serve as local laboratories for studying the conditions of the early universe, where small, primitive galaxies formed stars at frantic rates.X-ray: (XMM):ESA/XMM-Newton, (Chandra): NASA/CXC/SAO; Optical: Univ.of Arizona/Mt Lemmon SkyCenter/Adam Block/Josep Drudis; Image Processing: NASA?CXC/SAO/L. Frattare M90A large spiral galaxy that is being stripped of its gas as it plunges at high speed through hot gas in the Virgo Cluster of galaxies. Chandra’s X-ray data (magenta) pinpoints high-energy point sources—such as X-ray binaries and supernova remnants—and diffuse hot gas nestled within the spiral disk imaged by Hubble (blue, brown and gold). A ground-based optical light image taken from New Mexico by Timothy Martin reveals red filaments of hydrogen gas streaming over 300,000 light-years behind the galaxy as it falls into the Virgo Cluster.X-ray: NASA/CXC/SAO; Optical: NASA/ESA/D. Thilker/J. Lee/PHANGS-HST Team; Full-field: Tim Martin; Image Processing: NASA/CXC/SAO/L. Frattare Centaurus AA giant elliptical galaxy undergoing a dusty merger, featuring a powerful jet of particles blasting tens of thousands of light-years into space. Chandra’s X-rays (blue) showcase the high-energy jet, with additional X-rays from IXPE (orange), while Webb infrared (magenta) and optical light (amber and white) from the European Southern Observatory expose a dark, churning dust lane. As one of the closest active galaxies to Earth, Cen A allows astronomers to study the effects of supermassive black hole jets in extraordinary detail.X-ray: (Chandra) NASA/CXC/SAO, X-ray (IXPE): NASA/MSFC; Optical: ESO; Infrared: NASA/ESA/CSA/STScI; Image Processing: NASA/CXC/SAO/L. Frattare, K. Arcand, and J. Major M104Famous for its broad central bulge and dark outer dust ring, this galaxy sits at a nearly edge-on tilt to Earth. Chandra X-rays (cyan and orange) isolate compact point sources and hot gas in the galaxy’s sprawling halo, merged with Hubble optical light (warm white) and Webb infrared vision (purple-red dust lane). Studying M104 may help bridge the gap between spirals and ellipticals, helping astronomers better understand how a galaxy’s giant outer cloud of stars grows and ages alongside its inner disk.X-ray: NASA/CXC/SAO; Optical:NASA/Hubble Heritage Team/AURA/STScI; Infrared: NASA/ESA/CSA/STScI; Image Processing: NASA/CXC/SAO/L. Frattare Arp 143This ring galaxy system formed when a smaller companion galaxy punched straight through its center like a bullseye, creating a powerful cosmic shockwave. Chandra X-rays (purple) uncover bright X-ray binary systems scattered along the collision shock wave, laid over Hubble’s optical image (blue and white) of expanding stellar rings. Such head-on collisions can trigger vast ripple effects, sparking huge waves of star birth across entire galaxies.X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI/J. Dalcanton; Image Processing: NASA/CXC/SAO/L. Frattare NGC 4725A “one-armed” barred spiral galaxy surrounded by a prominent star-forming ring. Chandra’s X-ray data (magenta) pinpoints several bright X-ray sources, likely caused by growing black holes, embedded within the sweeping optical disk (soft blue and white) captured with the Mt. Lemmon Observatory. Galaxies with unusual single arms can offer a window into how the gravity from a passing galaxy can trigger bursts of star formation.X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI/NAOJ/R. Gendler; Image Processing: NASA/CXC/SAO/L. Frattare NGC 1385A barred spiral galaxy packed with regions where stars are actively forming. Chandra X-ray data (magenta) highlights stellar nurseries and X-ray binaries scattered along dusty spiral structures brought to life by Hubble optical (white and grey) and Webb infrared (orange and red) observations. Comparing multiwavelength data of barred spirals containing active star formation helps scientists map how local starbursts build up galactic mass over time.X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI; Infrared: NASA/ESA/CSA/STScI; Image Processing: NASA/CXC/SAO/L. Frattare NGC 660A rare “polar ring” galaxy where a tilted outer ring of stars and dust rotates over the galaxy’s poles, an unusual structure likely caused by a collision with another galaxy about a billion years ago. Chandra’s X-rays (purple) reveal a possible growing supermassive black hole in the center of the galaxy, plus X-ray binaries nestled within the stars and dust captured by the Gemini Observatory in optical light (gold, blue and white). Studying polar rings teaches us about the diverse effects of stellar collisions on the shapes of galaxies.X-ray: NASA/CXC/SAO; Optical:NSF/International Gemini Observatory/AURA; Image Processing: NASA/CXC/SAO/L. Frattare M82An irregular galaxy undergoing intense star formation because of a gravitational interaction with a neighboring galaxy hundreds of millions of years ago. Chandra X-rays (blue), supplemented by NuSTAR data, show towering superwinds of million-degree gas blowing thousands of light-years out of the galactic disk, with Hubble optical light (yellow, orange and white) showing the galaxy shape, and Webb and Spitzer detailing infrared dust emission (red). M82 was nicknamed the Cigar Galaxy mostly because of its edge-on angle to Earth, which makes its central disk look like an elongated, cigar-shaped oval with small optical telescopes. The galaxy illustrates how violent galactic “exhaust systems” can regulate a galaxy’s growth by venting gas outwards.X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI; Infrared: NASA/ESA/CSA/STScI; Image Processing: NASA/CXC/SAO/L. Frattare, J. Major, and K. Arcand NGC 3256A pair of colliding, gas-rich spiral galaxies merging into a single massive system. Chandra’s X-ray data (pink) isolates point sources and shock-heated gas, Hubble’s optical light (blue and white) captures tidal tails of stars, and Webb’s infrared vision (red and orange) cuts through the dust to show hidden star formation. Galaxy collisions like this offer a preview of our far future, showing what might happen if our own Milky Way collides and merges with the nearby Andromeda Galaxy.X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI; Infrared: NASA/ESA/CSA/STScI; Image Processing: NASA/CXC/SAO/L. Frattare NGC 3938A face-on spiral galaxy whose orientation gives us an unobstructed view of its disk. X-ray emissions from Chandra (magenta) detail energetic X-ray binaries and supernova remnants scattered across dust lanes in an optical image (white, blue and gold) from Adam Block with Mt. Lemmon Observatory. Face-on orientations are important for galactic studies because they provide the most unobstructed views of a galaxy’s stars and gas.X-ray: NASA/CXC/SAO; Optical: Adam Block/Mount Lemmon SkyCenter/University of Arizona; Image Processing: NASA/CXC/SAO/L. Frattare NGC 4631A spiral galaxy viewed from its side, featuring a giant halo of hot gas blowing out of its stellar disk. X-rays from Chandra and ESA’s XMM-Newton (purple and royal blue) trace hot gas driven out by supernovas and black holes and neutron stars pulling gas from their companions, while optical light (light blue, gold and white) from ground-based observer R. Jay GaBany showcases dense dust lanes. Edge-on views of galaxies allow astronomers to study how flat their stellar disks are and provide the clearest views of material located above or below the disk.X-ray: NASA/CXC/SAO; Optical: ©2011-2015 by R Jay GaBany, Cosmotography.com; Image Processing: NASA/CXC/SAO/L. Frattare

