Discovering WASP-189b: Superhot Jupiter Reveals Star’s Chemical Makeup, Astronomers Find

Astronomers utilizing the Immersion Grating Infrared Spectrometer (IGRINS) at the International Gemini Observatory’s Gemini South Telescope have made groundbreaking discoveries regarding WASP-189b’s atmospheric composition. Their findings indicate that the planet’s elemental composition closely aligns with that of its host star, offering compelling evidence that the planet inherits its chemical makeup from the protoplanetary disk from which it formed.

Artist’s impression of super-hot Jupiter. Image credit: Sci.News.

WASP-189, classified as a 730-million-year-old A-type star, is located 322 light-years away in the constellation Libra.

Also known as HD 133112, this star is significantly larger than our Sun and boasts a temperature exceeding 2,000 degrees Celsius.

First discovered in 2018, WASP-189b is a gas giant that orbits its star at a distance roughly 1.6 times that of Jupiter.

This exotic planet lies about 20 times closer to its star than Earth is to the Sun, completing an orbit in a mere 2.7 days.

According to Arizona State University graduate student Jorge Antonio Sanchez and colleagues, “Superhot Jupiter has temperatures sufficient to vaporize rock-forming elements, such as magnesium, silicon, and iron. This presents a unique opportunity to observe these elements through spectroscopy, a technique that identifies chemicals by analyzing light spectra.”

The astronomers harnessed the IGRINS instrument to capture high-resolution thermal emission spectra of WASP-189b.

They successfully identified neutral iron, magnesium, silicon, water, carbon monoxide, and hydroxyl groups within the exoplanet’s atmosphere.

“The IGRINS data reveals that WASP-189b exhibits a magnesium to silicon ratio identical to that of its host star,” they noted.

This pivotal finding offers the first observational evidence supporting a commonly held hypothesis regarding planetary formation, paving the way for deeper insights into exoplanet creation and evolution.

Gas giants like WASP-189b are believed to possess outer gas layers whose chemical makeup is heavily influenced by the protoplanetary disk from which they originated.

Researchers suspect that the ratio of rock-forming elements in the protoplanetary disk mirrors that of the host star, as they formed from the same primordial matter cloud.

This inferred chemical connection between a star and its surrounding planets is frequently utilized to model the composition of rocky exoplanets.

Previously observed only within our solar system, this link has now been directly documented on distant planets.

“WASP-189b represents a critical observational milestone in understanding terrestrial planet formation, as it allows for measurable quantities to confirm the similarities in stellar composition and the proportion of rocky materials that form alongside planets,” Sanchez stated.

Dr. Michael Rhine, an astronomer at Arizona State University, added, “Our study showcases the capabilities of ground-based, high-resolution spectrometers to analyze key species like magnesium and silicon, two essential elements in rocky planet formation. This advancement opens a new frontier in exoplanet atmospheric studies.”

The findings of this research were published in a paper in the journal Nature Communications on February 18, 2026.

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JA Sanchez et al. 2026. The magnesium to silicon ratio in the exoplanet’s atmosphere. Nat Commune 17, 2902; doi: 10.1038/s41467-026-69610-x

Source: www.sci.news

Astronomers Uncover Second Generation Stars in Pictor II Galaxy: New Discoveries in Stellar Evolution

Discover PicII-503: A Protostar in the Ancient Pictor II Dwarf Galaxy



This striking image of PicII-503 highlights a second-generation star with the lowest iron content ever recorded outside our Milky Way galaxy. Image credits: CTIO / NOIRLab / DOE / NSF / AURA / University of Alaska Anchorage TA Chancellor and NSF NOIRLab / M. Zamani and D. de Martin, NSF NOIRLab / Anirudh Chiti / Alex Drlica-Wagner.

“This marks the first definitive detection of element formation in protogalaxies,” stated Dr. Aniru Chitty, a postdoctoral researcher at the University of Chicago, now at Stanford University.

“This discovery fills a crucial gap in understanding the origin of elements during the universe’s formative years.”

In the primordial epochs following the Big Bang, the cosmos was relatively simple, comprised almost entirely of hydrogen, helium, and lithium, giving rise to giant stars primarily formed by these elements.

More complex elements, like calcium and gold, were scarce since they had to be synthesized within stars themselves.

At the cores of these massive stars, nuclear fusion processes created increasingly heavier elements.

When these stars eventually exploded, they contributed to the formation of new stars, perpetuating this cycle until a diverse array of elements emerged, forming the universe we know today.

“To track elemental formation, we must search for stars with minimal heavy elements, as these accumulate over time,” explained University of Chicago astronomer Alexander Gee.

Using the Magellan Telescope at Las Campanas Observatory and ESO’s Very Large Telescope, astronomers identified a significant candidate star within the ultrafaint dwarf galaxy Pictor II.

This star, identified as PicIII-503, exhibits a remarkable structure, with an iron content approximately 1/100,000 times lower than that of our Sun.

This extraordinary finding not only generates excitement but also offers insights into the enigmatic origins of these early stars.

Consequently, since PicIII-503 remains within its original protogalaxy, astronomers have uncovered vital information regarding its formation theory, particularly related to the star’s explosive death.

“Upon the demise of a massive star, it possesses an ‘onion-skin’ structure: lighter elements like carbon reside in outer layers while heavier elements are found inside,” Gee noted.

“A weak explosion may only eject the outer layers, allowing the heavier inner materials to coalesce with neighboring gas and dust, which can form future generations of stars.”

“However, a vigorous explosion could propel these materials far beyond the small galaxies that existed during that era,” he added.

This exciting discovery provides context for the abundance of carbon-rich stars observed in our Milky Way, illuminating their origin, Dr. Chitty emphasized.

For more on the discovery of PicIII-503, refer to the research paper published in Nature Astronomy.

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A. Chitty et al. Enrichment by the first stars of relic dwarf galaxies. Nat Astron published online on March 16, 2026. doi: 10.1038/s41550-026-02802-z

Source: www.sci.news

New Catalog of Rocky Exoplanets in the Habitable Zone Revealed by Astronomers

Utilizing data from ESA’s Gaia mission and NASA’s Exoplanet Archive, astronomers at Cornell University have discovered 45 rocky exoplanets in the habitable zone and 24 within the more specific 3D habitable zone. This groundbreaking research aids scientists in their quest for extraterrestrial life.

Artist’s impression of a planetary system around a star slightly hotter than the Sun. Image credit: Gillis Rowley.

“With over 6,000 known exoplanets from successful ground and space investigations, the research landscape has evolved significantly,” said Professor Lisa Kaltenegger of Cornell University and colleagues.

The expanding catalog of exoplanets enables astronomers to compile a targeted list for examining the boundaries of the habitable zone empirically.

This study reveals the identification of 45 rocky worlds that could potentially support life in the habitable zone, with an additional 24 in the narrower 3D habitable zone, suggesting a more cautious view on the heat a planet can endure.

Highlighted exoplanets include notable names such as Proxima Centauri b, Trappist 1f, and Kepler 186f, alongside lesser-known entities like TOI-715b.

Noteworthy planets include TRAPPIST-1d, e, f, g located 40 light-years from Earth, and LHS 1140 b, which is 48 light-years away. The possibility of liquid water on these planets hinges on their capacity to retain atmospheres.

Planets that receive light similar to that of Earth from the Sun are among the transiting candidates TRAPPIST 1e, TOI-715b, Kepler 1652b, Kepler 442b, and Kepler 1544b, as well as the star-wobble planets Proxima Centauri b, Gliese 1061d, Gliese 1002b, and Wolf 1069b.

The researchers also anticipate that planets on the edge of the habitable zone might clarify the limits of habitability and validate current scientific theories.

“Though the habitable zone concept has evolved since the 1970s, new observations are critical for determining whether adaptations are necessary,” stated Professor Kaltenegger.

Diagram displaying the boundaries of habitable zones across various star types, including rocky exoplanets. Image credit: Gillis Lowry / Pablo Carlos Budassi.

Moreover, exoplanets with unique elliptical orbits can monitor how variations in heat affect habitability, providing insights into whether a planet must remain in the habitable zone to sustain life.

Transiting planets useful for assessing habitability at the inner edge include K2-239d, TOI-700e, K2-3d, along with the star-wobble planets Wolf 1061c and Gliese 1061c.

On the outer edges of the habitable zone, planets like TRAPPIST-1g, Kepler-441b, and Gliese 1002c will be critical to exploring colder environments.

“Determining the factors that enhance the likelihood of life is complex, but narrowing down the best targets for observation is an essential first step,” remarked Gillis Rowley, a graduate student at San Francisco State University.

The research team has categorized optimal planets for observational techniques to maximize the chances of detecting signs of life.

This curated list will direct astronomers in their investigations using advanced instruments like the NASA/ESA/CSA James Webb Space Telescope, the future Nancy Grace Roman Space Telescope, the Very Large Telescope, the Habitable World Observatory, and the proposed Large Interferometer for Exoplanets (LIFE) project.

“Observing these small exoplanets is crucial to understanding their atmospheres and refining theories about their habitable zones,” concluded Lowry.

The research team’s paper is published today in the Royal Astronomical Society Monthly Notices.

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Abigail Ball et al. 2026. Exploring the boundaries of the habitable zone: A catalog of rocky exoplanets in the habitable zone. MNRAS 547 (3): stag028; doi: 10.1093/mnras/stag028

Source: www.sci.news

Astronomers Observe Dramatic Aftermath of Catastrophic Planetary Collision

The captivating flickering of the young F-type star, Gaia-20ehk, along with the expanding dust cloud encircling it, indicates a dramatic planetary collision unfolding in real time. This event provides a unique opportunity to observe the violent processes involved in the formation of nascent planetary systems.



A planetary collision around the star Gaia20ehk. Image credit: Andy Tzanidakis.

Located approximately 11,000 light-years from Earth in the constellation Leo, Gaia20ehk is a stable “main sequence” star, typically known for its steady and predictable luminosity. However, since 2016, this star has exhibited violent flickering.

“Initially, the star’s light output was consistent, but it has since dropped by around 3 degrees,” remarked Anastasios (Andy) Tzanidakis, a doctoral candidate at the University of Washington. “By 2021, the situation escalated dramatically.”

“Such behavior is unexpected for stars like our Sun. When we observed this, we thought, ‘What could be happening here?'”

The flickering of Gaia20ehk is not due to the star itself. Instead, it is caused by a cloud of rocks and dust obstructing the light as it orbits the system.

The astounding source of this debris appears to be a catastrophic planetary collision.

“It’s remarkable that multiple telescopes captured this impact in real time,” Tzanidakis stated.

“There are only a handful of documented planetary collisions, and none possess as many parallels to the impacts that formed Earth and the Moon.”

“Observing similar events in other parts of the galaxy could significantly enhance our understanding of our planet’s formation.”

Additionally, evidence suggests this impact may closely resemble the one that created the Earth and Moon approximately 4.5 billion years ago.

This dust cloud orbits Gaia20ehk at about 1 astronomical unit, the same distance from its star as Earth is from the Sun.

At this distance, materials could eventually cool and solidify into structures akin to the Earth-Moon system.

“How rare was the event that shaped the Earth and Moon? This inquiry is essential to the field of astrobiology,” commented James Davenport, a professor at the University of Washington.

“The Moon seems to play a crucial role in making Earth a habitable place, shielding it from some asteroids, influencing ocean tides and weather patterns, and potentially even facilitating geological activity.”

“Currently, the prevalence of these dynamics remains uncertain, but as we observe more collisions, we will gain clearer insights.”

The team’s research paper will be published in today’s Astrophysical Journal Letters.

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Anastasios Zanidakis & James R.A. Davenport. 2026. Gaia-GIC-1: Evolving catastrophic planetesimal impact candidate. APJL 1000, L5; doi: 10.3847/2041-8213/ae3ddc

Source: www.sci.news

Astronomers Discover Neutron Star Collision in Surprising Cosmic Environment

Astronomers have utilized NASA’s Chandra X-ray Observatory along with other advanced telescopes to investigate a transient gamma-ray burst event known as GRB 230906A. This burst originated from a faint dwarf galaxy hidden within a vast flow of intergalactic gas. The discovery indicates that neutron star mergers—violent collisions responsible for producing heavy elements like gold and platinum—can occur far away from the luminous centers of galaxies, which may elucidate why some bursts appear to lack a defined host galaxy.



GRB 230906A originated in a small galaxy in a gas stream approximately 4.7 billion light-years from Earth. Image credit: NASA / CXC / Pennsylvania State University / S. Dichiara / ESA / STScI / ERC BHianca 2026 / Fortuna and Dichiara, CC BY-NC-SA 4.0 / SAO / P. Edmonds.

A neutron star is the remnants left after a massive star depletes its nuclear fuel, collapses, and violently explodes.

Despite their compact size, neutron stars possess a mass greater than our Sun and are incredibly dense.

These celestial bodies are considered among the most extreme entities in the universe.

In recent years, astronomers have gathered evidence of neutron star mergers occurring within larger galaxies.

However, this recent revelation highlights that neutron star collisions can also take place within smaller galaxies.

“Discovering a neutron star collision in such an unexpected location is a pivotal moment for our field,” stated Dr. Simone DiChiara, an astronomer from Pennsylvania State University.

“This finding may hold the key to resolving two significant mysteries in astrophysics.”

The first question this groundbreaking neutron star collision site may clarify is why gamma-ray bursts from neutron star mergers often do not appear at the central regions of galaxies.

The second mystery this discovery could illuminate concerns the presence of heavy elements like gold and platinum in stars located far from a galaxy’s core.

This neutron star collision is intriguingly situated in a gas stream spanning approximately 600,000 light-years, originating from a diminutive galaxy about 4.7 billion light-years away.

This gas flow likely emerged hundreds of millions of years ago during a galactic collision that stripped gas and dust from the involved galaxies, leaving remnants in intergalactic space.

“Our discovery reveals a collision within a collision,” remarked Dr. Eleonora Troja of the University of Rome.

“The merging of galaxies instigated a surge of star formation, ultimately leading to the birth and subsequent collision of neutron stars over millions of years.”

To identify the GRB 230906A phenomenon, which occurred on September 6, 2023, astronomers employed multiple NASA telescopes, including the Chandra X-ray Observatory, Fermi Gamma-ray Space Telescope, Neil Gehrels Swift Observatory, and the Hubble Space Telescope.

Fermi detected neutron star collisions by recognizing the characteristic gamma-ray burst (GRB) signals.

Following initial location analysis by the interplanetary network, the precise location of the object was further defined using the advanced observational capabilities of Chandra, Swift, and Hubble.

NASA’s initiative is part of a growing global network dedicated to monitoring cosmic phenomena to uncover the secrets of the universe.

“Chandra’s pinpoint accuracy in X-ray localization made this research possible,” said Dr. Brendan O’Connor, a postdoctoral fellow at Carnegie Mellon University.

“Without this data, connecting the burst to a specific cosmic source would have been unattainable.”

“Once Chandra provided us with a precise location, Hubble’s exceptional sensitivity unveiled a small, faint galaxy in that area.”

“We managed to achieve this groundbreaking discovery by synergizing various research elements.”

This insight might elucidate why certain GRBs seem to lack identifiable host galaxies.

It suggests that some host galaxies may be too diminutive to be discerned in standard optical surveys conducted by ground-based observatories.

GRB 230906A’s unusual positioning could also contribute to the understanding of how astronomers found heavy elements like gold and platinum in stars situated far from their galaxy centers.

These stars are generally believed to have formed from older gas that had less opportunity to accumulate heavy elements from supernova events.

Collisions between neutron stars can synthesize heavy elements, including gold and platinum, via various nuclear reactions, similar to those observed in a well-documented neutron star collision from 2017.

Events like GRB 230906A can produce such elements that eventually disperse throughout the galactic outskirts and can appear in future generations of stars.

Another potential explanation for this explosion is its positioning within a more distant galaxy located behind the cluster of galaxies.

“We consider this a less likely explanation compared to the presence of small galaxies,” the researchers concluded.

This groundbreaking finding is detailed in the research paper published in the Astrophysical Journal Letters.

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S. Dichiara et al. 2026. A merger within a merger: Chandra identifies short GRB 230906A in exceptional circumstances. APJL 999, L42; doi: 10.3847/2041-8213/ae2a2f

Source: www.sci.news

Astronomers Uncover Hidden Structure of the Early Universe: Breakthrough Discoveries Explained

Astronomers have utilized spectral data from the Hobby-Eberly Telescope at McDonald Observatory to construct the most intricate 3D map of faint cosmic structures dating back 9 to 11 billion years, unveiling galaxies and intergalactic gas previously undetectable by telescopes.



