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Astronomers de-fog exoplanet atmospheres with new cloud-detecting method

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Sand clouds form every morning but clear up by nightfall on WASP-94A b, a well-studied gas giant in a constellation located nearly 700 light years away from Earth.

The research, which uses data from the James Webb Space Telescope (JWST), is among the first to detect cloud cycles on a Hot Jupiter exoplanet. By isolating the clouds, researchers can more accurately measure the planet’s atmosphere and provide one of the clearest pictures to date of the planet’s composition — a significant advance in planetary science.

“I’ve been looking at exoplanets for 20 years, and general cloudiness has been a thorn in our side. We’ve known for quite a while that clouds are pervasive on Hot Jupiter planets, which is annoying because it’s like trying to look at the planet through a foggy window,” said co-author and program PI, David Sing, a Bloomberg Distinguished Professor of Earth and Planetary Sciences at Johns Hopkins. “Not only have we been able to clear the view, but we can finally pin down what the clouds are made out of and how they’re condensing and evaporating as they move around the planet.”

The results are published today in the journal Science.

To study WASP-94A b in the Microscopium constellation, Sing and his team of researchers gathered data as the planet passed directly in front of its star. Using the high-powered, space-based JWST, the researchers were able to take separate measurements of WASP-94A b’s leading edge as it started to cross in front of the star and the trailing edge as the planet completed its transit. At the leading edge, the air flows from the night side of the planet to the day side, effectively making it the morning. Air flows from day to night at the trailing edge, making it the evening.

Observations revealed that mornings and evenings on WASP-94A b have extremely different weather patterns: mornings are riddled with clouds made of magnesium silicate, a common mineral found in rocks, while the evening has clear skies.

The researchers think one of two things could be happening. Powerful winds might lift clouds high into the sky on the cooler side of the planet and then plunge downward on the hotter dayside, dragging the clouds deep into the planet’s interior and effectively burying them out of sight before sunset. Alternatively, the phenomenon may be akin to morning fog burning off on Earth, but on an extreme scale. Clouds would form in the darkness of the planet’s nightside. As they drift into the scorching heat of over 1,000 degrees on the day side, the chemicals that make up the clouds boil away, and the clouds simply vaporize.

“It was a huge surprise. People have expected some differences, like its cooler in the morning than the evening—that’s something natural that we experience here on Earth,” Sing said. “But what we saw was a real dichotomy between the weather on both sides of the planet, and huge differences in cloud coverage, and that changes our whole picture of the planet.”

Because the evenings are clear of clouds, the researchers could look to the trailing edge specifically to see what the atmosphere of the planet looked like—something the Hubble telescope could not provide.

Artistic representation of WASP-94A b, a gas giant in the Microscopium constellation. Clouds build as air flows over the dark side of the planet, reaching a large swell by daybreak. The clouds dissipate on the dayside, leaving clear skies in the early evening.  Credit:Hannah Robbins/Johns Hopkins University

“With the Hubble telescope, when we used to do this type of observation, we got an average view of the whole planet with data from the clouds and the atmosphere squished together and indistinguishable,” said first author Sagnick Mukherjee, a postdoctoral fellow at Arizona State University who was a student at Johns Hopkins and UC Santa Cruz at the time of the research. “This approach with the JWST lets us localize our observations, which helped us see the cloud cycle.”

When the researchers looked at the clear evening sky, they found that WASP-94A b was much more like Jupiter than they thought. Previously, when the clouds were averaged in, the data suggested the planet was made of hundreds of times more oxygen and carbon than Jupiter—a finding that baffled researchers given it couldn’t be explained by planet formation theory. The new data, however, shows WASP-94A b has only five times the amount of oxygen and carbon.

Hot Jupiter planets orbit much closer to their stars—closer even than Mercury to the sun—and therefore are much hotter and are exposed to more radiation. Because of their extreme environments, these planets also make good laboratories to study the chemistry and physics of cloud dynamics.

Using WASP-94 Ab as a benchmark, the team looked at eight other hot gas giants and discovered the same distinctive cloud cycle on two other worlds: WASP-39 b and WASP-17 b. Next, Sing and his team will be using data from a new large JWST program to study cloud cycling across a wide variety of exoplanets, including an eccentric gas giant planet in the habitable zone.

 

Also Read:

Space News: Planetary-scale ‘heat wave’ discovered in Jupiter’s atmosphere

Webb space Telescope Captures Clearest View of Neptune’s Rings, Unusual Moon ‘Triton’

 

 

Massive Stars Found To Control Star Formation In Nearby Molecular Cloud

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New evidence has been unearthed which show that massive stars can initiate star formation in nearby areas thus helping shape the evolution of star-forming regions.

Stars are born inside vast clouds of gas and dust known as molecular clouds. While most stars in our Galaxy have masses similar to the Sun, a few are much larger (more than eight times the mass of the Sun). Although these massive stars are rare, they play a significant role in shaping their surroundings and sometimes even contribute to the formation of the next generation of stars.

Scientists from the Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital, an autonomous research institute under the Department of Science and Technology (DST), Government of India,  investigated a region known as Bright Rimmed Cloud 44 (BRC 44), situated approximately 900 parsecs from Earth within the Cepheus OB2 star-forming complex and found that massive stars give out UV radiation that propagates into the cloud, giving birth to new stars.


Fig: The CO (black color) and 1.4 GHz NVSS (white color) contours are overplotted on the 8 µm Spitzer image of the region. Circles represent the identified YSO candidates. The red circles are optically visible YSOs (Group 1), green circles are embedded. Young YSOs(Group 2), and magenta circles are identified as BD candidates.

Bright Rimmed Clouds get their name from their glowing edges, which shine brightly when exposed to intense ultraviolet (UV) radiation from nearby massive stars. In the case of BRC 44, the researchers found that UV radiation from a massive star ionizes the surface of the cloud, which leads to heating and compression of the gas. This compression creates shock waves that propagate into the cloud, increasing its density and triggering the formation of new stars.

The research, led by Mr. Rishi C., a PhD scholar along with Dr. Neelam Panwar and other researchers from India, UK, China & Thailand, employed a multi-wavelength approach to study the region. Observations were done using the 3.6-m Devasthal Optical Telescope (DOT) and the Devasthal Fast Optical Telescope (DFOT) in India, along with the data from the Spitzer Space Telescope and radio observations from the Purple Mountain Observatory in China. By combining optical, infrared, and radio data, the scientists were able to study both the stars and the surrounding gas in great detail.

One of the most exciting results of the study is the discovery of 22 new young stellar objects in BRC 44. Among these are several brown dwarfs—objects that are smaller than normal stars to sustain hydrogen fusion in their cores. Finding such low-mass objects provides essential clues about how stars and sub-stellar objects form under the influence of massive stars. Apart from this finding, they also found two groups of young stars, with one group formed from the interplay of cloud and radiation from the nearby massive star and the other group formed around the same time as the massive star.