X-rays are critical for the study of galaxies, revealing unique and important information about these cosmic building blocks. For example, Chandra exposes gas that has been superheated to millions of degrees by winds from massive stars, the outflows from supermassive black holes, and the debris from exploded stars. These are key sources of elements in our bodies, in the air we breathe, and the planet we live on. Chandra also sees some of the hottest and most energetic galactic phenomena in the universe, forming a more complete picture of how galaxies live, interact, and evolve when combined with data from other types of light and telescopes.

Spiral and star-forming engines

Face-on spiral galaxies like Messier 33 and NGC 3938 offer unobstructed views of places where energetic pairs of stars and cosmic explosions live along spiral arms. Barred spirals like NGC 1672 and NGC 1385 show how central bar-shaped collections of stars, gas, and dust funnel fuel inward to ignite bursts of star formation. NGC 4725 reveals how star formation can be triggered by a previous collision with another galaxy. Meanwhile, edge-on views of NGC 4631 (the Whale Galaxy) and the starburst Messier 82 (the Cigar Galaxy) showcase giant halos and superwinds of million-degree gas driven thousands of light-years into space by intense explosions of stars, enriching surrounding intergalactic space with vital elements.

Active galactic nuclei, black hole outflows

Powerful, growing black holes in the cores of their host galaxies, known as active galactic nuclei, send energy outward in outbursts and jets that impact entire galaxies. In Centaurus A, Chandra and IXPE data expose a high-energy particle jet blasting tens of thousands of light-years into space from its central engine. In Messier 106, jets from the supermassive black hole heat surrounding gas to create spiral arms that are different from those typically found in spiral galaxies. Meanwhile, the iconic Sombrero Galaxy (Messier 104) highlights a supermassive black hole embedded in a colossal stellar bulge, where Chandra’s X-rays map a diffuse halo of million-degree gas and hot stellar remnants surrounding its sweeping dust lanes.

Collisions, mergers, cosmic disruptions

The gallery also showcases galaxies undergoing extreme gravitational transformations. A direct impact in Arp 143 acts like a cosmic bullseye, creating an expanding ring galaxy and triggering waves of star birth. Violent mergers, such as NGC 3256 and the dust-shrouded starburst II Zw 096, reveal the kind of chaotic galaxy collisions that dominated the early universe and offer a preview of the Milky Way’s distant future merger with nearby galaxy Andromeda. NGC 1569 acts as a local laboratory for studying early universe starbursts, NGC 660 showcases a rare “polar ring” galaxy where a ring of stars orbits over its poles, and Messier 90 shows a spiral galaxy plowing through the Virgo Cluster, having its star-forming gas violently stripped away.

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

Read more from NASA’s Chandra X-ray Observatory

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About the AuthorMegan Watzke

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Details Last Updated Aug 25, 2026 EditorLee MohonContactMegan Watzkemwatzke@cfa.harvard.eduJoel Wallacejoel.w.wallace@nasa.govLocationMarshall Space Flight Center Related Terms

• Chandra X-Ray Observatory
• Active Galaxies
• Astrophysics
• Elliptical Galaxies
• Galaxies
• Galaxies, Stars, & Black Holes Research
• Galaxy Mergers
• Interacting Galaxies
• Irregular Galaxies
• Marshall Astrophysics
• Marshall Space Flight Center
• Spiral Galaxies
• The Universe

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4 Min Read Galactic Gems Glisten in New Gallery From NASA’s Chandra

Galaxies are like cosmic gems, each with characteristics including size and shape that make them distinct. A new gallery released today from NASA’s Chandra X-ray Observatory and other telescopes displays a collection of galactic images that showcase this variety.

Astronomers put galaxies into three main categories: spirals like our own Milky Way with arms emanating from their cores, ellipticals that are older and likely the results of mergers, and irregulars that can encompass a wide range of galactic phenomena.

This gallery displays a collection of 16 galactic images from Chandra and other telescopes. Astronomers put galaxies into three main categories: spirals like our own Milky Way, ellipticals that are older and likely the results of mergers, and irregulars that can encompass a wide range of galactic phenomena. All types are represented in this collection. Each galactic image contains X-ray data from Chandra combined with data from telescopes such as NASA’s Webb, Hubble, IXPE, Swift, and NuSTAR, and others both in space and on the ground.Credit: NASA/CXC/SAO

See full gallery

Just as gems reveal the history of Earth through how they were forged over billions of years, these galactic gems are a way to study Earth’s place in our home galaxy of the Milky Way. By looking outward to other galaxies, we learn more about our own – including clues to its past and future.

There are 16 new images in this galactic gallery. Each one contains X-ray data from Chandra that has been collected across Chandra’s decades in space. This high-energy data has been combined with data from telescopes such as NASA’s James Webb and Hubble Space Telescopes, IXPE (Imaging X-ray Polarimetry Explorer), Neil Gehrels Swift Observatory, NuSTAR (Nuclear Spectroscopic Telescope Array), and others both on the ground and in space.

