This Laser Could Find Fossil Microbes on Mars

According to Darwin, life on Earth may have first appeared in warm little ponds. This simple idea is also a cornerstone in our search for the origin of life. The ponds were rich in important chemicals, and when lightning struck, somehow, it all got going.

If the idea is correct, the same thing may have happened on Mars. If it did, and if fossilized evidence of microbes on the planet exists, a new laser could find it.

We may never know exactly how life started. It appeared to start about 4 billion years ago on Earth, confined to water for about 3 billion, until our planet developed a UV-blocking ozone layer.

If life ever appeared on Mars, it also likely occurred billions of years ago when the planet was warm and wet. There’s a strong possibility that it was also confined to water for a long time. If it did, then ancient sediments could hold fossilized evidence of microbes.

NASA’s Perseverance rover landed in Jezero Crater, an ancient paleolake with deep sediments, in an attempt to detect evidence of ancient life. Jezero also contains an ancient river delta, an excellent place for sediments to collect and potentially preserve microbial evidence.

Perseverance carries a laser as part of its Supercam instrument, an improved version of MSL Curiosity’s Chemcam instrument and laser. Supercam analyzes rocks and soils and searches for organic compounds that are biosignatures of ancient microbial life.

Now, scientists are working on a new laser that could detect microbial fossils on Mars. The device will examine gypsum deposits for signs of these fossils. The device has already been tested in Mars-analogue gypsum deposits in Algeria.

The method is explained in new research published in Frontiers in Astronomy and Space Sciences. Its title is “The search for ancient life on Mars using morphological and mass spectrometric analysis: an analog study in detecting microfossils in Messinian gypsum.” The lead author is Youcef Sellam, a PhD student at the Physics Institute at the University of Bern.

“Our findings provide a methodological framework for detecting biosignatures in Martian sulfate minerals, potentially guiding future Mars exploration missions,” said Sellam. “Our laser ablation ionization mass spectrometer, a spaceflight-prototype instrument, can effectively detect biosignatures in sulfate minerals. This technology could be integrated into future Mars rovers or landers for in-situ analysis.”

Sellam is referring to sulphate minerals, including gypsum, left behind when bodies of water dry up. The minerals precipitate out and collect as deposits, as has happened repeatedly in the Mediterranean Sea during the Messinian salinity crisis.

“The Messinian Salinity Crisis occurred when the Mediterranean Sea was cut off from the Atlantic Ocean,” said Sellam. “This led to rapid evaporation, causing the sea to become hypersaline and depositing thick layers of evaporites, including gypsum. These deposits provide an excellent terrestrial analog for Martian sulfate deposits.”

We know something similar happened on Mars because gypsum deposits are plentiful. Since these deposits form rapidly, there’s a chance for fossils to be preserved before they can decompose.

“Gypsum has been widely detected on the Martian surface and is known for its exceptional fossilization potential,” explained Sellam. “It forms rapidly, trapping microorganisms before decomposition occurs, and preserves biological structures and chemical biosignatures.”

Gypsum deposits on Earth have been extensively studied for evidence of microbes.

These images, taken from separate research into gypsum deposits on Earth, show different types of microbial colonization in gypsum deposits. Panels B and C, for example, show zones rich in algal cells. More info here. Image Credit: Jehlicka et al. 2025.

“Prokaryotic communities are often found dwelling within modern evaporites, such as gypsum, forming in sabkhas, lacustrine, and marine terrestrial sediments,” the authors explain in their paper. “They mainly participate in carbon, iron, sulphur, and phosphate biogeochemical cycles, extracting water and using various survival strategies to avoid ecological stresses. Consequently, investigating these fossil filaments may enhance our comprehension of the cryptic conditions that led to the formation of the Primary Lower Gypsum unit during the Messinian Salinity Crisis, the biosignature preservation potential of gypsum, and the possible preservation of such fossils in ancient, hydrated sulphate deposits on Mars.”

Detecting evidence in Earth’s gypsum deposits is relatively simple. However, doing it on Mars is rife with challenges. Since scientists already know that Mediterranean gypsum deposits hold evidence of life, Sellam went to test the method there.

Sellam and his co-researchers tested their method at the Sidi Boutbal (SB) quarry in the Lower Chelif basin in Algeria. “The Chelif Basin is one of the largest Messinian peripheral sub-basins, characterized by an elongated and ENE–WSW oriented structure spanning over 260 km in length and 35 km in width,” the authors explain in their paper. The quarry contains gypsum deposits that are tens of meters thick.

