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By NASA
6 min read
Preparations for Next Moonwalk Simulations Underway (and Underwater)
With one of its solar arrays deployed, NASA’s Lunar Trailblazer sits in a clean room at Lockheed Martin Space. The large silver grate attached to the spacecraft is the radiator for HVM³, one of two instruments that the mission will use to better understand the lunar water cycle.Lockheed Martin Space There’s water on the Moon, but scientists only have a general idea of where it is and what form it is in. A trailblazing NASA mission will get some answers.
When NASA’s Lunar Trailblazer begins orbiting the Moon next year, it will help resolve an enduring mystery: Where is the Moon’s water? Scientists have seen signs suggesting it exists even where temperatures soar on the lunar surface, and there’s good reason to believe it can be found as surface ice in permanently shadowed craters, places that have not seen direct sunlight for billions of years. But, so far, there have been few definitive answers, and a full understanding of the nature of the Moon’s water cycle remains stubbornly out of reach.
This is where Lunar Trailblazer comes in. Managed by NASA’s Jet Propulsion Laboratory and led by Caltech in Pasadena, California, the small satellite will map the Moon’s surface water in unprecedented detail to determine the water’s abundance, location, form, and how it changes over time.
“Making high-resolution measurements of the type and amount of lunar water will help us understand the lunar water cycle, and it will provide clues to other questions, like how and when did Earth get its water,” said Bethany Ehlmann, principal investigator for Lunar Trailblazer at Caltech. “But understanding the inventory of lunar water is also important if we are to establish a sustained human and robotic presence on the Moon and beyond.”
Future explorers could process lunar ice to create breathable oxygen or even fuel. And they could also conduct science. Using information from Lunar Trailblazer, future human or robotic scientific investigations could sample the ice for later study to determine where the water came from. For example, the presence of ammonia in ice samples may indicate the water came from comets; sulfur, on the other hand, could show that it was vented to the surface from the lunar interior when the Moon was young and volcanically active.
This artist’s concept depicts NASA’s Lunar Trailblazer in lunar orbit about 60 miles (100 kilometers) from the surface of the Moon. The spacecraft weighs only 440 pounds (200 kilograms) and measures 11.5 feet (3.5 meters) wide when its solar panels are fully deployed.Lockheed Martin Space “In the future, scientists could analyze the ice in the interiors of permanently shadowed craters to learn more about the origins of water on the Moon,” said Rachel Klima, Lunar Trailblazer deputy principal investigator at the Johns Hopkins Applied Physics Laboratory in Laurel, Maryland. “Like an ice core from a glacier on Earth can reveal the ancient history of our planet’s atmospheric composition, this pristine lunar ice could provide clues as to where that water came from and how and when it got there.”
Understanding whether water molecules move freely across the surface of the Moon or are locked inside rock is also scientifically important. Water molecules could move from frosty “cold traps” to other locations throughout the lunar day. Frost heated by the Sun sublimates (turning from solid ice to a gas without going through a liquid phase), allowing the molecules to move as a gas to other cold locations, where they could form new frost as the Sun moves overhead. Knowing how water moves on the Moon could also lead to new insights into the water cycles on other airless bodies, such as asteroids
Two Instruments, One Mission
Two science instruments aboard the spacecraft will help unlock these secrets: the High-resolution Volatiles and Minerals Moon Mapper (HVM3) infrared spectrometer and the Lunar Thermal Mapper (LTM) infrared multispectral imager.
Developed by JPL, HVM3 will detect and map the spectral fingerprints, or wavelengths of reflected sunlight, of minerals and the different forms of water on the lunar surface. The spectrometer can use faint reflected light from the walls of craters to see the floor of even permanently shadowed craters.
The LTM instrument, which was built by the University of Oxford and funded by the UK Space Agency, will map the minerals and thermal properties of the same lunar landscape. Together they will create a picture of the abundance, location, and form of water while also tracking how its distribution changes over time.
“The LTM instrument precisely maps the surface temperature of the Moon while the HVM3 instrument looks for the spectral signature of water molecules,” said Neil Bowles, instrument scientist for LTM at the University of Oxford. “Both instruments will allow us to understand how surface temperature affects water, improving our knowledge of the presence and distribution of these molecules on the Moon.”