NGC 1672A barred spiral galaxy featuring a prominent central bar or bridge of stars that channels gas toward its core. Chandra X-rays (purple) highlight growing black holes along the bar and core, merged with Hubble optical light (white, yellow and soft blue) and JWST infrared dust filaments (red). Studying barred spirals in action can help reveal how gas in our own Milky Way, which is also a barred spiral, feeds its central black hole and forms new stars.X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI/Hubble Heritage Team; Infrared: NASA/ESA/CSA/STScI/J. Lee and T. Williams; Image Processing: NASA/CXC/SAO/L. Frattare, J. Major, K. Arcand II Zw 096A chaotic, dust-shrouded system of merging galaxies forming stars at a furious rate. Chandra X-ray data (magenta) pinpoint powerful black hole activity and hot gas, while Hubble optical (blue and white) and Webb infrared (red and grey) data illuminate vast stellar nurseries hidden behind interstellar dust. Systems like II Zw 096 show us how powerful galaxy collisions shaped the early universe.X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI; Infrared: NASA/ESA/CSA/STScI; Image Processing: NASA/CXC/SAO/L. Frattare and J. Major M33A nearby, face-on spiral galaxy whose clear spiral arms offer an unhindered view of its stellar engine. X-ray data from Chandra (purple) highlights point sources like neutron stars and stellar-mass black holes pulling material off companion stars (systems called X-ray binaries), while optical data from the Very Large Telescope’s MUSE instrument (pink and grey) maps glowing pockets of hydrogen gas. Ultraviolet data from NASA’s Swift telescope (blue) reveals populations of young, massive stars sizzling across the spiral arms. M33’s proximity to us allows astronomers to audit individual high-energy objects and map how stellar feedback affects a galaxy’s ecosystem.X-ray: NASA/CXC/SAO; Optical: ESO/VLT; UV: NASA/Swift; Image Processing: NASA/CXC/SAO/L. Frattare NGC 4258A spiral galaxy famous for having two extra, “anomalous” spiral arms composed of hot gas. Chandra’s X-rays (royal blue) show superheated shockwaves created by central black hole jets, combined with optical light from Hubble (red, yellow and pale blue) and infrared dust filaments from Webb (bright orange). M106 helps show how supermassive black holes can create structural features that mimic star-bearing spiral arms, influencing a galaxy’s evolution.X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI; Infrared: NASA/ESA/CSA/STScI; Image Processing: NASA/CXC/SAO/L. Frattare NGC 1569A compact dwarf irregular galaxy undergoing a violent, compact burst of star formation. Chandra and XMM-Newton observations (blue and purple) reveal massive bubbles of million-degree gas inflated by stellar winds, set against a backdrop of optical light (magenta, orange and white) imaged by Adam Block. Dwarf starburst galaxies can serve as local laboratories for studying the conditions of the early universe, where small, primitive galaxies formed stars at frantic rates.X-ray: (XMM):ESA/XMM-Newton, (Chandra): NASA/CXC/SAO; Optical: Univ.of Arizona/Mt Lemmon SkyCenter/Adam Block/Josep Drudis; Image Processing: NASA?CXC/SAO/L. Frattare M90A large spiral galaxy that is being stripped of its gas as it plunges at high speed through hot gas in the Virgo Cluster of galaxies. Chandra’s X-ray data (magenta) pinpoints high-energy point sources—such as X-ray binaries and supernova remnants—and diffuse hot gas nestled within the spiral disk imaged by Hubble (blue, brown and gold). A ground-based optical light image taken from New Mexico by Timothy Martin reveals red filaments of hydrogen gas streaming over 300,000 light-years behind the galaxy as it falls into the Virgo Cluster.X-ray: NASA/CXC/SAO; Optical: NASA/ESA/D. Thilker/J. Lee/PHANGS-HST Team; Full-field: Tim Martin; Image Processing: NASA/CXC/SAO/L. Frattare Centaurus AA giant elliptical galaxy undergoing a dusty merger, featuring a powerful jet of particles blasting tens of thousands of light-years into space. Chandra’s X-rays (blue) showcase the high-energy jet, with additional X-rays from IXPE (orange), while Webb infrared (magenta) and optical light (amber and white) from the European Southern Observatory expose a dark, churning dust lane. As one of the closest active galaxies to Earth, Cen A allows astronomers to study the effects of supermassive black hole jets in extraordinary detail.X-ray: (Chandra) NASA/CXC/SAO, X-ray (IXPE): NASA/MSFC; Optical: ESO; Infrared: NASA/ESA/CSA/STScI; Image Processing: NASA/CXC/SAO/L. Frattare, K. Arcand, and J. Major M104Famous for its broad central bulge and dark outer dust ring, this galaxy sits at a nearly edge-on tilt to Earth. Chandra X-rays (cyan and orange) isolate compact point sources and hot gas in the galaxy’s sprawling halo, merged with Hubble optical light (warm white) and Webb infrared vision (purple-red dust lane). Studying M104 may help bridge the gap between spirals and ellipticals, helping astronomers better understand how a galaxy’s giant outer cloud of stars grows and ages alongside its inner disk.X-ray: NASA/CXC/SAO; Optical:NASA/Hubble Heritage Team/AURA/STScI; Infrared: NASA/ESA/CSA/STScI; Image Processing: NASA/CXC/SAO/L. Frattare Arp 143This ring galaxy system formed when a smaller companion galaxy punched straight through its center like a bullseye, creating a powerful cosmic shockwave. Chandra X-rays (purple) uncover bright X-ray binary systems scattered along the collision shock wave, laid over Hubble’s optical image (blue and white) of expanding stellar rings. Such head-on collisions can trigger vast ripple effects, sparking huge waves of star birth across entire galaxies.X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI/J. Dalcanton; Image Processing: NASA/CXC/SAO/L. Frattare NGC 4725A “one-armed” barred spiral galaxy surrounded by a prominent star-forming ring. Chandra’s X-ray data (magenta) pinpoints several bright X-ray sources, likely caused by growing black holes, embedded within the sweeping optical disk (soft blue and white) captured with the Mt. Lemmon Observatory. Galaxies with unusual single arms can offer a window into how the gravity from a passing galaxy can trigger bursts of star formation.X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI/NAOJ/R. Gendler; Image Processing: NASA/CXC/SAO/L. Frattare NGC 1385A barred spiral galaxy packed with regions where stars are actively forming. Chandra X-ray data (magenta) highlights stellar nurseries and X-ray binaries scattered along dusty spiral structures brought to life by Hubble optical (white and grey) and Webb infrared (orange and red) observations. Comparing multiwavelength data of barred spirals containing active star formation helps scientists map how local starbursts build up galactic mass over time.X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI; Infrared: NASA/ESA/CSA/STScI; Image Processing: NASA/CXC/SAO/L. Frattare NGC 660A rare “polar ring” galaxy where a tilted outer ring of stars and dust rotates over the galaxy’s poles, an unusual structure likely caused by a collision with another galaxy about a billion years ago. Chandra’s X-rays (purple) reveal a possible growing supermassive black hole in the center of the galaxy, plus X-ray binaries nestled within the stars and dust captured by the Gemini Observatory in optical light (gold, blue and white). Studying polar rings teaches us about the diverse effects of stellar collisions on the shapes of galaxies.X-ray: NASA/CXC/SAO; Optical:NSF/International Gemini Observatory/AURA; Image Processing: NASA/CXC/SAO/L. Frattare M82An irregular galaxy undergoing intense star formation because of a gravitational interaction with a neighboring galaxy hundreds of millions of years ago. Chandra X-rays (blue), supplemented by NuSTAR data, show towering superwinds of million-degree gas blowing thousands of light-years out of the galactic disk, with Hubble optical light (yellow, orange and white) showing the galaxy shape, and Webb and Spitzer detailing infrared dust emission (red). M82 was nicknamed the Cigar Galaxy mostly because of its edge-on angle to Earth, which makes its central disk look like an elongated, cigar-shaped oval with small optical telescopes. The galaxy illustrates how violent galactic “exhaust systems” can regulate a galaxy’s growth by venting gas outwards.X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI; Infrared: NASA/ESA/CSA/STScI; Image Processing: NASA/CXC/SAO/L. Frattare, J. Major, and K. Arcand NGC 3256A pair of colliding, gas-rich spiral galaxies merging into a single massive system. Chandra’s X-ray data (pink) isolates point sources and shock-heated gas, Hubble’s optical light (blue and white) captures tidal tails of stars, and Webb’s infrared vision (red and orange) cuts through the dust to show hidden star formation. Galaxy collisions like this offer a preview of our far future, showing what might happen if our own Milky Way collides and merges with the nearby Andromeda Galaxy.X-ray: NASA/CXC/SAO; Optical: NASA/ESA/STScI; Infrared: NASA/ESA/CSA/STScI; Image Processing: NASA/CXC/SAO/L. Frattare NGC 3938A face-on spiral galaxy whose orientation gives us an unobstructed view of its disk. X-ray emissions from Chandra (magenta) detail energetic X-ray binaries and supernova remnants scattered across dust lanes in an optical image (white, blue and gold) from Adam Block with Mt. Lemmon Observatory. Face-on orientations are important for galactic studies because they provide the most unobstructed views of a galaxy’s stars and gas.X-ray: NASA/CXC/SAO; Optical: Adam Block/Mount Lemmon SkyCenter/University of Arizona; Image Processing: NASA/CXC/SAO/L. Frattare NGC 4631A spiral galaxy viewed from its side, featuring a giant halo of hot gas blowing out of its stellar disk. X-rays from Chandra and ESA’s XMM-Newton (purple and royal blue) trace hot gas driven out by supernovas and black holes and neutron stars pulling gas from their companions, while optical light (light blue, gold and white) from ground-based observer R. Jay GaBany showcases dense dust lanes. Edge-on views of galaxies allow astronomers to study how flat their stellar disks are and provide the clearest views of material located above or below the disk.X-ray: NASA/CXC/SAO; Optical: ©2011-2015 by R Jay GaBany, Cosmotography.com; Image Processing: NASA/CXC/SAO/L. Frattare