The results, published in The Astrophysical Journal, show that massive stars play a complex role in the Galaxy. Instead of only destroying their surroundings, they can also trigger new star formation.

 

Also Read:

Astronomers Spot “Sneezing” Baby Stars Creating Massive Rings In Space

NASA’s Hubble finds spiraling stars ‘NGC 346’, providing window into early universe

 

 

Scientists Explore Differences in Extragalactic Jets Emerging From Black Holes

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A team of international astrophysicists have uncovered new insights into the mystery behind the differences in the appearances of extragalactic jets emerging from the environments of supermassive blackholes. They showed that the plasma composition can affect the appearances of these jets. This may help to unravel the mystery of matter content of relativistic jets.

At the centers of many distant galaxies reside supermassive black holes with masses millions to billions of times that of our Sun. These black holes don’t just eat everything, but can also act like powerful engines, launching narrow beams of plasma and energy known as “jets” that shoot into space at nearly the speed of light. These extragalactic jets can travel for thousands of light-years and emit radiation ranging from low-energy radio waves to high-energy gamma rays.

For a long time, astronomers have been wondering about a noticeable difference in radio images of extragalactic jets, first identified by Fanaroff & Riley in 1974. They broadly classified radio jets into two main categories: FR I & FR II. The FR I jets are “core-brightened,” meaning they are brightest near the core and gradually fade into diffuse structures as they move outward. The FR II jets, on the other hand, are “edge-brightened,” meaning they are fainter near the core but stay tightly focused over long distances until they hit the surrounding gas, creating giant “hot spots” at their tips.

Scientists have for long continued to debate whether this difference is due to the black hole itself, the environment around it, or the intrinsic properties of the jet, such as its speed, temperature, and magnetic strength, etc.

A new research published in The Astrophysical Journal by Mr. Priyesh Kumar Tripathi, Dr. Indranil Chattopadhyay, and Mr. Sanjit Debnath from Aryabhatta Research Institute of Observational Sciences (ARIES), Dr. Raj Kishore Joshi from the Nicolaus Copernicus Astronomical Center, Poland, Dr. Ritaban Chatterjee from Presidency University, Kolkata, and Dr. M. Saleem Khan from MJPRU Barelly, used advanced computer simulations to reveal that the secret to these differences may be due to the jet’s composition and the environment it travels through. The research team performed large 3D magnetohydrodynamic (MHD) simulations of these jets at kiloparsec scales using a numerical simulation code developed by the Numerical and Theoretical Astrophysics Group at ARIES. Notably, this code incorporates a relativistic equation of state, which can accurately handle a very large range of temperatures encountered at different regions of the jet.

The team discovered that a phenomenon called the “kink instability” is a major player in shaping these powerful, narrow jets, causing wiggles (small bend). In space, if this wiggle grows faster than the jet can flow forward, the jet beam disrupts, spreading its energy into a faint, diffuse cloud – the classic look of an FR I jet. Astrophysical jets aren’t made of ordinary matter. Instead, they are composed of plasma, a soup of charged particles including electrons, positrons (the antimatter twin of electrons), and sometimes heavier particles like protons. One of the study’s most significant findings is that the composition of jet plasma can determine its fate.

Jets can be made of mostly electrons and protons (Hadronic plasma), a mixture that includes positrons (the antimatter twin of the electron– Leptonic/Mixed plasma).

Fig: 3D Volume rendering of the jet tracer for electron-proton and mixed plasma jet

The simulations showed that jets rich in positrons (lepton-rich) are relatively hotter, causing them to expand and slow down. They often can’t stay straight and get twisted by the kink instability. As a result, they form a diffuse, FR I–like structure, where the jet gradually fades instead of ending in a bright hotspot. In contrast, jets composed primarily of electrons and protons were more likely to transition between morphologies, thereby changing their identity. This suggests that what we see through our telescopes might just be a snapshot of a long, evolving cosmic process.

 

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Astronomers study the surface composition of a nearby super-Earth

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Using MIRI (Mid Infrared Instrument) on board the James Webb Space Telescope (JWST), a team of researchers led by former MPIA (Max Planck Institute for Astronomy, Heidelberg, Germany) PhD student Sebastian Zieba (Center for Astrophysics | Harvard & Smithsonian, Cambridge, USA) and Laura Kreidberg, MPIA Director and study PI (principal investigator), analysed the surface composition of the rocky exoplanet LHS 3844 b. Beyond characterizing exoplanetary atmospheres, this kind of deciphering the geological properties of planets orbiting distant stars is the next step in unveiling their nature. The results of this investigation are now published in the journal Nature Astronomy.

A dark and airless rocky super-Earth

LHS 3844 b is a rocky planet 30% bigger than Earth and orbits a cool red dwarf star once within roughly 11 hours. Whirling just three stellar diameters above the host star’s surface, the planet is tidally locked to its orbit. This means one rotation takes just as long as one revolution. As a result, the same hemisphere of LHS 3844 b always faces its star, producing a constant dayside with an average temperature of about 1000 Kelvin (approximately 725 Degrees Celsius or 1340 Degrees Fahrenheit). The LHS 3844 system is only 48.5 light-years (14.9 parsecs) away from Earth.

“Thanks to the amazing sensitivity of JWST, we can detect light coming directly from the surface of this distant rocky planet. We see a dark, hot, barren rock, devoid of any atmosphere.” – Laura Kreidberg, MPIA.

With its dark surface, LHS 3844 b may resemble a larger version of the Moon or the planet Mercury. This conclusion is based on analysing the infrared radiation received from the planet’s hot dayside. However, when measuring this radiation, we cannot see the planet directly; instead, we register the repeating change in brightness we receive from the star and the orbiting planet combined.

MIRI divided a portion of the planet’s infrared emission, ranging from 5 to 12 micrometres, into smaller wavelength sections and measured the brightness per wavelength bin. This is what astronomers call a spectrum, a rainbow-like distribution of the light’s components. Another data point, obtained from observations with the Spitzer Space Telescope and published a few years ago, augmented the analysis.

Constraining geological activity

Similar to how exoplanetary atmosphere research has benefited from climate science, this emerging field of exoplanetary geology draws on Earth-based geologic knowledge. Zieba, Kreidberg, and their collaborators ran models and accessed template libraries of rocks and minerals known from Earth, the Moon, and Mars to see what infrared signatures they would produce under the conditions on LHS 3844 b. Comparing observation-based data with these computations confidently ruled out a composition comparable to Earth’s crust, typically silicate-rich minerals such as granite.

Although this result is not very surprising – even in the Solar System, Earth is the only planet with such a crust – it may reveal details on LHS 3844 b’s geological history. Earth-like silicate-rich crusts are thought to form through a prolonged refinement process that requires tectonic activity and typically relies on water as a lubricant. The rocky material repeatedly melts and solidifies as it is mixed with mantle material, leaving the lighter minerals on the surface.

