March 2026 Total Lunar Eclipse: Your Questions Answered
On Tuesday, March 3, 2026, a total lunar eclipse will take place across several time zones. In this data visualization, the Moon moves from right to left, passing through Earth’s shadow and leaving in its wake an eclipse diagram with the times (in UTC) at various stages of the eclipse. Credit: NASA’s Scientific Visualization Studio
A total lunar eclipse will redden the Moon on March 3, 2026. Here’s what you need to know.
How does a lunar eclipse work?
A lunar eclipse occurs when Earth passes directly between the Sun and Moon, casting a gigantic shadow across the lunar surface and turning the Moon a deep reddish-orange. This alignment can only occur during a full Moon phase.
Alignment of the Moon, Earth, and Sun during a lunar eclipse (not to scale).
NASA’s Scientific Visualization Studio
How can I observe the eclipse?
You can observe a lunar eclipse without any special equipment. All you need is a line of sight to the Moon! For a more dramatic observing experience, seek a dark environment away from bright lights. Binoculars or a telescope can also enhance your view.
On March 3, totality will be visible in the evening from eastern Asia and Australia, throughout the night in the Pacific, and in the early morning in North and Central America and far western South America. The eclipse is partial in central Asia and much of South America. No eclipse is visible in Africa or Europe.
Map showing where the March 3, 2026 lunar eclipse is visible. Contours mark the edge of the visibility region at eclipse contact times, labeled in UTC.
The Moon begins to enter Earth’s umbra and the partial eclipse begins. To the naked eye, as the Moon moves into the umbra, it looks like a bite is being taken out of the lunar disk. The part of the Moon inside the umbra appears very dark.
Totality begins (3:04 a.m. PST, 6:04 a.m. EST, 11:04 UTC)
The entire Moon is now in the Earth’s umbra. The Moon is tinted a coppery red. Try binoculars or a telescope for a better view. If you want to take a photo, use a camera on a tripod with exposures of at least several seconds.
Totality ends (4:03 a.m. PST, 7:03 a.m. EST, 12:03 UTC)
As the Moon exits Earth’s umbra, the red color fades. It looks as if a bite is being taken out of the opposite side of the lunar disk from before.
Why is a lunar eclipse sometimes called a “blood Moon”?
During a total lunar eclipse, the Moon appears dark red or orange. This is because our planet blocks most of the Sun’s light from reaching the Moon, and the light that does reach the lunar surface is filtered through a thick slice of Earth’s atmosphere. It’s as if all of the world’s sunrises and sunsets are projected onto the Moon.
What else can I observe on the night of the eclipse?
As Earth’s shadow dims the lunar surface, constellations may be easier to spot than they usually are during a full Moon. At the time of the eclipse, the Moon will be in the constellation Leo, under the lion’s hind paws.
Several days later, on March 8, look for a “conjunction” of Venus and Saturn: from our perspective on Earth, these two planets will appear close to each other in the sky (though they’ll still be very distant from each other in space).
Visit our What’s Up guide for more skywatching tips, and find lunar observing recommendations for each day of the year in our Daily Moon Guide.
Caela Barry / Ernie Wright
NASA’s Goddard Space Flight Center
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NASA Analysis Shows La Niña Limited Sea Level Rise in 2025
This image of the Atlantic Ocean around Florida, the Bahamas, and Cuba was taken from the International Space Station in 2024. Coastal areas are particularly vulnerable to sea level rise. A NASA analysis shows that the global mean sea level rose 0.03 inches (0.08 centimeters) in 2025.
NASA
A mild La Niña caused greater rainfall over the Amazon basin, which offset rising sea levels due to record warming of Earth’s oceans.
The rise in the global mean sea level slowed in 2025 relative to the year before, an effect largely due to the La Niña conditions that persisted over most of the year. According to a NASA analysis, the average height of the ocean increased last year by 0.03 inches (0.08 centimeters), down from 0.23 inches (0.59 centimeters) in 2024.
The 2025 figure also fell below the long-term expected rate of 0.17 inches (0.44 centimeters) per year based on the rate of rise since the early 1990s. Though sea levels have increasingly trended upward in that period, years during which the rise in the average height was less usually have occurred during La Niñas — the part of the El Niño-Southern Oscillation cycle that cools the eastern Pacific Ocean, often leading to heavy rainfall over the equatorial portions of South America.