X-rays are critical for the study of galaxies, revealing unique and important information about these cosmic building blocks. For example, Chandra exposes gas that has been superheated to millions of degrees by winds from massive stars, the outflows from supermassive black holes, and the debris from exploded stars. These are key sources of elements in our bodies, in the air we breathe, and the planet we live on. Chandra also sees some of the hottest and most energetic galactic phenomena in the universe, forming a more complete picture of how galaxies live, interact, and evolve when combined with data from other types of light and telescopes.

Spiral and star-forming engines

Face-on spiral galaxies like Messier 33 and NGC 3938 offer unobstructed views of places where energetic pairs of stars and cosmic explosions live along spiral arms. Barred spirals like NGC 1672 and NGC 1385 show how central bar-shaped collections of stars, gas, and dust funnel fuel inward to ignite bursts of star formation. NGC 4725 reveals how star formation can be triggered by a previous collision with another galaxy. Meanwhile, edge-on views of NGC 4631 (the Whale Galaxy) and the starburst Messier 82 (the Cigar Galaxy) showcase giant halos and superwinds of million-degree gas driven thousands of light-years into space by intense explosions of stars, enriching surrounding intergalactic space with vital elements.

Active galactic nuclei, black hole outflows

Powerful, growing black holes in the cores of their host galaxies, known as active galactic nuclei, send energy outward in outbursts and jets that impact entire galaxies. In Centaurus A, Chandra and IXPE data expose a high-energy particle jet blasting tens of thousands of light-years into space from its central engine. In Messier 106, jets from the supermassive black hole heat surrounding gas to create spiral arms that are different from those typically found in spiral galaxies. Meanwhile, the iconic Sombrero Galaxy (Messier 104) highlights a supermassive black hole embedded in a colossal stellar bulge, where Chandra’s X-rays map a diffuse halo of million-degree gas and hot stellar remnants surrounding its sweeping dust lanes.

Collisions, mergers, cosmic disruptions

The gallery also showcases galaxies undergoing extreme gravitational transformations. A direct impact in Arp 143 acts like a cosmic bullseye, creating an expanding ring galaxy and triggering waves of star birth. Violent mergers, such as NGC 3256 and the dust-shrouded starburst II Zw 096, reveal the kind of chaotic galaxy collisions that dominated the early universe and offer a preview of the Milky Way’s distant future merger with nearby galaxy Andromeda. NGC 1569 acts as a local laboratory for studying early universe starbursts, NGC 660 showcases a rare “polar ring” galaxy where a ring of stars orbits over its poles, and Messier 90 shows a spiral galaxy plowing through the Virgo Cluster, having its star-forming gas violently stripped away.

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

Read more from NASA’s Chandra X-ray Observatory

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About the AuthorMegan Watzke

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Details Last Updated Aug 25, 2026 EditorLee MohonContactMegan Watzkemwatzke@cfa.harvard.eduJoel Wallacejoel.w.wallace@nasa.govLocationMarshall Space Flight Center Related Terms

• Chandra X-Ray Observatory
• Active Galaxies
• Astrophysics
• Elliptical Galaxies
• Galaxies
• Galaxies, Stars, & Black Holes Research
• Galaxy Mergers
• Interacting Galaxies
• Irregular Galaxies
• Marshall Astrophysics
• Marshall Space Flight Center
• Spiral Galaxies
• The Universe

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From left, Expedition 75 flight engineers Anil Menon of NASA (partially obscured and wearing the spacesuit with a red stripe on the legs) and Sophie Adenot of ESA (European Space Agency) work together during a six‑hour and 23‑minute spacewalk outside the International Space Station.

NASA

From left, Expedition 75 flight engineers Anil Menon of NASA (partially obscured and wearing the spacesuit with a red stripe on the legs) and Sophie Adenot of ESA (European Space Agency) work together during a six‑hour and 23‑minute spacewalk outside the International Space Station on Aug. 18, 2026. The pair will finish installing a high-speed communications antenna on Aug. 25, 2026.

Watch the spacewalk live.

Image credit: NASA

NASA

From left, Expedition 75 flight engineers Anil Menon of NASA (partially obscured and wearing the spacesuit with a red stripe on the legs) and Sophie Adenot of ESA (European Space Agency) work together during a six‑hour and 23‑minute spacewalk outside the International Space Station on Aug. 18, 2026. The pair will finish installing a high-speed communications antenna on Aug. 25, 2026.