Weighing only 440 pounds (200 kilograms) and measuring 11.5 feet (3.5 meters) wide when its solar panels are fully deployed, Lunar Trailblazer will orbit the Moon about 60 miles (100 kilometers) from the surface. The mission was selected by NASA’s SIMPLEx (Small Innovative Missions for Planetary Exploration) program in 2019 and will hitch a ride on the same launch as the Intuitive Machines-2 delivery to the Moon through NASA’s Commercial Lunar Payload Services initiative. Lunar Trailblazer passed a critical operational readiness review in early October at Caltech after completing environmental testing in August at Lockheed Martin Space in Littleton, Colorado, where it was assembled.
The orbiter and its science instruments are now being put through flight system software tests that simulate key aspects of launch, maneuvers, and the science mission while in orbit around the Moon. At the same time, the operations team led by IPAC at Caltech is conducting tests to simulate commanding, communication with NASA’s Deep Space Network, and navigation.
More About Lunar Trailblazer
Lunar Trailblazer is managed by JPL, and its science investigation and mission operations are led by Caltech with the mission operations center at IPAC. Managed for NASA by Caltech, JPL also provides system engineering, mission assurance, the HVM3 instrument, as well as mission design and navigation. Lockheed Martin Space provides the spacecraft, integrates the flight system, and supports operations under contract with Caltech.
SIMPLEx mission investigations are managed by the Planetary Missions Program Office at NASA’s Marshall Space Flight Center in Huntsville, Alabama, as part of the Discovery Program at NASA Headquarters in Washington. The program conducts space science investigations in the Planetary Science Division of NASA’s Science Mission Directorate at NASA Headquarters.
For more information about Lunar Trailblazer, visit:
https://www.jpl.nasa.gov/missions/lunar-trailblazer
News Media Contacts
Karen Fox / Molly Wasser
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Ian J. O’Neill
Jet Propulsion Laboratory, Pasadena, Calif.
818-354-2649
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Gordon Squires
IPAC, Pasadena, Calif.
626-395-3121
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Last Updated Oct 29, 2024 Related Terms
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By NASA
Hubble Space Telescope Home Hubble Captures a New View of… Hubble Space Telescope Hubble Home Overview About Hubble The History of Hubble Hubble Timeline Why Have a Telescope in Space? Hubble by the Numbers At the Museum FAQs Impact & Benefits Hubble’s Impact & Benefits Science Impacts Cultural Impact Technology Benefits Impact on Human Spaceflight Astro Community Impacts Science Hubble Science Science Themes Science Highlights Science Behind Discoveries Hubble’s Partners in Science Universe Uncovered Explore the Night Sky Observatory Hubble Observatory Hubble Design Mission Operations Missions to Hubble Hubble vs Webb Team Hubble Team Career Aspirations Hubble Astronauts News Hubble News Hubble News Archive Social Media Media Resources Multimedia Multimedia Images Videos Sonifications Podcasts E-books Lithographs Fact Sheets Glossary Posters Hubble on the NASA App More Online Activities 2 min read
Hubble Captures a New View of Galaxy M90
This eye-catching image offers us a new view of the spiral galaxy Messier 90 from the NASA/ESA Hubble Space Telescope. ESA/Hubble & NASA, D. Thilker, J This NASA/ESA Hubble Space Telescope image features the striking spiral galaxy Messier 90 (M90, also NGC 4569), located in the constellation Virgo. In 2019, Hubble released an image of M90 created with Wide Field and Planetary Camera 2 (WFPC2) data taken in 1994, soon after its installation. That WFPC2 image has a distinctive stair-step pattern due to the layout of its sensors. Wide Field Camera 3 (WFC3) replaced WFPC2 in 2009 and Hubble used WFC3 when it turned its aperture to Messier 90 again in 2019 and 2023. That data resulted in this stunning new image, providing a much fuller view of the galaxy’s dusty disk, its gaseous halo, and its bright core.