“Since LHS 3844 b lacks such a silicate crust, one may conclude that Earth-like plate tectonics does not apply to this planet, or it is ineffective,” says Sebastian Zieba. “This planet likely only contains little water.”

What can we deduce about the exoplanet’s rocky surface?

Instead, the dark surface points to a composition reminiscent of terrestrial or lunar basalt, or of Earth’s mantle material. However, the astronomers attempted an even more detailed characterization.

A statistical analysis of how well this spectrum fits various mineral mixtures and configurations revealed that extended solid areas of basalt or magmatic rock best match the observations. They are rich in magnesium and iron and can include olivine. Crushed material, such as rocks or gravel, also fits fairly well, whereas grains or powders are inconsistent with the observations due to their brighter appearance, at least at first glance.

Without a protective atmosphere, planets are subjected to space weathering, predominantly driven by hard, energetic radiation from the host star and impacts from meteorites of various sizes.

“It turns out, these processes not only slowly dissolve hard rocks into regolith, a layer of fine grains or powder as found on the Moon,” explains Zieba. “They also darken the layer by adding iron and carbon, making the regolith’s properties more consistent with the observations.”

Geologically fresh or weathered? Two possible scenarios

This assessment left the astronomers with two scenarios for the planet’s surface that match the data equally well. One involves a surface dominated by dark, solid rock composed of basaltic or magmatic minerals. Compared to geological timescales, space weathering alters its properties quickly. Therefore, the astronomers conclude that, in this scenario, the surface should be relatively fresh, produced by recent geological activity, such as widespread volcanism.

The second scenario also proposes a dark surface, comparable to the Moon or Mercury. Still, it accounts for prolonged space weathering, which leads to extended regions covered by a darkened regolith layer, a fine powder also present on the Moon, as evidenced by the iconic photos of the astronauts’ footprints. This alternative relies on longer periods of geological inactivity, thereby requiring conditions opposite to the first scenario.

Attempts to resolve the ambiguity

These two alternatives differ in the degree of recent geological activity required. On Earth and other active objects in the Solar System, a typical phenomenon during such activity is outgassing. Sulphur dioxide (SO2) is a gas commonly connected to volcanism. If present on LHS 3844 b in reasonable amounts, MIRI should have detected it. Still, it found nothing. Therefore, a recent period of activity seems unlikely, which leads the astronomers to favour the second scenario. If correct, LHS 3844 b may truly look much like Mercury indeed.

In order to test their idea, Zieba, Kreidberg, and their colleagues are already pursuing a more direct approach. They have obtained additional JWST observations, which should enable them to discern surface conditions by exploiting small differences in how solid slabs and powders emit or reflect light. The distribution of emission angles depends on surface roughness, which affects the amount of radiation received at a given viewing angle. This concept is successfully applied to characterizing asteroids in the Solar System. “We are confident the same technique will allow us to clarify the nature of LHS 3844 b’s crust and, in the future, other rocky exoplanets,” concludes Kreidberg.

 

Also Read:

Space News: Planetary-scale ‘heat wave’ discovered in Jupiter’s atmosphere

Future Spacecraft Material Found, Resists 4,000 Degrees Celsius

Outer solar system object has an atmosphere but shouldn’t

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A team of professional and amateur Japanese astronomers found evidence for a thin atmosphere around a small body in the outer Solar System. The object is so small that it should not have a sustainable atmosphere, raising questions about when and how the atmosphere formed. Future observations to better characterize the atmosphere will help solve these mysteries.

In the cold reaches of the outer Solar System lie thousands of small objects known as trans-Neptunian objects (TNOs) because they lie outside the orbit of Neptune. A thin atmosphere has been observed around Pluto, the most famous TNO, but studies of other TNOs have yielded negative results. Most TNOs are so cold, and their surface gravity so weak, that they are not expected to retain atmospheres.

But astronomers like to expect the unexpected, so they took advantage of a lucky “natural experiment” to look for an atmosphere around a TNO known as (612533) 2002 XV93. This object, abbreviated as 2002 XV93, has a diameter of approximately 500 km. For reference, Pluto’s diameter is 2,377 km. The orbit of 2002 XV93 is such that, as seen from Japan, it passed directly in front of a star on January 10, 2024. As the star disappears behind 2002 XV93, it might gradually fade, indicating that the light is being attenuated as it passes through a thin atmosphere; or it might suddenly wink out as it slips behind the solid surface of the TNO.

Artist’s conception of this research showing an imagined time sequence as a star passes behind a TNO with an atmosphere. Credit:NAOJ

A team of professional and amateur astronomers, led by Ko Arimatsu at NAOJ Ishigakijima Astronomical Observatory, observed the star as 2002 XV93 passed in front of it from multiple sites in Japan. The obtained data are consistent with attenuation by an atmosphere.

Calculations show that the atmosphere found around 2002 XV93 is expected to last less than 1000 years unless it is replenished. So it must have been created or replenished recently. Observations by the James Webb Space Telescope show no signs of frozen gases on the surface of 2002 XV93 that might sublimate to form an atmosphere. One possibility is that some event brought frozen or liquid gases from deep inside the TNO to the surface. Another possibility is that a comet crashed into 2002 XV93, releasing gas that formed a temporary atmosphere. Further observations are needed to distinguish between these two scenarios.

 

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XRISM finally solves famous star’s 50-year space mystery

Watching water droplets merge on the International Space Station

Curiosity rover detects never-before-seen organic compounds on Mars in new experiment

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NASA’s Curiosity Mars rover uncovered a diverse mix of organic molecules on Mars, including chemicals widely considered building blocks for the origin of life on Earth.

The findings, which come from a chemical experiment performed for the first time on another world, reveal that the Martian surface can preserve the kinds of molecules that could serve as signs of ancient life. However, this experiment cannot distinguish between organic compounds from potential past life on Mars and those formed through geologic processes or delivered by meteorites.

Definitively identifying signs of past life would require returning rock samples to Earth.

The study was led by Amy Williams, Ph.D., a professor of geological sciences at the University of Florida and a scientist on the Curiosity and Perseverance Mars rover missions. Curiosity landed on Mars in 2012 to find evidence that ancient Mars had conditions that could support microbial life billions of years ago; the Perseverance rover, which landed in 2021, was sent to look for signs of any ancient life that might have formed.

“We think we’re looking at organic matter that’s been preserved on Mars for 3.5 billion years,” said Williams, who helped develop this chemical experiment. “It’s really useful to have evidence that ancient organic matter is preserved, because that is a way to assess the habitability of an environment. And if we want to search for evidence of life in the form of preserved organic carbon, this demonstrates it’s possible.”

Williams and an international collaboration of researchers published their findings April 21 in the journal Nature Communications.

Among the 20-plus chemicals identified by the experiment, Curiosity spotted a nitrogen-bearing molecule with a structure similar to DNA precursors — a chemical never before spotted on Mars. The rover also identified benzothiophene, a large, double-ringed, sulfurous chemical often delivered to planets by meteorites.