This graph shows the rise in global mean sea level from 1993 to 2025 based on data from a series of five international satellites. The solid red line indicates an accelerating rate of increase, which has more than doubled over three-plus decades. The dotted red line projects future sea level rise.
NASA/JPL-Caltech
The current La Niña has been relatively mild. Even so, the extra precipitation it has poured on the Amazon River basin contributed to an overall shift of water from oceans to land. This effect tends to temporarily lower sea levels, offsetting the rise caused by melting glaciers and ice sheets and warming of the oceans, which raises sea levels through the expansion of water when the temperature increases. The net result in 2025 was a lower-than-average sea level rise.
“The weather gives us a wild ride, and what we saw with sea level rise last year is part of that ride,” said Josh Willis, a sea level researcher at NASA’s Jet Propulsion Laboratory in Southern California. “But that cycle is short-lived. The extra water in the Amazon is going to reach the oceans in less than a year, and rapid rise will soon return.”
Combined effects
To calculate the global mean sea level in 2025, scientists averaged data across space and time from Sentinel-6 Michael Freilich, the current official reference satellite for sea level measurements and one of a line of missions developed by NASA and its U.S. and European partners to track the height of about 90% of Earth’s oceans every 10 days.
Then, to better understand the factors that contributed to the rise last year, the researchers looked at measurements from other sources. Among them was the Gravity Recovery and Climate Experiment Follow-On (GRACE-FO), a twin-satellite mission launched by NASA and the German Research Centre for Geosciences that tracks the movement of water (liquid and frozen) by measuring changes in Earth’s gravity over land and ice masses.
The GRACE data indicated that even as ice loss from glaciers and ice sheets continued a long-term trend of water moving from land to oceans, an outsize amount of water moved in the opposite direction in 2025: The heavier-than-normal rainfall due to La Niña shifted water from the oceans to the Amazon basin.
Meanwhile, data from Argo, an international program that uses thousands of seaborne probes to measure ocean temperatures and salinity, showed record warming of the oceans in 2025.
The combined effect of the two factors — one tending to lower sea levels and the other tending to increase them — resulted in an average rise in sea level in 2025 that was less than the average rate based on the long-term data record.
Actionable, accurate, consistent
The continuous series of ocean-observing satellites started with TOPEX/Poseidon, which launched in 1992. Sentinel-6 Michael Freilich, launched in 2020 and took over in 2022 from its predecessor, Jason-3, which is still in orbit and celebrated its 10th launch anniversary on Jan. 17.
In coming months, Sentinel-6 Michael Freilich will pass the baton to its twin, Sentinel-6B, which launched in November. Sentinel-6B is expected to continue ocean measurements for at least five years.
Over more than three decades, the satellites have offered actionable, accurate, and consistent measurements at both local and global scales. These measurements have formed the basis for U.S. flood predictions, which are crucial for safeguarding coastal infrastructure and communities.
The dataset indicates that the average global sea level has gone up by 4 inches (10 centimeters) since 1993. While it’s not uncommon to see short-term ups and downs, the overall trend shows that the rate of annual sea level rise has more than doubled.
“As seas continue to rise globally, satellite monitoring empowers communities worldwide to anticipate risks and build resilience,” said Nadya Shiffer, head of physical oceanography programs at NASA Headquarters in Washington.
NASA Researchers Probe Tangled Magnetospheres of Merging Neutron Stars
7 min read
NASA Researchers Probe Tangled Magnetospheres of Merging Neutron Stars
New simulations performed on a NASA supercomputer are providing scientists with the most comprehensive look yet into the maelstrom of interacting magnetic structures around city-sized neutron stars in the moments before they crash. The team identified potential signals emitted during the stars’ final moments that may be detectable by future observatories.
“Just before neutron stars crash, the highly magnetized, plasma-filled regions around them, called magnetospheres, start to interact strongly. We studied the last several orbits before the merger, when the entwined magnetic fields undergo rapid and dramatic changes, and modeled potentially observable high-energy signals,” said lead scientist Dimitrios Skiathas, a graduate student at the University of Patras, Greece, who is conducting research for the Southeastern Universities Research Association in Washington at NASA’s Goddard Space Flight Center in Greenbelt, Maryland.