A line intensity map showcasing the distribution of excited hydrogen in the universe approximately 10 billion years ago. The stars denote areas where HETDEX has identified galaxies. The inset simulates the structure after optimizing the data by reducing background noise. Image credit: Maja Lujan Niemeyer / Max Planck Institute for Astrophysics / HETDEX / Chris Byrohl / Stanford University.

“Studying the early Universe reveals how galaxies have evolved into their current forms and the role that intergalactic gas plays in this transformation,” stated Dr. Maya Lujan Niemeyer, an astronomer at the Max Planck Institute for Astrophysics and Ludwig Maximilian University of Munich, and a key member of the Hobby-Eberly Telescope’s Dark Energy Experiment (HETDEX).

“Many objects from this epoch are faint and challenging to observe due to their vast distances,” she continued.

“Through a technique known as line intensity mapping, this innovative map enhances our understanding of these objects, adding complexity and depth to this crucial era of cosmic history.”

Although line intensity mapping is not a novel methodology, this is the first instance it has been employed to visualize Lyman alpha emissions with such exceptional precision across an extensive dataset.

The HETDEX project harnesses the capabilities of the Hobby-Eberly Telescope to catalog over 1 million luminous galaxies to decode the mysteries of dark energy.

What differentiates this project is its extensive measurement scope, equivalent to observing more than 2,000 full moons and amassing a colossal dataset of over 600 million spectra across an expansive area of the sky.

“We leverage only a fraction of our data—approximately 5%,” remarked Dr. Karl Gebhardt, principal investigator of HETDEX and an astronomer at the University of Texas at Austin.

“This leaves significant potential for future research utilizing the remaining data.”

“While HETDEX captures images of the entire sky, only a small subset of the collected data comprises sufficiently bright galaxies for our research,” noted Dr. Lujan Niemeyer.

“These galaxies are merely the beginning. In the vast expanses in between, lies an entire ocean of light awaiting discovery.”

To construct this groundbreaking map, astronomers employed a supercomputer at the Texas Advanced Computing Center to meticulously analyze approximately half a petabyte of HETDEX data.

Using the coordinates of luminous galaxies already detected by HETDEX, they inferred the positions of fainter galaxies and adjacent glowing gas.

Due to the gravitational forces that cause matter to cluster, the existence of one bright galaxy implies the presence of nearby celestial objects.

“This allows us to utilize known galaxy positions as reference points to ascertain distances to fainter celestial entities,” explained Dr. Eiichiro Komatsu, HETDEX scientist and astronomer at the Max Planck Institute for Astrophysics.

“The resultant map emphasizes regions surrounding bright galaxies while providing intricate details of the areas in between.”

“Simulation models exist for this cosmic era, yet they remain hypothetical; they do not represent the actual universe.”

“We now possess a foundational understanding that allows us to verify whether the astrophysics underlying these simulations holds true.”

For more on these remarkable findings, published on March 3, 2026, in the Astrophysical Journal.

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Maya Lujan Niemeyer and others, 2026. Lyα intensity mapping in HETDEX: Galaxy-Lyα intensity cross-power spectrum. APJ 999, 177; doi: 10.3847/1538-4357/ae3a98

Source: www.sci.news

Unlocking the Secrets: Astronomers Decode Zebra Stripes of the Crab Pulsar

Recent findings from the University of Kansas have unraveled a long-standing astrophysical mystery, revealing how the intricate interplay of gravity and magnetospheric plasma divides the radio emissions of a club pulsar—a remnant of the supernova witnessed by ancient astronomers in 1054 AD—into perfectly aligned “stripes.”

This composite image showcases the Crab Nebula, with the club pulsar centrally positioned. Image credit: X-ray – NASA / CXC / ASU / J. Hester et al.; Optics – NASA / HST / ASU / J. Hester et al.

In 1054 AD, Chinese astronomers documented an exceptionally bright new star, the most luminous object in the night sky after the moon, visible even in broad daylight for 23 days. This spectacular celestial event was also noted by Japanese, Arabian, and Native American astronomers.

Today, the Crab Nebula, found where this bright star once shone, is cataloged as Messier 1 (M1) or NGC 1952, located approximately 6,500 light-years away in the Taurus constellation.

Initially identified in 1731 by British physician and astronomer John Beavis, the Crab Nebula was later rediscovered in 1758 by French astronomer Charles Messier. Its name, reflecting its appearance, is derived from a painting by Irish astronomer Lord Rose in 1844.

The central star of the Crab Nebula is the Crab Pulsar, scientifically known as PSR B0531+21.

Due to their proximity and visibility, studying the Crab Nebula and its pulsars offers astronomers vital insights into the nature of nebulae, supernovae, and neutron stars.

“Gravity alters the shape of spacetime,” states Professor Mikhail Medvedev, one of the study’s authors.

“In the presence of a gravitational field, light does not travel in straight lines because space itself is curved,” he explains.

“What seems straight in flat spacetime appears curved under strong gravitational influence. Hence, gravity functions as a lens in curved spacetime.”

While gravitational lensing has often been discussed in relation to black holes, this case uniquely illustrates a “tug of war” between plasma and gravity creating the observed signals.

“In black hole imagery, gravity solely shapes the structure,” notes Professor Medvedev.

“In contrast, both gravity and plasma are at play in the club pulsar. This research presents a novel application of this combined effect.”

“An intriguing pattern emerges in the pulsar’s spectrum,” Professor Medvedev adds.

“Unlike a conventional broad spectrum like sunlight—which offers a continuous range of colors—the Crab’s high-frequency interpulses display discrete spectral bands. It’s like observing a rainbow with only selected ‘colors’ visible, leaving significant gaps in between.”

A large mosaic image of the Crab Nebula, a six-light-year wide remnant of a supernova explosion. Documented by Japanese, Chinese, and Native American astronomers around 1054 AD. Image credit: NASA / ESA / J. Hester / A. Loll, Arizona State University.

Typically, pulsar radio emissions are broader, noisier, and less organized compared to those from club pulsars.

“In the case of club pulsars, the stripes are exceptionally distinct, contrasting sharply with the complete darkness that separates them,” explains Professor Medvedev.

“There are shining bands and voids in between, with no gradual transition. No other pulsar displays this kind of banding. This uniqueness makes the club pulsar both intriguing and complex to comprehend.”

While former models could replicate the striped pattern, they failed to account for the high contrast actually seen in club pulsars.

Professor Medvedev has found that the plasma material surrounding the club pulsar contributes to the diffraction of electromagnetic pulses, which significantly influences the neutron star’s distinct zebra pattern.

By integrating Einstein’s theory of gravity into his analysis, Medvedev discovered its crucial role in shaping the club pulsar’s zebra stripe pattern.

“Prior theoretical models could reproduce the striped pattern, but not the observed contrast. Including gravity bridged that gap,” asserts Professor Medvedev.

“The plasma in a pulsar’s magnetosphere acts as a defocusing lens, while gravity serves as a focusing lens. Plasma tends to scatter light rays, whereas gravity draws them inward. When these dual effects converge, certain paths will offset each other.”

The synergy between defocused magnetospheric plasma and focusing gravity creates in-phase and out-of-phase interference bands of radio intensity, producing zebra stripes in club pulsars.

“The nature of symmetry suggests there are at least two pathways for light,” Medvedev observes.

“When two nearly identical paths converge on an observer, they create an interferometer. The signals amalgamate, reinforcing each other at specific frequencies (in phase) to yield bright bands, while at others (out of phase), they cancel each other out, generating darkness. This concept encapsulates the essence of interference patterns.”

“Little additional physics appears necessary to qualitatively explain the stripes.”

“Yet, quantitative enhancements could be implemented; the current model includes gravity in a static, lowest-order approximation.”

“Since pulsars rotate, incorporating rotational effects might lead to significant quantitative, if not qualitative, changes.”

The new research is set to be published in the Plasma Physics Journal.

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Mikhail V. Medvedev. 2026. Theory of the dynamic spectrum of club pulsar high-frequency interpulse stripes. Plasma Physics Journal, in press. arXiv: 2602.16955

Source: www.sci.news

Astounding Discovery: Astronomers Find Iron ‘Rod’ at the Center of a Mysterious Ring Nebula

Astronomers utilizing the WHT Extended Area Velocity Explorer (WEAVE), a cutting-edge instrument aboard the William Herschel Telescope on La Palma Island, have uncovered an intriguing elongated structure of ionized iron within the renowned Ring Nebula.



A composite image of the Ring Nebula featuring four WEAVE/LIFU emission line images. Image credit: Wesson et al., doi: 10.1093/mnras/staf2139.

The Ring Nebula, also known as Messier 57, M57, or NGC 6720, is a classic planetary nebula located approximately 2,000 light-years away in the constellation Lyra.

This nebula was first discovered by the French astronomer Charles Messier in January 1779 while he was on a mission to find comets.

Messier’s report about the discovery of Comet Bode reached fellow astronomer Antoine d’Alquier de Perpois shortly afterward, who subsequently rediscovered the Ring Nebula during his comet observations.

The newly identified rod-shaped cloud of iron atoms resides within the inner layer of this elliptical nebula.

Measuring about 500 times the length of Pluto’s orbit around the sun, this cloud’s atomic mass of iron is comparable to that of Mars.

This iron cloud was detected using the Large Integral Field Unit (LIFU) mode of the innovative WEAVE instrument on the 4.2-meter William Herschel Telescope, part of the Isaac Newton Group.

According to Dr. Roger Wesson, an astronomer from University College London and Cardiff University: “While the Ring Nebula has been extensively studied with various telescopes, WEAVE enables us to observe it in unprecedented detail, providing much richer information than previously available.”

“By continuously collecting spectra across the nebula, we can image it at any wavelength and analyze its chemical composition at any given location.”

“As we process the data and examine the images, we discover a never-before-seen ‘rod’ of ionized iron atoms at the heart of this iconic ring.”

The exact nature of the iron “rods” within the Ring Nebula remains uncertain.

Two potential scenarios emerge: the bar may offer new insights into the nebula’s formation and ejection by its parent star, or (more intriguingly) it could represent an arc of plasma from a rocky planet evaporating during the star’s initial expansion.

Professor Janet Drew, also from University College London, noted: “We need to investigate further, particularly to determine if the newly detected iron coexists with other elements. This could guide us toward the appropriate models to explore.”

“Currently, this crucial information is lacking.”

For more in-depth details, check out the findings published today in the Royal Astronomical Society Monthly Notices.

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R. Wesson et al. 2026. WEAVE Imaging Spectroscopy of NGC 6720: Iron Rods in the Ring. MNRAS 546 (1): staf2139; doi: 10.1093/mnras/staf2139

Source: www.sci.news

Astronomers Discover Celestial ‘Wake’ Linked to Betelgeuse’s Companion Star

Recent multi-year observations from the NASA/ESA Hubble Space Telescope, along with data from the Fred Lawrence Whipple and Roque de los Muchachos Observatories, have unveiled how a faint companion star, identified as Siwalha, has carved a path through the vast atmosphere of Betelgeuse. These findings illuminate long-standing mysteries regarding stellar evolution and advance our understanding of large-scale stellar dynamics.



Artist’s concept depicting the red supergiant star Betelgeuse alongside its orbiting companion. Image credit: NASA/ESA/Elizabeth Wheatley, STScI/Andrea Dupree, CfA.

Betelgeuse, an impressive 8-million-year-old red supergiant star, is prominently situated on the shoulder of the Orion constellation, approximately 724 light-years away from Earth.

With a radius roughly 1,400 times that of the Sun, Betelgeuse stands as one of the largest known stars in the universe.

Commonly referred to as Alpha Orionis or Alpha Ori, Betelgeuse is not just renowned for its size but also for its brightness, radiating more light than 100,000 suns combined.

As Betelgeuse nears the end of its life cycle, its impending explosion is expected to be so luminous that it will be visible in daylight for several weeks.

Astronomers have been meticulously monitoring variations in Betelgeuse’s brightness and surface characteristics for decades to uncover the underlying causes of its behavior.

Interest peaked in 2020 when Betelgeuse seemed to exhibit unusual “sneezing” behavior, suddenly dimming unexpectedly.

Two key periods of fluctuations have intrigued scientists: a short 400-day cycle, likely linked to the star’s own pulsations, and a longer 2,100-day period that remains more elusive.

Researchers have theorized various explanations for these fluctuations, including large convective cells, dust clouds, magnetic activities, and the possible presence of hidden companion stars.

A recent comprehensive study suggests that the longer secondary period is best explained by a low-mass companion star that orbits deep within Betelgeuse’s atmosphere. While some scientists reported possible detections, solid evidence was previously lacking—until now.

For the first time, astronomers have gathered compelling evidence that a companion star is indeed influencing the supergiant star’s atmosphere.

Data changes in the spectra of stars—colors of light emitted by different elements—and shifts in the gas’s speed and direction in the outer atmosphere confirm the presence of denser material and wake effects.

This peculiar signature appears soon after the companion star transits in front of Betelgeuse approximately every six years, further endorsing the theoretical model.

Dr. Andrea Dupree, an astronomer at Harvard University & Smithsonian Center for Astrophysics, commented, “It’s akin to a boat sailing through water; the companion star induces a ripple in Betelgeuse’s atmosphere that is directly observable in the data.”

“For the first time, we are witnessing definitive signs of this wake or gas signature, validating that Betelgeuse does indeed harbor a hidden companion that influences its observable characteristics and behavior.”

The team’s research paper will soon be published in the Astrophysical Journal.

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Andrea K. Dupree et al. 2026. Betelgeuse: Expanding trail of the companion star detected. APJ in press. arXiv: 2601.00470

Source: www.sci.news

First-Ever Measurement of Floating Exoplanet’s Mass by Astronomers

Gravitational microlensing surveys have unveiled populations of free-floating planets. Although their masses haven’t been directly measured due to distance-related challenges, statistics suggest that many of these rogue planets possess less mass than Jupiter. Recently, astronomers identified a groundbreaking microlensing event, termed KMT-2024-BLG-0792/OGLE-2024-BLG-0516. This event involved an exoplanet with approximately 21.9% of Jupiter’s mass, situated 9,785 light-years (3,000 parsecs) from the Milky Way’s center.

An artist’s impression of a free-floating exoplanet. Image credit: Sci.News.

Traditionally, planets are linked to stars, but research indicates that many traverse the galaxy independently.

Known as free-floating or rogue planets, these celestial bodies lack stellar companions.

Due to their low light emissions, they are primarily detected through their gravitational influences, a technique known as microlensing.

A significant challenge of this discovery method is determining the distances to these planets, complicating mass measurements.

This has left much of the data regarding these solitary objects speculative.

In a recent study, Dr. Subo Dong from Peking University and the National Astronomical Observatory of Japan and collaborators discovered a new free-floating planet, KMT-2024-BLG-0792/OGLE-2024-BLG-0516, via a brief microlensing event.

In contrast to prior approaches, they utilized a novel strategy by observing the microlensing phenomenon concurrently from Earth and space, leveraging multiple ground-based surveys alongside ESA’s Gaia space telescope.

Variations in the timing of light captured by these different locations facilitated measurements of microlens parallax, enabling researchers to calculate the planet’s mass and position through finite source modeling.

“Based on comparisons with the statistical characteristics of other microlensing events and simulation predictions, we conclude that this object didn’t originate as an isolated entity (like a brown dwarf) but likely formed within a protoplanetary disk (like a planet),” the astronomers noted.

“Subsequent dynamic processes likely ejected it from its formation site, resulting in a free-floating object.”

For further details, check out the study published in this month’s Science: paper.

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Subo Dong et al. 2026. Microlensing of free-floating planets caused by heavy objects in Saturn’s vicinity. Science 391 (6780): 96-99; doi: 10.1126/science.adv9266

Source: www.sci.news

Astronomers Unveil Merging Mystery: Champagne Galaxy Cluster is Two Colliding Clusters

Astronomers unveiled a remarkable giant galaxy cluster known as RM J130558.9+263048.4 on December 31, 2020. Due to its bubble-like appearance and superheated gas, they aptly named it the Champagne Cluster. The stunning new composite image of this galaxy cluster features X-ray data from NASA’s Chandra X-ray Observatory combined with optical information from the Legacy Survey.