Watch the spacewalk live.

Image credit: NASA

Aurora chasers are on alert after NOAA's Space Weather Prediction Center (SWPC) issued a moderate (G2) geomagnetic storm watch for Friday (Aug. 28), as coronal mass ejections (CMEs) launched from the sun yesterday (Aug. 25) head toward Earth.

The CME arrival follows a powerful M6.9 solar flare from restless sunspot region 4513 on Aug. 25. NOAA's SWPC has also issued a minor (G1) geomagnetic storm watch for Thursday (Aug. 27), as a stream of fast solar wind from a coronal hole is expected to buffet Earth ahead of the incoming CMEs

The M6.98 solar flare erupted from the active sunspot region 4513 and peaked at 6 a.m. EDT (1000 GMT), according to SpaceWeatherLive. 4513 has been particularly active over the previous 24 hours, firing off a barrage of solar flares including five powerful M-class eruptions. Solar flares are ranked by strength into five classes — A, B, C, M and X — with each class 10 times more powerful than the one before it. M-class flares are the second-strongest category, sitting just below the most powerful X-class eruptions.

The eruption also triggered a moderate (R2) radio blackout across the sunlit side of Earth, affecting high-frequency radio communications over parts of Africa, Europe and the Arctic.

High-frequency radio blackouts from the M-class solar flare on Aug. 25. (Image credit: NOAA Space Weather Prediction Center)CME incoming and possible northern lights?

The M6.9 flare wasn't the only eruption to launch material into space on Aug. 25. Several CMEs left the sun that day and NOAA's SWPC now anticipates their arrival at Earth.

NOAA's SWPC has issued a moderate (G2) geomagnetic storm watch for Aug. 28.

Before then, a coronal hole high-speed stream is forecast to reach Earth, prompting a minor (G1) geomagnetic storm watch for Aug. 27. NOAA forecasts isolated G1 to G2 conditions across Aug. 27-28 due to the combined influence of the high-speed solar wind stream and the incoming CME activity.

During G2 geomagnetic storm conditions, the northern lights can push farther south than usual, potentially becoming visible across parts of the northern U.S. and northern Europe.

NOAA's Space Weather Prediction Center has issued a geomagnetic storm watch for Aug. 27-28. (Image credit: NOAA's Space Weather Prediction Center)

If the glancing CME arrival coincides with the high-speed solar wind stream, the two influences could work together to ramp up geomagnetic activity and potentially enhance aurora activity.

How much of an impact the CME ultimately has will depend on its exact arrival time and, crucially, the orientation of its magnetic field when it reaches Earth. A strong southward magnetic field would interact more effectively with Earth's magnetic field, increasing the chances of stronger geomagnetic activity.

We'll be keeping a close eye on the latest models and space weather forecasts as Friday approaches and will update this story as more information becomes available.

Editor's note: This story was updated on Aug. 26 at 4:00 a.m. EDT (0800 GMT) to include NOAA's latest forecast and geomagnetic storm watches for Aug. 27 and Aug. 28.

On Aug. 25, 1997, NASA launched the Advanced Composition Explorer, or ACE satellite to study energetic particles traveling through space.

It lifted off from Kennedy Space Center in Florida on a Delta II rocket and spent the next three and a half months making its way to its orbital post near the L1 Lagrangian point, a point of gravitational equilibrium between Earth and the sun. There, the spacecraft is monitoring the stream of accelerated particles coming from the sun known as the solar wind.

ACE provides 24/7 continuous coverage of the solar wind, which lets scientists know when to expect geomagnetic storms that can disrupt communication satellites and power grids on Earth.

Why it mattered

A Boeing Delta II rocket launches NASA's Advanced Composition Explorer satellite from Launch Complex 17A at the Cape Canaveral Air Force Station in Florida on Aug. 25, 1997. (Image credit: NASA)

The ACE satellite is a NASA sentinel survivor.

When it launched in 1997, NASA hoped the ACE satellite mission would last up to five years as it monitored solar wind speeds and conditions, as well as the flow of other critical charged particles through space, such as galactic cosmic rays, as well as interplanetary and interstellar particles.

As of today, ACE has been hard at work for 29 years and shows no signs of stopping. It's one of NASA's oldest still-operating sun-monitoring spacecraft (the Solar and Heliospheric Observatory, or SOHO, is two years older, as it launched in 1995).

ACE serves as a core part of NASA's early-warning system for incoming space weather. It's nine primary instruments were between 10 and 10,000 times better than any sensors flown in space when the satellite launched in 1997. In 2005, one of those instruments — the Solar Energetic Particle Ionic Charge Analyzer — stopped sending data, but it is the only instrument to be lost during ACE's lifetime, NASA has said.

Want more space history? Check out our full On This Day In Space Story archive and watch our On This Day In Space videos on YouTube.

ESA astronaut Sophie Adenot and NASA astronaut Anil Menon complete a spacewalk on Aug. 18, 2026. (Image credit: Roscosmos/Anna Kikina)

Intensely focused and tethered to a floating laboratory in the vacuum of space, two astronauts spent over 6 hours working on the International Space Station during a historic spacewalk.

What is it?

Two astronauts aboard the ISS set out on a spacewalk recently (Aug. 18). European Space Agency astronaut Sophie Adenot and NASA astronaut Anil Menon set out recently a historic spacewalk.

This was Adenot's first spacewalk and, in journeying out into the darkness of space she became the first French woman to conduct a spacewalk (or, formally, an extravehicular activity, or EVA).

In this snapshot from the space station, you can see Adenot on the left and Menon on the right, both hard at work on their mission.

On this spacewalk, which took the pair 6 hours and 23 minutes, the astronauts were tasked with removing a failed antenna from the space station. However, while it was a successful outing, the pair didn't have enough time to replace the old antenna with a new, working one.

Why is it incredible?

Getting to space is hard enough. And then once you're there, venturing out of an orbiting laboratory into the darkness of space to do a physically demanding but technically complex repair job on that laboratory is certainly no picnic.

But these two astronauts pushed through almost six-and-a-half hours of grueling space work to remove the broken antenna before running out of time. And this big step forward in this fix is critical, as these antennae help to connect the space station to Earth, which is of the utmost importance.

The antenna, a "Space-to-Ground" antenna, started malfunctioning months ago and a second antenna has temporarily taken over. But this solution was temporary and a more permanent replacement was needed as this antenna ensures that astronauts on the space station can quickly transmit critical information back down to Mission Control back on Earth.