New supercomputer simulations explore the tangled magnetic structures around merging neutron stars. Called magnetospheres, the highly magnetized, plasma-filled regions start to interact as the city-sized stars close on each other toward their final orbits. Magnetic field lines can connect both stars, break, and reconnect, while currents surge through surrounding plasma moving at nearly the speed of light. The simulations show that as these systems merge to produce one kind of gamma-ray burst — the universe’s most powerful class of explosions — they emit tell-tale X-rays and gamma rays that future observatories should be able to detect. NASA’s Goddard Space Flight Center
A paper describing the findings published Nov. 20, 2025, in the The Astrophysical Journal.
Neutron star mergers produce a particular type of GRB (gamma-ray burst), the most powerful class of explosions in the cosmos.
Most investigations have naturally concentrated on the spectacular mergers and their aftermaths, which produce near-light-speed jets that emit gamma rays, ripples in space-time called gravitational waves, and a so-called kilonova explosion that forges heavy elements like gold and platinum. A merger observed in 2017 dramatically confirmed the long-predicted connections between these phenomena — and remains the only event seen so far to exhibit all three.
Neutron stars pack more mass than our Sun into a ball about 15 miles (24 kilometers) across, roughly the length of Manhattan Island in New York City. They form when the core of a massive star runs out of fuel and collapses, crushing the core and triggering a supernova explosion that blasts away the rest of the star. The collapse also revs up the core’s rotation and amplifies its magnetic field.
In our simulations, the magnetosphere behaves like a magnetic circuit that continually rewires itself as the stars orbit.
Constantinos Kalapotharakos
Newborn neutron stars can spin dozens of times a second and wield some of the strongest magnetic fields known, up to 10 trillion times stronger than a refrigerator magnet. That’s strong enough to directly transform gamma-rays into electrons and positrons and rapidly accelerate them to energies far beyond anything achievable in particle accelerators on Earth.
“In our simulations, the magnetosphere behaves like a magnetic circuit that continually rewires itself as the stars orbit. Field lines connect, break, and reconnect while currents surge through plasma moving at nearly the speed of light, and the rapidly varying fields can accelerate particles,” said co-author Constantinos Kalapotharakos at NASA Goddard. “Following that nonlinear evolution at high resolution is exactly why we need a supercomputer!”
Using the Pleiades supercomputer at NASA’s Ames Research Center in California’s Silicon Valley, the team ran more than 100 simulations of a system of two orbiting neutron stars, each with 1.4 solar masses. The goal was to explore how different magnetic field configurations affected the way electromagnetic energy — light in all of its forms — left the binary system. Most of the simulations describe the last 7.7 milliseconds before the merger, enabling a detailed study of the final orbits.
“Our work shows that the light emitted by these systems varies greatly in brightness and is not distributed evenly, so a far-away observer’s perspective on the merger matters a great deal,” said co-author Zorawar Wadiasingh at the University of Maryland, College Park and NASA Goddard. “The signals also get much stronger as the stars get closer and closer in a way that depends on the relative magnetic orientations of the neutron stars.”
Magnetic field lines anchored to the surfaces of each star sweep behind them as the stars orbit. Field lines may directly connect one star to the other as the orbits shrink, while lines already linking the stars may break and reconfigure.
One value of studies like this is to help us figure out what future observatories might be able to see and should be looking for in both gravitational waves and light.
Demosthenes Kazanas
Using the simulations, the team also computed electromagnetic forces acting on the stars’ surfaces. While the effects of gravity dominate, these magnetic stresses could accumulate in strongly magnetized systems. Future models may help reveal how magnetic interactions influence the last moments of the merger.
“Such behavior could be imprinted on gravitational wave signals that would be detectable in next-generation facilities. One value of studies like this is to help us figure out what future observatories might be able to see and should be looking for in both gravitational waves and light,” said Goddard’s Demosthenes Kazanas.