The Champagne Cluster appears as a luminous array of galaxies amidst a vibrant neon purple cloud. The cluster reveals over 100 galaxies split into two groups, with notable variations among them. Foreground stars display diffraction spikes surrounded by a subtle haze. Many small galaxies showcase blue, orange, or red tones and exhibit varied shapes. This indicates a multifaceted nature, while the central purple gas cloud emitted by Chandra signals a high-temperature region, indicative of two colliding clusters. Image credit: NASA / CXC / UCDavis / Bouhrik others. / Legacy Survey / DECaLS / BASS / MzLS / SAO / P. Edmonds / L. Frattare.

Recent research led by astronomer Faik Bourik from the University of California, Davis, utilized instruments from NASA’s Chandra X-ray Observatory and ESA’s XMM Newton Observatory to investigate the Champagne Cluster.

The team also analyzed data from the DEIMOS multi-object spectrometer located at the W. M. Keck Observatory.

“Our new composite image indicates that the Champagne Galaxy Cluster consists of two galaxy clusters merging to form a larger cluster,” the astronomers stated.

“In typical observations, multimillion-degree gas is roughly circular, but in the Champagne Cluster, it spans from top to bottom, highlighting the collision of two clusters.”

“Distinct clusters of individual galaxies are prominently visible above and below the center,” they added.

“Remarkably, the mass of this hot gas exceeds that of all 100 or more individual galaxies within the newly formed cluster.”

“This cluster is also abundant in invisible dark matter, a mysterious substance that pervades the universe.”

The Champagne Cluster is part of a rare category of merging galaxy clusters, akin to the well-known Bullet Cluster, where the hot gas from each cluster collides, slows, and creates a clear separation from the heaviest galaxies.

By comparing this data with computer simulations, researchers propose two potential histories for the Champagne Cluster.

One theory suggests that the two star clusters collided over 2 billion years ago, followed by an outward movement due to gravity, leading them to a subsequent collision.

Alternatively, another link posits a single collision about 400 million years ago, after which the clusters have begun moving apart.

“Further studies on the Champagne Cluster could illuminate how dark matter reacts during high-velocity collisions,” the scientists concluded.

For more insights, refer to their published paper in July 2025, featured in the Astrophysical Journal.

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Faik Bourik others. 2025. New dissociated galaxy cluster merger: discovery and multiwavelength analysis of the Champagne Cluster. APJ 988, 166;doi: 10.3847/1538-4357/ade67c

Source: www.sci.news

Rediscovery of a Long-Lost Star: Astronomers Find Celestial Object Missing for Over 130 Years

Telescope Capture at Grasslands Observatory

Credit: Tim Hunter et al. (2025)

A long-lost star, discovered by the legendary astronomer Edward Emerson Barnard in 1892, has been astonishingly rediscovered in its original location.

Barnard was not just any astronomer; he made significant contributions to the field, including the discovery of Jupiter’s fifth moon, Amalthea, in 1892—nearly three centuries after Galileo’s initial discoveries. Recently, his observations have gained renewed interest due to a puzzling article he published in 1906, titled “Unexplained Observations.”

On a particular morning, Barnard noted a star near Venus while using his telescope to search for its satellite. He estimated its brightness to be around 7th magnitude on the astronomical scale, where fainter objects bear higher numbers. Typically, under dark skies, stars of magnitude 6 are the faintest visible to the human eye.

Beneath the stars at the Bonner Cathedral, which cataloged all stars brighter than magnitude 9.5, Barnard’s 7th magnitude star was conspicuously absent. Instead, the only celestial body he found nearby was a significantly dimmer 11th magnitude star—about 100 times less bright.

Could it have been a large asteroid? “Ceres, Pallas, Juno, and Vesta were elsewhere,” he surmised. Some theorized that the 11th magnitude star he eventually observed in that region might have temporarily brightened. Other scientists speculated that Barnard could have been deceived by a “ghost” image of Venus through the telescope. The mystery lingered until late December 2024 when a dedicated group of astronomers sought to unravel it.

“In a weekly Zoom meeting dubbed ‘Asteroid Lunch,’ I brought it up,” says Tim Hunter.

Hunter, an Arizona-based amateur astronomer and co-founder of the International Dark Sky Association, along with both amateur and professional astronomers, evaluated all previous hypotheses and found flaws in them.

As doubts began to consume the group, Roger Ceragioli, an optical engineer from the University of Arizona, revisited the ghost theory by observing Venus at dawn using a vintage telescope similar to Barnard’s. Much to his surprise, although Venus was not positioned where Barnard had seen it, “the star emerged clearly in my field of view,” he noted. This led him to theorize that the star must be bright enough to be visible at dawn, even though the star map revealed it to be only 8th magnitude and therefore relatively faint.

The group’s conclusive findings suggested that Barnard’s purported 7th magnitude star was indeed the 11th magnitude star noted later—appearing brighter due to the dawn light. Using a 36-inch telescope at the Lick Observatory in California, Barnard first spotted this star alongside Venus, but no equally bright stars were visible in the area.

Understanding Star brightness measurement was a specialized skill in Barnard’s era. It had only been refined by astronomers focusing on variable stars, which Barnard had not formally studied. Thus, his mistake was rather excusable, as Ceragioli suggests.

Hunter affirms Barnard’s legacy remains intact, saying, “We’re all big fans of Barnard. It’s a minor error in an impressive career.”

 

Chile: The World Capital of Astronomy

Discover the astronomical wonders of Chile, home to the world’s most advanced observatory and unrivaled stargazing opportunities under some of the clearest skies on Earth.

Source: www.newscientist.com

NASA Astronomers Classify Near-Earth Asteroids: Latest Findings – Sciworthy

Researchers exploring the solar system’s history focus on a diverse range of comets and asteroids, particularly those classified as Near-Earth Objects (NEOs). These celestial bodies not only offer insights into the origins of water and organic materials but also continue to impact planets across the solar system, including Mars, Earth, Venus, and Mercury. Their close proximity to Earth facilitates detection and observation with smaller telescopes, increasing the potential for successful interceptions, potentially involving rovers and landers.

An international research team has recently classified and identified 39 new NEOs between February 2021 and September 2024, utilizing two advanced telescopes: Itaparica Observatory (OASI) in Brazil, along with the 2.15-meter Jorge Sahade telescope at Complejo Astronomico El Leoncito (CASLEO) in Argentina.

The research team used these telescopes to study variations in the brightness of NEOs over time. Since NEOs are essentially blocks of ice or rock that reflect sunlight rather than emit light, their visibility from Earth is influenced by the angle between Earth and the Sun along with their size, shape, and structure. By measuring the periodic changes in brightness, scientists calculated the rotation rates of these objects.

The diameters of the 39 NEOs varied from 0.1 to 10 kilometers (0.06 to 6 miles), with most ranging between 0.5 to 3 kilometers (0.3 to 2 miles). Their shapes ranged from nearly spherical to elongated, cigar-like forms. The team successfully determined the rotation periods for 26 of these NEOs, noting that the shortest rotation cycle was just over two hours while the longest approached 20 hours. Notably, 16 of these NEOs rotated in under 5 hours, suggesting that many are fast-rotating bodies.

The study established that a rotation period exceeding 2.2 hours is the upper limit for small NEOs known as rubble pile asteroids, which are loose formations held together by self-gravity. Beyond this threshold, centrifugal forces could destabilize them. Conversely, those NEOs under 250 meters (820 feet) tend to be more solid, dubbed monoliths. The findings indicated that smaller and medium-sized NEOs exhibit varied structures and formation histories.

Using advanced imaging techniques through telescope lenses that filter specific light wavelengths, the researchers analyzed the chemical composition of 34 NEOs. They employed 2 additional filters alongside 4 filters designed for green and red wavelengths, including near-infrared wavelengths. Their results revealed that 50% of the NEOs are silica-based, resembling many terrestrial rocks, with 23.5% comprising carbon-rich materials, approximately 9% metals, and around 6% basaltic elements. The remaining composition was a mixture of carbon and silicates as well as calcium and aluminum.

While the chemical analysis largely aligned with previous findings, the researchers found a lack of olivine—a mineral typically prevalent in smaller asteroids. This absence can be attributed to the fact that most sampled NEOs exceeded 200 meters (660 feet), surpassing the typical size for olivine-rich asteroids.

This research enriches our understanding of NEOs and their physical and chemical properties. The team advocates for an integrated research approach that leverages technology and multi-telescope observations to effectively characterize small celestial objects. Future studies should prioritize close monitoring of NEOs, especially those approaching their rotation threshold, and employ radar observations to confirm the existence of potential binary pairs. By analyzing reflected visible and near-infrared light, researchers can further unveil the chemical makeup of the asteroid surfaces.


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Astronomers Uncover Direct Evidence of Supermassive Stars in the Early Universe

Astronomers utilizing the NASA/ESA/CSA James Webb Space Telescope have identified the chemical signature of a protostar with a mass between 1,000 and 10,000 times that of the Sun in GS 3073, an early galaxy with a redshift of 5.55 (approximately 1 billion years post-Big Bang).



A primordial supermassive star in the early universe. Image credit: Gemini AI.

In 2022, it was suggested by astronomers that supermassive stars formed naturally within turbulent flows of rare cold gas during the early universe, thus accounting for the existence of quasars less than a billion years after the Big Bang.

“Our recent finding helps to unravel a cosmic enigma that has persisted for two decades,” stated Dr. Daniel Whalen of the University of Portsmouth.

“GS 3073 offers the first observational proof of these colossal stars.”

“These astronomical behemoths would have radiated intensely for a brief period before collapsing into enormous black holes, leaving behind chemical imprints detectable billions of years later.”

“Much like Earth’s dinosaurs, they were massive and rudimentary, with lifespans spanning just 250,000 years—an ephemeral moment in cosmic time.”

The cornerstone of this discovery involved assessing the nitrogen-to-oxygen ratio in the GS 3073 galaxy.

This galaxy presents a nitrogen-to-oxygen ratio of 0.46, significantly exceeding what can be accounted for by any known type of star or stellar explosion.

“Chemical abundances serve as the universe’s fingerprints, and the pattern from GS 3073 is unlike that produced by typical stars,” remarked Dr. Devesh Nandal, an astronomer at the University of Virginia, Harvard University, and the Smithsonian Center for Astrophysics.

“This unprecedented nitrogen concentration aligns with a single known source: protostars that are thousands of times more massive than the Sun.”

“This suggests that the first generation of stars included genuine supermassive objects that contributed to the creation of early galaxies and may have planted the seeds for contemporary supermassive black holes.”

The researchers performed modeling of stars with masses between 1,000 and 10,000 solar masses to predict their evolution and the elements they would produce.

They identified a specific mechanism for generating substantial nitrogen. (i) These colossal stars fuse helium, forming carbon in their cores. (ii) Carbon seeps into the outer shell, where hydrogen is undergoing fusion. (iii) Carbon merges with hydrogen, resulting in nitrogen through the carbon/nitrogen/oxygen (CNO) cycle. (iv) Convection disseminates nitrogen throughout the star. (v) Eventually, this nitrogen-rich material is expelled into space, enriching the surrounding gas.

This mechanism spans millions of years during the star’s helium burning phase, leading to the excess nitrogen observed in GS 3073.

The team’s models predict that upon demise, these massive stars do not explode. Instead, they collapse directly into gigantic black holes with masses reaching thousands of solar masses.

Interestingly, GS 3073 harbors an actively feeding black hole at its core, which could potentially be the remnant of one of these supermassive first stars.

If validated, this would simultaneously clarify two mysteries: the origin of nitrogen and the formation of black holes.

The study also revealed that this nitrogen signature is exclusive to specific mass ranges.

“Stars below 1,000 solar masses or above 10,000 solar masses do not generate chemical patterns suitable for this signature, indicating a ‘sweet spot’ for such enrichment,” scientists noted.

of study Published in Astrophysics Journal Letter.

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Devesh Nandal others. 2025. A protostar between 1000 and 10,000 MSun created a nitrogen surplus in GS 3073 at z = 5.55. APJL 994, L11; doi: 10.3847/2041-8213/ae1a63

Source: www.sci.news

Astronomers Uncover Strange Explosion from the Supermassive Black Hole in NGC 3783

Utilizing ESA’s XMM-Newton along with the X-ray Imaging and Spectroscopy Mission (XRISM)—a collaborative endeavor led by JAXA, ESA, and NASA—astronomers detected an ultrafast outflow from the supermassive black hole in NGC 3783, moving at 19% the speed of light (57,000 km/s).

An artist’s conception of NGC 3783’s wind-blown supermassive black hole. Image credit: ESA/ATG Europe.

NGC 3783 is a luminous barred spiral galaxy located about 135 million light-years away in the Centaurus constellation.

This galaxy was initially discovered by British astronomer John Herschel on April 21, 1835.

Also referred to as ESO 378-14, LEDA 36101, or 2XMM J113901.7-374418, it is a prominent member of the NGC 3783 group, which contains 47 galaxies.

NGC 3783 hosts a rapidly rotating supermassive black hole with a mass of 2.8 million solar masses.

“We have never witnessed a black hole producing winds at such speeds before,” stated Dr. Li Gu, an astronomer at the Netherlands Space Research Organization (SRON).

“Swift bursts of X-ray light from a black hole immediately provoke superfast winds, and for the first time, we observe how these winds develop within just a day.”

During 10 days of observations, mainly using the XRISM space telescope, astronomers monitored the emergence and acceleration of a burst from NGC 3783’s supermassive black hole.

While such explosions are typically attributed to intense radiation, in this instance, the likely cause is a sudden shift in the magnetic field, akin to solar flares caused by the Sun’s outbursts.

It is known that supermassive black holes emit X-rays, but this marks the first occasion where astronomers have distinctly observed rapid ejections during these X-ray bursts.

This finding emerged from the longest continuous observation conducted by XRISM to date.

Over these 10 days, scientists noted fluctuations in the brightness of the X-rays, particularly within the soft X-ray band.

Such fluctuations, including explosions lasting three days, are not uncommon for supermassive black holes.

What sets this explosion apart is the simultaneous expulsion of gas from the black hole’s accretion disk—a swirling disc of matter in orbit around the black hole.

This gas was expelled at astonishing speeds, hitting 57,000 km/s, or 19% of the speed of light.

Researchers identified the origin of this gas as a region approximately 50 times larger than the black hole itself.

Within this chaotic region, gravitational and magnetic forces are in extreme interaction.

The emission is believed to be the result of a phenomenon known as magnetic reconnection, which occurs when the magnetic field rapidly reorganizes and releases vast amounts of energy.

“This is an unparalleled opportunity to explore the mechanisms behind ultrafast ejections,” Dr. Gu remarked.

“The data indicate that magnetic forces, resembling those involved in coronal mass ejections from the Sun, are responsible for the acceleration of the outflow.”

“A coronal mass ejection occurs when a hefty plume of hot solar plasma is hurled into space.”

“In contrast, supermassive black holes can produce similar events, but these eruptions are 10 billion times more potent and far smaller than solar phenomena we’ve observed.”

Scientists propose that the black hole activity observed may mirror its solar counterpart, driven by an abrupt burst of magnetic energy.

This challenges the widely-held theory that black holes expel matter predominantly through intense radiation or extreme heat.

These findings provide fresh insights into how black holes not only consume matter but can also expel it back into space under specific conditions.

This feedback process plays a critical role in galaxy evolution, affecting nearby stars and gas and potentially contributing to the structure of the universe as we know it.

“This discovery highlights the effective collaboration that underpins all ESA missions,” noted XMM-Newton project scientist and ESA astronomer Dr. Eric Courkers.

“By focusing on an active supermassive black hole, the two telescopes unveiled something unprecedented: rapid, ultrafast flare-induced winds similar to those generated by the Sun.”

“Interestingly, this suggests that solar physics and high-energy physics may operate in surprisingly similar fashions throughout the universe.”

The team’s paper was published in the December 9, 2025 issue of the journal Astronomy and Astrophysics.

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Gu Lee Yi et al. 2025. Investigating NGC 3783 with XRISM. III. Emergence of ultra-high-speed outflow during soft flares. A&A 704, A146; doi: 10.1051/0004-6361/202557189

Source: www.sci.news

Astronomers Uncover 50-Million-Light-Year-Long Spinning Cosmic Web Filament

A recently uncovered galactic filament measures at least 50 million light-years in length and is situated 140 million light-years away. A galaxy orbits around the filament’s core, making it one of the largest rotating structures found to date.



Illustration depicting the rotation (right) of neutral hydrogen in a galaxy situated within an elongated filament (center). The galaxies demonstrate coherent bulk rotational motion that traces a large-scale cosmic web (left). Image credit: Lyla John.