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Fully autonomous space mission operations require the ability to detect faults and compensate for them without human intervention. To address this challenge and provide model-based support for system design and operations, it is important to connect fault management (FM) and model-based systems engineering (MBSE). This approach was successfully demonstrated with the model-based generation of a failure modes and effects analysis and fault trees using NASA’s HelioSwarm mission early design information.

As NASA strives to push the boundaries of space travel with the Artemis program and the agency’s upcoming deep-space science missions, increased system autonomy and resiliency have inevitably become key technology needs. Autonomous operations require fault management (FM) software to detect issues that occur in space so they can be mitigated automatically without human intervention. Designing autonomous missions requires a multi-disciplinary approach that connects FM with the model-based systems engineering (MBSE) approach used in mission design to ensure that resilient, fault-tolerant systems are architected, modeled, and integrated during the design phase.

To address this need, NASA awarded a Phase II Small Business Innovation Research (SBIR) contract to Qualtech Systems Inc. (QSI) for development of FM capabilities and enhancements to its commercially available toolset, TEAMS® (a product that resulted from commercialization of the company’s earlier NASA-sponsored SBIR work), to support HelioSwarm and other NASA heliophysics missions.

The QSI Approach

One of the most important tasks in this effort was to connect system health management (SHM) and FM to the systems engineering (SE) process. Together, SHM/FM consists of a set of mechanisms that ensure that mission goals are achieved by preventing failures from occurring, or detecting and then mitigating them if they do occur. The SE process coordinates, cross-checks, and integrates system elements to achieve mission goals and is integral during the design, specification, and verification and validation (V&V) of systems. NASA often employs a model-based approach for its SE process, using Systems Modeling Language (SysML) as the framework.

Despite their inherently close relationship to SE in practice, SHM/FM practices have typically not been tightly integrated with SE. Often, SHM/FM is incorporated only after a nominal system is designed, which essentially makes SHM/FM a bandage fix for problems after they occur, without considering how issues might have been prevented. In addition, SE and SHM/FM often involve separate sets of subject matter experts with stove-piped knowledge repositories. This situation can lead to use of modeling methodologies and analyses processes that yield inconsistent results, and can potentially result in inefficiencies throughout the mission life cycle.

This NASA-funded QSI team’s approach integrates SHM/FM directly within the MBSE process from the beginning of a project. This method enables the FM design to be evaluated in an operational context by showing how the SHM/FM schemes mitigate the effects of simulated component-level physical and functional failures. This technique also facilitates trade studies to evaluate the merits of various FM architectures during the design phase.

Under this SBIR effort, QSI worked with the SysML v2 Submission Team (SST) — an assorted group of end users, vendors, academics, and government liaisons involved in the development of specifications for SysML v2, which is the latest iteration of SysML. The QSI team incorporated FM concepts and modeling standards into SysML v2, then they demonstrated how SysML v2 models could translate to the failure space models produced by the QSI toolset.

This capability enables systems engineers to use QSI’s commercial modeling tool set andanalyze the FM aspects of a system design captured in SysML v2. By capturing the causes and impacts of failures, QSI’s toolset enables mission designers to perform Fault Modes, Effects, and Criticality Analyses (FMECAs) and Fault Tree Analyses (FTAs) to analyze, quantify, and improve the diagnostics and availability of the system. Furthermore, the toolset recommends design improvements (e.g., optimal location of sensors onboard the spacecraft) based on the results from such analyses, and it provides these recommendations in industry-standard formats that can be easily understood and incorporated into the design.

During this SBIR effort, theQSI toolset was also enhanced to interface with an MBSE framework and facilitate the creation, evaluation, and selection of FM concepts for a mission design. The toolset now enables FM concepts to be tested early in the design process so that adequate detection and diagnosis can be built into the system design, which could potentially lower the total cost of development, facilitate enhanced communication and coordination among mission team members, and reduce development risks (cost and schedule).

The HelioSwarm Demonstration

HelioSwarm will transform our understanding of turbulence in the solar wind and the connected Sun–Earth system. The mission uses a constellation, or “swarm,” of one hub and eight co-orbiting small satellites to make the first simultaneous, multiscale measurements of magnetic-field fluctuations and proton flows in the dynamic cislunar space environment. Because plasma turbulence transfers energy across many scales, from fluid-scale motions to kinetic-scale particle dynamics, it cannot be fully understood from a single measurement point, or from measurements at only a single scale. HelioSwarm’s spacecraft will fly with separations ranging from tens to thousands of kilometers, allowing scientists to reconstruct the three-dimensional structure and dynamics of turbulent space plasma. These observations will reveal how energy moves through the solar wind, transforming our understanding of fundamental plasma processes that operate near Earth, around the Sun, and throughout the universe.

Plasma turbulence is the process by which energy contained in fluctuating magnetic fields and plasma motion cascades from large to smaller spatial scales. When the cascade approaches small spatial scales associated with kinetic dissipation, the energy transfers into particle heat. Without turbulent cascades in space plasmas, most of the universe would be far colder than observed. Because of the fundamental thermodynamic role it plays in fluids, including space plasmas, many contend that turbulent fluids are the most important unsolved problem in classical physics.

The QSI team created a SysML v2 design model of HelioSwarm subsystems and top-level mission requirements, capturing the flowdown from mission goals to the design. The team then used its enhanced toolset to translate the HelioSwarm SysML v2 model into an FM model. The HelioSwarm models consist of key subsystems of the hub spacecraft and eight node satellites, including subsystems for command and data handling; electric power; attitude control; propulsion, thermal, and separation hardware payload sensors; and ground and space communications. Using the QSI toolset, mission designers then generated FMECAs and FTAs that were translated into a standardized SysML report. Furthermore, these FM analyses generated recommendations (e.g., for sensor placement) that were provided as proposed updates to the system design. This process will support the design of small spacecraft swarms with inherent redundancy to enhance science observations and other NASA goals, such as providing mission support for lunar surface operations.

Relevance to future NASA missions and non-NASA applications

The technology developed via this latest SBIR effort could be of high value for future NASA missions — especially those that require autonomous operation. The QSI TEAMS® toolset was baselined for Vehicle Systems Management functions on NASA’s Gateway project and retains applicability to future human-rated spacecraft. System design engineers could use this technology to incorporate fault mitigation strategies to improve design with additional insight into the overall system resilience — right at the beginning of the design phase.

This technology may also have applications outside of NASA. Comprehensive and efficient FM analyses and architecture trade studies are of critical importance to complex and high-value military systems such as aircraft, surface ships, submarines, and even modern ground-fighting vehicles. Additionally, this technology could be applicable to emerging commercial space systems, civilian aircraft and maritime systems, transportation, and power generation and distribution equipment.
 