These figures from the research show gypsum deposits in the Mediterranean, including the Sidi Boutbal quarry in Algeria, where the researchers tested their method. The black stars in C, D, and E show the sampled gypsum unit. Image Credit: Sellam et al. 2025.

The researchers used several methods in their work, including optical microscopy, scanning electron microscopy with energy-dispersive X-ray spectroscopy, and spatially resolved laser ablation mass spectrometry (LIMS). These aren’t new technologies, but combining them into an instrument that can be carried by a rover is new.

In their tests in Algeria, the researchers used a miniature laser-powered mass spectrometer, which can analyze the chemical composition of a sample in detail as fine as a micrometre. They also sampled gypsum and analyzed it using the mass spectrometer and an optical microscope. Many natural rock formations can mimic microbial fossils, so they followed criteria to distinguish between potential microbial fossils and natural rock formations. Microbial fossils display morphology which is irregular, sinuous, and potentially hollow.

In their paper, the authors report finding “a densely interwoven network of brownish, sinuous, and curved fossil filaments of various sizes.”

A is an optical microscope image of permineralized filamentous microfossils, and G is a scanning electron microscope of the same microfossils. Image Credit: Sellam et al. 2025.

Their method also detects the presence of chemical elements necessary for life, carbonaceous material, and minerals like clay or dolomite, which can be influenced by the presence of bacteria. “The inner layer of the filament is morphologically and compositionally distinct from the gypsum, mainly composed of Ca, S, O, and traces of Si,” the authors write.

This is a Scanning Electron Microscope and Energy Dispersive X-ray (SEM-EDX) spectrum of the same area. Red shows the predominant mineral, blue shows clay minerals, and yellow shows the inner layer of the fossil filaments. Image Credit: Sellam et al. 2025.

The authors found not only fossil filaments, but also dolomite, clay minerals, and pyrite surrounding the gypsum they were embedded in. This is important because their presence signals the presence of organic life. Prokaryotes supply elements that clays need to form and also help dolomite form, which often forms in the presence of gypsum. The only way that dolomite can form without life present is under high pressures and temperatures. To scientists’ knowledge, those conditions weren’t present on early Mars.

This is interesting progress, but there’s still lots of work to do.

It starts with identifying clay and dolomite in Martian gypsum. Along with other biosignatures, this indicates that fossilized life is there. If the system can identify other chemical minerals, that would help, too. Ultimately, finding organically formed filaments at the same time would be solid evidence that the planet once supported life.

“While our findings strongly support the biogenicity of the fossil filament in gypsum, distinguishing true biosignatures from abiotic mineral formations remains a challenge,” cautioned Sellam. “An additional independent detection method would improve the confidence in life detection. Additionally, Mars has unique environmental conditions, which could affect biosignature preservation over geological periods. Further studies are needed.”

If this method proves to be reliable, it’ll have to wait a while before being implemented.

The ESA’s Rosalind Franklin rover will launch to Mars in 2028. It will look for subsurface chemical and morphological evidence of life. Its instruments have already been chosen. Other nations and agencies have missions to Mars in the planning and proposal stages, but none of them are full-featured rovers like Curiosity and Perseverance.

However, another rover mission to Mars in the future is almost a certainty. Maybe this technology will be ready to go by then.

“Although the Messinian Salinity Crisis, during which the Primary Lower Gypsum formed, remains only partially understood, future astrobiological investigations on Mars should consider hydrated sulphate deposits as promising indicators of ancient Martian environmental conditions. This contribution underscores that hydrated sulphates serve as archives of biological history on Earth and potentially on Mars, should evidence of past life be found,” the authors conclude.

• Press Release: Laser-powered device tested on Earth could help us detect microbial fossils on Mars
• Published Research: The search for ancient life on Mars using morphological and mass spectrometric analysis: an analog study in detecting microfossils in Messinian gypsum

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Can We Develop a More Accurate Habitable Zone Using Sulfur?

The habitable zone of a planetary system is based on a simple idea: if a planet is too close to its star then conditions are too hot for life, and if a planet is too distant then things are too cold. It’s broadly based on the estimated temperature/distance range for liquid water to exist on a planet’s surface, since life as we know it needs liquid water to exist. The problem with this definition is that it’s too crude to be very useful. For example, both Venus and Mars are at the inner and outer edges of the Sun’s habitable zone, but neither are really habitable. But now that we have observed hundreds of planetary systems, we can start to pin down the zone more accurately. One way to do this is to look at sulfur chemistry.