Cosmic filaments stand as the largest known structures in the universe, comprising extensive thread-like formations of galaxies and dark matter that serve as the framework of the cosmos.

They also function as “highways” through which matter and momentum funnel into galaxies.

A nearby filament, home to numerous galaxies spinning in the same direction, represents an excellent opportunity to investigate how galaxies developed their current spin and gas content.

This structural arrangement could also provide a basis to test theories regarding how the universe’s rotation accumulates over vast distances.

In a recent study, astronomer Lyra Jung and colleagues from the University of Oxford discovered that 14 nearby hydrogen-rich galaxies form a slender line stretching approximately 5.5 million light-years long and 117,000 light-years wide.

This alignment exists within a considerably larger cosmic filament, about 50 million light-years long, which encompasses over 280 additional galaxies.

Notably, many of these galaxies seem to rotate in the same direction as the filament itself, a pattern that exceeds what would be expected if their rotation were random.

This observation challenges existing models and implies that the universe’s structure may have a more potent and prolonged impact on galaxy rotation than was previously assumed.

Astronomers observed that galaxies flanking the filament’s core were moving in opposite directions, suggesting that the entire formation is in motion.

The team employed a model of filament mechanics to estimate a rotational speed of 110 km/s and calculated the radius of the filament’s dense core region to be about 163,000 light-years.

“What makes this structure remarkable is not just its size, but also the interplay of spin arrangement and rotational motion,” stated Dr. Jung.

“You can liken it to a teacup ride at a theme park. Each galaxy represents a spinning teacup, but the entire platform, the cosmic filament, is also in rotation.”

“This dual motion provides valuable insights into how galaxies acquire rotation from the larger structures they inhabit.”

The filaments appear to be relatively young and undisturbed.

The significant number of gas-rich galaxies, minimal internal motion, and their so-called dynamically cool state imply that the galaxy is still in its formative stages.

Hydrogen serves as the fundamental material for star formation, meaning that galaxies rich in hydrogen gas are actively gathering and retaining the necessary fuel to create stars.

Thus, exploring these galaxies could yield insights into both the early and ongoing phases of galaxy evolution.

Hydrogen-rich galaxies also serve as excellent indicators of gas flow along cosmic filaments.

Due to atomic hydrogen’s susceptibility to motion, its presence aids in mapping how gas is directed through filaments and into galaxies, shedding light on how angular momentum travels through the cosmic web and influences galaxy shape, rotation, and star formation.

“This filament serves as a fossil record of the universe’s flow,” remarked astronomer Dr. Madalina Tudrache from the Universities of Cambridge and Oxford.

“It helps us comprehend how galaxies gain rotation and evolve over time.”

The researchers used data from the MeerKAT radio telescope in South Africa, one of the most powerful telescopes globally, comprising an array of 64 linked satellite dishes.

This rotating filament was detected via an extensive sky survey known as MIGHTEE.

By integrating this data with optical observations from the DESI and SDSS surveys, the study revealed cosmic filaments displaying both spin alignment and bulk rotation in coherent galaxies.

Professor Matt Jarvis from the University of Oxford stated: “This highlights the ability to combine data from various observatories to achieve a deeper understanding of how vast structures and galaxies form in the Universe.”

The findings are detailed in the following article: paper in Royal Astronomical Society Monthly Notices.

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Madalina N. Tudrache and others. 2025. A 15 Mpc rotating galactic filament with redshift z = 0.032 is available for purchase. MNRAS 544 (4): 4306-4316; doi: 10.1093/mnras/staf2005

Source: www.sci.news

Astronomers May Have Detected Signs of the Largest Star Ever Observed

Artist’s Impression of Population III Stars in the Early Universe

Noir Lab/NSF/AURA/J. da Silva/Space Engine/M. Zamani

The James Webb Space Telescope (JWST) offers astronomers a unique opportunity to explore distant galaxies that exist far beyond the early Universe. Some of these galaxies exhibit chemical signatures that may suggest the presence of exotic supermassive stars, possibly weighing up to 10,000 times that of our Sun.

These enormous stars are puzzling, as our current understanding suggests that stars in the nearby universe generally have a maximum size limit. “Our models for galaxy evolution are predicated on the assumption that stars cannot exceed around 120 solar masses,” explains Devesh Nandal at the Harvard-Smithsonian Center for Astrophysics, Massachusetts. “While we had theorized about stars potentially larger than this, there were no observational data to validate it.”

That all changed recently. Nandal and his team analyzed JWST observations of a distant galaxy dubbed GS 3073, discovering its chemical signature contained an unexpectedly high concentration of nitrogen. Though elevated nitrogen levels have also been noted in several other remote galaxies,

For most galaxies, nitrogen concentrations aren’t high enough to cause ambiguity and can be attributed to certain classes of relatively ordinary stars or other cosmic phenomena. However, this isn’t the case for GS 3073, as Nandal asserts that the nitrogen levels are simply too elevated.

There exists a hypothetical category of protostar referred to as a Population III star, which models indicate can grow to considerable sizes. Simulations suggest that if these stars form, they would produce significantly more nitrogen than typical stars. Nandal and his co-researchers concluded that only a handful of Population III stars—ranging from 1,000 to 10,000 solar masses—could account for the excess nitrogen observed in GS 3073. “Our research provides the most compelling evidence yet for the existence of Population III supermassive stars in the early universe,” he declares.

However, some scholars challenge whether only supermassive Population III stars can account for this data, or if they do so accurately. “Population III should be linked with an environment where elements heavier than helium are scarce,” notes Roberto Maiorino of Cambridge University. “Conversely, GS 3073 is a fairly chemically mature galaxy, which makes it seem ill-suited for the types of environments typically associated with Population III.”

On the other hand, John Regan from Maynooth University in Ireland suggests that this may simply be an unusual galaxy. “When we look back at the early universe, what we see are incredibly strange, exotic galaxies. It’s challenging to assert that we shouldn’t expect the formation of supermassive stars simply because it’s peculiar; you just claimed these galaxies are quite bizarre,” he states.

If these colossal stars truly exist, they may unlock mysteries related to the formation of supermassive black holes in the universe’s distant past. Should they originate from supermassive stars instead of conventional stars, we could gain critical insights into how these black holes achieved their immense sizes in what appears to be a relatively brief time frame.

Confirming the existence of supermassive stars in GS 3073 and other nitrogen-rich galaxies from the early Universe is complex, and additional discoveries of these chemical signatures may be necessary. “It’s quite challenging to bolster the argument for their existence; establishing definitive signatures is difficult,” Regan lamented. “Nonetheless, this indication is incredibly robust.”

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Source: www.newscientist.com

Astronomers Simulate Formation of Early Star Clusters – Sciworthy

The universe has undergone significant changes. Examining the contrasts between the universe as we perceive it today and its origin nearly 14 billion years ago is a crucial area of study for astrophysicists and cosmologists. Their focus is primarily on the first billion years following the Big Bang, when the first stars and galaxies began to emerge, marking the dawn of the universe. This was the initial phase when celestial objects began to emit light on their own rather than merely reflecting the remnants of the Big Bang, and it was also the first occurrence when elements heavier than helium started forming via nuclear fusion in stars.

In a recent study, a group of scientists utilized computer simulations to explore what star clusters looked like during the dawn of the universe. Their objective was to create models of star and galaxy formation that could be confirmed by new observations made by the JWST. This approach will enhance astronomers’ understanding of galaxy formation in the early universe, particularly the influence of galaxies on dark matter, which remains enigmatic, during the birth of the first stars from cosmic dust.

The research employed a cosmological simulation code called Arepo to recreate the dawn of the universe within a three-dimensional box measuring 1.9 megaparsecs on each side. This size converts to 60 quintillion kilometers or 40 quintillion miles. Within this box, the simulation contained 450 million particles representing early elemental matter, including hydrogen, helium, various isotopes, ions, and molecules that formed together. Additionally, it incorporated particles simulating known dark matter, which is affected by gravity but does not interact with other forces. When these aggregates of particles coalesced and surpassed a specific mass threshold known as jeans mass, the code indicated the formation of a star.

The team aimed to identify where the simulated stars and particles formed structures like star clusters, galaxies, and galaxy clusters. They implemented a method to group particles that were sufficiently adjacent to be considered connected, utilizing a friend of friends algorithm. By executing multiple iterations of this algorithm in the simulated universe—some focused on dark matter and others on ordinary matter such as stars, dust, and gas—the researchers sought to ascertain the arrangement of matter in the early universe.

The resulting simulated clusters were found to have dimensions comparable to actual clusters observed by astronomers in the early universe. However, no real clusters with metal-rich stars matching those in the simulations have yet been identified. Furthermore, the number of stars present in the simulated cluster was consistent with previous observations of distant star clusters recorded by the JWST. Many simulated star clusters were unstable, indicating they were not fully bound by their internal gravity. The team also found that as stable star clusters began merging into larger structures, such as galaxies, they became unstable once more.

An unexpected finding emerged from the study. The friend-of-a-friend algorithm produced varying results when assessing dark matter versus ordinary matter. The discrepancy reached up to 50%, implying that an algorithm targeting dark matter might detect only half the objects identified by an algorithm focused on regular matter. This variance depended on the mass of the identified star clusters or galaxies, particularly evident for objects within a moderate size range of 10,000 to 100,000 solar masses and very low masses around 1,000 solar masses.

The researchers could not ascertain the reasons behind this phenomenon, suggesting their simulations might be overly simplistic for accurately representing all conditions present during the universe’s dawn. Notably, they mentioned the absence of newly formed stars ejecting materials into space in their simulations. Consequently, they proposed treating their discovery as an upper limit on the frequency of star-like and, by extension, star-containing objects forming in the early universe. Their results might illustrate instances in nature where star formation occurs extremely efficiently, yet sorting out the roles of all involved processes remains necessary.

The conclusion drawn was that cosmic dawn clusters could have coalesced to create the foundations of modern galaxies or possibly evolved into the luminous cores of later galaxies. Additionally, the simulated clusters appeared to be strong candidates for forming medium-sized black holes, the remnants of which may be detectable with deep-space telescopes.


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Astronomers Reveal Pleiades Star Cluster is Integral to a Vast Stellar Structure

The Pleiades star cluster, also referred to as the Seven Sisters and Messier 45, is an open star cluster situated around 440 light-years away from Earth in the Taurus constellation. It forms the central core of a larger network that includes several known star clusters scattered over 600 parsecs (1,950 light-years). This network is known as the Greater Pleiades Complex and comprises at least 3,091 stars.



Pleiades star cluster. Image credit: NASA / ESA / AURA / California Institute of Technology / Palomar Observatory.

Stars originate from clouds of dust and gas. Clumps of this material come together and eventually collapse under their gravity, creating the hot core that becomes a star.

Star formation typically occurs in bursts, with numerous stars being born in rapid succession.

A collection of stars that form from the same molecular cloud is known as a star cluster.

These stars remain gravitationally bound to one another for thousands of years.

Over tens to hundreds of millions of years, the materials that birthed them are expelled by cosmic winds, radiation, and various astrophysical phenomena.

As this occurs, individual stars can merge into their host galaxies, making it complex to ascertain their relationships and trace their origins, especially after more than 100 million years have elapsed.

In a recent study, Dr. Luke Buuma from the Carnegie Institution for Science Observatory and his colleagues concentrated on the Pleiades star cluster.

Utilizing data from NASA’s TESS mission, ESA’s Gaia spacecraft, and the Sloan Digital Sky Survey (SDSS), they discovered that this cluster is the core of a broader structure of related stars spanning over 1,950 light-years.

“We refer to this as the Greater Pleiades Complex,” Dr. Bouma stated.

“It includes at least three known groups of stars, and likely two additional ones.”

“We confirmed that most members of this structure have origins in the same gigantic stellar nursery.”

A key aspect of their methodology is that a star’s rotation rate decreases with age.

The study utilized a combination of TESS’s stellar rotation data (made to detect exoplanets) and Gaia’s stellar motion observations (designed for mapping the Milky Way).

With this information, they developed a new method based on rotation to identify stars that share common origins.

“For the first time, by amalgamating data from Gaia, TESS, and SDSS, we confidently identified a new member of the Pleiades cluster,” reported Dr. Buma.

“Data from each mission alone was not enough to reveal the full scope of the structure.”

“However, when we integrated stellar motions from Gaia, rotations from TESS, and chemical data from SDSS, a coherent picture took shape.”

“It’s akin to piecing together a jigsaw puzzle, where every dataset provides a different piece of a larger whole.”

Besides their comparable ages, the authors highlighted that the stars in the Greater Pleiades cluster share similar chemical compositions and were once much closer to one another.

The fifth generation of SDSS data was employed for the chemical abundance analysis.

“The Pleiades star cluster has been pivotal in human observations of stars since ancient times,” Dr. Buma remarked.

“This research marks a significant advancement in understanding the changes in the Pleiades star cluster since its formation 100 million years ago.”

The researchers believe their findings carry broad implications.

The Pleiades is not merely an astrophysical benchmark for young stars and exoplanets but also a significant cultural symbol, referenced in the Old Testament and Talmud, celebrated as Matariki in New Zealand, and represented on the Subaru logo in Japan.

Professor Andrew Mann of the University of North Carolina at Chapel Hill stated, “We are starting to understand that many stars near the Sun belong to extensive star clusters with intricate structures.”

“Our study provides a novel method to uncover these hidden connections.”

A paper detailing the survey results has been published this week in the Astrophysical Journal.

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Andrew W. Boyle et al. 2025. Missing Sister Found: TESS and Gaia Reveal Dissolving Pleiades Complex. APJ 994, 24; doi: 10.3847/1538-4357/ae0724

Source: www.sci.news

Astronomers Uncover New Planetary Nebula in the Large Magellanic Cloud

Astronomers have identified a faint planetary nebula during a spectroscopic examination of stars in NGC 1866, a vast young globular cluster within the Milky Way satellite galaxy, known as the Large Magellanic Cloud. This nebula, designated Ka LMC 1, is situated near the core of NGC 1866.



This image shows NGC 1866 overlaid with a false-color representation from the MUSE data cube, highlighting the ionized shell of planetary nebula Ka LMC 1 as a red ring. The grayscale inset details the sizes of the ionization shells of singly ionized nitrogen. [N II] and doubly ionized oxygen [O III]. A magnified Hubble image reveals a pale blue star at the center, likely the hot central star of Ka LMC 1. Image credit: AIP / MM Roth / NASA / ESA / Hubble.

NGC 1866 is located at the edge of the Large Magellanic Cloud, approximately 160,000 light-years from Earth.

This cluster, also referred to as ESO 85-52 and LW 163, was discovered by Scottish astronomer James Dunlop on August 3, 1826.

Surprisingly, NGC 1866 is a young globular cluster positioned close enough for individual star studies.

In a recent spectroscopic investigation of NGC 1866, astronomers analyzed spectra captured by the MUSE Integral Field Spectrometer on ESO’s Very Large Telescope.

They made an unexpected and intriguing discovery: the ionized shell of a planetary nebula.

A subsequent study utilized images from the NASA/ESA Hubble Space Telescope to explore the nature of the object, which has been named Ka LMC 1.

“Planetary nebulae signify a late phase in a star’s evolution, during which the star consumes hydrogen for nucleosynthesis, expands as a red giant in a shell-burning phase, and eventually sheds most of its mass into a large, expanding shell. The remaining core then contracts and heats up, eventually cooling to become a white dwarf,” explained lead author Dr. Howard Bond, an astronomer at Pennsylvania State University and the Space Telescope Science Institute, along with his colleagues.

“Once the core surpasses 35,000 degrees, the shell ionizes and becomes visible through emission lines at specific wavelengths.”

The research team noted that Hubble images depict the hot central star of the Ka LMC 1 nebula.

“Ka LMC 1 is a genuine enigma. A young star cluster aged 200 million years implies that its progenitor star must be significantly massive,” noted astronomer Professor Martin Roth from the Potsdam Leibniz Institute for Astrophysics, the Institute for Physics and Astronomy at the University of Potsdam, and the German Center for Astrophysics.

“However, such a star would quickly evolve towards a cooling white dwarf stage.”

“Reconciling the age of the planetary nebula’s expanding shell with the theoretical evolutionary trajectory of its central star has been challenging.”

“This object undoubtedly demands further detailed observations to clarify its characteristics.”

“It presents a rare opportunity to observe star evolution over a timeframe that usually spans millions, if not billions, of years.”

“Yet, the evolution of massive central stars occurs in merely a few thousand years, making it possible to align with the timeline of the nebula’s expansion.”