“The same stuff that rained down on Mars from meteorites is what rained down on Earth, and it probably provided the building blocks for life as we know it on our planet,” Williams said.

NASA’s Curiosity Mars rover took this selfie at a location nicknamed “Mary Anning” after a 19th century English paleontologist. This was the site of the chemical experiment uncovering diverse organic molecules on Mars, in the Glen Torridon region, which scientists believe was a site where ancient conditions would have been favorable to supporting life, if it ever was present.Credit:NASA/JPL-Caltech/MSSS

Led by NASA’s Jet Propulsion Laboratory, Curiosity Mars landed in Gale crater, in a former lake bed, in August 2012. The rover conducted the experiment in 2020 in the Glen Torridon region of the crater, an area rich in the clay minerals that indicate the area once contained water. Those clays can hold on to and preserve organic chemicals better than other minerals, making them a prime target for uncovering these compounds.

The experiment was conducted by the instrument suite known as the Sample Analysis at Mars, or SAM. Led in part by Jennifer Eigenbrode, Ph.D., an astrobiologist at NASA’s Goddard Space Flight Center and co-author of the new study, SAM has been responsible for many of the mission’s most important discoveries about organic chemistry, atmosphere and habitability on Mars.

Using a chemical known as TMAH, the experiment broke apart larger organic molecules so they could be analyzed by onboard instruments within SAM. With only two cups of the TMAH chemical onboard Curiosity, success required careful planning and choosing the most favorable location to sample.

The promising results come as future missions — including the Rosalind Franklin mission to Mars and the Dragonfly expedition to Saturn’s moon Titan — plan to bring the TMAH test onboard to search for organic compounds.

“We now know that there are big complex organics preserved in the shallow subsurface of Mars, and that holds a lot of promise for preserving large complex organics that might be diagnostic of life,” Williams said.

 

Also Read:

NASA’s Perseverance Rover Gets the Dirt on Mars

What’s Mars made of ? Japanese study throws light and opens up new study

 

‘Dancing Jets’ from black hole reveal extraordinary cosmic power

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A new study led by Curtin University has harnessed a global-scale radio telescope network to capture detailed images revealing the extraordinary power of jets emitted by black holes, offering strong confirmation of long-standing theories about their role in shaping the Universe’s structure.

Published in Nature Astronomy, the research found that the jets from Cygnus X-1—a system containing the first confirmed black hole and a supergiant companion star—generate energy comparable to the output of around 10,000 Suns.

To record the measurement, researchers used an array of linked up telescopes separated by large distances to observe the black hole jets being buffeted by the winds of the star as the black hole moved around its orbit – much like how strong winds on Earth can push around water in a fountain.

By knowing the power of the wind and measuring how much the jets were bent, the researchers could determine the instantaneous power of the jets for the first time.

In addition, they were able to determine the speed of the black hole’s jets – about half the speed of light, or 150,000 km per second – another measurement that has challenged scientists for decades.

The strong stellar wind from the supergiant star pushes the jets launched by the black hole away from the star. This causes the jet direction to vary as the black hole and the supergiant star move around their orbit./ International Centre for Radio Astronomy Research (ICRAR)

The research was led from the Curtin Institute of Radio Astronomy (CIRA) and the Curtin node of the International Centre for Radio Astronomy Research (ICRAR), in collaboration with the University of Oxford.

Lead author Dr Steve Prabu, who worked at CIRA at the time of the research and who is now based at the University of Oxford, said researchers were able to make the measurement using a sequence of images of the “dancing jets” – a term he used to describe the jets’ movement pattern as they were repeatedly deflected in different directions by the supergiant star’s powerful winds as the star and black hole moved around their orbits.

Dr Prabu said the measurement allowed scientists to understand what fraction of the energy released around black holes could be deposited into the surrounding environment, thereby changing the environment.

“A key finding from this research is that about 10 per cent of the energy released as matter falls in towards the black hole is carried away by the jets,” Dr Prabu said.

“This is what scientists usually assume in large-scale simulated models of the Universe, but it has been hard to confirm by observation until now.”

Co-author Professor James Miller-Jones, from CIRA and the Curtin node of ICRAR, said previous methods could only measure the average jet power over thousands or even millions of years, preventing accurate comparisons with the X-ray energy released instantaneously from the infalling matter.

“And because our theories suggest that the physics around black holes is very similar, we can now use this measurement to anchor our understanding of jets, whether they are from black holes 10 or 10 million times the mass of the Sun,” Professor Miller-Jones said.

“With radio telescope projects such as the Square Kilometre Array Observatory currently under construction in Western Australia and South Africa, we expect to detect jets from black holes in millions of distant galaxies, and the anchor point provided by this new measurement will help calibrate their overall power output.

“Black hole jets provide an important source of feedback to the surrounding environment and are critical to understanding the evolution of galaxies.”

 

Also Read:

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Scientists Explore Potential Black Holes In Dwarf Galaxies

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A recent study has examined whether some of the universe’s smallest galaxies—particularly dwarf spheroidal galaxies orbiting the Milky Way—could host black holes, offering fresh insight into how these cosmic objects form and evolve over time.

 

Artemis II Mission Accomplished: Crew Re-Entry Updates, Splash down and Safe return home [Watch Videos]

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  • Artemis II launched aboard NASA’s Space Launch System, carrying four astronauts in the Orion spacecraft on a deep-space mission beyond low Earth orbit.
  • The crew conducted system checks and performed a historic lunar flyby, travelling thousands of kilometres beyond the Moon before beginning their return journey.
  • After completing a roughly 10-day mission, Orion safely re-entered Earth’s atmosphere and splashed down in the Pacific Ocean, marking the first crewed lunar mission since Apollo.

Watch as the Artemis II crew returns to Earth, splashing down.

See visualization of plasma build up around the space craft, repelling of that heat on Integrity seat shield To splash down in pacific ocean( from timestamp 1:26:15)  in below  video posted by NASA on X.

NASA’s Artemis II mission return home details:

6:25 p.m.

NASA’s Artemis II mission is scheduled to splash down at about 8:07 p.m. EDT (5:07 p.m. PDT) off the coast of San Diego. After splashdown, a combined NASA and U.S. military team, will retrieve the crew and transport them by helicopter to the USS John P. Murtha. Once aboard the ship, the astronauts will undergo post-mission medical evaluations before returning to shore to board an aircraft bound for NASA’s Johnson Space Center in Houston.

Watch live return coverage on NASA+, Amazon Prime, Apple TV, Netflix, HBO Max, Discovery+, Peacock and Roku. Learn how to stream NASA content through a variety of online platforms, including social media.

7:15 p.m.

The Artemis II Crew – NASA astronauts Reid Wiseman, Victor Glover, Christina Koch and CSA (Canadian Space Agency) astronaut Jeremy Hansen are preparing for re-entry aboard the Orion spacecraft/NASA

7:33 p.m.