A new paper in Science Advances looks at how sulfur chemistry can better define the inner border of a star’s habitable zone. The authors note that the key is whether a planet can maintain a surface ocean. Many inner planets are warm enough to have liquid oceans early on but lose those oceans over time. Venus is a good example of this. Early Venus was likely very Earth-like, but the lack of a strong magnetic field and water-rich volcanic activity meant Venus’s early oceans boiled away.

Even from light-years away, the difference between Venus and Earth is striking. If alien astronomers were to observe the atmospheres of both, they would see that Earth has a mix of nitrogen and oxygen, while Venus has a mostly carbon dioxide atmosphere rich in sulfur dioxide. From this, they would know that Earth has oceans while Venus does not. Both planets have plenty of sulfur, but Earth’s oceans prevent large amounts of sulfur dioxide from forming. It takes dry surface chemistry to create sulfur dioxide.

The authors show how the presence of atmospheric sulfur is a marker for an oceanless planet. For sunlike stars, this could be used to narrow the habitable zone and select better candidates for alien life. If an inner planet has a sulfur-rich atmosphere, there’s no need to look further. There is, however, a catch.

While dry, warm planets would tend to generate plenty of sulfur compounds, ultraviolet light tends to break these molecules up. So, the team demonstrates, while the presence of atmospheric sulfur proves a planet is dry, the opposite is not always true. A dry planet orbiting a high-UV star would also lack sulfur compounds. To demonstrate this, the team looked at the red dwarf system TRAPPIST-1, which has at least three potentially habitable planets. They found that the UV levels for these worlds are too high to use the sulfur test. This is a real bummer, since red dwarf planets are the most common home for potentially habitable worlds, and most of those planets are bathed in much more UV than Earth since they orbit their star so closely.

So this study shows that sulfur chemistry is a useful tool for finding life, though not as useful as we’d like. It will take more chemical identifiers to narrow down the habitable zones for red dwarfs.

Reference: Jordan, Sean, Oliver Shorttle, and Paul B. Rimmer. “Tracing the inner edge of the habitable zone with sulfur chemistry.” Science Advances 11.5 (2025): eadp8105.

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A Hybrid Hydrogen Drive Train Could Eliminate Aircraft Emissions

Air travel produces around 2.5% of all global CO2 emissions, and despite decades of effort in developing alternative fuels or more efficient aircraft designs, that number hasn’t budged much. However, NASA, also the US’s Aeronautics administration, has kept plugging away at trying to build a more sustainable future for air travel. Recently, they supported another step in that direction by providing an Institute for Advanced Concepts (NIAC) grant to Phillip Ansell of the University of Illinois Urbana-Champaign to develop a hybrid hydrogen-based aircraft engine.

The grant focuses on developing the Hydrogen Hybrid Power for Aviation Sustainable Systems (Hy2PASS) engine, a hybrid engine that uses a fuel cell and a gas turbine to power an aircraft. Hybrid systems have been tried before, but Hy2PASS’s secret sauce is its use of air handling.

In hybrid aircraft systems, there’s typically a fuel cell and a gas turbine. The fuel cell takes hydrogen as an input and creates electrical energy as output. In a typical hybrid system, this electrical energy would power a compressor, whose output was directly coupled to turning the turbine. However, in Hy2PASS, the compressor itself is decoupled from the turbine, though it still supplies oxygen to it. It then also supplies oxygen to the fuel cell’s cathode, allowing for its continued operation.

AI generated video on the Hy2PASS system.

This method has a few advantages, but the most significant one is the dramatic increase in efficiency it allows. The waste heat created at that mechanical connection is eliminated by uncoupling the compressor directly from the turbine. Also, it allows the compressor to be run at different pressures, allowing an algorithm to optimize its speed while ignoring the necessary speed of the turbine.

Additionally, the emissions from the entire system are essentially just water. So, this hybrid system effectively eliminates the emissions created by this kind of hybrid engine altogether. So, in theory, at least, this type of propulsion system would be the holy grail that NASA and the rest of the aviation industry have been seeking for years.

There’s still a long way to go to make this system a reality. The Phase I NIAC grant will focus on proving the system’s concept. Importantly, it will also require an understanding of another aircraft system and “mission trajectory optimization” to minimize the energy requirements of any future use case for the system. That sounds like there would be some limitations for how the system might be used in practice, though fleshing that out as part of Phase I seems a reasonable use case.

Interview with Dr. Ansell, the PI on the Hy2PASS project.