The team, which includes Alice Harding at the Los Alamos National Laboratory in New Mexico and Paul Kolbeck at the University of Washington in Seattle, then used the simulated fields to identify where the highest-energy emission would be produced and how it would propagate.
This view of a supercomputer simulation of merging, magnetized neutron stars highlights regions producing the highest-energy light. Brighter colors indicate stronger emission. These regions produce gamma rays with energies trillions of times greater than that of visible light, but likely none of it could escape. That’s because the highest-energy gamma rays quickly convert to particles in the presence of the stars’ powerful magnetic fields. However, gamma rays at lower energies, with millions of times the energy of visible light, can exit the merging system, and the resulting particles may also radiate at still lower energies, including X-rays. The emission varies rapidly and is highly directional, but it could potentially be detected by future facilities.
NASA’s Goddard Space Flight Center/D. Skiathas et al. 2025
In the chaotic plasma surrounding the neutron stars, particles transform into radiation and vice versa. Speedy electrons emit gamma rays, the highest-energy form of light, through a process called curvature radiation. A gamma-ray photon can interact with a strong magnetic field in a way that transforms it into a pair of particles, an electron and a positron.
The study found regions producing gamma rays with energies trillions of times greater than that of visible light, but likely none of it could escape. The highest-energy gamma rays quickly converted to particles in the presence of powerful magnetic fields. However, gamma rays at lower energies, with millions of times the energy of visible light, can exit the merging system, and the resulting particles may also radiate at still lower energies, including X-rays.
The finding suggests that future medium-energy gamma-ray space telescopes, especially those with wide fields of view, may detect signals originating in the runup to the merger if gravitational-wave observatories can provide timely alerts and sky localization. Today, ground-based gravitational-wave observatories, such as LIGO (Laser Interferometer Gravitational-Wave Observatory) in Louisiana and Washington, and Virgo in Italy, detect neutron star mergers with frequencies between 10 and 1,000 hertz and can enable rapid electromagnetic follow-up.
ESA (European Space Agency) and NASA are collaborating on a space-based gravitational-wave observatory named LISA (Laser Interferometer Space Antenna), planned for launch in the 2030s. LISA will observe neutron-star binaries much earlier in their evolution at far lower gravitational-wave frequencies than ground-based observatories, typically long before they merge.
Future gravitational-wave observatories will be able to alert astronomers to systems on the verge of merging. Once such systems are found, wide-field gamma-ray and X-ray observatories could begin searching for the pre-merger emission highlighted by these simulations.
Routine observation of events like these using two different “messengers” — light and gravitational waves — will provide a major leap forward in understanding this class of GRBs, and NASA researchers are helping to lead the way.
A new image from NASA’s James Webb Space Telescope of a portion of the Helix Nebula highlights comet-like knots, fierce stellar winds, and layers of gas shed off by a dying star interacting with its surrounding environment. Webb’s image also shows the stark transition between the hottest gas to the coolest gas as the shell expands out from the central white dwarf.
NASA, ESA, CSA, STScI; Image Processing: Alyssa Pagan (STScI)
NASA’s James Webb Space Telescope has zoomed into the Helix Nebula to give an up-close view of the possible eventual fate of our own Sun and planetary system. In Webb’s high-resolution look, the structure of the gas being shed off by a dying star comes into full focus. The image reveals how stars recycle their material back into the cosmos, seeding future generations of stars and planets, as NASA explores the secrets of the universe and our place in it.
In the image from Webb’s NIRCam (Near-Infrared Camera), pillars that look like comets with extended tails trace the circumference of the inner region of an expanding shell of gas. Here, blistering winds of fast-moving hot gas from the dying star are crashing into slower moving colder shells of dust and gas that were shed earlier in its life, sculpting the nebula’s remarkable structure.
NASA’s Nancy Grace Roman Space Telescope is now assembled following the integration of its two major segments, shown in this time-lapse.
Credits: NASA/Sophia Roberts
Technicians have completed the construction of NASA’s Nancy Grace Roman Space Telescope.
The Roman observatory is slated to launch no later than May 2027, with the team aiming for as early as fall 2026. The mission will revolutionize our understanding of the universe with its deep, crisp, sweeping views of space.