Orion’s crew and service module have separated. The crew module continues on its path towards Earth while the service module will harmlessly burn up in Earth’s atmosphere over the Pacific Ocean. The Artemis II return trajectory is designed to ensure any remaining debris does not pose a hazard to land, people, or shipping lanes.

7:37 p.m.

Orion performed the crew module raise burn, adjusting the spacecraft’s orientation to align its heat shield for re-entry.

7:53 p.m.

At 7:53 p.m. EDT,  The Orion spacecraft reached Earth’s atmosphere 400,000 feet above the planet’s surface, traveling 35 times the speed of sound and about 1,956 statute miles from the splashdown site. This is where the spacecraft first encounters the upper atmosphere and begins its guided descent. Shortly after, Orion is in a planned communications blackout expected to last about six minutes as plasma built around the crew capsule during heating.

8:00 p.m.

NASA has reestablished communications contact with the Artemis II crew aboard the Orion spacecraft as it returns to Earth.

8:03 p.m.

At 23,400 feet, the drogue parachutes on Orion deployed to slow and stabilize the spacecraft. Orion’s velocity drops to 479 feet per second and is .8 miles from splashdown.

8:04 p.m.

At 5,400 feet, Orion’s drogue parachutes were cut and the three main parachutes deployed, reducing velocity to less than 200 feet per second and guiding Orion on its final descent and splashdown.

8:07 p.m.

SPLASHDOWN!

NASA’s Artemis II crew in their Orion spacecraft is back on Earth. They successfully completed a parachute-assisted splashdown in the Pacific Ocean off the coast of San Diego at 8:07 p.m. EDT (5:07 p.m. PDT).
NASA

NASA’s Artemis II crew in their Orion spacecraft is back on Earth. They successfully completed a parachute-assisted splashdown in the Pacific Ocean off the coast of San Diego at 8:07 p.m. EDT (5:07 p.m. PDT).

Engineers will conduct several additional tests while Orion is in the water before powering down the spacecraft and handing it over to the recovery team aboard the USS John P. Murtha. The recovery team is on site and headed to the capsule to begin assisting the crew out of Orion.

The Orion spacecraft with the Artemis II crew inside is seen floating in the Pacific Ocean after splashing down at 8:07 p.m. EDT on April 10, 2026.
NASA

Orion has begun crew module power down, a planned post-splashdown step in which flight controllers shut down nonessential systems and transition the capsule into its recovery configuration. This reduces power demand and prepares the spacecraft for crew extraction as recovery teams move in.

8:12 p.m.

At the direction of the NASA recovery director, team members from the agency and the U.S. military now are approaching the spacecraft in inflatable boats.

Approximately an hour after splashdown, the crew will be extracted from Orion and then flown to the USS John P. Murtha. U.S. Navy helicopters will then transport them to the ship. Once aboard, the astronauts will undergo post-mission medical evaluations before returning to shore to board an aircraft bound for NASA’s Johnson Space Center in Houston.

When ready, Navy divers will attach a cable, called the winch line, to Orion to pull the spacecraft into a specially designed cradle inside the ship’s well deck. Four additional tending lines will be secured to attachment points on the crew module while under tow.

Once Orion is positioned above the cradle assembly, technicians will drain the well deck and secure the capsule.

After it is secure aboard the ship, teams will return Orion to U.S. Naval Base San Diego before returning it to NASA’s Kennedy Space Center in Florida for inspection. Once there, technicians will thoroughly examine the spacecraft, retrieve onboard data, remove payloads, and conduct additional post-flight checks.

9:34 p.m.

The Artemis II crew – NASA astronauts Reid Wiseman, Victor Glover, and Christina Koch, and CSA (Canadian Space Agency) astronaut Jeremy Hansen — have been safely extracted from the Orion spacecraft.

The Artemis II crew is seen on an inflatable raft, called the front porch, after exiting the spacecraft. The Artemis II mission successfully splashed down in the Pacific Ocean at 8:07 p.m. EDT on April 10, 2026.
9:56 p.m.

The Artemis II crew has been hoisted into U.S. helicopters and are being flown to the USS John P. Murtha.

Artemis II Commander and NASA astronaut Reid Wiseman is being hoisted into a U.S. military helicopter before being transported to the USS John P. Murtha.
Artemis II mission specialist and NASA astronaut Christina Koch is being hosted into a U.S. military helicopter before being flown to the USS John P. Murtha. NASA

9:58 p.m.

The Artemis II crew is safely aboard the USS John P. Murtha, where they will undergo post-mission medical evaluations in the ship’s medical bay before traveling back to shore to board a NASA aircraft bound for the agency’s Johnson Space Center in Houston.

NASA will hold a post-splashdown news conference at 10:35 p.m. EDT from the agency’s Johnson Space Center in Houston. Participants include:

  • NASA Associate Administrator Amit Kshatriya
  • Lori Glaze, acting associate administrator, Exploration Systems Development Mission Directorate
  • Rick Henfling, entry flight director, Artemis II
  • Howard Hu, manager, Orion Program
  • Shawn Quinn, manager, Exploration Ground Systems Program

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Artemis II Update-26, Day 10: Crew Completes Final Burn Before Splashdown

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At 2:53 p.m. EDT, the Orion spacecraft ignited its thrusters for 8 seconds, producing a change in velocity of 4.2 feet-per-second and pushing Artemis II toward Earth. NASA astronauts Reid Wiseman, Victor Glover, Christina Koch and CSA (Canadian Space Agency) astronaut Jeremy Hansen reviewed procedures and monitored the spacecraft’s configuration and navigation data.

The crew continues to wrap up cabin configuration for re-entry and move into their entry checklist.

Splashdown is targeted for 8:07 p.m. EDT (5:07 p.m. PDT) off the coast of San Diego, where NASA’s recovery team will be standing by to welcome the Artemis II crew home.

Watch live return coverage on NASA+, Amazon Prime, Apple TV, Netflix, HBO Max, Discovery+, Peacock and Roku, starting at 6:30 p.m. Learn how to stream NASA content through a variety of online platforms, including social media. Coverage will continue until NASA and Department of War personnel safely assist the crew out of Orion and transport them to the USS John P. Murtha.

 

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Artemis II Update-25, Day 10: Crew Sets for Final Burn, Splashdown

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The Artemis II crew — NASA astronauts Reid Wiseman, Victor Glover, Christina Koch and CSA (Canadian Space Agency) astronaut Jeremy Hansen — began the final phase of their journey home to the songs “Run to the Water” by Live, selected by the crew, and “Free” by Zac Brown Band, as they prepared for their third return trajectory correction burn and shifted into full re-entry and splashdown preparations. When they woke up, they were 61,326 miles from Earth.

Splashdown is targeted for 8:07 p.m. EDT (5:07 p.m. PDT) off the coast of San Diego, where a combined NASA and U.S. military recovery team will be standing by to welcome the Artemis II crew home.