According to a study published on November 7, 2025, in Publications of the Astronomical Society of the Pacific.

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Howard E. Bond et al. 2025. A faint planetary nebula was accidentally discovered in the massive young LMC star cluster NGC 1866. pasp 137, 114202; doi: 10.1088/1538-3873/ae1664

Source: www.sci.news

Astronomers Acquire Post-Perihelion Images of Interstellar Comet 3I/ATLAS

Recent observations of 3I/ATLAS, the third interstellar object confirmed to traverse the solar system following 1I/Oumuamua and 2I/Borisov, reveal a sophisticated multi-jet configuration.

The image of 3I/ATLAS was captured by Lowell Observatory astronomer Qicheng Zhang on October 31, 2025. Image credit: Qicheng Zhang / Lowell Observatory.

Discovered on July 1, 2025, by the NASA-funded ATLAS (Asteroid Terrestrial Impact Last Alert System) survey telescope in Rio Hurtado, Chile, 3I/ATLAS is also referred to as C/2025 N1 (ATLAS) and A11pl3Z.

Originating from the direction of the Sagittarius constellation, this comet holds the designation of being the most dynamically extreme object recorded, characterized by its hyperbolic orbit with high eccentricity and extreme hyperbolic velocity.

3I/ATLAS came closest to the Sun, reaching perihelion, on October 30, 2025.

This interstellar visitor approached within 1.4 AU (astronomical units), or approximately 210 million km, of the Sun, which is just inside Mars’ orbit.

At perihelion, the comet traveled at a remarkable speed of about 68 km/s, and its proximity to the Sun temporarily rendered it invisible to Earth’s telescopes.

Following perihelion, it will once again be observable through telescopes until December as it gradually distances itself from both the Sun and Earth, returning to interstellar space.

The initial post-perihelion optical image of 3I/ATLAS (as shown above) was captured. This was announced on October 31 by astronomer Zhang Qicheng of Lowell Observatory using the Discovery Telescope.

This image of 3I/ATLAS was taken on November 8, 2025 by astronomers from the ICQ Comet Observation Group. Image credit: M. Jaeger / G. Lehmann / E. Prosperi.

On November 8th, three astronomers from the ICQ Comet Observation Group observed the comet situated 29 degrees from the Sun in the sky.

The images they captured depict a complex jet structure with at least seven jets, including several anti-tail planes.

“Given the multitude of jets emerging in various directions, the noted non-gravitational acceleration of 3I/ATLAS implies that more than 10 to 20 percent of its initial mass would need to be ejected near perihelion,” remarked Professor Avi Loeb of Harvard University discussing the ICQ images. He stated,

“Only a small fraction of this mass carries the necessary momentum in the favored direction.”

“Consequently, the debris cloud enveloping 3I/ATLAS likely constitutes a considerable portion of the comet’s original mass.”

This 3I/ATLAS image was taken on November 9, 2025, by astronomers from the British Astronomical Society. Image credit: Michael Buechner / Frank Niebling.

On November 9th, two astronomers from the British Astronomical Association (BAA) studied the comet using two telescopes.

Their combined image displayed a long “smoking” tail along with two anti-tail jets.

“3I/ATLAS is expected to make its closest approach to Earth on December 19, 2025, making the multijet structure an intriguing target for future observations with the Hubble and Webb telescopes,” Professor Loeb mentioned discussing the BAA images. He noted.

The minimum distance to Earth will be 269 million km, roughly 100 times the extent of the jet structure illustrated in the image.

Source: www.sci.news

Astronomers Reveal Aging Stars Could Be Devouring Nearby Giant Exoplanets

During the concluding phase of their main sequence life, stars with mass comparable to the Sun experience a transformative evolution. This evolutionary process is likely to affect the surrounding planetary systems. As the star expands in its post-main-sequence stage, astronomers anticipate that most exoplanets detected to date may be engulfed by the growing star.



An artist’s impression of a sun-like star engulfing a giant exoplanet. Image credits: International Gemini Observatory / NOIRLab / NSF / AURA / M. Garlick / M. Zamani

Utilizing data from NASA’s Transiting Exoplanet Survey Satellite (TESS), astronomers Edward Bryant and Vincent Van Eylen studied 456,941 stars that have just commenced their post-main sequence phase.

By employing a computer algorithm, they targeted giant planets with short orbital periods (those that complete an orbit in less than 12 days) and searched for consistent dips in brightness that would indicate these planets transiting in front of their host stars.

They discovered 130 planets and planet candidates, including 33 previously unknown, closely orbiting these stars.

The researchers observed that such planets are less likely to exist around stars that have expanded and cooled sufficiently to be categorized as red giants (more evolved stars), implying that many of these planets might have already been destroyed.

Dr. Bryant, an astronomer at University College London and the University of Warwick, stated: “This provides compelling evidence that as stars progress beyond the main sequence, planets can rapidly spiral out of existence.”

“This topic has been debated and theorized for some time, but we can now observe this phenomenon directly and quantify it at the level of stellar populations.”

“We expected to observe this phenomenon, but we were still astonished by how effectively these stars can consume nearby planets.”

“This destruction is believed to stem from a gravitational tug-of-war between the planet and the star, known as tidal interactions.”

“As the star evolves and expands, these interactions intensify.”

“Just as the moon influences the Earth’s oceans, creating tides, planets also exert a pull on their stars.”

“These interactions decelerate the planet, reducing its orbit and causing it to spiral inward, ultimately resulting in its disintegration or absorption by the star.”

“In the coming billions of years, our sun will expand and transform into a red giant,” mentioned Dr. Van Eylen, an astronomer at University College London.

“Will the planets in our solar system endure this transformation? Our findings suggest that, in some instances, planets do not survive.”

“Earth may be better off than the giant planets much closer to the stars we examine.”

“However, we only analyzed the initial part of the post-main-sequence phase, spanning the first one or two million years. There is still ample opportunity for stellar evolution.”

“Unlike the giant planets lost in our investigation, Earth has the potential to endure the Sun’s red giant phase. However, life on Earth is likely to be extinguished.”

The team’s paper was published on October 15, 2025, in Royal Astronomical Society Monthly Notices.

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Edward M. Bryant and Vincent Van Eylen. 2025. Determine the impact of post-main sequence stellar evolution on the population of passing giant planets. MNRAS 544 (1): 1186-1214; doi: 10.1093/mnras/staf1771

Source: www.sci.news

Astronomers Discover Unexpectedly Large Black Hole in Nearby Diminutive Galaxy

Remarkably, Segue 1, an extremely faint dwarf galaxy, is positioned at the center of this image.

CDS, Strasbourg, France/CDS/Aladdin

Astoundingly, a supermassive black hole appears to reside at the heart of a nearby galaxy previously believed to be dominated by dark matter. Segue 1 is scarcely a galaxy, hosting merely around 1,000 stars compared to the Milky Way’s vast hundreds of billions. Yet, it seemingly contains a black hole with a mass approximately 10 times greater than the combined total of all its stars.

Segue 1 and similar dwarf galaxies lack sufficient stars to generate the gravitational force needed to hold them intact. To address this anomaly, physicists have long speculated that dark matter—a mysterious, invisible substance—fills the universe, contributing additional gravity.

Recently, Nathaniel Lujan and colleagues at the University of Texas at San Antonio began exploring computer models of Segue 1. They anticipated that the model yielding the best fit would be one characterized by dark matter. “After running hundreds of thousands of models, we were unable to find a viable solution,” Lujan remarks. “Eventually, we decided to experiment with the black hole mass, and that dramatically changed the results.”

The model that closely aligned with the observations of Segue 1 featured a black hole with a mass around 450,000 times that of the Sun. This discovery was particularly unexpected—not only due to the galaxy’s scarcity of stars but also considering its age. With so few stars, Segue 1 is estimated to have formed merely 400 million years following the universe’s initial star formation. Time constraints make it challenging for such a massive black hole to develop, especially since the much larger Milky Way likely consumed most of the gas that could have nourished Segue 1 shortly after its inception.

“This suggests there may be far more supermassive black holes than previously assumed,” Lujan states. If true, this could clarify some of the gravitational effects formerly attributed to dark matter, though it remains uncertain whether Segue 1 is typical of all dwarf galaxies. The quest for additional supermassive black holes continues.

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Source: www.newscientist.com

Astronomers Develop 3D Temperature Map of the Exoplanet WASP-18b

A newly released map of WASP-18b, a hot Jupiter exoplanet located approximately 325 light-years from Earth, showcases an atmosphere characterized by distinct temperature zones. Within this region, the scorching temperatures are capable of decomposing water vapor.

Hot Jupiter WASP-18b. Image credit: NASA’s Goddard Space Flight Center.

The WASP-18b map represents the first implementation of a method known as 3D eclipse mapping, or spectroscopic eclipse mapping.

This study features a 2D model. The paper, published in 2023 by members of the same research team, illustrated how eclipse mapping can leverage the sensitive observations from the NASA/ESA/CSA James Webb Space Telescope.

“This technique is unique in that it can simultaneously survey all three dimensions: latitude, longitude, and altitude,” stated Dr. Megan Weiner Mansfield, an astronomer at the University of Maryland and Arizona State University.

“This enables a greater level of detail than previously possible for studying these celestial objects.”

With this technology, astronomers can now begin to chart the atmospheric variations of many similar exoplanets observable through Webb, resembling how Earth-based telescopes once scrutinized Jupiter’s Great Red Spot and its striped cloud formations.

“Eclipse mapping allows us to capture images of exoplanets whose host stars are too bright for direct observation,” remarked Dr. Ryan Challenor, an astronomer at Cornell University and the University of Maryland.

“Thanks to this telescope and groundbreaking technology, we can start to understand exoplanets similarly to the neighboring worlds in our solar system.”

Detecting exoplanets is quite challenging as they typically emit less than 1% of the brightness of their host star.

Mapping a solar eclipse involves measuring a small fraction of the total brightness as the planet orbits behind the star, obscuring and revealing areas of the star in the process.

Scientists can link minute changes in light to specific regions, creating brightness maps. These maps can be rendered in various colors and translated into three-dimensional temperature readings based on latitude, longitude, and altitude.

“It’s quite difficult because you’re looking for changes where small sections of the Earth become obscured and then revealed,” Challenor explained.

WASP-18b has a mass approximately 10 times that of Jupiter, completes its orbit in just 23 hours, and achieves temperatures around 2,760 degrees Celsius (5,000 degrees Fahrenheit). Its strong signal makes it an excellent candidate for testing new mapping techniques.

While previous 2D maps relied on a single wavelength or color of light, the 3D map re-evaluated the same observations using Webb’s Near Infrared Imager and Slitless Spectrometer (NIRISS) across multiple wavelengths.

“Each color corresponds to different temperatures and altitudes within WASP-18b’s gaseous atmosphere, allowing them to be combined into a 3D map,” Dr. Challenor noted.

“Mapping at wavelengths that water absorbs can indicate the layers of water in the atmosphere, while wavelengths that water doesn’t absorb facilitate deeper probing.”

“When combined, these provide a three-dimensional temperature map of the atmosphere.”

The new perspective uncovered spectroscopically distinct zones (with varying temperatures and potentially different chemical compositions) on the visible dayside of WASP-18b (the side that perpetually faces its star due to its tidally locked orbit).

The planet exhibits a circular “hotspot” that receives the most direct stellar light, with winds insufficient to redistribute the heat.

Surrounding the hotspot is a cooler “ring” located closer to the planet’s visible outer edge.

Interestingly, the measurements indicated that water vapor levels within the hotspot were lower than the average for WASP-18b.

“We believe this suggests that the heat in this area is so intense that water is beginning to decompose,” explained Challenor.

“This was anticipated by theory, but it’s exhilarating to confirm it through actual observations.”

“Further observations from Webb could enhance the spatial resolution of this pioneering 3D eclipse map.”

“Already, this technique will aid in refining temperature maps of other hot Jupiters, which comprise hundreds of the more than 6,000 exoplanets discovered to date.”

Dr. Mansfield expressed: “It’s thrilling that we now possess the tools to visualize and map the temperature of another planet in such intricate detail.”

“We can apply this technique to other exoplanet types. For instance, even if a planet lacks an atmosphere, we might be able to use this method to map surface temperatures and discern its composition.”

“While WASP-18b was more predictable, we believe there’s potential to observe phenomena we never anticipated before.”

The map of WASP-18b is detailed in a paper published in the journal Nature Astronomy.

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RC Challenor et al.. Horizontal and vertical exoplanet thermal structures from JWST spectroscopic eclipse maps. Nat Astron published online October 28, 2025. doi: 10.1038/s41550-025-02666-9

Source: www.sci.news

Astronomers Observe Coronal Mass Ejection from Young Sun-Like Star

On Earth, we may not often realize it, but the sun regularly ejects massive clumps of plasma into space known as coronal mass ejections (CMEs). Astronomers, utilizing the NASA/ESA Hubble Space Telescope along with ground-based telescopes in Japan and South Korea, have begun to detect signs of multi-temperature CMEs. EK Draconis, a young G-type main sequence star, is located 112 light-years away in the northern constellation Draco.

Artist’s depiction of the coronal mass ejection from EK Draconis. Image provided by: National Astronomical Observatory of Japan

“Researchers believe that CMEs may have significantly impacted the development of life on Earth, given that the Sun was quite active in its early days,” stated Kosuke Namegata, an astronomer at Kyoto University, along with his colleagues.

“Historically, studies have indicated that young stars similar to our Sun often produce intense flares that surpass the largest solar flares recorded in contemporary times.”

“The massive CMEs from the early Sun could have drastically influenced the primordial conditions on Earth, Mars, and Venus.”

“Nevertheless, the extent to which these youthful stellar explosions produce solar-like CMEs remains uncertain.”

“Recent years have seen the detection of cold plasma in CMEs via ground-based optical methods.”

“However, the high speeds and frequent occurrences of significant CMEs predicted in earlier studies have yet to be confirmed.”

In their investigation, the authors concentrated on EK Draconis, a youthful solar analog estimated to be between 50 million and 125 million years old.

Commonly referred to as EK Dra and HD 129333, the star shares effective temperature, radius, and mass characteristics that make it an excellent analog for the early Sun.

“Hubble captured far-ultraviolet emission lines sensitive to high-temperature plasma, while three ground-based telescopes simultaneously recorded hydrogen alpha lines tracking cooler gas,” the astronomers explained.

“These synergistic multi-wavelength spectroscopic observations enabled us to observe both the hot and cold components of the eruption instantaneously.”

This research presents the first evidence of a multitemperature CME originating from EK Draconis.

“Our findings indicate that high-temperature plasma at around 100,000 K was ejected at speeds ranging from 300 to 550 km/s, followed approximately 10 minutes later by a lower-temperature gas around 10,000 K ejected at a speed of 70 km/s,” the astronomers reported.

“The hotter plasma contained significantly more energy than the cooler plasma. This implies that frequent intense CMEs in the past may have sparked strong shocks and high-energy particles capable of eroding or chemically altering the early atmospheres of planets.”

“Theoretical and experimental research suggests that robust CMEs and high-energy particles could play a key role in generating biomolecules and greenhouse gases vital for the emergence and sustainability of life on early planets.”

“Consequently, this discovery carries substantial implications for understanding the habitability of planets and the conditions under which life may have arisen on Earth—and potentially elsewhere.”

The team’s study was published in the journal Nature Astronomy.

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Namekata K. et al. Signs of multi-temperature coronal mass ejections identified in a young solar analog. Nat Astron published online on October 27, 2025. doi: 10.1038/s41550-025-02691-8

Source: www.sci.news

Astronomers Identify Three Earth-Sized Exoplanets in a Close Binary Star System

A researcher suggests that the binary star system TOI-2267 is likely home to two warm Earth-sized exoplanets and an additional candidate. A new paper published in the journal Astronomy and Astrophysics discusses these findings.



Artist’s impression of the binary star system TOI-2267. Image credit: Mario Sucerquia, Grenoble-Alpes University.

The system, known as G 222-3 or TIC 459837008, consists of the M5 type star TOI-2267A and the M6 type star TOI-2267B, which are separated by approximately 8 astronomical units.

Located about 22 parsecs (73.5 light-years) from the Sun in the constellation Cepheus, TOI-2267 presents a fascinating planetary arrangement.

Dr. Sebastian Zuniga Fernández, an astronomer at the University of Liege, stated, “Our analysis shows a distinct planetary configuration: two planets orbiting one star and a third planet orbiting its companion star.”

This discovery makes TOI-2267 the first known binary star system to host planets that transit around both stars.