More than a thousand technicians and engineers assembled Roman from millions of individual components. Many parts were built and tested simultaneously to save time. Now that the observatory is assembled, it will undergo a spate of testing prior to shipping to NASA’s Kennedy Space Center in Florida in summer 2026.
NASA’s freshly assembled Nancy Grace Roman Space Telescope will revolutionize our understanding of the universe with its deep, crisp, sweeping infrared views of space. The mission will transform virtually every branch of astronomy and bring us closer to understanding the mysteries of dark energy, dark matter, and how common planets like Earth are throughout our galaxy. Roman is on track for launch by May 2027, with teams working toward a launch as early as fall 2026. Credit: NASA’s Goddard Space Flight Center
Telescope
The Optical Telescope Assembly is the heart of the Roman observatory. It consists of a primary mirror, which was designed and built at L3Harris Technologies in Rochester, New York, plus nine additional mirrors and supporting structures and electronics.
The Roman team got a jumpstart by receiving the telescope’s primary mirror, which will collect and focus light from cosmic objects near and far, from another government agency and then modifying it to meet NASA’s needs. Using this mirror, Roman will capture stunning space vistas with a field of view at least 100 times larger than Hubble’s.
Roman will peer through dust and across vast stretches of space and time to study the universe using infrared light, which human eyes can’t see. The amount of detail these observations will reveal is directly related to the size of the telescope’s mirror, since a larger surface gathers more light and measures finer features. Roman’s primary mirror is 7.9 feet (2.4 meters) across, the same size as the Hubble Space Telescope’s main mirror but less than one-fourth the weight (410 pounds, or 186 kilograms) thanks to major improvements in technology.
“The telescope will be the foundation of all of the science Roman will do, so its design and performance are among the largest factors in the mission’s survey capability.”
Josh Abel
lead Optical Telescope Assembly systems engineer at NASA Goddard
The Roman team modified the inherited mirror’s shape and surface to meet the mission’s science objectives. The mirror sports a layer of silver less than 400 nanometers thick — about 200 times thinner than a human hair. The silver coating was specifically chosen for Roman because of how well it reflects near-infrared light. Roman’s mirror is so finely polished that the average bump on its surface is only 1.2 nanometers tall — more than twice as smooth as the mission requires. If the mirror were scaled to be Earth’s size, these bumps would be just a quarter of an inch high. NASA/Chris Gunn
Roman’s secondary mirror, photographed here, is 22 inches across. It’s a critical part of the forward structure assembly, which also includes the support structure. NASA/Chris Gunn
An optical technician lays on a diving board suspended between NASA’s Nancy Grace Roman Space Telescope’s primary and secondary mirrors. The photo is a projected reflection through the telescope’s optical path. The technician shines a beam of light through the optical system toward the future location of the Wide Field Instrument, showing how light from cosmic sources will travel through the telescope once the mission launches. NASA/Chris Gunn
Optical engineer Bente Eegholm inspects the surface of Roman’s primary mirror. NASA/Chris Gunn
The primary mirror, in concert with other optics, will send light to Roman’s two science instruments: the Wide Field Instrument and Coronagraph Instrument. When light enters Roman’s 2.4-meter aperture, it will be reflected and focused by the curved primary mirror and then reflected and focused once more by the secondary mirror. Then, light from different parts of the sky splits off toward each instrument, so Roman will be able to use both at once.
The telescope was delivered Nov. 7, 2024, to the largest clean room at NASA’s Goddard Space Flight Center in Greenbelt, Maryland.
Upon arrival at NASA’s Goddard Space Flight Center, Roman’s Optical Telescope Assembly was lifted out of the shipping fixture and placed with other mission hardware in Goddard’s largest clean room. Then, it was installed onto Roman’s Instrument Carrier, a structure that will keep the telescope and Roman’s two instruments optically aligned. NASA/Sydney Rohde
Detectors
Meanwhile, technicians at Goddard and Teledyne Scientific & Imaging were developing the detector array. This device will convert starlight into electrical signals, which will then be decoded into 288-megapixel images of large patches of the sky. The combination of Roman’s fine resolution and enormous images has never been possible on a space-based telescope before.
Roman uses state-of-the-art sensors that build on the legacy of the infrared detectors in NASA’s Hubble and Webb instruments. Roman’s focal plane, however, is much larger to capture a much larger field of view.