The inner regions of M90’s disk are sites of star formation, seen here in red H-alpha light from nebulae. M90 sits among the galaxies of the relatively nearby Virgo Cluster, and its orbit took M90 on a path near the cluster’s center about three hundred million years ago. The density of gas in the inner cluster weighed on M90 like a strong headwind, stripping enormous quantities of gas from the galaxy and creating the diffuse halo we see around it. This gas is no longer available to form new stars in M90, with the spiral galaxy eventually fading as a result.
M90 is located 55 million light-years from Earth, but it’s one of the very few galaxies getting closer to us. Its orbit through the Virgo cluster has accelerated so much that M90 is in the process of escaping the cluster entirely. By happenstance, it’s moving in our direction. Astronomers have measured other galaxies in the Virgo cluster at similar speeds, but in the opposite direction. As M90 continues to move toward us over billions of years, it will also be evolving into a lenticular galaxy.
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Claire Andreoli
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Last Updated Oct 17, 2024 Editor Andrea Gianopoulos Location NASA Goddard Space Flight Center Related Terms
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Since its 1990 launch, the Hubble Space Telescope has changed our fundamental understanding of the universe.
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This beautiful spiral is expected to evolve into a lenticular galaxy.
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By NASA
4 min read
Preparations for Next Moonwalk Simulations Underway (and Underwater)
Researchers think meltwater beneath Martian ice could support microbial life.
The white material seen within this Martian gully is believed to be dusty water ice. Scientists believe this kind of ice could be an excellent place to look for microbial life on Mars today. This image, showing part of a region called Dao Vallis, was captured by NASA’s Mars Reconnaissance Orbiter in 2009.NASA/JPL-Caltech/University of Arizona These holes, captured on Alaska’s Matanuska Glacier in 2012, are formed by cryoconite — dust particles that melt into the ice over time, eventually forming small pockets of water below the glacier’s surface. Scientists believe similar pockets of water could form within dusty water ice on Mars.Kimberly Casey CC BY-NC-SA 4.0 While actual evidence for life on Mars has never been found, a new NASA study proposes microbes could find a potential home beneath frozen water on the planet’s surface.
Through computer modeling, the study’s authors have shown that the amount of sunlight that can shine through water ice would be enough for photosynthesis to occur in shallow pools of meltwater below the surface of that ice. Similar pools of water that form within ice on Earth have been found to teem with life, including algae, fungi, and microscopic cyanobacteria, all of which derive energy from photosynthesis.
“If we’re trying to find life anywhere in the universe today, Martian ice exposures are probably one of the most accessible places we should be looking,” said the paper’s lead author, Aditya Khuller of NASA’s Jet Propulsion Laboratory in Southern California.
Mars has two kinds of ice: frozen water and frozen carbon dioxide. For their paper, published in Nature Communications Earth & Environment, Khuller and colleagues looked at water ice, large amounts of which formed from snow mixed with dust that fell on the surface during a series of Martian ice ages in the past million years. That ancient snow has since solidified into ice, still peppered with specks of dust.
Although dust particles may obscure light in deeper layers of the ice, they are key to explaining how subsurface pools of water could form within ice when exposed to the Sun: Dark dust absorbs more sunlight than the surrounding ice, potentially causing the ice to warm up and melt up to a few feet below the surface.
The white edges along these gullies in Mars’ Terra Sirenum are believed to be dusty water ice. Scientists think meltwater could form beneath the surface of this kind of ice, providing a place for possible photosynthesis. This is an enhanced-color image; the blue color would not actually be perceptible to the human eye.NASA/JPL-Caltech/University of Arizona Mars scientists are divided about whether ice can actually melt when exposed to the Martian surface. That’s due to the planet’s thin, dry atmosphere, where water ice is believed to sublimate — turn directly into gas — the way dry ice does on Earth. But the atmospheric effects that make melting difficult on the Martian surface wouldn’t apply below the surface of a dusty snowpack or glacier.
Thriving Microcosms
On Earth, dust within ice can create what are called cryoconite holes — small cavities that form in ice when particles of windblown dust (called cryoconite) land there, absorb sunlight, and melt farther into the ice each summer. Eventually, as these dust particles travel farther from the Sun’s rays, they stop sinking, but they still generate enough warmth to create a pocket of meltwater around them. The pockets can nourish a thriving ecosystem for simple lifeforms..