For additional details about this effort, see the relevant TechPort entries: here, here, and here.
Project Lead(s): Dr. Sudipto Ghoshal, Mr. Deepak Haste, Qualtech Systems, Inc.
Sponsoring Organization(s): NASA Ames Research Center

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Details Last Updated Aug 25, 2026 EditorNASA Science Editorial Team Related Terms

• Technology Highlights
• HelioSwarm

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Fully autonomous space mission operations require the ability to detect faults and compensate for them without human intervention. To address this challenge and provide model-based support for system design and operations, it is important to connect fault management (FM) and model-based systems engineering (MBSE). This approach was successfully demonstrated with the model-based generation of a failure modes and effects analysis and fault trees using NASA’s HelioSwarm mission early design information.

As NASA strives to push the boundaries of space travel with the Artemis program and the agency’s upcoming deep-space science missions, increased system autonomy and resiliency have inevitably become key technology needs. Autonomous operations require fault management (FM) software to detect issues that occur in space so they can be mitigated automatically without human intervention. Designing autonomous missions requires a multi-disciplinary approach that connects FM with the model-based systems engineering (MBSE) approach used in mission design to ensure that resilient, fault-tolerant systems are architected, modeled, and integrated during the design phase.

To address this need, NASA awarded a Phase II Small Business Innovation Research (SBIR) contract to Qualtech Systems Inc. (QSI) for development of FM capabilities and enhancements to its commercially available toolset, TEAMS® (a product that resulted from commercialization of the company’s earlier NASA-sponsored SBIR work), to support HelioSwarm and other NASA heliophysics missions.

The QSI Approach

One of the most important tasks in this effort was to connect system health management (SHM) and FM to the systems engineering (SE) process. Together, SHM/FM consists of a set of mechanisms that ensure that mission goals are achieved by preventing failures from occurring, or detecting and then mitigating them if they do occur. The SE process coordinates, cross-checks, and integrates system elements to achieve mission goals and is integral during the design, specification, and verification and validation (V&V) of systems. NASA often employs a model-based approach for its SE process, using Systems Modeling Language (SysML) as the framework.

Despite their inherently close relationship to SE in practice, SHM/FM practices have typically not been tightly integrated with SE. Often, SHM/FM is incorporated only after a nominal system is designed, which essentially makes SHM/FM a bandage fix for problems after they occur, without considering how issues might have been prevented. In addition, SE and SHM/FM often involve separate sets of subject matter experts with stove-piped knowledge repositories. This situation can lead to use of modeling methodologies and analyses processes that yield inconsistent results, and can potentially result in inefficiencies throughout the mission life cycle.

This NASA-funded QSI team’s approach integrates SHM/FM directly within the MBSE process from the beginning of a project. This method enables the FM design to be evaluated in an operational context by showing how the SHM/FM schemes mitigate the effects of simulated component-level physical and functional failures. This technique also facilitates trade studies to evaluate the merits of various FM architectures during the design phase.

Under this SBIR effort, QSI worked with the SysML v2 Submission Team (SST) — an assorted group of end users, vendors, academics, and government liaisons involved in the development of specifications for SysML v2, which is the latest iteration of SysML. The QSI team incorporated FM concepts and modeling standards into SysML v2, then they demonstrated how SysML v2 models could translate to the failure space models produced by the QSI toolset.

This capability enables systems engineers to use QSI’s commercial modeling tool set andanalyze the FM aspects of a system design captured in SysML v2. By capturing the causes and impacts of failures, QSI’s toolset enables mission designers to perform Fault Modes, Effects, and Criticality Analyses (FMECAs) and Fault Tree Analyses (FTAs) to analyze, quantify, and improve the diagnostics and availability of the system. Furthermore, the toolset recommends design improvements (e.g., optimal location of sensors onboard the spacecraft) based on the results from such analyses, and it provides these recommendations in industry-standard formats that can be easily understood and incorporated into the design.

During this SBIR effort, theQSI toolset was also enhanced to interface with an MBSE framework and facilitate the creation, evaluation, and selection of FM concepts for a mission design. The toolset now enables FM concepts to be tested early in the design process so that adequate detection and diagnosis can be built into the system design, which could potentially lower the total cost of development, facilitate enhanced communication and coordination among mission team members, and reduce development risks (cost and schedule).

The HelioSwarm Demonstration

HelioSwarm will transform our understanding of turbulence in the solar wind and the connected Sun–Earth system. The mission uses a constellation, or “swarm,” of one hub and eight co-orbiting small satellites to make the first simultaneous, multiscale measurements of magnetic-field fluctuations and proton flows in the dynamic cislunar space environment. Because plasma turbulence transfers energy across many scales, from fluid-scale motions to kinetic-scale particle dynamics, it cannot be fully understood from a single measurement point, or from measurements at only a single scale. HelioSwarm’s spacecraft will fly with separations ranging from tens to thousands of kilometers, allowing scientists to reconstruct the three-dimensional structure and dynamics of turbulent space plasma. These observations will reveal how energy moves through the solar wind, transforming our understanding of fundamental plasma processes that operate near Earth, around the Sun, and throughout the universe.

Plasma turbulence is the process by which energy contained in fluctuating magnetic fields and plasma motion cascades from large to smaller spatial scales. When the cascade approaches small spatial scales associated with kinetic dissipation, the energy transfers into particle heat. Without turbulent cascades in space plasmas, most of the universe would be far colder than observed. Because of the fundamental thermodynamic role it plays in fluids, including space plasmas, many contend that turbulent fluids are the most important unsolved problem in classical physics.

The QSI team created a SysML v2 design model of HelioSwarm subsystems and top-level mission requirements, capturing the flowdown from mission goals to the design. The team then used its enhanced toolset to translate the HelioSwarm SysML v2 model into an FM model. The HelioSwarm models consist of key subsystems of the hub spacecraft and eight node satellites, including subsystems for command and data handling; electric power; attitude control; propulsion, thermal, and separation hardware payload sensors; and ground and space communications. Using the QSI toolset, mission designers then generated FMECAs and FTAs that were translated into a standardized SysML report. Furthermore, these FM analyses generated recommendations (e.g., for sensor placement) that were provided as proposed updates to the system design. This process will support the design of small spacecraft swarms with inherent redundancy to enhance science observations and other NASA goals, such as providing mission support for lunar surface operations.

Relevance to future NASA missions and non-NASA applications

The technology developed via this latest SBIR effort could be of high value for future NASA missions — especially those that require autonomous operation. The QSI TEAMS® toolset was baselined for Vehicle Systems Management functions on NASA’s Gateway project and retains applicability to future human-rated spacecraft. System design engineers could use this technology to incorporate fault mitigation strategies to improve design with additional insight into the overall system resilience — right at the beginning of the design phase.

