Category: 7. Science

  • Cancer immunotherapies linked to increased risk of liver cholestasis

    Cancer immunotherapies linked to increased risk of liver cholestasis

    A global study reveals that cutting-edge cancer immunotherapies, while lifesaving, carry a hidden risk: they may trigger cholestasis, a serious liver condition where bile flow stalls. Analyzing 634 patient reports from global drug-safety databases (FAERS and VigiBase), scientists found immunotherapy patients had a significantly higher risk of cholestasis than chemotherapy recipients. Those under 65 faced greater danger, and women developed symptoms weeks earlier than men (Median 1.17 vs. 1.90 months).

    Anti-PD-1 drugs (e.g., pembrolizumab) and combination therapies posed the highest risk. In mice, combined anti-CTLA-4/anti-PD-L1 drugs caused severe bile duct injury. Molecular analysis linked the condition to disrupted bile acid metabolism and inflammation pathways.

    This isn’t about abandoning immunotherapies-they save lives. But we must monitor liver function aggressively, especially in the first month for women and young adults. Catching cholestasis early prevents irreversible damage.”


    Peng Luo, PhD, senior author of Southern Medical University

    Surprisingly, cholestasis often occurred without classic hepatitis symptoms, suggesting routine liver tests alone may miss it. The team urges adding bile acid level checks to standard monitoring.

    Source:

    Journal reference:

    Yan, X., et al. (2025). Immunotherapy-induced cholestasis in cancer: insights from the two real-world pharmacovigilance databases of FAERS and vigiBase. International Journal of Surgery. doi.org/10.1097/js9.0000000000002607.

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  • Scientists Say Protein Separates Message-Bearing ‘Bubbles’ at Intersection Between Brain Cells, Deepening Understanding of Cognition

    Scientists Say Protein Separates Message-Bearing ‘Bubbles’ at Intersection Between Brain Cells, Deepening Understanding of Cognition

    FOR IMMEIDATE RELEASE

    Newswise — Researchers at Johns Hopkins Medicine say they unexpectedly found new information about a protein’s special role in getting brain cells to communicate at the right time and place in experiments with genetically engineered mice.

    The finding about the protein intersectin, they say, advances scientific understanding of a key process in how the mammalian brain forms memories and learns, and may help advance treatments for cognitive disorders including Down syndrome, Alzheimer’s disease and Huntington’s disease.

    A report of the new findings, funded in part by the National Institutes of Health, was published July 8 in the journal Nature Neuroscience

    Specifically, the researchers found that intersectin keeps tiny, message-carrying bubbles inside brain cells in a particular location until they are ready to be released to activate a neighboring brain cell. The protein does so by creating a physical boundary between these bubbles, similar to how oil separates from water.

    Message transfer from brain cell to brain cell is key to information processing, learning and forming memories. The bubbles, synaptic vesicles, are housed within the synapse — the connection point where brain cells communicate. In typical synapses within the brains of mammals, 300 synaptic vesicles are clustered together in the intersection between any two brain cells, but only a few of these vesicles are used for such message transfer, researchers say. Pinpointing how a synapse knows which vesicles to use has long been a target of research by those who study the biology and chemistry of thought.

    “We found that these tiny bubbles have a distinct domain where they want to be,” says Shigeki Watanabe, Ph.D., associate professor of cell biology at Johns Hopkins Medicine, who led the research. “Keeping them at particular locations within a synapse enables the brain to decide how and when to use them while thinking and processing information.”

    In an effort to better understand the operation of these synaptic vesicles, Watanabe and his team designed a study that first focused on endocytosis, a process in which brain cells recycle synaptic vesicles after they are used for neuronal communication.

    Already aware of intersectin’s general role in endocytosis and neuronal communication, the scientists genetically engineered mice to lack the gene that codes for intersectin. However, and somewhat to their surprise, Watanabe says removing the protein did not appear to halt endocytosis in brain cells.

    The research team refocused their experiments, taking a closer look at the synaptic vesicles themselves.

    Using a high-resolution fluorescence microscope to observe where intersectin is in a synapse, the researchers found it in between vesicles that are used for neuronal communication and those that are not, as if they are physically separating the two.