Watch live return coverage on NASA+, Amazon Prime, Apple TV, Netflix, HBO Max, Discovery+, Peacock and Roku starting at 6:30 p.m. Learn how to stream NASA content through a variety of online platforms, including social media.

Final return burn sets Orion for home

The third return burn will occur at 2:53 p.m., refining Orion’s path for atmospheric entry and splashdown. During the maneuver, the spacecraft will make precise adjustments to stay on its targeted course home.

NASA’s Artemis II re-entry and splashdown timeline and streaming coverage. Splashdown is targeted for 8:07 p.m. EDT (5:07 p.m. PDT) off the coast of San Diego, where NASA’s recovery team will be standing by to welcome the Artemis II crew home.NASA

Artemis II splashdown timeline

A carefully timed sequence will guide Orion through the final stages of descent:

  • 7:33 p.m.: Orion’s crew module will separate from the service module, exposing its heat shield for the spacecraft’s return through Earth’s atmosphere, where it will encounter temperatures of about 3,000 degrees Fahrenheit.
  • 7:37 p.m.: Following separation, Orion will perform an 18 second crew module raise burn beginning to set the proper entry angle and align the heat shield for atmospheric interface.
  • 7:53 p.m.: When Orion reaches 400,000 feet above Earth’s surface while traveling nearly 35 times the speed of sound. The crew is expected to experience up to 3.9 Gs in the planned entry profile. This moment marks the spacecraft’s first contact with the upper atmosphere and the start of a planned six-minute communications blackout as plasma builds around the capsule.
  • 8:03 p.m.: Around 22,000 feet in altitude, the drogue parachutes will deploy, slowing and stabilizing the capsule as Orion nears splashdown.
  • 8:04 p.m.: At around 6,000 feet, the drogues will release, and the three main parachutes will deploy, reducing Orion’s speed to less than 136 mph.
  • 8:07 p.m.: Slowing to 20 mph, Orion will splash down in the Pacific Ocean off the coast of San Diego, completing the Artemis II crew’s return to Earth and a 694,481-mile journey.
  • From there, teams from NASA and the U.S. military will extract the crew from Orion and fly them via helicopter to the USS John P. Murtha.
  • Within two hours after splashdown, the crew will be extracted from Orion and flown to the USS Murtha. Recovery teams will retrieve the crew, assist them onto an inflatable raft, and then use helicopters to deliver them to the ship. Once aboard, the astronauts will undergo post‑mission medical evaluations before returning to shore where awaiting aircraft will take them to NASA’s Johnson Space Center in Houston.

The Artemis II mission began with the successful liftoff of NASA’s SLS (Space Launch System) rocket on April 1 at 6:35 p.m. from Launch Pad 39B at Kennedy Space Center in Florida, sending the first humans toward the Moon since 1972.

During the mission, the astronauts completed a historic lunar flyby, marking humanity’s return to the vicinity of the Moon for the first time in more than 50 years. Throughout the flight, the crew and teams on the ground have evaluated Orion’s systems in the deep‑space environment, including a series of tests in which astronauts directly operated and interacted with the spacecraft.

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Artemis II Update-24, Day 9: Second Return Correction Burn Complete

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Thrusters Fire To Steer Orion Home:

At 10:53 p.m. EDT, the Orion spacecraft executed a brief nine-second thruster burn, increasing its velocity by 5.3 feet per second and nudging the Artemis II crew further along their return path to Earth.

With the maneuver complete, the crew has now crossed the halfway mark on their journey home.

Temporary Signal Loss Resolved

Roughly two hours before the burn, mission teams encountered an unexpected return link loss of signal during a data rate transition, briefly disrupting the flow of communications and telemetry from the spacecraft.

Two-way contact was subsequently restored, allowing flight controllers and crew to resume preparations for the scheduled maneuver without further delay.

art002e016204 (April 6, 2026) – NASA astronaut and Artemis II Pilot Victor Glover pictured here in the Orion spacecraft during the Artemis II lunar flyby. Glover and his fellow crewmates spent approximately seven hours taking turns at the Orion windows capturing science data to share with their team back on Earth. At closest approach, they came within 4,067 miles of the Moon’s surface.NASA

Re-Entry Briefings And Next Steps

Earlier in the day, officials from NASA provided additional details on re-entry and splashdown procedures during a mission status briefing.

The next key milestone—a third return trajectory correction burn—is planned for April 10 at approximately 1:53 p.m., ahead of final re-entry operations.

Splashdown Target Remains On Track

NASA continues to target splashdown at 8:07 p.m. (5:07 p.m. PDT) on Friday, April 10, off the coast of San Diego, as the Artemis II mission enters its final phase of return.

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Monitoring over deep space network before artemis II signal acquisition

Who is Dan Florez in Artemis Mission Program

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Dan Florez is one of the NASA test directors for the Exploration Ground Systems Program. The test directors are a group of 20 engineers at the agency’s Kennedy Space Center in Florida who plan and execute integrated testing for Artemis missions. Their work includes developing timelines and procedures for launch countdown, propellant loading, emergency egress, pad and launch abort scenarios, recovery operations, and more. They help lead the ground systems team in all areas of testing.

At the time of Artemis I launch, Florez and his fellow test directors had already developed the launch countdown timelines for Artemis II.

“We were really focused on loading that spacecraft with cryogenic propellants and successfully launching it. With Artemis II, we’re going to have to do all that again, but in the middle of that, we’re going to have to embed the crew timeline to get the crew safely inside the spacecraft, get all the systems checked out, and launch them into space,” Florez said. “And we have to do the same thing on the tail end through recovery. So, there’s a lot of complexities when you have the human element thrown into the operation.”

Since Artemis I, Florez has focused his work even more heavily on the human element, taking on rescue and recovery operations.

“We have to have a plan to go get to the crew if we have an abort, if we land anywhere in the world within 24 hours,” said Florez. “My role right now is to do a lot of that coordination to make sure we have all the assets and all the resources in place to get to the crew.”

When the Artemis II crew returns to Earth aboard the Orion spacecraft, Florez will be there, prepared and ready with NASA’s Landing and Recovery Team and the U.S. military.

“We have a great partnership with the military. We have the Human Spaceflight Support Office within the Air Force that support us directly for not just for recovery operations, but also for any of the rescue operations”.

Dan Florez, NASA Test Director, Exploration Ground Systems Program

Recovery operations are routinely verified and validated in what is called an underway recovery test. NASA and Navy teams board a U.S. Navy ship and travel off the coast of San Diego to test retrieving the capsule and getting the crew safely on the ship. In late February 2024, the Artemis II crew joined the recovery team’s eleventh iteration of testing called, URT-11.

“It was really great to have that perspective of having astronauts in the loop during our test operations,” said Florez. “Everywhere along the way, we got feedback from them.”