This technology may also have applications outside of NASA. Comprehensive and efficient FM analyses and architecture trade studies are of critical importance to complex and high-value military systems such as aircraft, surface ships, submarines, and even modern ground-fighting vehicles. Additionally, this technology could be applicable to emerging commercial space systems, civilian aircraft and maritime systems, transportation, and power generation and distribution equipment.
 
For additional details about this effort, see the relevant TechPort entries: here, here, and here.
Project Lead(s): Dr. Sudipto Ghoshal, Mr. Deepak Haste, Qualtech Systems, Inc.
Sponsoring Organization(s): NASA Ames Research Center

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Details Last Updated Aug 25, 2026 EditorNASA Science Editorial Team Related Terms

• Technology Highlights
• HelioSwarm

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The final frontier is getting more and more contested, so satellite companies are investing in some self-defense.

At least one of them is, anyway. Florida-based Lonestar Data Holdings announced today (Aug. 25) that it has contracted Polish startup Ares Shield to provide protection for its off-Earth data centers, in a deal worth up to $6 million.

"Our clients entrust us with mission-critical data, which is why we treat the security of our orbital infrastructure as the foundation of our entire service," Lonestar CEO Stephen Eisele said in a statement today. "Ares Shield technology offers a unique solution that allows us to further protect our satellites without the risk of generating space debris. For a company whose product is data security, it is a compelling option."

Lonestar has already tested its data-storage tech on four space missions, including two that went to the moon.

For example, one of the company's devices hit the gray dirt aboard Intuitive Machines' Athena lander in March 2025. Athena toppled over shortly after touchdown, but Lonestar's mini data center achieved its desired milestones regardless, according to the company.

Such work has helped inform the development of Lonestar's first commercial space-based offering — a platform called StarVault, which will store customer data at a healthy remove from natural disasters and other issues that could crop up here on terra firma.

"StarVault combines Lonestar's advanced cryptographic key escrow capabilities with space-based data storage infrastructure, creating a new class of digital resilience — extending secure data beyond Earth," the company said in a statement in April.

The first StarVault payload is currently scheduled to fly aboard Sidus Space's LizzieSat-4, which is manifested on SpaceX's Transporter 18 rideshare mission. That flight is expected to launch from California's Vandenberg Space Force Base in late October.

Other StarVault missions will follow, as Lonestar builds a data-storage network in low Earth orbit and, perhaps, more far-flung locales.

No GPS available in space? A satellite experiment may have a solution for that.

NASA's Starling mission — made up of a swarm of four cubesats in low Earth orbit (LEO) — is testing out navigation by using other satellites as moving landmarks. The hope is that this tech will allow future missions to navigate if GPS is not available.

The three-year-old tech demo will be extended beyond its previous expiration date this year until at least 2028, NASA announced on Monday (Aug. 17). The aim is to get the most out of the onboard experiment, a collaboration with industry partner EraDrive called FALCON (short for "Fast Autonomous Lost-in-space Catalog-based Optical Navigation").

"As NASA prepares for more missions beyond Earth's orbit, technologies like FALCON can support lunar satellite swarms, distributed science missions and human exploration," NASA officials said in Monday's statement.

While NASA's applications are civilian, alternative GPS solutions are also being investigated by the U.S. Department of Defense (DoD) out of concern that the limited number of GPS satellites could be vulnerable to adversaries. Earlier this year, for example, Space Force entities SpaceWERX and Space Systems Command jointly launched an initiative aiming for new ideas for "positioning, navigation and timing" (PNT) capabilities in space.

The aim of FALCON, however, is to deal with sheer distance. While satellites in Earth orbit have ample access to purpose-built navigational markers such as GPS, that access rapidly thins out as missions go farther afield. And this isn't just an abstract concern; NASA aims to send astronauts to the surface of the moon again as soon as 2028 on the Artemis IV mission, as part of a larger effort to build a moon base.

Industry and the military are also very interested in the moon and the area around it, known as cislunar space — and how best to navigate in the new environment. The moon's orbit also introduces complications to navigation; in 2025, for example, Canada's Outer Space Institute reported that "mass concentrations," or mascons, pull down on orbiting satellites and may affect their pathway, in some cases even inducing crashes into the lunar surface.

But before testing at the moon, NASA wants to learn more closer to home. It partnered with EraDrive, an autonomous spacecraft navigation company that originated with a group at Stanford University, which provided flight software and algorithms for FALCON. The experiment uses data from Starling's cameras, as well as a catalog on the spacecraft that charts thousands of known satellites and space objects around it.

The mission not only is trying out "GPS-independent navigation" but is also showcasing space situational awareness, or SSA — that is, the ability to understand the environment around the spacecraft (including other satellites). Some other spacecraft, like SpaceX's Starlink broadband satellites, use SSA to automatically dodge threats of space debris in LEO.

Starling's team is hoping to bring even more capabilities for navigation and SSA. "The results from FALCON can have far-reaching implications for on-orbit space-traffic monitoring, collision avoidance and alternative navigation," Roger Hunter, program manager for NASA's small spacecraft and distributed systems program, said in the statement.

NASA plans a to build a permanent base on the moon over the next decade or so, via a step-by-step approach. (Image credit: NASA)

FALCON notched two major milestones in its first three years. For PNT, the spacecraft used its cameras to observe other satellites and objects — and to match their information with the onboard database, which includes roughly 20,000 objects from publicly available DoD records. "FALCON then used the observed and verified objects as reference points to determine Starling's orbit," NASA stated.

FALCON's in-orbit observations also helped mission managers better understand the pathways of 200 individual objects, beyond the orbital estimates in the DoD catalog. The estimating work was performed over just three days and autonomously, meaning ground operators did not participate.

"The self-orbit determination capability made possible through FALCON is a first for spacecraft using optical cameras, to navigate by their relative position to other objects in space," NASA stated. "Separately, the catalog-update experiments produced better object position predictions onboard Starling than those provided by ground stations."

Starling's four spacecraft operate at an altitude of about 350 miles (565 km), which is about 6 miles (10 km) higher than originally planned. That's because SpaceX advised mission managers that Starling's mission plan put it at risk of coming close to Starlink satellites already operating in an orbital shell at 340 miles (555 km), according to Space News. By comparison, the International Space Station typically orbits slightly lower than Starling or Starlink, at 250 miles (400 km).

All of which is to say that the Starling mission demonstrates operations in crowded conditions. But in the future, NASA is hoping to port the lessons learned to the moon and Mars for science applications — meaning, to improve measurements from spacecraft — as well as for interplanetary traffic management.