    To further understand the role of intersectin at this location, they used an electron microscope to visualize synaptic vesicles in action across one billionth of a meter. In all the nerve cells from mice lacking this protein, the scientists say synaptic vesicles close to the membrane were absent from the release zone of the synapse, the place where the bubbles would discharge to nearby neurons.

    “This suggested that intersectin regulates release, rather than recycling, of these vesicles at this location of the synapse,” says Watanabe.

    Using a technique called zap and freeze microscopy, the scientists stimulated neurons in the brains of mice to capture the movement of synaptic vesicles on a millisecond timescale and at a nanometer resolution.

    In normal mice, the scientists saw vesicles fusing with the brain cell membrane within a millisecond after stimulation. Then, new synaptic vesicles came and filled the vacated release sites of the synapse within about 15 milliseconds.

    In two genetically engineered lines of mice, one lacking intersectin and another lacking the endophilin protein, which binds to intersectin, new vesicles could not be recruited to the vacated release sites. Similarly, vesicles within nerve cells of mice with mutations that blocked the interaction of these two proteins also slowed the local replenishment of synaptic vesicles that carry information from neuron to neuron.

    “When information is processed in the brain, this replenishment process needs to happen in just a few milliseconds,” says Watanabe. “When you don’t have vesicles staged and ready to go at the release sites or the active zones, then neurotransmission cannot continue.”  

    In future research, the scientists say they aim to better understand how intersectin shuttles new synaptic vesicles to release sites.

    Funding support for this research was provided by the National Institutes of Health (GM118177, FA95501610052, R01GM136711, S10 OD016374, P50CA098252), the Air Force Research Laboratory, the Defense Advanced Research Projects Agency, the Sol Goldman Pancreatic Cancer Research Center, a Johns Hopkins Discovery Award, the W.W. Smith Charitable Trust Award, the National Science Foundation, the American Heart Association, a Johns Hopkins Albstein Research Scholarship, the Wellcome Trust, the John Fell Fund, La Caixa Foundations, EU-Horizon 2020 MIA-Portugal, Deutsche Forschungsgemeinschaft; the German Center for Neurodegenerative Diseases, the European Research Council, the Human Frontiers Science Organization, the German Dementia Association, and the Guangzhou Elite Project.

    Additional researchers who conducted the study are Tyler Ogunmowo, Chintan Patel, Renee Pepper, Annie Ho, Sumana Raychaudhuri and Brady Maher of Johns Hopkins; Christian Hoffmann, Han Wangfrom and Dragomir Milovanovic from the German Center for Neurodegenerative Diseases, Sindhuja Gowrisankaran and Johanna Idel from the European Neuroscience Institute; Benjamin Cooper from the Max Planck Institute for Multidisciplinary Sciences and Ira Milosevic from the University of Oxford.


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  • Good news for Mars settlers? Red Planet glaciers are mostly pure water ice, study suggests

    Good news for Mars settlers? Red Planet glaciers are mostly pure water ice, study suggests

    Martian glaciers are mostly pure ice across the Red Planet, suggesting they might potentially be useful resources for any explorers that might land there one day, a new study finds.

    For decades, scientists have often seen glaciers coated in dust on the slopes of the mountains of Mars. Previous research suggested these were either glaciers that were comprised mostly of rock and as little as 30% ice, or debris-covered glaciers that were more than 80% ice.

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  • Tricorder Microscope Training During ESA PANGEA 2025

    Tricorder Microscope Training During ESA PANGEA 2025

    ESA astronaut Thomas Pesquet collect a spectra from a rusty rock composed mainly by mafic minerals like olivines and pyroxenes, the same that could characterize the lunar mantleLarger image — ESA

    Editor’s note: Astronaut Thomas Pesquet carries out investigations with the spectrometer associated with the ESA Electronic FieldBook

    A key aspect to understanding a new location during an Away Team Mission is understanding the local atmosphere and mineralogy.

    In the case of examining minerals and life forms in locations such as caves, wells, or other isolated locations, the atmosphere may cary considerably from what is seen on the surface. Having a system that can do in situ analysis can be vital – not only for science but also for crew safety.