Greg Mosby
research astrophysicist at NASA Goddard
The detectors, each the size of a saltine cracker, have 16 million tiny pixels apiece, providing the mission with exquisite image resolution. Eighteen were incorporated into the focal plane array for Roman’s camera, and another six are reserved as flight-qualified spares.
Detector Array
Detector Array
NASA/Chris Gunn
NASA/Chris Gunn
NASA/Chris Gunn
NASA/Chris Gunn
Detector Array
Detector Array
Roman’s Detectors
Mosaic Plate Assembly
Most telescopes are designed to focus incoming light toward a central point, so their view is sharpest in the middle. By tweaking the curvatures and tilts of three mirrors, Roman focuses light instead onto a ring around the center. The detectors in Roman’s Wide Field Instrument are laid out in an arch shape to sit along part of that ring. This design helps Roman capture a much wider area with equally sharp imaging. And since the observatory’s Coronagraph is placed on another part of the ring, both instruments can operate simultaneously while benefiting from the telescope’s best resolution. Credit: NASA/Chris Gunn
Principal technician Billy Keim installs a cover plate over the detectors for NASA’s Nancy Grace Roman Space Telescope. Credit: NASA/Chris Gunn
Once complete and tested, the detector array was inserted into the mission’s primary instrument: a sophisticated camera called the Wide Field Instrument, which was assembled and tested at Goddard and BAE Systems, Inc.
Wide Field Instrument
The Wide Field Instrument, or WFI, is an infrared camera that will give Roman the same angular resolution as Hubble but with a field of view at least 100 times larger. Its sweeping cosmic surveys will help scientists discover new and uniquely detailed information about planets beyond our solar system, untangle mysteries like dark energy, and map how matter is structured and distributed throughout the cosmos. The mission’s broad, crisp view will produce an extraordinary resource for a wide range of additional investigations.
Using this instrument, each Roman image will capture a patch of the sky bigger than the apparent size of a full moon. The mission will gather data hundreds of times faster than Hubble, adding up to 20,000 terabytes (20 petabytes) over the course of its five-year primary mission.
This photo shows Roman’s Wide Field Instrument arriving at the big clean room at NASA’s Goddard Space Flight Center. About the size of a commercial refrigerator, this instrument will help astronomers explore the universe’s evolution and the characteristics of worlds outside our solar system. Unlocking these cosmic mysteries and more will offer a better understanding of the nature of the universe and our place within it. NASA/Chris Gunn
Technicians install Roman’s Wide Field Instrument in the biggest clean room at NASA’s Goddard Space Flight Center in Greenbelt, Md. This marked the final step to complete the Roman payload, which also includes a Coronagraph instrument and the Optical Telescope Assembly. NASA/Chris Gunn
After completing final integration, Ball Aerospace technicians transport the Nancy Grace Roman Space Telescope’s Wide Field Instrument (WFI) into Ball’s largest thermal vacuum chamber to begin environmental testing at a Ball facility in Boulder, Colorado. Ball Aerospace
Technicians from both BAE and Goddard put the WFI together in a clean room in Boulder, Colorado. Then the team completed full environmental testing in space-like conditions and delivered the WFI to Goddard in summer 2024. It was joined to other observatory systems the following winter.
Coronagraph Instrument
Technicians at NASA’s Jet Propulsion Laboratory built the Coronagraph Instrument. The Coronagraph will demonstrate new technologies for directly imaging planets around other stars. It will block the glare from distant stars and make it easier for scientists to see the faint light from planets in orbit around them. The Coronagraph aims to photograph worlds and dusty disks around nearby stars in visible light to help us see giant worlds that are older, colder, and in closer orbits than the hot, young super-Jupiters direct imaging has mainly revealed so far.
The coronagraph team will conduct a series of pre-planned observations for three months spread across the mission’s first year-and-a-half of operations, after which the mission may conduct additional observations based on scientific community input.