“This is a common phenomenon on Earth,” said co-author Phil Christensen of Arizona State University in Tempe, referring to ice melting from within. “Dense snow and ice can melt from the inside out, letting in sunlight that warms it like a greenhouse, rather than melting from the top down.”
Christensen has studied ice on Mars for decades. He leads operations for a heat-sensitive camera called THEMIS (Thermal Emission Imaging System) aboard NASA’s 2001 Mars Odyssey orbiter. In past research, Christensen and Gary Clow of the University of Colorado Boulder used modeling to demonstrate how liquid water could form within dusty snowpack on the Red Planet. That work, in turn, provided a foundation for the new paper focused on whether photosynthesis could be possible on Mars.
In 2021, Christensen and Khuller co-authored a paper on the discovery of dusty water ice exposed within gullies on Mars, proposing that many Martian gullies form by erosion caused by the ice melting to form liquid water.
This new paper suggests that dusty ice lets in enough light for photosynthesis to occur as deep as 9 feet (3 meters) below the surface. In this scenario, the upper layers of ice prevent the shallow subsurface pools of water from evaporating while also providing protection from harmful radiation. That’s important, because unlike Earth, Mars lacks a protective magnetic field to shield it from both the Sun and radioactive cosmic ray particles zipping around space.
The study authors say the water ice that would be most likely to form subsurface pools would exist in Mars’ tropics, between 30 degrees and 60 degrees latitude, in both the northern and southern hemispheres.
Khuller next hopes to re-create some of Mars’ dusty ice in a lab to study it up close. Meanwhile, he and other scientists are beginning to map out the most likely spots on Mars to look for shallow meltwater — locations that could be scientific targets for possible human and robotic missions in the future.
News Media Contacts
Andrew Good
Jet Propulsion Laboratory, Pasadena, Calif.
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andrew.c.good@jpl.nasa.gov
Karen Fox / Molly Wasser
NASA Headquarters, Washington
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Last Updated Oct 17, 2024 Related Terms
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By NASA
5 min read
Preparations for Next Moonwalk Simulations Underway (and Underwater)
This artist’s concept depicts a potential volcanic moon between the exoplanet WASP-49 b, left, and its parent star. New evidence indicating that a massive sodium cloud observed near WASP-49 b is produced by neither the planet nor the star has prompted researchers to ask if its origin could be an exomoon.NASA/JPL-Caltech The existence of a moon located outside our solar system has never been confirmed but a new NASA-led study may provide indirect evidence for one.
New research done at NASA’s Jet Propulsion Laboratory reveals potential signs of a rocky, volcanic moon orbiting an exoplanet 635 light-years from Earth. The biggest clue is a sodium cloud that the findings suggest is close to but slightly out of sync with the exoplanet, a Saturn-size gas giant named WASP-49 b, although additional research is needed to confirm the cloud’s behavior. Within our solar system, gas emissions from Jupiter’s volcanic moon Io create a similar phenomenon.
Although no exomoons (moons of planets outside our solar system) have been confirmed, multiple candidates have been identified. It’s likely these planetary companions have gone undetected because they are too small and dim for current telescopes to detect.
The sodium cloud around WASP-49 b was first detected in 2017, catching the attention of Apurva Oza, formerly a postdoctoral researcher at NASA’s Jet Propulsion Laboratory and now a staff scientist at Caltech, which manages JPL. Oza has spent years investigating how exomoons might be detected via their volcanic activity. For example, Io, the most volcanic body in our solar system, constantly spews sulfur dioxide, sodium, potassium, and other gases that can form vast clouds around Jupiter up to 1,000 times the giant planet’s radius. It’s possible that astronomers looking at another star system could detect a gas cloud like Io’s even if the moon itself were too small to see.