Artemis II launched at 6:35 p.m. EDT April 1, from Launch Complex 39B, sending NASA astronauts Reid Wiseman, Victor Glover, and Christina Koch, and CSA (Canadian Space Agency) astronaut Jeremy Hansen, on their approximately 10-day mission around the Moon.

A wave breaks inside the well deck of USS Somerset as teams work to recover the Crew Module Test Article (CMTA), a full scale replica of the Orion spacecraft, as they practice Artemis recovery operations during Underway Recovery Test-12 off the coast of California, Thursday, March 27, 2025. NASA/Joel Kowsky

Florez and his colleagues are prepared and ready to apply everything they tested to recover the crew.

“Watching them launch is going to be great. I’m going to be happier when they land”.

Dan Florez, NASA Test Director, Exploration Ground Systems Program

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Deep Space Network Establishes Contact With Artemis II Spacecraft

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The acquisition of the radio frequency signal from the Artemis II crewed mission to the Moon by NASA’s Deep Space Network (DSN) is indicated by the peak in the data signal shown below on the computer screen.

Credits: NASA/JPL-Caltech

Soon after the mission’s launch on April 1, 2026, at 6:35 p.m. EDT, NASA’s Near Space Network led communications with the Orion capsule. Then, communications were handed off to the DSN, marking the first time in over 50 years that the network would be communicating with a crewed spacecraft traveling through deep space.

The Space Flight Operations Facility at NASA’s Jet Propulsion Laboratory in Southern California (where this photo was taken) operates the DSN, which comprises three complexes in Goldstone, California; Madrid, Spain; and Canberra, Australia. Each complex consists of several radio frequency antennas that communicate with dozens of robotic spacecraft exploring the solar system in addition to the Artemis II mission.

A graphical representation of the Deep Space Network’s radio frequency antennas indicate signal acquisition from NASA’s Artemis II mission to the Moon on April 1, 2026, inside the Space Flight Operations Facility at NASA’s Jet Propulsion Laboratory in Southern California. Two antennas at the Madrid Deep Space Communications Complex, Deep Space Station 54 and 56, can be seen communicating with Artemis II (the signals are labelled “EM2”, short for “Exploration Mission 2”; elsewhere they are labelled “ART2” for “Artemis II”).

A similar visualization can be found at DSN Now, which details all the missions that the network is communicating with 24 hours a day, seven days a week.

NASA

The DSN is managed by JPL for the agency’s Space Communications and Navigation program, which is located at NASA Headquarters within the Space Operations Mission Directorate. The DSN allows missions to track, send commands to, and receive scientific data from faraway spacecraft. JPL is managed by Caltech in Pasadena, California, for NASA.

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Monitoring over deep space network before artemis II signal acquisition

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Blanca Renteria, operations chief for the Artemis Deep Space Network (DSN), monitored incoming data from the Space Flight Operations Facility at Jet Propulsion Laboratory shortly after Artemis II lifted off on April 1, 2026.

The launch took place at 6:35 p.m. EDT from Kennedy Space Center, with mission control teams quickly transitioning to deep space communication support.

The Space Flight Operations Facility manages NASA’s DSN, a worldwide system consisting of three primary complexes located in Goldstone, California; Madrid, Spain; and Canberra, Australia.

Each site is equipped with multiple radio-frequency antennas that maintain continuous communication with numerous robotic missions across the solar system, alongside the crewed Artemis II spacecraft.

NASA

Backbone Of Deep Space Communication

The DSN is operated by JPL under NASA’s Space Communications and Navigation programme, based at the agency’s headquarters within the Space Operations Mission Directorate.

This network enables mission teams to track spacecraft, transmit commands, and receive scientific data across vast distances. The Jet Propulsion Laboratory itself is managed by the California Institute of Technology in Pasadena, California, on behalf of NASA.

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What’s the longstanding tradition at JPL before any launch and other major space mission events

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A Ritual Before Liftoff

A container of “lucky peanuts” was placed above workstations inside the Space Flight Operations Facility at Jet Propulsion Laboratory ahead of the Artemis II launch on April 1, 2026.

The quirky ritual—eating peanuts before major mission events—has long been observed at JPL, seen by teams as a symbol of good fortune before critical operations.

Control Centre Behind Deep Space Communication

The Space Flight Operations Facility oversees NASA’s Deep Space Network (DSN), a global communication system comprising three major complexes located in Goldstone, California; Madrid, Spain; and Canberra, Australia.

Each site houses multiple radio-frequency antennas that maintain constant contact with dozens of spacecraft across the solar system, including the crewed Artemis II mission.

NASA

A Critical Link To Spacecraft

Managed by JPL under NASA’s Space Communications and Navigation programme, the DSN operates from the agency’s headquarters within the Space Operations Mission Directorate.

The network plays a vital role in tracking spacecraft, transmitting commands, and receiving scientific data from distant missions. The Jet Propulsion Laboratory itself is run by the California Institute of Technology in Pasadena, California, on behalf of NASA.

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JPL’s Mission Control Steps Up For Artemis II Deep Space Operations

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Mission Control Comes Alive In California

Inside the Space Flight Operations Facility at Jet Propulsion Laboratory, the Artemis II mission took center stage on April 1, 2026, moments before liftoff. The central display featured the mission patch, while adjacent screens mapped real-time activity across the agency’s Deep Space Network (DSN), with active antennas highlighted as they transmitted and received signals.

From Launch To Deep Space Communication

Shortly after launch at 6:35 p.m. EDT from Kennedy Space Center, initial communications were managed through NASA’s Near Space Network.

Control was then handed over to the DSN, marking a significant milestone—the first time in more than five decades that the network was tasked with maintaining contact with a crewed spacecraft journeying through deep space.

Credits: NASA/JPL-Caltec

A Global Network Tracking The Mission

The DSN, operated from the Space Flight Operations Facility, consists of three major complexes located in Goldstone, California; Madrid, Spain; and Canberra, Australia.

Each site houses multiple high-powered radio antennas, forming a global system capable of maintaining continuous communication with spacecraft across the solar system—including Artemis II.

The Backbone Of Space Communication

Managed by JPL under NASA’s Space Communications and Navigation programme at headquarters, the DSN serves as a critical link between Earth and deep-space missions.

It enables mission teams to track spacecraft, transmit commands, and receive scientific data from vast distances. The Jet Propulsion Laboratory itself is operated by the California Institute of Technology in Pasadena, California, on behalf of NASA.

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Artemis II Update-23, Day 9: Crew Prepares To Come Home

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Final Day In Orbit

On their final full day in space, the Artemis II crew began the morning with “Lonesome Drifter” by Charley Crockett as their spacecraft closed in on Earth from a distance of 147,337 miles.

Astronauts Reid Wiseman, Victor Glover, and Christina Koch of NASA, along with Jeremy Hansen of the Canadian Space Agency, are spending the day preparing for their scheduled return on Friday, April 10. Activities include reviewing re-entry protocols and executing a trajectory correction maneuver.