Dr. Francisco Pozuelos from the Andalucía Astronomical Institute remarked, “Our findings set several records, making this star system the most compact and coolest known planet-planet pair, and it is the first observed instance of a planet transiting both components.”

Astronomers utilized the SPECULOOS and TRAPPIST telescopes along with their proprietary detection software, SHERLOCK, to identify the three planetary signals.

“Uncovering three Earth-sized planets within such a compact binary star system is an exceptional opportunity,” Dr. Zuniga-Fernández noted.

“This will enable us to scrutinize the limits of planet formation models in complex environments and deepen our understanding of the variety of planetary structures in our galaxy.”

The two confirmed planets, TOI-2267b and TOI-2267c, have orbital periods of 2.28 days and 3.49 days, respectively.

The authors currently cannot determine which star in the binary system the planets orbit.

When orbiting TOI-2267A, TOI-2267b and TOI-2267c exhibit radii of 1 and 1.14 Earth sizes, while their radii become 1.22 and 1.36 Earth radii when orbiting TOI-2267B.

Furthermore, researchers detected a third strong signal with a period of 2.03 days, which is still classified as a planetary candidate, having sizes of 0.95 or 1.13 Earth radii depending on whether it orbits TOI-2267A or TOI-2267B.

Dr. Pozuelos added, “This system serves as a genuine natural laboratory for exploring how rocky planets can form and persist under extreme mechanical conditions that were previously thought to endanger their stability.”

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S. Zuniga-Fernandez et al. 2025. Two warm Earth-sized exoplanets and an Earth-sized candidate planet in the M5V-M6V binary star system TOI-2267. A&A 702, A85; doi: 10.1051/0004-6361/202554419

Source: www.sci.news

Astronomers Unveil Moon Concealed in Earth’s Shadow

Astronomers have identified a peculiar “moon” that casts a shadow on Earth as it navigates through space. Dubbed quasi-moons, these entities don’t orbit our planet in a traditional manner, yet they maintain proximity as they travel around the sun.

According to a new study published in the American Astronomical Society Research Notes, this space rock may have been a companion to Earth for as long as 60 years.

The object, identified as 2025 PN7, is small enough that it might have evaded earlier detections. While its exact dimensions remain uncertain, researchers estimate it to be around 30 meters (98 feet) in diameter—approximately the wingspan of a typical short-haul airliner—making it the tiniest known quasi-moon associated with Earth.







“With rapid technological progress, we’re identifying near-Earth objects faster than ever,” said Dr. Darren Baskill, an astronomy lecturer at the University of Sussex, in BBC Science Focus. “The sensitivity of digital cameras has improved, allowing us to detect these faint objects, and computers can effectively process vast data sets.”

At its closest approach, this object comes within 300,000 km (186,400 miles) of Earth. Usually, it remains about 384,000 km (238,600 miles) away, but its horseshoe-shaped orbit can take it as far as 297 million km (185 million miles) from our planet.

Consequently, it’s only detectable when nearby, as occurred in August 2025, when researchers from Spain’s Complutense University of Madrid spotted it from the PanSTARRS Observatory in Hawaii.

Upon reviewing historical records, scientists identified it as a potential Earth companion for decades.

“The primary question is, where did 2025 PN7 originate?” Baskill noted. “At its closest, 2025 PN7 will be roughly the same distance from Earth as the Moon, providing insights into the Moon’s possible origin.

“Another clue can be observed on a clear night: the Moon is full of craters. Each impact casts debris into the atmosphere, and some material may escape the Moon’s gravity and be launched into space.”

Moon’s craters offer clues to the origin of space rocks – Photo credit: Getty

Another hypothesis suggests that the space rock originated in the asteroid belt, but Baskill states, “It’s challenging to gather sufficient light from such a moving object to determine its chemical composition and origin.”

He further added, “Astronomers must be patient and wait to observe PN7 when it’s at its brightest, closest to Earth.”

2025 PN7 is just one of seven quasi-satellites currently orbiting near Earth. The other is the space rock Kamooarewa, which is the target of China’s Tianwen-2 mission. Launched in May 2025, Tianwen-2 aims to collect samples from asteroids to understand more about Earth’s origins and asteroid formation.

“These near-Earth objects, due to their occasional close passes, might become prime targets for the inaugural mining operations beyond Earth, or even enter Earth’s atmosphere,” Baskill remarked.

PN7 will remain in existence until 2085 when it will be pulled from orbit by gravitational forces.

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Source: www.sciencefocus.com

Astronomers Capture Direct Images of Brown Dwarfs Orbiting Nearby Red Dwarfs

Astronomers utilized the Subaru Telescope, W.M. Keck Observatory, and ESA’s Gaia mission to capture images of the brown dwarf companion orbiting the M dwarf star LSPM J1446+4633.



NIRC2 image of J1446 taken in August 2023. The white arrow indicates the location of the new companion J1446B. Image provided by: Uyama et al., doi: 10.3847/1538-3881/ae08b6.

LSPM J1446+4633 (J1446) is a nearby mid-M dwarf, situated 17 parsecs (55 light-years) away.

The newly identified brown dwarf orbits its parent star at a distance approximately 4.3 times that of the Earth from the sun, completing an orbit every 20 years.

This object, designated J1446B, has a mass ranging from 20 to 60 times that of Jupiter.

“The success of this discovery was due to the combination of three complementary observational methods: (i) radial velocity (RV) measurements via long-term infrared spectroscopic monitoring by Subaru’s IRD instrument, (ii) high-resolution near-infrared imaging with advanced adaptive optics at the W.M. Keck Observatory, and (iii) precise astronomical acceleration measurements from ESA’s Gaia mission,” stated California State University astronomer Taichi Uyama and his team.

“By integrating these datasets and applying Kepler’s laws, we were able to determine the dynamic mass and orbital parameters of J1446B with unprecedented precision.”

“Radial velocity data by itself cannot differentiate between mass and orbital inclination, but the addition of direct imaging and Gaia data resolves this ambiguity.”

“The Subaru IRD-SSP program provided crucial RV data, while Keck’s cutting-edge adaptive optics allowed for the direct detection of the companion star at very close distances from the host star.”

“Previous studies have shown that astronomical acceleration from Hipparcos and Gaia can be combined with direct imaging to detect and analyze companion objects.”

“However, Hipparcos was unable to measure faint red dwarf stars like J1446.”

“Our study is the first to apply Gaia-only acceleration data to such a system, successfully constraining the orbit and dynamical mass of a brown dwarf companion.”

Near-infrared observations of J1446B indicated a brightness variation of about 30%, hinting at dynamic atmospheric phenomena such as clouds or storms.

“This finding serves as a significant benchmark for testing brown dwarf formation theories and atmospheric models,” the astronomers noted.

“Future spectroscopic studies may enable researchers to map the weather patterns on this intriguing object.”

“This achievement highlights the efficacy of combining ground-based and space-based observatories in discovering hidden worlds beyond our solar system.”

The team’s paper was published in Astronomy Magazine.

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Taichi Uyama et al. 2025. Direct Image Exploration for Companions with Subaru/IRD Strategic Program II. A brown dwarf companion star was discovered around the nearby medium-M dwarf LSPM J1446+4633. A.J. 170, 272; doi: 10.3847/1538-3881/ae08b6

Source: www.sci.news

Astronomers Discover Water Activity in Interstellar Object 3I/ATLAS

Astronomers have detected hydroxyl (OH) gas, a chemical indicator of water, from the interstellar object 3I/ATLAS using an ultraviolet/optical telescope on NASA’s Neil Gehrels Swift Observatory.



Stacked images of the interstellar comet 3I/ATLAS obtained with NASA’s Neil Gehrels Swift Observatory: the first was captured on July 31 and August 1, 2025 (visit 1, upper half), and the second was on August 19, 2025 (visit 2, lower half). Image credit: Xing et al., others, doi: 10.3847/2041-8213/ae08ab.

The identification of the third interstellar object, 3I/ATLAS, on July 1, 2025, initiated a comprehensive characterization effort globally.

Learning from prior discoveries of interstellar objects 1I/Oumuamua and 2I/Borisov, an observation campaign was implemented to swiftly measure its initial brightness, morphology, light curve, color, and optical and near-infrared spectra.

Given the apparent brightness and early extension of the coma, there was suspicion of a gas outburst, yet none was detected.

Investigating the early activity of interstellar objects is crucial for understanding their chemical and physical evolution as they approach the Sun, as this may signify the first notable heating during their extensive dynamic lifetimes.

“The discovery of water marks a significant step in our grasp of how interstellar comets evolve,” stated Dennis Bordewitz, an astronomer from Auburn University.

“For solar system comets, water serves as a baseline for scientists to gauge their total activity and track how sunlight stimulates the release of other gases.”

“This is the chemical standard against which all assessments of volatile ice in cometary cores are made.”

“Detecting the same signal in an interstellar object means we can for the first time position 3I/ATLAS on the same scale employed to study comets indigenous to our Solar System. This is a progress toward juxtaposing the chemistry of planetary systems throughout our Milky Way galaxy.”

“What’s fascinating about 3I/ATLAS is the location of this water activity.”

Swift noticed the hydroxyl groups when the comet was nearly three times further from the Sun than Earth (well beyond the area where water ice on the surface could easily sublimate), recording a water loss rate of approximately 40 kg per second. At such distances, most solar system comets remain inactive.

The robust ultraviolet signal from 3I/ATLAS implies there might be additional mechanisms at play. Possibly, sunlight is warming small ice particles expelled from the core, causing them to vaporize and contribute to the surrounding gas cloud.

Such extensive water sources have only been detected on a limited number of far-off comets, suggesting intricate layered ice that holds clues regarding their formation.

Every interstellar comet discovered to date has unveiled a distinct aspect of planetary chemistry beyond our Sun.

Collectively, these observations illustrate that the composition of comets and the volatile ice that constitutes them can vary considerably from one system to another.

These variations imply the diversity of planet-forming environments and how factors like temperature, radiation, and composition ultimately influence planetary formation and, in some instances, the materials that lead to life.

Capturing the ultraviolet signals from 3I/ATLAS was a technological achievement in itself.

Swift employs a compact 30 cm telescope, yet from its orbit above Earth’s atmosphere, it can detect wavelengths of ultraviolet light that are largely absorbed by the atmosphere.

Free from sky glare or air interference, Swift’s ultraviolet/optical telescope achieves the sensitivity comparable to that of ground-based telescopes with 4-meter apertures for these wavelengths.

Its rapid targeting abilities allowed astronomers to analyze comets just weeks after their discovery, well before they become too faint or too close to the Sun for space study.

“When we observe water from an interstellar comet or its subtle ultraviolet signature (OH), we are interpreting notes from another planetary system,” Bordewitz notes.

“This indicates that the components essential for life’s chemical processes are not exclusive to us.”

“All interstellar comets we’ve observed thus far have been unexpectedly intriguing,” remarked Dr. Zexy Shin, a postdoctoral fellow at Auburn University.

“‘Oumuamua was dry, Borisov was rich in carbon monoxide, and now Atlas is revealing water at a distance we didn’t anticipate.”

“Each of these cases is transforming our understanding of how planets and comets form around stars.”

A study detailing the survey findings was published on September 30th in Astrophysics Journal Letter.

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Zexy Shin et al. 2025. Water production rate of interstellar object 3I/ATLAS. APJL 991, L50; doi: 10.3847/2041-8213/ae08ab

Source: www.sci.news

Astronomers Say: Infant Space Is Warm, Not Cold, Before It Begins to Illuminate

Astronomers utilizing CSIRO’s Murchison Wide Field Array (MWA) telescope are on the quest to uncover the elusive period of reionization. This early stage in the universe’s history has been theorized but remains undetected by radio telescopes. This period marks the end of the universe’s dark ages, occurring approximately a billion years post-Big Bang, during which intergalactic gases transform from opaque to transparent, enabling light from the first stars and galaxies to permeate the cosmos.

A glimpse of the sky observed in radio waves by the Murchison Wide Field Array. Image credit: Nunhokee et al. / ICRAR / Curtin University.

“Our research was conducted in two phases,” stated Dr. Riddhima Nunhokey, an astronomer at Curtin University Node of the International Center for Radio Astronomical Research for All Sky Astrophysics (ICRAR).

“In the initial phase, we discovered the first signs of heating in the intergalactic gas—the intergalactic medium—around 800 million years after the Big Bang.”

“To examine this primordial phase of the universe, we must isolate faint signals from this epoch while eliminating all other sources of cosmic radio emissions.”

“These sources include emissions from nearby celestial bodies, interference from Earth’s atmosphere, and even noise generated by the telescope itself.”

“Only after meticulously subtracting these ‘foreground signals’ can we discern the signals from the era of reionization.”

“From this study, we have developed methods to manage foreground contamination and remove unwanted signals, thus enhancing our understanding of telescopes and improving the clarity of detected signals.”

“We are also able to integrate nearly a decade’s worth of MWA data, allowing us to make observations over a longer timeframe than before.”

“This is another reason we are closer than ever to detecting the signals.”

The team asserts that the enhanced quality and quantity of this new dataset made this discovery feasible.

The cold universe is producing signals that resemble these new data.

This absence of signals indicates that reionization must have commenced from a “cold start,” implying that the universe was “preheated” prior to the reionization phase.

“As the universe expands, intergalactic gases cool down, and thus we expect them to become extremely cold,” explained Professor Cathryn Trott, an astronomer at ICRAR’s Curtin University Node, associated with Astro 3D and the Curtin Institute of Radio Astronomy.

“Our measurements suggest that there is a certain level of heating present. While it may not be substantial, it does indicate that extremely cold reionization is unlikely, and that’s quite intriguing.”

“This study implies that this heating is probably influenced by energy from early black holes and primordial X-ray sources resulting from stellar remnants spread across the universe.”

The findings are presented in two papers in the Astrophysical Journal.

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CD Nunhokee et al. 2025. The 21 cm power spectrum limit of z = 6.5–7.0 based on Murchison wide field array observations. APJ 989, 57; doi:10.3847/1538-4357/adda45

Cathryn M. Trott et al. 2025. Utilizing Gaussian information to enhance the limit of the 21 cm signal at z = 6.5–7.0 using Murchison wide field array data. APJ 991, 211; doi: 10.3847/1538-4357/adff80

Source: www.sci.news

Astronomers Unveil Stunning Image of the M87 Black Hole Jet

Jets erupting from the black hole at the heart of the Galaxy M87

Jan Röder; Maciek Wielgus et al. (2025)

Over a hundred years ago, Heber Curtis identified the inaugural black hole jet, a tremendous stream of heated plasma emerging from the supermassive black hole located in the core of the Galaxy M87. The James Webb Space Telescope is currently scrutinizing this jet with remarkable precision.

Since its initial observation in 1918, the M87 jet gained fame for being connected to the first imaged black hole in 2019; however, it has been analyzed by various telescopes and is arguably the most extensively studied black hole jet. Yet, many aspects of its behavior, like some intensely luminous regions and darker spiral-shaped sections, still lack thorough explanation. Astronomers suspect these may be the result of jet beam refocusing or varying chains that form upon interacting with new materials like the dense gaseous regions. Nonetheless, the fundamental mechanisms remain elusive.

Recently, Maciek Wielgus from the Institute of Astrophysics in Andalusia, Spain, along with his colleagues, utilized the James Webb Space Telescope (JWST) to further unveil the famous luminous features of the M87 jets. They also succeeded in capturing a striking and less frequently observed counterjet that shoots out in the opposite direction from the other side of the black hole.

Wielgus and his team analyzed data retrieved from another project examining the M87 star, where JWST’s infrared sensors proved particularly effective. The overwhelming starlight complicated the jet analysis, necessitating the data to be re-evaluated to filter out the extraneous light. “This is a classic example of what astronomers often describe as using another’s discarded data,” notes Wielgus.

The first bright region identified in the jet is termed Hubble Space Telescope 1, in acknowledgment of the discovering telescope, and is believed to result from the jet’s compression entering a higher pressure environment. This phenomenon resembles the bright diamond-shaped patterns seen in rocket engine exhausts.

Researchers can also observe the far end of the jet on the opposite side of M87. As it propels away from us at speeds nearing the speed of light, Einstein’s theory of special relativity renders it much dimmer than it inherently is. However, when this beam encounters another area of gas with varying pressures, it expands and becomes perceptible.

This indicates the end of the material foam surrounding M87, alongside the visible termination of the jet nearest to us. With the imaging of the other end of the jet in such detail in infrared, astronomers can commence modeling the gas structures present within this bubble, states Wielgus.