Exomoons — moons around planets outside our solar system — are most likely too small to observe directly with current technology. In this video, learn how scientists tracked the motion of a sodium cloud 635 light-years away and found that it could be created by volcanos on a potential exomoon. NASA/JPL-Caltech Both WASP-49 b and its star are composed mostly of hydrogen and helium, with trace amounts of sodium. Neither contains enough sodium to account for the cloud, which appears to be coming from a source that is producing roughly 220,000 pounds (100,000 kilograms) of sodium per second. Even if the star or planet could produce that much sodium, it’s unclear what mechanism could eject it into space.
Could the source be a volcanic exomoon? Oza and his colleagues set out to try to answer that question. The work immediately proved challenging because from such a great distance, the star, planet, and cloud often overlap and occupy the same tiny, faraway point in space. So the team had to watch the system over time.
A Cloud on the Move
As detailed in a new study published in the Astrophysical Journal Letters, they found several pieces of evidence that suggest the cloud is created by a separate body orbiting the planet, though additional research is needed to confirm the cloud’s behavior. For example, twice their observations indicated the cloud suddenly increased in size, as if being refueled, when it was not next to the planet.
New NASA-led research suggests a sodium cloud seen around the exoplanet WASP-49 b might be created by a volcanic moon, which is depicted in this artist’s concept. Jupiter’s fiery moon Io produces a similar cloud. NASA/JPL-Caltech They also observed the cloud moving faster than the planet in a way that would seem impossible unless it was being generated by another body moving independent of, and faster, than the planet.
“We think this is a really critical piece of evidence,” said Oza. “The cloud is moving in the opposite direction that physics tells us it should be going if it were part of the planet’s atmosphere.”
While these observations have intrigued the research team, they say they would need to observe the system for longer to be sure of the cloud’s orbit and structure.
A Chance of Volcanic Clouds
For part of their sleuthing, the researchers used the European Southern Observatory’s Very Large Telescope in Chile. Oza’s co-author Julia Seidel, a research fellow at the observatory, established that the cloud is located high above the planet’s atmosphere, much like the cloud of gas Io produces around Jupiter.
They also used a computer model to illustrate the exomoon scenario and compare it to the data. The exoplanet WASP-49 b orbits the star every 2.8 days with clocklike regularity, but the cloud appeared and disappeared behind the star or behind the planet at seemingly irregular intervals. Using their model, Oza and team showed that a moon with an eight-hour orbit around the planet could explain the cloud’s motion and activity, including the way it sometimes seemed to move in front of the planet and did not seem to be associated with a particular region of the planet.
“The evidence is very compelling that something other than the planet and star are producing this cloud,” said Rosaly Lopes, a planetary geologist at JPL who co-authored the study with Oza. “Detecting an exomoon would be quite extraordinary, and because of Io, we know that a volcanic exomoon is possible.”
A Violent End
On Earth, volcanoes are driven by heat in its core left over from the planet’s formation. Io’s volcanoes, on the other hand, are driven by Jupiter’s gravity, which squeezes the moon as it gets closer to the planet then reduces its “grip” as the moon moves away. This flexing heats the small moon’s interior, leading to a process called tidal volcanism.
If WASP-49 b has a moon similar in size to Earth’s, Oza and team estimate that the rapid loss of mass combined with the squeezing from the planet’s gravity will eventually cause it to disintegrate.
“If there really is a moon there, it will have a very destructive ending,” said Oza.
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Calla Cofield
Jet Propulsion Laboratory, Pasadena, Calif.
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Last Updated Oct 10, 2024 Related Terms
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By NASA
X-ray: NASA/CXC/Queen’s Univ. Belfast/M. Nicholl et al.; Optical/IR: PanSTARRS, NSF/Legacy Survey/SDSS; Illustration: Soheb Mandhai / The Astro Phoenix; Image Processing: NASA/CXC/SAO/N. Wolk NASA’s Chandra X-ray Observatory and other telescopes have identified a supermassive black hole that has torn apart one star and is now using that stellar wreckage to pummel another star or smaller black hole, as described in our latest press release. This research helps connect two cosmic mysteries and provides information about the environment around some of the bigger types of black holes.