If the project is successful, and given Dr. Ansell’s track record of consistently meeting NASA design objectives, that seems a good bet. It is possible that someday soon, a hydrogen-powered aircraft could be in the air again. And this time, it will be a key player in eliminating emissions from one of the most important industries in the world.

Learn More:
NASA – Hydrogen Hybrid Power for Aviation Sustainable Systems (Hy2PASS)
UT – Multimode Propulsion Could Revolutionize How We Launch Things to Space
UT – Reaction Engines Goes Into Bankruptcy, Taking the Hypersonic SABRE Engine With it
UT – NASA is Working on Electric Airplanes

Lead Image:
Artist’s concept of the Hy2PASS engine
Credit – NASA / Phillip Ansell

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China’s Tianwen-2 Is About to Launch. Here’s What We Know About Its Target Kamo’oalewa

Researchers study enigmatic asteroid Kamo’oalewa, as China’s first asteroid sample return mission moves toward launch.

China is about to get in to the asteroid sample return game. The CNSA (China National Space Administration) has recently announced that its Tianwen-2 mission has arrived at the Xichang Space Center. The mission will launch this May, on a Long March 3B rocket with the agency’s first solar system exploration mission of the year.

The mission was originally named ZhengHe, after a 15^th century explorer. Tianwen-2 is a follow-on to China’s Tianwen-1, the nation’s first successful Mars orbiter-lander mission. Set to launch this coming May, Tianwen-2 will perform an ambitious first: not only will it explore asteroid 469219 Kamo’oalewa, but it will head onward to Comet 311P/PanSTARRS, in a first-ever asteroid-comet exploration mission for the agency.

A Tantalizing Worldlet

Certainly, asteroid Kamo’oalewa is an intriguing space rock. An Apollo Group Near Earth Asteroid, Kamo’oalewa is a rare quasi-satellite of the Earth. Discovered on the night of April 27^th, 2016 from the Haleakala Observatory, the asteroid received the provisional designation 2016 HO3. The formal name means ‘oscillating fragment’ in the Hawaiian language. The asteroid currently fluctuates from being a quasi-satellite and horseshoe orbit between the Sun-Earth L1-L2 and L4-L5 Lagrange points, respectively. One day—perhaps a 100 million of years or so in the future—Kamo’oalewa may ultimately strike the Earth or the Moon.

A reddish object, Kamo’oalewa is either an S- or L-type asteroid, about 40 to 100-meters in size. The asteroid also bears a striking spectral resemblance to Apollo 14 and Luna 24 soil returns, suggesting it may in fact be ejecta from the impact that formed the Giordano Bruno crater on the Moon. The farside crater is thought to be about 4 million years old.

Giordano Bruno crater on the lunar farside. Credit: NASA/LRO

Following Asteroid Kamo’alewa

A recent study out of the European Space Agency’s Near-Earth Objects Coordination Centre (NEOCC) entitled Astrometry, Orbit Determination and Thermal Inertia of the Tianwen-2 Target Asteroid (469219) Kamo’oalewa is looking to better understand the tiny world ahead of the mission’s arrival. Specifically, the study looks to refine the orbit of the asteroid, and understand how the Yarkovsky and YORP (Yarkovsky-O’Keefe-Radzievskii-Paddack) effects act on the orbit and rotation of the asteroid over time. The Yarovsky Effect is the result of how sunlight alters the path of small asteroids over time, as they absorb solar energy and re-emit it as heat. YORP is a similar phenomena, but includes the scattering of sunlight due to the shape and surface structure of the asteroid. Kamo’oalewa is a fast rotator, spinning on its axis once every 27 minutes. This will add to the challenge of grabbing a sample.

“We observed Kamo’oalewa and precisely measured its position in the sky,” lead researcher on the study Marco Fenucci (ESA/ESRIN/NEO Coordination Centre) told Universe Today. “Thanks to these new measurements, we were able to determine the Yarkovsky effect with a signal-to-noise ratio of 14, and the overall accuracy of the orbit was improved.”

Our best view yet of asteroid Kamo’oalewa. Credit: ESA/NEOCC/Loiano Astronomical Station

The study used current observations from the Calar Alto Observatory in Spain and Loiano Astronomical Station based in Italy, as well as pre-discovery observations found in the Sloan Digital Sky Survey (SDSS) from 2004. These were especially challenging for the team to incorporate, as SDSS used a unique drift scan method to complete images. Also, an NEO asteroid like Kamo’oalewa has a relatively fast proper motion against the starry background. These two factors presented a challenge to pinning the asteroid’s time and location down in earlier images.