    Using a common smartphone platform allows adaptation of this technology by a broader number of users here on Earth by virtue of using a easily obtained smartphone platform.

    Astrobiology, Astrogeology

    Explorers Club Fellow, ex-NASA Space Station Payload manager/space biologist, Away Teams, Journalist, Lapsed climber, Synaesthete, Na’Vi-Jedi-Freman-Buddhist-mix, ASL, Devon Island and Everest Base Camp veteran, (he/him) 🖖🏻

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  • Rainy tropics could face unprecedented droughts as an Atlantic current slows | CU Boulder Today

    Rainy tropics could face unprecedented droughts as an Atlantic current slows | CU Boulder Today

    Some of the rainiest places on Earth could see their annual precipitation nearly halved if climate change continues to alter the way ocean water moves around the globe.

    In a new CU Boulder-led study published July 30 in Nature, scientists revealed that even a modest slowdown of a major Atlantic Ocean current could dry out rainforests, threaten vulnerable ecosystems and upend livelihoods across the tropics.

    “That’s a stunning risk we now understand much better,” said lead author Pedro DiNezio, associate professor in CU Boulder’s Department of Atmospheric and Oceanic Sciences, adding that parts of the Amazon rainforest could see up to a 40% reduction in annual precipitation.

     

    The AMOC makes up half of the global thermohaline circulation, a large, conveyor belt–like ocean current system driven by temperature and salinity. (Credit: Avsa/Wikimedia) 

    The ocean conveyor belt

    The Atlantic Meridional Overturning Circulation (AMOC) is a massive system of ocean currents that moves water through the Atlantic Ocean, transporting warm, salty water from the tropics to the North Atlantic. The AMOC plays an important role in regulating the climate by redistributing heat from the southern to the northern hemisphere. It also makes sure the tropical rain belt, a narrow band of heavy precipitation near the equator, stays north of it.

    As the climate warms, melting polar ice and increasing rainfall will dilute the ocean’s surface waters, making them less dense and potentially slowing down the circulation. The impact of a weakened AMOC on the tropics remains uncertain, because scientists have only been monitoring the system directly for two decades.

    As a technician at a National Oceanic and Atmospheric Administration (NOAA) lab in Miami in 2005, DiNezio helped calibrate some of the earliest measurements of AMOC. At the time, he had no idea that he’d be studying that very same system two decades later.

    “A few years ago, this monitoring system recorded signs of a decline in the AMOC, but it later rebounded. So we weren’t sure if it was just a fluke. The problem is, we haven’t been measuring the ocean long enough to detect meaningful long-term change,” DiNezio said.

    While scientists are uncertain whether the AMOC has already begun to decline, climate models predict the system will eventually weaken because of climate change.

    Predicting the future

    DiNezio and his team set out to explore how a future slowing of these critical ocean currents could impact global precipitation patterns.  

    “Changes in rainfall are very difficult to predict, because so many factors are involved in making rain, like moisture, temperature, wind and clouds. Many models struggle to predict how the pattern will change in a warming world,” DiNezio said.

    The team turned to climate records from about 17,000 years ago, when the AMOC last slowed down significantly due to natural causes. Evidence of precipitation preserved in cave formations, as well as lake and ocean sediments revealed how rainfall patterns responded to the slowdown during that period.

    Drawing on that data, DiNezio’s team identified the computer models that best captured those ancient rainfall shifts and used them to predict how the patterns could change in the future.

    Their best models predict that as the AMOC weakens and cools the northern Atlantic, this temperature drop would spread toward the tropical Atlantic and into the Caribbean. This change, on top of rising global temperatures, will lead to significant reductions in precipitation over Central America, the Amazon, and West Africa.

    “This is bad news, because we have these very important ecosystems in the Amazon,” said DiNezio. The Amazon rainforest contains almost two years of global carbon emissions, making it a major carbon sink on Earth. “Drought in this region could release vast amounts of carbon back into the atmosphere, forming a vicious loop that could make climate change worse.”

    While DiNezio said the AMOC is unlikely to stop completely, even a small reduction in its strength could lead to changes across the entire tropical region, increasing the risk of reaching a tipping point. But how fast and how much it slows depends on the degree of future climate change.