The Mystery of the Universe: Cheshire, England

Join some of the leading scientific minds for a weekend exploring the enigmas of the universe. Engage in an exciting agenda that includes a visit to the renowned Lovell telescope.

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Source: www.newscientist.com

Astronomers Uncover the Most Distant Black Hole Ever Detected

A newly identified supermassive black hole resides in the center of the “Little Red Dot” galaxy, known as Capers-LRD-Z9, existing merely 500 million years after the Big Bang.



Artistic impressions of Capers-Lrd-Z9. Image credit: Erik Zumalt, University of Texas, Austin.

“Finding a black hole like this pushes the limits of what we can currently detect,” remarked Dr. Anthony Taylor, a postdoctoral researcher at the University of Texas at Austin.

“We’re truly expanding the boundaries of technological capability today.”

“While astronomers have identified more distant candidates, clear spectroscopic signatures for black holes have yet to be found,” noted Dr. Stephen Finkelstein from the University of Texas at Austin.

The astronomers conducted their research using data from the NASA/ESA/CSA James Webb Space Telescope, as part of the CAPERS (Candels-Area Prism Epoch of Reionization Survey) program.

Initially regarded as a mere speck in the program images, Capers-LRD-Z9 is now recognized as part of a newly classified category of galaxies called Little Red Dots.

“The find of the Little Red Dot was a surprising revelation from initial Webb data. It did not resemble the galaxies captured by the NASA/ESA Hubble Space Telescope,” Dr. Finkelstein explained.

“We are currently working to understand what they are and how they formed.”

Capers-Lrd-Z9 contributes to the growing evidence that the ultra-large black hole plays a critical role in the unusual luminosity of small red dots.

Typically, such brightness signifies a galaxy teeming with stars. However, in the absence of substantial stellar mass, these small red dots cease to exist.

These galaxies may also help clarify what causes the distinct red hue observed in small red dots, which is altered to a red wavelength as it passes through surrounding gas clouds encircling the black hole.

“I’ve observed these clouds in other galaxies,” Dr. Taylor stated.

“When I compared this object to others, it was unmistakable.”

Capers-LRD-Z9 merits attention due to the immense size of its black hole.

It’s estimated to be as massive as 300 million solar masses, equating to half the total star mass within the galaxy. This size is notably large, even among supermassive black holes.

By discovering such massive black holes early on, astronomers provide a unique opportunity to investigate the growth and evolution of these entities.

Black holes existing in later epochs had diverse opportunities for growth over their lifetimes, yet this was not the case during the initial hundreds of millions of years.

“This reinforces the increasing evidence that early black holes grew much faster than previously believed,” Dr. Finkelstein mentioned.

“Or they might have originated much larger than our models suggested.”

These findings are detailed in a paper published in the Astrophysical Journal.

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Anthony J. Taylor et al. 2025. Capers-Lrd-Z9: Gasensing Little Dot hosts Broadline’s active galactic nucleus at z = 9.288. apjl 989, L7; doi: 10.3847/2041-8213/ade789

Source: www.sci.news

Astronomers Discover Vast Numbers of Black Holes 12.8 Billion Light Years Away, Actively Growing

The immense black hole at the center of Radio Quasar RACS J032021.44-352104.1 (shortened to RACS J0320-35) is currently expanding at one of the fastest rates ever recorded.



Artist illustrations and x-ray images from Chandra for Racs J0320-35. Image credits: NASA/CXC/INAF-BRERA/IGHINA et al. / SAO / M. WEISS / N. WOLK.

The black hole residing in RACS J0320-35 has a mass approximately 1 billion times greater than that of the sun.

This system is situated about 12.8 billion light-years away from Earth, meaning astronomers are observing it as it existed just 920 million years after the universe’s inception.

It emits more X-rays than any other black hole identified in the universe’s first billion years.

Black holes are the driving force behind what scientists refer to as quasars.

This luminous giant’s energy is fueled by the significant amount of material that falls into the black hole.

The same research team discovered this black hole two years prior, but further observations from Chandra were required in 2023 to gain more insights.

Data from X-ray observations suggests that this black hole is expanding at a rate that exceeds the typical limits for such objects.

“It was somewhat surprising to observe such a dramatic growth in this black hole,” commented Dr. Luca Idina, an astronomer at the Harvard & Smithsonian Center for Astrophysics.

As material is drawn towards the black hole, it heats up and generates intense radiation across a wide spectrum, including X-rays and optical light. This radiation creates pressure on the infalling material.

Once the falling speed reaches a critical threshold, the radiation pressure counterbalances the black hole’s gravity, making it usually impossible for material to fall inward more rapidly. This upper limit is known as the Eddington limit.

Researchers believe that black holes growing slower than the Eddington limit must originate with solar masses exceeding 10,000, allowing them to achieve a mass of 1 billion solar masses in the early universe.

Such massive black holes may originate from unique processes, often linked to incredibly dense clouds of gas that contain heavier elements than helium.

Interestingly, RACS J0320-35 is expanding at a remarkable speed, estimated to be 2.4 times greater than the Eddington limit, indicating that its formation may have followed a more typical path, beginning with a mass of less than 100 solar masses resulting from massive star explosions.

“By determining a black hole’s mass and growth rate, we can infer its initial size,” said Dr. Alberto Moretti, an astronomer at INAF-Osservatorio Astronomico di Brera.

“This calculation permits us to evaluate various theories regarding the formation of black holes.”

To investigate how rapidly this black hole is growing (at rates between 300 and 3,000 solar masses per year), researchers compared the theoretical model with Chandra’s X-ray spectra, assessing the X-rays emitted at various energy levels.

The findings indicated that Chandra’s spectrum closely matched their expectations based on a model for black holes developing beyond the Eddington limit.

Supporting data from optical and infrared observations further corroborates the conclusion that this black hole is accumulating mass faster than the Eddington limit permits.

“How did the universe generate the first generation of black holes?” mused Dr. Thomas Connor, an astronomer at the Harvard & Smithsonian Center for Astrophysics.

“This is one of the most pressing questions in astrophysics, and this singular object propels our quest for answers.”

Moreover, this research also sheds light on the origins of the jets of particles emitted by some black holes that approach the speed of light, as observed in RACS J0320-35.

“Jets like these are uncommon in quasars, suggesting that the accelerated growth of black holes may play a role in the formation of these jets,” the author remarked.

Their paper is set to be published in the Astrophysical Journal.

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Luca Idina et al. 2025. X-ray investigation of the possibility of Super Eddington accretion in a wireless loudsal of Z = 6.13. apjl 990, L56; doi: 10.3847/2041-8213/aded0a

Source: www.sci.news

Astronomers Discover Rare Cloud-Forming Chemicals in Ancient Brown Dwarfs Dating Back a Billion Years

Utilizing data gathered by NSF’s Gemini South Telescope and NASA/ESA/CSA James Webb Space Telescope, astronomers have identified methane signatures (CH4), water (H2O), and silane (SiH4) in the cold brown dwarf gas WISEA J153429.75-104303.3 (shortened to W1534). Silanes are predicted to act as significant reservoirs of silicon, the element responsible for the large clouds of gas that surround giant worlds, but their presence had remained undetected until now, masked by the development of deep silicate clouds in the observable atmosphere.

This artist’s illustration depicts a brown dwarf with an atmosphere filled with gas and dust clouds. Image credits: Noirlab/NSF/Aura/R. Proctor.

The W1534, referred to as the accident, is situated approximately 50 light years from Earth in the Libra constellation.

This brown dwarf was likely formed between 100 and 120 billion years ago and ranks among the oldest brown dwarfs discovered to date.

First identified in 2020 by citizen scientists participating in the Backyard Worlds: Planet 9 Citizen Science Project, its unusual light profile captivated astronomers.

Using two of the world’s most advanced terrestrial and space-based telescopes, astronomers examined its atmosphere to analyze its properties and composition.

The survey commenced with NSF’s Noirlab Astronomer Sandy Leggett capturing near-infrared images of W1534 with a Gemini South telescope in Chile, part of the International Gemini Observatory.

This initial work laid the groundwork for further explorations using Webb, guided by Noirlab Astronomer Aaron Meisner.

“W1534 is quite faint, and Gemini South is the only ground-based telescope capable of detecting it,” Dr. Meisner stated.

“The Gemini discovery paved the way for Webb’s observations by revealing the deeper atmospheric layers of this mysterious object and enabling us to determine the exposure time necessary to gather useful near-infrared data on its composition.”

Within W1534’s atmosphere, the team uncovered the crucial signature of silane, a compound formed from silicon and four hydrogen atoms.

Planetary scientists have long theorized the existence of this molecule within gas giants, attributing potential significance to its role in cloud formation within the atmosphere.

Despite extensive searches, its atmospheric presence has remained elusive in our solar system’s gas giants, Jupiter and Saturn, although thousands of studies on brown dwarfs and gas giants orbiting other stars have occurred.

This marks the first discovery of silanes in any brown dwarf, exoplanet, or solar system object.

The absence of this molecule in all but one singular brown dwarf suggests intriguing insights into the chemistry occurring in such an ancient environment.

“Often, it is these extreme objects that help us understand the average,” remarked Dr. Jackie Faherty, a researcher at the American Museum of Natural History.

The presence of silanes in W1534’s atmosphere implies that in very ancient objects, silicon is capable of bonding with hydrogen to form lighter molecules that can ascend to the upper layers of a gas giant’s atmosphere.

In contrast, more recently formed objects, such as Jupiter and Saturn, result in silicon bonding with readily available oxygen, producing heavier molecules that settle deeper into the atmospheric layers.

The evidence gleaned from W1534’s atmosphere further validates astronomers’ comprehension of gas giant cloud formation and sheds light on how primitive conditions influence atmospheric composition.

Moreover, it indicates that worlds formed billions of years ago display characteristics distinctly different from those formed during the early solar system.

“The formation and detection of silanes highlight an essential relationship among composition, cloud formation, and atmospheric mingling in cold brown dwarfs and planetary atmospheres,” the authors concluded.

Their paper is published in the journal Nature.

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jk faherty et al. 2025. A silicate precursor silane detected in cold, low-metallic brown dwarfs. Nature 645, 62-66; doi:10.1038/s41586-025-09369-1

Source: www.sci.news

Astronomers Discover Protoplanets Forming in Disk Gaps Around Young Solar Analogues

Astronomers have successfully captured direct images of the 4.9 Jupiter Mass Protoplanet using ESO’s Very Large Telescope (VLT) sphere instruments, revealing clear gaps in the multi-ring protoplanetary disk. The star Whispit 2 (TYC 5709-354-1) is a solar analog, approximately 5 million years old, located 133 parsecs (434 light-years) away in the constellation Aquila.

This image taken with the ESO’s Very Large Telescope captures the first clear observation of a protoplanet within a disk featuring multiple rings. Image credit: ESO/Van Capelleveen et al.

A protoplanetary disk is typically accompanied by a ring and is a disc-shaped structure of gas and dust surrounding a young star.

These disks are the birthplaces of planets, with rings often suggesting the presence of hungry planets within the disk.

Initially, particles within the spinning disk begin to accumulate, drawing in more material from the surrounding disk until gravitational forces take hold, leading to the formation of an embryonic planet.

“Discovering Wispit 2B was an extraordinary experience. We were incredibly fortunate,” stated Dr. Richelle Van Capelleveen, an astronomer at the Leiden Observatory.

“Wispit 2, a younger version of our Sun, belongs to a small group of young stars, and we didn’t anticipate uncovering such an impressive system.”

“This system will serve as a benchmark for many years to come.”

“We’ve encountered many instances in our research,” remarked Christian Ginsky, a researcher at Galway University.

“However, in this case, we detected a remarkably unexpected and beautiful multi-ring dust disk.”

“Upon first encountering this multi-ring disk, I realized I had to attempt to detect the planets within it, immediately requesting follow-up observations.”

Astronomer captured a stunning transparent image of Whispit 2B situated in the gap of the disk, confirming that the planet orbits its host star.

“Wispit 2B marks the first clear detection of a planet on a multi-ring disk, providing an ideal setting for studying the interactions of planetary disks and their evolution,” they noted.

The Wispit 2B was observed in near-infrared light, retaining its brightness and heat from the initial formation phase.

The same is true for planets detected in visible light using the 6.5m Magellan Telescope MAGAO-X AO system and the large binocular interferometer (LBTI) Lmircam instrument.

This detection at specific wavelengths indicates that the planet is actively gathering gas as it develops its atmosphere.

“Located within the birth disk, Wispit 2B exemplifies a planet that can be utilized to explore current models of planet formation,” stated PhD student Chloe Lawler from Galway University.

The researchers estimated the radius of the disk surrounding Wispit 2B to be 380 AU (astronomical units) or about 380 times the distance between the Earth and the Sun.

“The discovery of Wispit 2B is remarkable,” commented Jake Byrne, a student pursuing an M.Sc. at Galway University.

The findings are detailed in two papers published in the Astrophysics Journal Letter.

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Richelle F. Van Capelvein et al. 2025. Wide separation planet (Wispit): A gap clear planet Wispit 2 of a multi-ring disc around a young solar-shaped star. apjl 990, L8; doi: 10.3847/2041-8213/ADF721

Laird M. Crows et al. 2025. Wide Separate Planet (Wispit): Discovery of GAPHα Protoplanet Wispit 2B Magao-X. apjl 990, L9; doi: 10.3847/2041-8213/adf7a5

Source: www.sci.news

Astronomers Uncover One of the Brightest and Fastest Radio Bursts Yet Recorded

Designated FRB 20250316A, this event, referred to as rbfloat (the brightest radio flash recorded to date), took place in the outer region of the nearby Spiral Galaxy NGC 4141.



Infrared image of Galaxy NGC 4141 featuring the rapid wireless burst FRB 20250316A. Image credits: NASA/ESA/CSA/CFA/Blanchard et al. / P. Edmonds.

The Fast Radio Burst (FRB) is a brief yet intense explosion of radio waves, primarily originating from distances beyond our galaxy.

The first FRB was detected in 2007, but an earlier observation was made six years ago in archival data from the Magellan Cloud Pulsar Survey.

These bursts last only a millisecond, hinting at the peculiar distributed pattern of radio pulsars.

They emit as much energy in a millisecond as the Sun releases over 10,000 years, yet the underlying cause remains a mystery.

Some theories propose that the characteristics of these bursts align with technologies of advanced civilizations, potentially arising from magnetized neutron stars or black holes interacting with surrounding gas.

The FRB 20250316A event was discovered on March 16, 2025. Located in the constellation Major Ursa, NGC 4141 is about 130 million light-years away.

Detection was accomplished using the Chime Outgar Array, where Canadian radio telescopes saw upgrades enabling precise FRB localization.

“With the Chime Outrigger, we’ve finally managed to capture these fleeting cosmic signals in real-time. We can narrow them down to specific stellar environments and individual galaxies,” noted one researcher.

Subsequently, Dr. Cook and her team employed the NASA/ESA/CSA James Webb Space Telescope to seek infrared signals from the same location.

“This was a unique opportunity to direct Webb’s powerful infrared capabilities toward the FRB’s position,” said Dr. Peter Blanchard, an astronomer at Harvard’s Center for Astrophysics.

“We were rewarded with remarkable results, revealing a faint source of infrared light very close to where the radio burst took place.”

“This could be the first object linked to an FRB found in another galaxy,” he added.

The infrared data from Webb indicated an object named NIR-1, likely a giant red star or possibly a giant middle-aged star.

A red giant is a sun-like star nearing the end of its life, expanding and becoming brighter, while the other possibilities are larger than the Sun.

Although these stars may not directly generate the FRB, they could possess invisible companions, such as neutron stars, that strip material from the red giants and massive stars. This mass transfer process might have triggered the FRB.

The advantages of a relatively close and precise location, coupled with sharp Webb images, permit the clearest observation of individual stars located near the FRB.

“Numerous theories have been proposed to explain FRBs, but up until now, there has been no data to test most of these ideas,” stated Professor Ed Berger from the Harvard & Smithsonian Center for Astrophysics.

“Isolating individual stars near the FRB is a significant improvement over previous searches, and we’re beginning to understand the stellar systems that could produce these powerful bursts.”

However, the red giant or massive star might not be connected to the FRB, prompting researchers to explore a larger area for further clues.

They discovered that the FRB was situated near a small cluster of young massive stars.

Given this positioning, they theorized that the giant stars in the cluster may collapse and form magnetars, leading to the FRB.

Magnetars are too dim to be directly seen in Webb’s observations.