An Enigmatic World

“Thanks to the accurate measurement of the Yarkovsky effect on Kamo’oalewa, we were able to estimate the surface thermal inertia,” says Fenucci. “Our best estimate indicates that the thermal inertia is smaller than that of Bennu and Ryugu (the target for JAXA’s Hayabusa2 mission). A low value of thermal inertia is usually due to the presence of regolith on the surface of the asteroid. The presence of regolith was not expected on such fast rotators.”

Certainly, the tiny world is worthy of further scrutiny. Any information will be handy leading up the Tianwen-2’s arrival. Like NASA’s OSIRIS-REx, which sampled asteroid 101955 Bennu in 2020, Tianwen-2 will use a touch-and-go sample technique, in addition to an anchor-and-attach method to acquire its samples of asteroid Kamo’oalewa.

“Kamo’oalewa will be the smallest asteroid visited by a spacecraft, and also the one with the shortest rotation period,” says Fenucci. “In terms of composition, the spectrum is similar to that of S-type asteroids, for example, Itokawa or Eros.” The reddish aspect of the asteroid in the visible-to-near infrared part of the spectrum, however, remains a mystery. “This is a typical feature of lunar regolith,” says Fenucci. “However, this particular feature can also be caused by space weathering. The Tianwen-2 mission should give an answer to the question of the origin of Kamo’oalewa.”

Tianwen-2 Mission Timeline

Currently rendezvous with the asteroid is set for 2026, with a departure in 2027. The CNSA team hopes to nab about 100 grams of Kamo’oalewa, about the mass of medium-sized apple. After that, the mission will dispatch its return capsule on Earth flyby in late 2027. Then, it will head onward to explore periodic comet 311/P PanSTARRS. The mission will reach the comet in 2034.

The Tianwen-2 spacecraft to carry out a sample-return targeting near-Earth asteroid 469219 Kamo?oalewa has arrived at Xichang spaceport. Launch date not revealed, but expected around May. english.news.cn/20250220/d95…

[image or embed]

— Andrew Jones (@andrewjonesspace.bsky.social) February 20, 2025 at 6:08 AM

China has certainly taken a prudent, incremental path to space exploration. CNSA’s Chang’e program has returned samples of the lunar near and far side. Tianwen-1 was successful at Mars, scoring a combination orbiter, lander and rover on the Red Planet, all in one mission. China also has long term plans to combine these proven techniques in a Mars sample return mission of their own. This could launch as early as 2028.

It will be exciting to see asteroid Kamo’oalewa up close, as Tianwen-2 attempts to unravel the origin story for this elusive world.

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One of the Most Massive Black Holes in the Universe Lurks at the Center of the Cosmic Horsehoe

In 2007, astronomers discovered the Cosmic Horseshoe, a gravitationally lensed system of galaxies about five-and-a-half billion light-years away. The foreground galaxy’s mass magnifies and distorts the image of a distant background galaxy whose light has travelled for billions of years before reaching us. The foreground and background galaxies are in such perfect alignment that they create an Einstein Ring.

New research into the Cosmic Horseshoe reveals the presence of an Ultra-Massive Black Hole (UMBH) in the foreground galaxy with a staggering 36 billion solar masses.

There’s no strict definition of a UMBH, but the term is often used to describe a supermassive black hole (SMBH) with more than 5 billion solar masses. SMBHs weren’t “discovered” in the traditional sense of the word. Rather, over time, their existence became clear. Also, over time, more and more massive ones were measured. There’s a growing need for a name for the most massive ones, and that’s how the term “Ultra-Massive Black Hole” originated.

The discovery of the enormously massive black hole in the Cosmic Horseshoe is presented in new research. It’s titled “Unveiling a 36 Billion Solar Mass Black Hole at the Centre of the Cosmic
Horseshoe Gravitational Lens,” and the lead author is Carlos Melo-Carneiro from the Instituto de Física, Universidade Federal do Rio Grande do Sul in Brazil. The paper is available at arxiv.org.

There was a revolution in physics in the late 19th/early 20th century as relativity superseded Newtonian physics and propelled our understanding of the Universe to the next level. It became clear that space and time were intertwined rather than separate and that massive objects could warp spacetime. Even light wasn’t immune, and Einstein gave the idea of black holes—which dated back to John Michell’s ‘dark stars’—a coherent mathematical foundation. In 1936, Einstein predicted gravitational lensing, though he didn’t live long enough to enjoy the visual proof we enjoy today.