    “We still have time, but we need to rapidly decarbonize the economy and make green technologies widely available to everyone in the world. The best way to get out of a hole is to stop digging,” DiNezio said. 

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  • Effects of Ultraviolet Radiation on Sub-Neptune Exoplanet Hazes Through Laboratory Experiments

    Effects of Ultraviolet Radiation on Sub-Neptune Exoplanet Hazes Through Laboratory Experiments

    Streamlined schematic of the experimental setup, simulated atmospheric compositions and conditions, UV bombardment process, measurements, and experimental outcomes. Two laboratory hazes were produced (the initial conditions varying only in the minor carbon source) in the PHAZER chamber (He et al. 2017) by exposing the gas mixture at room temperature to an AC plasma source. After the hazes were produced, each half of the films were exposed to UV radiation under two different filters. The transmittance and reflectance spectra pre– and post–UV irradiation of both samples were measured using a FTIR spectrometer to quantify molecular changes and destruction during the irradiation process. — astro-ph.EP

    Temperate sub-Neptune exoplanets could contain large inventories of water in various phases, such as water-worlds with water-rich atmospheres or even oceans.

    Both space-based and ground-based observations have shown that many exoplanets likely also contain photochemically-generated hazes. Haze particles are a key source of organic matter and may impact the evolution or origin of life.

    In addition, haze layers could provide a mechanism for lower-atmospheric shielding and ultimately atmospheric retention. Often orbiting close to M-dwarf stars, these planets receive large amounts of radiation, especially during flaring events, which may strip away their atmospheres.

    M-dwarf stars are known to have higher stellar activity than other types of stars, and stellar flares have the potential to accelerate atmospheric escape. In this work, we present results on laboratory investigations of UV radiation effects simulating two different stellar flare energies on laboratory-produced exoplanet hazes made under conditions analogous to water-world atmospheres.

    We find that both simulated flares altered the overall transmittance and reflectance of the hazes, and higher energy “flares” make those alterations more pronounced. On a larger scale, these laboratory-made hazes show potential signs of degradation over the simulated flaring period. Our results provide insight into the effects that stellar flaring events have on potential exoplanet haze composition and the ability for water-world-like exoplanets to retain their atmospheres.

    Lori Huseby, Sarah E. Moran, Neil Pearson, Tiffany Kataria, Chao He, Cara Pesciotta, Sarah M. Hörst, Pierre Haenecour, Travis Barman, Vishnu Reddy, Nikole K. Lewis, Véronique Vuitton

    Comments: 19 pages, 11 figures, Accepted for publication in PSJ
    Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Instrumentation and Methods for Astrophysics (astro-ph.IM)
    Cite as: arXiv:2505.13692 [astro-ph.EP] (or arXiv:2505.13692v1 [astro-ph.EP] for this version)
    https://doi.org/10.48550/arXiv.2505.13692
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    Submission history
    From: Lori Huseby
    [v1] Mon, 19 May 2025 19:51:01 UTC (6,941 KB)
    https://arxiv.org/abs/2505.13692

    Astrobiology,

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  • Huge hidden flood bursts through the Greenland ice sheet surface

    Huge hidden flood bursts through the Greenland ice sheet surface

    Scientists have discovered a previously-undetected flood under the Greenland ice sheet that spilled out with such force that it burst through nearly 300 feet (91 meters) of solid ice.

    The phenomenon occurred in 2014 and caused 24 billion gallons (90 billion liters) of meltwater to punch out from a subglacial lake under the ice sheet. It is the first time such an event has ever been documented in the country.

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  • Requirements For Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory

    Requirements For Joint Orbital Characterization of Cold Giants and Habitable Worlds with Habitable Worlds Observatory

    The phase curve of a planet over one rotation at eight different illumination phases. The images at the right show renderings of the planet’s illuminated surface throughout the observation. Each curve represents a different viewing geometry, the observer-planet-star angle, with the corresponding planetary illumination phase shown by the colored circles in the legend. The top (blue) curve shows a fully illuminated planet, while the lower curves show various partial illumination scenarios down to a completely dark planet (purple). The gray curve represents the classical edge-on viewing case exhibiting the full range of phase variations. — astro-ph.SR

    We determine optimal requirements for the joint detection of habitable-zone planets and cold giant planets with the Habitable Worlds Observatory (HWO).