The team examined various other potential explanations for the FRB, including objects from dense clusters of older stars and more giant stars.

These alternatives were deemed unlikely as they were brighter than the faint stars they observed.

“Regardless of whether the connection to the stars is real or not, we’ve learned a great deal about the origins of these bursts,” said Dr. Blanchard.

“If the double star system isn’t the solution, our findings imply that isolated magnetars could be responsible for the FRB.”

Another possible explanation for the infrared signals is that they may be reflected light from flares associated with the objects that triggered the radio bursts, potentially from magnetars. If this is the case, the infrared rays might diminish over time.

The team suggests more observations with Webb to search for such variations.

“We have taken a novel approach to unraveling the mystery of FRBs using Webb’s precise imaging, focusing on the exact position of the emitted FRBs,” Professor Berger remarked.

“We cannot predict when and where the next FRB will emerge, so we must be prepared to deploy Webb promptly when the moment arises.”

The team’s research paper was published in Astrophysics Journal Letters.

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Peter K. Blanchard et al. 2025. apjl 989, L49; doi: 10.3847/2041-8213/ADF29F

Source: www.sci.news

Astronomers Investigate Methods to Enhance Searches for Alien Technosignatures

A recent study indicates that a group of astronomers in Pennsylvania, along with NASA’s Jet Propulsion Laboratory, can determine when and where human deep space transmissions are most likely to be detected by extraterrestrial observers beyond our solar system. They can use observed patterns to inform searches for alien intelligence.

Analysis conducted on deep spacenetwork uplink transmission logs over the last two decades et al. It was found that these emissions mainly targeted the Sun or various planets. Image credit: Gemini AI.

“Humans primarily communicate with probes sent to explore spacecraft and other planets like Mars,” stated Pinken Hwang, a graduate student in Pennsylvania.

“Nevertheless, planets such as Mars do not obstruct entire transmissions, enabling spacecraft or celestial bodies along these interplanetary communication pathways to potentially detect signals.

“This implies that when searching for extraterrestrial communications, we need to consider planets outside our solar system that might align with our signals.”

“SETI researchers frequently scan the universe for indicators of past or current technology, referred to as Technosignatures, as potential signs of intelligent life.”

“By analyzing the direction and frequency of our most prevalent signals, we shed light on where we should enhance our chances of discovering alien technical stations.”

In this research, scientists scrutinized logs from NASA’s Deep Space Network (DSN), a global facility that enables two-way radio communication with human-made objects in space, serving as a relay to send commands and receive data from spacecraft.

They meticulously aligned the DSN logs with spacecraft location data to pinpoint the timing and direction of radio communications emanating from Earth.

Even though some countries have their own deep space networks, researchers argue that the NASA-operated DSN effectively represents the types of communications coming from Earth, as NASA has spearheaded the most profound space missions to date.

“The DSN establishes crucial connections between Earth and interplanetary missions, such as the NASA New Horizons spacecraft and the NASA/CSA James Webb Space Telescope.”

“It emits some of humanity’s most powerful and sustained radio signals into space, and the public logs of these transmissions have enabled our team to identify temporal and spatial patterns over the past 20 years.”

This study concentrated on transmissions directed into deep space, such as signals sent to interplanetary spacecraft, rather than those intended for low-Earth orbit satellites.

The researchers found that deep-space radio signals primarily targeted spacecraft close to Mars.

Other frequent transmissions were directed at telescopes situated at the Lagrange points near Earth and various planets. These points are areas where the gravitational forces of the Sun and Earth keep the telescope in a relatively fixed position from the perspective of Earth.

“Based on data from the last 20 years, we found that if extraterrestrial intelligence exists where we can observe the alignment of Earth and Mars, there is a 77% chance it falls within our transmission path.

“Furthermore, if they can see consistency with another planet in a solar system, there is a 12% chance they are on that transmission path.”

“However, these opportunities are quite substantial if planetary alignment is not observed.”

The team emphasized the need for humans to search for interplanetary alignments to enhance their quest for Technosignatures.

Astronomers routinely examine exoplanets during alignments with their host stars. In fact, the majority of known exoplanets were discovered by observing a star dimming as a planet passes in front of it.

“We only recently started detecting a significant number of exoplanets in the last 10 to 20 years, so we still lack knowledge about many systems that include more than two transiting exoplanets,” Fan noted.

“With the imminent launch of NASA’s Nancy Grace Roman Space Telescope, we anticipate the detection of 100,000 previously unknown exoplanets, which should significantly expand our search area.”

Our solar system is relatively flat, with most planets orbiting in the same plane, consequently, most DSN transmissions occurred within 5 degrees of Earth’s orbital plane.

If the solar system were metaphorically likened to a dinner plate with planets and objects lying on its surface, human transmissions would predominantly travel along the surface instead of leaping out into space at steep angles.

The authors also calculated that average DSN transmissions can be detected approximately 23 light-years away using telescopes similar to ours.

“Focusing on solar systems within 23 light-years, particularly those aligned in the plane towards Earth, could enhance our search for extraterrestrial intelligence,” they concluded.

The team is currently strategizing on identifying these systems and estimating how often they receive signals from Earth.

“Humanity is still in the early stages of our space exploration journey, and as we extend our missions into the solar system, transmissions to other planets will only increase,” remarked Professor Jason Wright of Penn.

“We have quantified ways to improve future searches for extraterrestrial intelligence by using our deep space communications as a benchmark to target systems with specific orientations and planetary alignments.”

The team’s paper was published online today in the Astrophysics Journal Letters.

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Ping Chen Fan et al. 2025. Detection of extraterrestrial civilizations employing a global-level deep space network. apjl 990, L1; doi: 10.3847/2041-8213/adf6b0

Source: www.sci.news

Astronomers Uncover Remarkably Rare Hierarchical Quadruple Material Systems

A newly identified quadruple star system, referred to as UPM J1040-3551 AABBAB, comprises a pair of cold brown dwarfs along with young red dwarfs.



An artistic depiction of the UPM J1040-3551 system amidst the Milky Way, as seen by the ESA Gaia satellite. On the left, the UPM J1040-3551 AA&AB is portrayed as a distant bright orange dot, showcasing the two M-shaped stars in orbit. Conversely, in the foreground on the right, a pair of cold brown dwarfs – UPM J1040-3551 BA & BB – have been on a long trajectory from each other for decades, collectively orbiting the UPM J1040-3551 AAB in a vast orbit taking over 100,000 years to complete. Image credits: Jiaxin Zhong / Zenghua Zhang.

The UPM J1040-3551 AABBAB system is situated in the constellation Antlia, approximately 82 light-years from Earth.

In this system, AAB denotes the brighter pairs AA and AB, while BAB refers to the more distant sub-components BA and BB.

“The hierarchical structure of this system makes the findings particularly intriguing, as it is essential for maintaining stable orbits over extended periods,” explains Professor Zenghua Zhang from Nanjing University.

“These two objects have orbited individually for decades, but collectively they have circled a common center of mass for more than 100,000 years.”

The two pairs are separated by 1,656 astronomical units (Au), where 1 Au represents the average distance from the Earth to the Sun.

The brighter pair, UPM J1040-3551 AAB, appears orange when viewed in visible wavelengths.

These stars possess a temperature of 3,200 K (approximately 2,900 degrees Celsius) and have a mass about 17% that of the Sun.

With a visual magnitude of 14.6, this pair is roughly 100,000 times dimmer than Polaris, the North Star, when viewed at visible wavelengths.

The fainter pair, UPM J1040-3551 BAB, comprises two cooler brown dwarfs that emit almost no visible light and are about 1,000 times dimmer than the AAB pair in near-infrared wavelengths.

These brown dwarfs are classified as T-type, with temperatures of 820 K (550 degrees Celsius) and 690 K (420 degrees Celsius), respectively.

“This is the first documented case of a quadruple system featuring a pair of T-type brown dwarfs orbiting two stars,” states Dr. Maricruz Gálvez-Ortiz, an astronomer at the Spanish Center for Astronomy.

“This discovery presents a unique opportunity for studying these enigmatic objects.”

“Brown dwarfs, alongside a diverse array of stellar companions, are invaluable for establishing age benchmarks,” comments Hugh Jones, a professor at the University of Hertfordshire.

“The UPM J1040-3551 system is particularly significant, as H-Alpha emissions from the bright pairs suggest that the system is relatively young, estimated to be between 200 and 300 million years old.”

The research team is optimistic that high-resolution imaging techniques could eventually resolve the brown dwarf pairs, facilitating precise measurements of their orbital dynamics and masses.

“This system offers a dual benefit for brown dwarf science,” remarks Adam Burgaster, a professor at the University of California, San Diego.

“It serves as both an age benchmark for calibrating cold atmospheric models and a mass benchmark for validating evolutionary models, provided that we can effectively resolve and track these brown dwarf binaries.”

“The discovery of the UPM J1040-3551 system marks a significant milestone in enhancing our understanding of these elusive objects and the various formation pathways of stellar systems near our Solar System.”

Findings are detailed in a study published in Monthly Notices of the Royal Astronomical Society.

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Zh Zhang et al. 2025. Benchmark Brown Dwarf – I. Blue M2 + T5 Wide Binary and Possible Young People [M4 + M4] + [T7 + T8] Hierarchical rectangles. mnras 542(2): 656-668; doi: 10.1093/mnras/staf895

Source: www.sci.news

Astronomers Uncover New Clues About Interstellar Comet 3I/Atlas

Hubble Space Telescope Image of Interstellar Comet 3i/Atlas. The telescope tracked the comet, causing background stars to appear as streaks.

NASA, ESA, David Jewitt (UCLA)/Joseph DePasquale (STScI)

The telescope’s observations of the Interstellar Comet 3i/Atlas have shown it resembles a comet found beyond our solar system. Intriguing aspects, like the substantial amounts of water detected even far from the sun, may shed light on the ancient stellar system from which it originated.

Objects from other solar systems that pass through ours are extremely rare. Discovered in July, 3i/Atlas is the third such interstellar visitor, following Oumuamua in 2017 and Borisov in 2019. Remarkably, its visit has only been a few months long.

Scientists speculate that its high speed may indicate that it originates from a star system billions of years older than our own. Initial estimates suggested it has a diameter of approximately 20 kilometers, but details about the extensive plume of water and gas remain limited.

Toni Santana Ross from the University of Barcelona and colleagues have utilized ground-based telescopes to observe the comet and its tail, finding it contains moderate amounts of dust. Notably, the dust appears to increase as the comet approaches the sun, mirroring patterns seen in comets from our outer solar system. “It’s a typical object; there’s nothing particularly strange about it,” states Santana Ross.

Astronomers have also monitored comets via space. Researcher collaborating found that the Hubble Space Telescope might estimate the comet’s size between 320 meters and 5.6 kilometers, and it likely started off much smaller.

Comets usually contain ice, which vaporizes as they near the sun, creating water vapor in their tails. Utilizing the Neil Gehrels Swift Observatory Satellite, Zexi Xing from Auburn University has detected water in the comet’s tail located significantly farther from the sun than is typical for comets. The amount of water detected suggests that about 20% of the comet’s surface is responsible for this production, exceeding typical solar system comet proportions.

Such prolific water generation may indicate that 3i/Atlas originates from a star system much older than ours, hypothesizes Cyrielle Opitom at the University of Edinburgh. This is due to older stellar systems generally having higher water content compared to other molecules. “It might be that because it formed earlier, it retains more water than other molecules, but it’s premature to reach a conclusion,” she remarks.

Astronomers are also scouring historical data to determine if the telescope mistakenly detected a comet. Adina Feinstein and her team at Michigan State University have found that the transit exoplanet survey satellite (TESS) was operationally searching for planets around other stars and incidentally captured a comet between May 7 and June 3. “It just happened that we were observing the exact region where 3i/Atlas was at that moment,” says Feinstein.

The comet was found to be surprisingly bright at that time, suggesting it was releasing significant amounts of water or gas even at considerable distances from the sun. “We didn’t detect transits in regions of our solar system where water would typically start to react,” highlights Feinstein.

In this distant region, the likelihood of finding water is low, with gases such as carbon monoxide and carbon dioxide being more common, according to Opitom. “This is a pattern seen in comets from our solar system; they can exhibit activity at much greater distances due to these volatile materials.”

Yet, the fact that it was active so far from the sun could indicate that this comet has not been significantly exposed to starlight throughout its life, notes Matthew Jenge from Imperial College London.

“What this implies is that this comet was ejected from the fringes of another solar system,” Genge describes. While the exact cause of its ejection is uncertain, it’s possible that gravitational forces from a nearby star could have set it on a trajectory towards us, he explains.

Opitom mentions that the James Webb Space Telescope has recently conducted its observations and that astronomers will analyze the data in the upcoming weeks, promising more insights into 3i/Atlas soon.

As comets approach their closest point to the sun in October, astronomers will have the opportunity to measure the gases they emit. This will provide important insights not only into the characteristics of the comet itself but also into the composition of the molecules in its active tail, which may reveal details about the formation of 3i/Atlas, according to Opitom.

Similar to previous interstellar objects, speculations about potential alien technology exist, but Santana Ross has found no supporting evidence. “If you take a holiday photo and see something tall with a long neck and four legs, you might think of it as an alien, but it’s most likely a giraffe,” he quips. “There’s no reason to believe this is anything unusual or evidence of something extraordinary.”

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Source: www.newscientist.com

Astronomers Uncover the Largest Black Holes Yet

Astronomers have discovered and quantified the largest black hole ever found. This colossal black hole approaches the theoretical maximum size allowable in the universe and is approximately 10,000 times the mass of Sagittarius A*, the supermassive black hole located at the center of the Milky Way.

This Hubble image features a horseshoe-shaped gravity lens (from center to right). Behind it is a blue galaxy, distorted into a horseshoe-shaped ring by the space-time distortion caused by the massive orange galaxies in the foreground. Image credits: NASA/ESA/Hubble.

The newly identified ultramassive black hole resides in the Space Horseshoe Gravity Lens System, which is among the largest known strong gravitational lenses.

This lens system, referred to as SDSS J1148+1930 and CSWA 1, lies 5 billion light years away in the Leo constellation.

“Typically, mass measurements of black holes in such distant systems can only be done when they are active,” remarks PhD Carlos Melo from Universidade Federativa do Rio Grande do Sul.

“However, these estimates based on accretion are often fraught with significant uncertainty.”

“Our method integrates strong gravitational lenses with stellar dynamics to yield more direct and reliable measurements, even in these distant systems.”

“The black holes we discovered rank among the top 10 largest black holes known, possibly even the largest,” adds Professor Thomas Collett from the University of Portsmouth.

“Most existing mass measurements for black holes are indirect and come with high uncertainties, so I can’t definitively say which one is the largest. But our new method provides much greater confidence in the mass of this black hole.”

The research team employed a synergy of gravitational lenses and stellar motions to locate the space horseshoe-shaped black holes.

This technique is considered the gold standard for black hole mass measurement, but galaxies are often too small in the sky to resolve areas containing these supermassive black holes, limiting effectiveness in distant contexts.

“The inclusion of a gravitational lens allowed us to explore further into the cosmos,” noted Professor Collett.

“We observed the influence of a black hole in two specific ways: it alters the path light takes as it navigates through the black hole, and stars in the galaxy’s core are observed moving incredibly fast (almost 400 km/s).”

“By correlating these two measurements, we can confidently establish the black hole’s authenticity.”

“This discovery pertains to a ‘dormant’ black hole, which does not actively consume material at the time of observation,” Melo explained.

“The detection relied solely on its immense gravitational pull and its effects on surrounding matter.”

“What’s particularly thrilling is that this method enables us to identify and gauge the masses of these elusive supermassive black holes across the universe, even when they lie completely dormant.”

An intriguing aspect of the Cosmic Horseshoe system is that its host galaxy is classified as a fossil group.

Fossil groups represent the final phase of the universe’s most colossal gravitationally-bound structures, formed from the collapse of a single, large galaxy devoid of bright companions.

“It is plausible that the supermassive black holes originally found in the companion galaxy contributed to the formation of the supermassive black holes we have identified,” Professor Collett noted.

“Thus, we can observe both the conclusion of galaxy formation and the cessation of black hole growth.”

The team’s paper was published today in Monthly Notices of the Royal Astronomical Society.

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Carlos R Melo-Carneiro et al. 2025. We are pleased to announce the discovery of a 36 billion solar-mass black hole at the core of the Cosmic Horseshoe Gravity Lens. MNRAS 541(4): 2853-2871; doi: 10.1093/mnras/staf1036

Source: www.sci.news