Now, we know of thousands of gravitational lenses, and they’ve become one of astronomers’ naturally occurring tools. They exist because of their enormous black holes.

The lensing foreground galaxy in the Cosmic Horseshoe is named LRG 3-757. It’s a particular type of rare galaxy called a Luminous Red Galaxy (LRG), which are extremely bright in infrared. LRG 3-757 is also extremely massive, about 100 times more massive than the Milky Way and is one of the most massive galaxies ever observed. Now we know that one of the most massive black holes ever detected occupies the center of this enormous galaxy.

“Supermassive black holes (SMBHs) are found at the centre of every massive galaxy, with their masses tightly connected to their host galaxies through a co-evolution over cosmic time,” the authors write in their paper.

Astronomers don’t find stellar-mass black holes at the heart of massive galaxies and they don’t find SMBHs at the heart of dwarf galaxies. There’s an established link between SMBHs and their host galaxies, especially massive ellipticals like LRG 3-757. This study strengthens that link.

The research focuses on what’s called the MBH-sigma_e Relation. It’s the relationship between an SMBH’s mass and the velocity dispersion of the stars in the galactic bulge. Velocity dispersion (sigma_e) is a measurement of the speed of the stars and how much they vary around the average speed. The higher the velocity dispersion, the faster and more randomly the stars move.

When astronomers examine galaxies, they find that the more massive the SMBH, the greater the velocity dispersion. The relationship suggests a deep link between the evolution of galaxies and the growth of SMBHs. The correlation between an SMBH’s mass and its galaxy’s velocity dispersion is so tight that astronomers can get a good estimate of the SMBH’s mass by measuring the velocity dispersion.

However, the UMBH in the Cosmic Horseshoe is more massive than the MBH-sigma e Relation suggests.

“It is expected that the most massive galaxies in the Universe, such as brightest cluster galaxies (BCGs), host the most massive SMBHs,” the authors write. Astronomers have found many UMBHs in these galaxies, including LRG 3-757. “Nonetheless, the significance of these UMBHs lies in the fact that
many of them deviate from the standard linear MBH?sigma_e relation” the researchers explain.

LRG 3-757 deviates significantly from the correlation. “Our findings place the Cosmic Horseshoe ~1.5 sigma above the MBH?sigma_e relation, supporting an emerging trend observed in BGCs and other massive galaxies,” the authors write. “This suggests a steeper MBH?sigma_e relationship at the highest masses, potentially driven by a different co-evolution of SMBHs and their host galaxies.”

This figure from the research shows the relationship between the SMBH mass and the host effective
velocity dispersion. The black solid line represents the relation from previous research in 2016, with dashed and dotted lines showing the 1 sigma and 3 sigma scatter, respectively. Horseshoe is labelled and clearly deviates from established relationship. The other galaxies labelled nearby also contain UMBHs that deviate significantly. Image Credit: Melo-Carneiro et al. 2025.

What’s behind this decoupling of the MBH?sigma_e relation in massive galaxies? Some stars might have been removed from the galaxy in past mergers, affecting the velocity dispersion.

LRG 3-757 could be part of a fossil group, according to the authors. “The lens of the Horseshoe is unique in that is at ? = 0.44 and that has no comparably massive companion galaxies — it is likely a fossil group,” they write.

Fossil groups are large galaxy groups that feature extremely large galaxies in their centers, often LRGs. Fossil groups and LRGs represent a late stage of evolution in galaxies where activity has slowed. Few stars form in LRGs so they’re “red and dead.” There’s also little to no interaction between galaxies.

“Fossil groups, as remnants of early galaxy mergers, may follow distinct evolutionary pathways compared to local galaxies, potentially explaining the high BH mass,” the authors write.

LRG 3-757 could’ve experienced what’s called “scouring.” Scouring can occur when two extremely massive galaxies merge and affects the velocity dispersion of stars in the galaxy’s center. “In this process, the
binary SMBHs dynamically expel stars from the central regions of the merged galaxy, effectively reducing the stellar velocity dispersion while leaving the SMBH mass largely unchanged,” the authors explain.

Another possibility is black hole/AGN feedback. When black holes are actively feeding they’re called Active Galactic Nuclei. Powerful jets and outflows from AGN can quench star formation and possibly alter the central structure of the galaxy. That could decouple the growth of the SMBH from the velocity dispersion.