This artist’s illustration shows a disk of material (red, orange, and yellow) that was created after a supermassive black hole (depicted on the right) tore apart a star through intense tidal forces. Over the course of a few years, this disk expanded outward until it intersected with another object — either a star or a small black hole — that is also in orbit around the giant black hole. Each time this object crashes into the disk, it sends out a burst of X-rays detected by Chandra. The inset shows Chandra data (purple) and an optical image of the source from Pan-STARRS (red, green, and blue).
In 2019, an optical telescope in California noticed a burst of light that astronomers later categorized as a “tidal disruption event”, or TDE. These are cases where black holes tear stars apart if they get too close through their powerful tidal forces. Astronomers gave this TDE the name of AT2019qiz.
Meanwhile, scientists were also tracking instances of another type of cosmic phenomena occasionally observed across the Universe. These were brief and regular bursts of X-rays that were near supermassive black holes. Astronomers named these events “quasi-periodic eruptions,” or QPEs.
This latest study gives scientists evidence that TDEs and QPEs are likely connected. The researchers think that QPEs arise when an object smashes into the disk left behind after the TDE. While there may be other explanations, the authors of the study propose this is the source of at least some QPEs.
In 2023, astronomers used both Chandra and Hubble to simultaneously study the debris left behind after the tidal disruption had ended. The Chandra data were obtained during three different observations, each separated by about 4 to 5 hours. The total exposure of about 14 hours of Chandra time revealed only a weak signal in the first and last chunk, but a very strong signal in the middle observation.
From there, the researchers used NASA’s Neutron Star Interior Composition Explorer (NICER) to look frequently at AT2019qiz for repeated X-ray bursts. The NICER data showed that AT2019qiz erupts roughly every 48 hours. Observations from NASA’s Neil Gehrels Swift Observatory and India’s AstroSat telescope cemented the finding.
The ultraviolet data from Hubble, obtained at the same time as the Chandra observations, allowed the scientists to determine the size of the disk around the supermassive black hole. They found that the disk had become large enough that if any object was orbiting the black hole and took about a week or less to complete an orbit, it would collide with the disk and cause eruptions.
This result has implications for searching for more quasi-periodic eruptions associated with tidal disruptions. Finding more of these would allow astronomers to measure the prevalence and distances of objects in close orbits around supermassive black holes. Some of these may be excellent targets for the planned future gravitational wave observatories.
The paper describing these results appears in the October 9, 2024 issue of the journal Nature. The first author of the paper is Matt Nicholl (Queen’s University Belfast in Ireland) and the full list of authors can be found in the paper, which is available online at: https://arxiv.org/abs/2409.02181
NASA’s Marshall Space Flight Center manages the Chandra program. The Smithsonian Astrophysical Observatory’s Chandra X-ray Center controls science operations from Cambridge, Massachusetts, and flight operations from Burlington, Massachusetts.
Read more from NASA’s Chandra X-ray Observatory.
Learn more about the Chandra X-ray Observatory and its mission here:
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Visual Description
This release features an artist’s rendering that illustrates the destructive power of a supermassive black hole. The digital image depicts a disk of stellar material surrounding one such black hole. At its outer edge a neighboring star is colliding with and flying through the disk.
The black hole sits halfway down our right edge of the vertical image. It resembles a jet black semicircle with a domed cap of pale blue light. The bottom half of the circular black hole is hidden behind the disk of stellar material. In this illustration, the disk is viewed edge on. It resembles a band of swirling yellow, orange, and red gas, cutting diagonally from our middle right toward our lower left.
Near our lower left, the outer edge of the stellar debris disk overlaps with a bright blue sphere surrounded by luminous white swirls. This sphere represents a neighboring star crashing through the disk. The stellar disk is the wreckage of a destroyed star. An electric blue and white wave shows the hottest gas in the disk.
As the neighboring star crashes through the disk it leaves behind a trail of gas depicted as streaks of fine mist. Bursts of X-rays are released and are detected by Chandra.
Superimposed in the upper left corner of the illustration is an inset box showing a close up image of the source in X-ray and optical light. X-ray light is shown as purple and optical light is white and beige.
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Chandra X-ray Center
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Lane Figueroa
Marshall Space Flight Center, Huntsville, Alabama
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