    Analysis of 164 nearby stars shows that a coronagraph outer working angle (OWA) of 1440 milliarcseconds (mas) is necessary to achieve 80-90% visibility of cold giants. Approximately 40 precursor radial velocity measurements with 1 m/s precision are required to adequately constrain orbital parameters before HWO observations.

    We demonstrate that 6-8 astrometric measurements distributed across the mission timeline, compared to radial velocity constraints alone and to astrometry constraints alone, significantly improve orbital parameter precision, enabling direct determination of orbital inclination with uncertainties of 0.8-3 degrees.

    For habitable-zone planet characterization, 4-5 epochs provide moderate confidence, while high-confidence (95%) confirmation requires 8+ observations.

    These specifications are essential for the comprehensive characterization of planetary system architectures and understanding the potential habitability of terrestrial exoplanets.

    Sabina Sagynbayeva, Asif Abbas, Stephen R. Kane, Eric L. Nielsen, William Thompson, Sarah Blunt, Malena Rice, Jessie L. Christiansen, Caleb K. Harada, Elisabeth R. Newton, Yasuhiro Hasegawa, Philip J. Armitage, Tansu Daylan

    Comments: In review in ApJ
    Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Instrumentation and Methods for Astrophysics (astro-ph.IM); Solar and Stellar Astrophysics (astro-ph.SR)
    Cite as: arXiv:2507.21443 [astro-ph.EP] (or arXiv:2507.21443v1 [astro-ph.EP] for this version)
    https://doi.org/10.48550/arXiv.2507.21443
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    Submission history
    From: Sabina Sagynbayeva
    [v1] Tue, 29 Jul 2025 02:32:25 UTC (13,631 KB)
    https://arxiv.org/abs/2507.21443

    Astrobiology,

    Explorers Club Fellow, ex-NASA Space Station Payload manager/space biologist, Away Teams, Journalist, Lapsed climber, Synaesthete, Na’Vi-Jedi-Freman-Buddhist-mix, ASL, Devon Island and Everest Base Camp veteran, (he/him) 🖖🏻

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  • Mapping Water Ice With Infrared Broadband Photometry

    Mapping Water Ice With Infrared Broadband Photometry

    Positions of the final literature sample of background stars with spectroscopically measured 3 µm optical depths, overlaid on a Planck 857 GHz (350 µm) image of the Milky Way. Different symbols (colors and shapes) indicate the data source, as detailed in Table 1. The sample spans more than 180 deg in Galactic longitude, covering a diverse set of nearby star-forming regions. — astro-ph.GA

    Interstellar ices play a fundamental role in the physical and chemical evolution of molecular clouds and star-forming regions, yet their large-scale distribution and abundance remain challenging to map.

    In this work, I present the ice color excess method, which parametrizes the peak optical depth (τmax3.0) of the prominent 3μm absorption feature, which is predominantly caused by the presence of solid H2O.

    The method builds on well-established near-infrared color excess techniques and uses widely available infrared broadband photometry. Through detailed evaluation of passband combinations and a comprehensive error analysis, I construct the ice color excess metric Λ(W1−I1). This parameter emerges as the optimal choice that minimizes systematic errors while leveraging high-quality, widely available photometry from Spitzer and WISE data archives.

    To calibrate the method, I compile from the literature a sample of stars located in the background of nearby molecular clouds, for which spectroscopically measured optical depths are available. The empirical calibration yields a remarkably tight correlation between τmax3.0 and Λ(W1−I1).

    This photometric technique opens a new avenue for tracing the icy component of the interstellar medium on Galactic scales, providing a powerful complement to spectroscopic surveys and enabling new insights into the environmental dependence of the formation and evolution of icy dust grains.