Artist view of an active supermassive black hole and its powerful jets. Image Credit: ESO/L. Calçada

“A third scenario posits that such UMBH could be remnants of extremely luminous quasars, which experienced rapid SMBH accretion episodes in the early Universe,” the authors write.

The researchers say that more observations and better models are needed “to explain the scatter in the ?BH ? sigma e relation at its upper end.”

More observations are on the way thanks to the Euclid mission. “The Euclid mission is expected to discover hundreds of thousands of lenses over the next five years,” the authors write in their conclusion. The Extremely Large Telescope (ELT) will also contribute by allowing more detailed dynamical studies of the velocity dispersion.

“This new era of discovery promises to deepen our understanding of galaxy evolution and the interplay between baryonic and DM components,” the authors conclude.

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Glaciers Worldwide are Melting Faster Causing Sea Levels to Rise More

Anthropogenic climate change is creating a vicious circle where rising temperatures are causing glaciers to melt at an increasing rate. In addition to contributing to rising sea levels, coastal flooding, and extreme weather, the loss of polar ice and glaciers is causing Earth’s oceans to absorb more solar radiation. The loss of glaciers is also depleting regional freshwater resources, leading to elevated levels of drought and the risk of famine. According to new findings by an international research effort, there has been an alarming increase in the rate of glacier loss over the last ten years.

The research was conducted by the Glacier Mass Balance Intercomparison Exercise (GlaMBIE) team, a major research initiative coordinated by the World Glacier Monitoring Service (WGMS). Located at the University of Zurich in collaboration with the University of Edinburgh and Earthwave Ltd, this international data repository and data analyzing service generates community estimates of glacier mass loss globally. The paper that details their research and findings, “Community estimate of global glacier mass changes from 2000 to 2023,” was published on February 19th in the journal Nature.

As part of their efforts, the team coordinated the compilation, standardization, and analysis of field measurements and data from optical, radar, laser, and gravimetry satellite missions. These include satellite observations from NASA’s Terra Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) and Ice, Cloud, and Land Elevation Satellite-2 (ICESat-2), the NASA-DLR Gravity Recovery and Climate Experiment (Grace), the GLR’s TanDEM-X mission, and the ESA’s CryoSat missions, and more.

Combining data from multiple sources, the Glambie team produced an annual time series of global glacier loss from 2000 to 2023. In 2000, glaciers covered about 705,221 square km (272,287 mi2) and held an estimated 121,728 billion metric tons (134,182 US tons) of ice. Over the next twenty years, they lost 273 billion tonnes of ice annually, approximately 5% of their total volume, with regional losses ranging from 2% in the Antarctic and Subantarctic to 39% in Central Europe. To put that in perspective, this amounts to what the entire global population consumes in 30 years.

In short, the amount of ice lost rose to 36% during the second half of the study (2012 and 2023) compared to the first half (2000-2011). Glacier mass loss over the whole study period was 18% higher than the meltwater from the Greenland Ice Sheet and more than double that from the Antarctic Ice Sheet. Michael Zemp, a noted glaciologist who co-led the study, said in an ESA press release:

“We compiled 233 estimates of regional glacier mass change from about 450 data contributors organized in 35 research teams. Benefiting from the different observation methods, Glambie not only provides new insights into regional trends and year-to-year variability, but we could also identify differences among observation methods. This means that we can provide a new observational baseline for future studies on the impact of glacier melt on regional water availability and global sea-level rise.”

This photograph, taken in 2012, shows the Golubin Glacier in Kyrgyzstan, in Central Asia. Credit: M. Hoelzle (2012)

Globally, glaciers collectively lost 6,542 tonnes (7,210 tons) of ice, leading to a global sea-level rise of 18 mm (0.7 inches). However, the rate of glacier ice loss increased significantly from 231 billion tonnes per year in the first half of the study period to 314 billion tonnes per year in the second half – an increase of 36%. This rise in water loss has made glaciers the second-largest contributor to global sea-level rise, surpassing the contributions of the Greenland Ice Sheet, Antarctic Ice Sheet, and changes in land water storage. Said UZH glaciologist Inés Dussaillant, who was involved in the Glambie analyses:

“Glaciers are vital freshwater resources, especially for local communities in Central Asia and the Central Andes, where glaciers dominate runoff during warm and dry seasons. But when it comes to sea-level rise, the Arctic and Antarctic regions, with their much larger glacier areas, are the key players. However, almost Thione-quarter of the glacier contribution to sea-level rise originates from Alaska.”