Securing The Cabin For Re-Entry

Christina Koch and Jeremy Hansen are leading preparations inside the capsule, securing loose equipment, removing storage netting, and adjusting crew seating configurations for re-entry.

The crew will also assess updated weather forecasts, recovery team readiness, and the mission timeline. Simultaneously, they are reviewing post-landing procedures to ensure a smooth transition once back on Earth.

Artemis II infographic showcasing the missions entry, descent, and landing milestones. This graphic was presented by Artemis II Flight Director Rick Henfling during the mission status briefing to the media and public on April 8, 2026 at NASA’s Johnson Space Center in Houston.NASA

Trajectory Correction Burn

A key maneuver is scheduled for 9:53 p.m. EDT, when Orion’s thrusters will fire for a second return trajectory correction burn.

This adjustment is designed to fine-tune the spacecraft’s path toward Earth and align it precisely for atmospheric entry. During the burn, Jeremy Hansen will oversee procedure execution and monitor navigation and propulsion systems.

Infographic featuring the Artemis II Orion lofted entry sequence. This graphic was presented by Artemis II Flight Director Rick Henfling during the mission status briefing to the media and public on April 8, 2026 at NASA’s Johnson Space Center in Houston.
NASA

Countdown To Splashdown

Ground teams are making final preparations for splashdown, expected around 8:07 p.m. (5:07 p.m. PDT) on April 10 off the coast of San Diego.

The re-entry sequence will begin with the separation of Orion’s service module at approximately 7:33 p.m., followed by a final trajectory adjustment at 7:37 p.m. The spacecraft will then execute roll maneuvers and accelerate to nearly 23,864 mph before entering Earth’s atmosphere.

A communications blackout is expected at 7:53 p.m. as plasma builds up around the capsule, lasting about six minutes. During this phase, astronauts may experience forces up to 3.9 Gs.

Infographic displaying the Artemis II Orion parachute sequence. This graphic was presented by Artemis II Flight Director Rick Henfling during the mission status briefing to the media and public on April 8, 2026 at NASA’s Johnson Space Center in Houston.
NASA

Parachute Deployment And Landing

After re-establishing communication, Orion will jettison its forward bay cover and deploy drogue parachutes at around 22,000 feet. Main parachutes will follow at approximately 6,000 feet, slowing the capsule for a safe ocean landing.

Ground track map displaying the Artemis II Orion parachute sequence. This graphic was presented by Artemis II Flight Director Rick Henfling during the mission status briefing to the media and public on April 8, 2026 at NASA’s Johnson Space Center in Houston.
NASA

Recovery And Return To Houston

Within two hours of splashdown, the crew will be retrieved and transported to the USS John P. Murtha via helicopter.

Once aboard, astronauts will undergo initial medical evaluations before returning to shore and boarding a flight to Johnson Space Center in Houston for post-mission debriefing and recovery.

U.S. Navy MH-60 Seahawks from Helicopter Sea Combat Squadron (HSC) 23 are seen arriving on the flight deck of USS John P. Murtha as they prepare to conduct air operations training as NASA, U.S. Navy, and U.S. Air Force teams prepare for the the return of the Artemis II crewmembers to Earth, Monday, April 6, 2026, in the Pacific Ocean off the coast of California. NASA’s Artemis II mission is taking NASA astronauts Reid Wiseman, commander; Victor Glover, pilot; Christina Koch, mission specialist; and CSA (Canadian Space Agency) astronaut Jeremy Hansen, mission specialist on a 10-day journey around the Moon and back aboard their Orion spacecraft. Wiseman, Glover, Koch, and Hansen are scheduled to splash down off the coast of San Diego at approximately 5:07 p.m. PDT (8:07 p.m. EDT) on Friday, April 10.
NASA/Bill Ingalls

 

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Artemis II mission: LUCA and LESA support Artemis safety, success as crew prepares return journey

 

Artemis II mission: LUCA and LESA support Artemis safety, success as crew prepares return journey

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NASA’s Artemis II mission is drawing support from a pair of nearly identical control rooms in Alabama, each playing a distinct role in keeping astronauts safe and operations on track as the crew heads back to Earth, Friday, April 10.

At the National Aeronautics and Space Administration’s Marshall Space Flight Center in Huntsville, two facilities, the Lunar Utilization Control Area (LUCA) and the Lander Engineering Support Area (LESA), are working in tandem during the mission. Both are housed within the Huntsville Operations Support Center, a hub designed to provide real-time technical and scientific support.

Though similar in appearance, the two rooms serve different purposes. LUCA focuses on science operations linked to Artemis, while LESA is geared toward engineering support, particularly for future missions that will land astronauts on the Moon.

LUCA (Lunar Utilization Control Area) at NASA Marshall is specially designed to support a wide variety of science operations on and around the Moon – and beyond. Engineers in the LUCA monitored operations for the Lunar Node-1 experiment, an autonomous navigation payload that was part of the first NASA Commercial Lunar Payload Services (CLPS) launch on Intuitive Machines’ Nova-C lunar lander in 2024. NASA Marshall flight controllers will use the LUCA again for Artemis II to monitor science operations.
NASA/Charles Beason

Officials say the flexibility of the Huntsville center allows it to adapt to evolving mission needs. The facility has previously supported programs including the Commercial Crew Program, the Space Launch System rocket and research aboard the International Space Station.

Teams operating from LUCA are currently supporting science experiments tied to deep space conditions. These include studies examining how microgravity and radiation affect the human body, including immune response and overall performance. Data gathered during Artemis II is expected to shape planning for future crewed missions beyond Earth orbit.

Support engineers will use the LESA (Lander Engineering Support Area) at NASA Marshall to monitor human landing system (HLS) for the first crewed Artemis missions.
NASA/Charles Beason

In parallel, LESA teams are monitoring Artemis II operations in real time, using the mission as a live test case to refine procedures ahead of future lunar landings. Engineers, safety specialists and flight operations experts form part of the Human Landing System Mission Insight Support Team, which will eventually play a central role in supporting lander systems during Moon missions.

The Huntsville Operations Support Center also provides a range of technical services, including spacecraft command and telemetry management, global voice communications, and live and recorded video support. It also deploys specialized software tools that enable seamless data exchange between systems located far apart, allowing teams across different locations to work in sync.

By integrating these capabilities into both LUCA and LESA, NASA enables continuous coordination between engineers, scientists and mission operators worldwide.

Artemis II, which recently carried astronauts around the Moon, is part of NASA’s broader Artemis program aimed at returning humans to the lunar surface. The program is also intended to lay the groundwork for future missions to Mars, with lessons from current flights feeding directly into long-term exploration plans.

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Artemis II Update-22, Day 8: Crew conducts key tests as they begin their return journey

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Artemis II moved into another critical phase of its return journey as the crew began Flight Day 8 with a focus on testing systems and preparing for reentry.