    Stefan Meingast

    Comments: Accepted for publication in Astronomy & Astrophysics on July 24, 2025
    Subjects: Astrophysics of Galaxies (astro-ph.GA)
    Cite as: arXiv:2507.18688 [astro-ph.GA] (or arXiv:2507.18688v1 [astro-ph.GA] for this version)
    https://doi.org/10.48550/arXiv.2507.18688
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    From: Stefan Meingast
    [v1] Thu, 24 Jul 2025 18:00:00 UTC (1,293 KB)
    https://arxiv.org/abs/2507.18688

    Astrobiology, Astrochemistry,

    Explorers Club Fellow, ex-NASA Space Station Payload manager/space biologist, Away Teams, Journalist, Lapsed climber, Synaesthete, Na’Vi-Jedi-Freman-Buddhist-mix, ASL, Devon Island and Everest Base Camp veteran, (he/him) 🖖🏻

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  • The SWAN View Of Dense Gas In the Whirlpool – A Cloud-scale Comparison Of N2H+, HCO+, HNC And HCN Emission In M51

    The SWAN View Of Dense Gas In the Whirlpool – A Cloud-scale Comparison Of N2H+, HCO+, HNC And HCN Emission In M51

    Molecular gas mass surface densities Σmol, star formation rate surface densities ΣSFR, stellar mass surface density Σ∗, dynamical equilibrium pressure PDE as well as CO velocity dispersion σCO at 3′′ resolution. We show contours of integrated N2H + emission (0.75, 2,4 K km/s) on top. — astro-ph.GA

    Tracing dense molecular gas, the fuel for star formation, is essential for the understanding of the evolution of molecular clouds and star formation processes.

    We compare the emission of HCN(1-0), HNC(1-0) and HCO+(1-0) with the emission of N2H+(1-0) at cloud-scales (125 pc) across the central 5×7 kpc of the Whirlpool galaxy, M51a, from “Surveying the Whirlpool galaxy at Arcseconds with NOEMA” (SWAN).

    We find that the integrated intensities of HCN, HNC and HCO+ are more steeply correlated with N2H+ emission compared to the bulk molecular gas tracer CO, and we find variations in this relation across the center, molecular ring, northern and southern disk of M51.

    Compared to HCN and HNC emission, the HCO+ emission follows the N2H+ emission more similarly across the environments and physical conditions such as surface densities of molecular gas, stellar mass, star-formation rate, dynamical equilibrium pressure and radius. Under the assumption that N2H+ is a fair tracer of dense gas at these scales, this makes HCO++ a more favorable dense gas tracer than HCN within the inner disk of M51.

    In all environments within our field of view, even when removing the central 2 kpc, HCN/CO, commonly used to trace average cloud density, is only weakly depending on molecular gas mass surface density. While ratios of other dense gas lines to CO show a steeper dependency on the surface density of molecular gas, it is still shallow in comparison to other nearby star-forming disk galaxies.

    The reasons might be physical conditions in M51 that are different from other normal star-forming galaxies. Increased ionization rates, increased dynamical equilibrium pressure in the central few kpc and the impact of the dwarf companion galaxy NGC 5195 are proposed mechanisms that might enhance HCN and HNC emission over HCO+ and N2H+ emission at larger-scale environments and cloud scales.

    Sophia K. Stuber, Eva Schinnerer, Antonio Usero, Frank Bigiel, Jakob den Brok, Jerome Pety, Lukas Neumann, María J. Jiménez-Donaire, Jiayi Sun, Miguel Querejeta, Ashley T. Barnes, Ivana Bešlic, Yixian Cao, Daniel A. Dale, Cosima Eibensteiner, Damian Gleis, Simon C. O. Glover, Kathryn Grasha, Ralf S. Klessen, Daizhong Liu, Sharon Meidt, Hsi-An Pan, Toshiki Saito, Mallory Thorp, Thomas G. Williams

    Comments: Accepted for publication in A&A
    Subjects: Astrophysics of Galaxies (astro-ph.GA)
    Cite as: arXiv:2507.19439 [astro-ph.GA] (or arXiv:2507.19439v1 [astro-ph.GA] for this version)
    https://doi.org/10.48550/arXiv.2507.19439
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    From: Sophia Stuber
    [v1] Fri, 25 Jul 2025 17:15:59 UTC (6,415 KB)
    https://arxiv.org/abs/2507.19439

    Astrobiology, Astrochemistry,

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