These results will provide environmental scientists with a refined baseline for interpreting observational differences arising from different methods and for calibrating models. They hope this will help future studies of global ice loss by narrowing the projection uncertainties for the twenty-first century. These research findings are the culmination of many years of cooperative studies and observations, which included the use of satellites that were not specifically designed to monitor glaciers globally. As co-author Noel Gourmelen, a lecturer in Earth Observation of the Cryosphere at the University of Edinburgh, said:

“The research is the result of sustained efforts by the community and by space agencies over many years, to exploit a variety of satellites that were not initially specifically designed for the task of monitoring glaciers globally. This legacy is already producing impact with satellite missions being designed to allow operational monitoring of future glacier evolution, such as Europe’s Copernicus CRISTAL mission which builds on the legacy of ESA’s CryoSat.”

The study also marks an important milestone since it was released in time for the United Nations’ International Year of Glaciers’ Preservation and the Decade of Action for Cryospheric Sciences (2025–2034). Said Livia Jakob, the Chief Scientific Officer & Co-Founder at Earthwave, hosted a large workshop with all the participants to discuss the findings. “Bringing together so many different research teams from across the globe in a joint effort to increase our understanding and certainty of glacier ice loss has been extremely valuable. This initiative has also fostered a stronger sense of collaboration within the community.”

The study also illustrates the importance of collective action on climate change, which is accelerating at an alarming rate. Research that quantifies glacial loss, rising sea levels, and other impacts is key to preparing for the worst. It’s also essential to the development of proper adaptation, mitigation, and restoration strategies consistent with the recommendations made by the UN Intergovernmental Panel on Climate Change (IPCC).

Further Reading: ESA

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A Chinese Satellite Tests Orbital Refuelling

Satellites often face a disappointing end: despite having fully working systems, they are often de-orbited after their propellant runs out. However, a breakthrough is on the cards with the launch of China’s Shijian-25 satellite which has been launched into orbit to test orbital refuelling operations. The plan; docking with satellite Beidou-3 G7 and transferring 142 kilograms of hydrazine to extend its life by 8 years! It’s success will mean China plans to develop a network of orbital refuelling stations!

Like cars on Earth, satellites need fuel to manoeuvre and for their constantly decaying orbits to be boosted. But unlike vehicles on the ground, when satellites run out of propellant, they become expensive space debris. This challenge has driven the development of orbital refuelling technology, which could extend satellite lifespans and transform space operations.

An artist’s conception of ERS-2 in orbit. ESA

The International Space Station (ISS) offers one of the most well known examples of an orbiting ‘satellite’ and it too needs to deal with boosting its orbit. The problem is the drag imposed upon the structures by gas in our atmosphere. In the case of the ISS, docked supply craft are typically used to fire their engines to reposition ISS to the correct altitude. Without these periodic “orbital boosts,” the ISS would eventually lose altitude and reenter the atmosphere.

The International Space Station (ISS) in orbit. Credit: NASA

A significant milestone in autonomous refuelling came in 2007 with DARPA’s Orbital Express mission. This demonstration involved two spacecraft: the ASTRO servicing vehicle and a prototype modular satellite called NextSat. Over three months, they performed multiple autonomous fuel transfers and component replacements, proving that robotic spacecraft could conduct complex servicing operations without direct human control.

The technology continues to advance with China’s Shijian-25 satellite (launched on 6 January 2025) representing another step forward in orbital refuelling capabilities. The mission aims to demonstrate refuelling operations in geosynchronous orbit approximately 36,000 kilometres above Earth. This is particularly significant because geosynchronous orbits often host communications satellites that benefit from life extension.

The technical challenges of orbital refuelling are considerable though. Spacecraft must achieve extremely precise rendezvous and docking while travelling in excess of 28,000 kilometres per hour. The fuel transfer system must prevent leaks, which could be hazardous to both spacecraft and create hazardous debris. Adding to the challenge is that many satellites were never designed with refuelling in mind, lacking any form of standardised fuel ports or docking interfaces.

Orange balls of light fly across the sky as debris from a SpaceX rocket launched in Texas is spotted over Turks and Caicos Islands on Jan. 16, in this screen grab obtained from social media video. Credit: Marcus Haworth/Reuters

Looking ahead, several companies and space agencies are developing orbital refuelling systems. These range from dedicated “gas station” satellites to more versatile servicing vehicles that can perform repairs and upgrades alongside refuelling. As the technology advances, it could significantly change how we operate in space, making satellite operations more sustainable and cost-effective.

Source : China successfully sent Shijian-25 satellite

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