The Roman Coronagraph was integrated with the Instrument Carrier in a clean room at NASA’s Goddard Space Flight Center in Greenbelt, Md., in October 2024. NASA/Sydney Rohde
April 9, 2025The Roman Coronagraph was peppered with radio waves to test its response to stray electrical signals. The test was performed inside a chamber lined with foam padding that absorbs the radio waves to prevent them from bouncing off the walls. Credit: NASA/JPL-Caltech. NASA/JPL-Caltech
PIA26273
This photo features the optical bench for Roman’s Coronagraph Instrument. Light from the telescope will be directed to the optical bench and pass through series of lenses, filters, and other components that ultimately suppress light from a star while allowing the light from orbiting planets to pass through. Mirrors redirect the light and keep it contained within the optical bench. In this image, the bench was partly assembled at the start of the instrument’s integration and testing period. The large black circles are surrogate components that were standing in for the actual instrument hardware. NASA/JPL-Caltech
By 2025, all of Roman’s components were complete and undergoing testing as subsystems. Technicians installed test versions of the Solar Array Sun Shield panels onto the Outer Barrel Assembly — a part of the observatory that will protect and shade the primary mirror — inside Goddard’s largest clean room in preparation for testing.
The team covered Roman’s telescope section in a protective tent and pushed it out of the clean room using pressurized air to float it like a hovercraft. Then they lifted it onto a shaker table for vibration testing to simulate launch stress. Then, technicians moved the components into the Space Environment Simulator chamber for a month of testing at low pressure and different temperatures, mimicking space-like conditions.
Solar Panels
Roman’s Solar Array Sun Shield is made up of six panels, each covered in solar cells. The two central panels will remain fixed to the Outer Barrel Assembly while the other four will deploy once Roman is in space, swinging up to align with the center panels.
The panels will spend the entirety of the mission facing the Sun to provide a steady supply of power to the observatory’s electronics. This orientation will also shade much of the observatory and help keep the instruments cool, which is critical for an infrared observatory. Since infrared light is detectable as heat, excess warmth from the spacecraft’s own components would saturate the detectors and effectively blind the telescope.
In this photo, technicians install solar panels onto the outer portion of the Roman observatory. Roman’s inner portion is in the background just left of center. NASA/Sydney Rohde
The Roman solar panels are covered in a total of 3,902 solar cells that will convert sunlight directly into electricity much like plants convert sunlight to chemical energy. When tiny bits of light, called photons, strike the cells, some of their energy transfers to electrons within the material. This jolt excites the electrons, which start moving more or jump to higher energy levels. In a solar cell, excited electrons create electricity by breaking free and moving through a circuit, sort of like water flowing through a pipe. The panels are designed to channel that energy to power the observatory. Credit: NASA/Sydney Rohde
Technicians installed Roman’s solar panels in June of 2025, followed by the Lower Instrument Sun Shield — a smaller set of panels that will play a critical role in keeping Roman’s instruments cool and stable. Technicians practiced deploying the solar panels and Deployable Aperture Cover — a visor-like sunshade.
By fall 2025, the observatory was in two major segments. The inner portion included the telescope, instrument carrier, two instruments, and spacecraft bus while the outer portion consisted of the outer barrel assembly, deployable aperture cover, and solar panels. The outer portion passed a shake test and an intense sound blast while the inner portion underwent a 65-day thermal vacuum test.
Over the course of several hours, technicians meticulously connected the inner and outer segments of NASA’s Nancy Grace Roman Space Telescope, as shown in this time-lapse. Next, Roman will undergo final testing prior to moving to the launch site at NASA’s Kennedy Space Center in Florida for launch preparations in summer 2026. Credit: NASA/Sophia Roberts
NASA/Sophia Roberts
“With Roman’s construction complete, we are poised at the brink of unfathomable scientific discovery. In the mission’s first five years, it’s expected to unveil more than 100,000 distant worlds, hundreds of millions of stars, and billions of galaxies. We stand to learn a tremendous amount of new information about the universe very rapidly after Roman launches.”
Julie Mcenery
Roman senior project scientist at NASA Goddard
Now, Roman will undergo testing as a full observatory. Roman will move to the launch site at NASA’s Kennedy Space Center in Florida for launch preparations in summer 2026. Roman is slated to launch by May 2027, but the team is on track for launch as early as fall 2026. Follow along on the journey to launch at nasa.gov/roman.
