The newly identified Stephenson 2 DFK 52, an extraordinary red supergiant, is situated within the expansive stellar cluster RSGC2.
This image showcases the red supergiant star Stephenson 2 DFK 52 and its surroundings. Image credits: Alma / ESO / NAOJ / NRAO / Siebert et al.
RSGC2 is a cluster containing at least 26 red supergiants located at the base of the Milky Way’s diagonal crux spiral arm, approximately 5,800 parsecs (18,917 light-years) away.
Also referred to as Stephenson 2, this cluster is an active site for recent star formation where the arms intersect with galaxy bulges.
A team of astronomers led by Mark Siebert from Chalmers University of Technology observed the RSGC2 star using the Atacama Large Millimeter/submillimeter Array (ALMA).
“What we catch in this image of Stephenson 2 DFK 52 is indeed a supermassive red star that is shedding clouds of gas and dust as it approaches the end of its lifecycle,” they explained.
“Such nebulae are typically found around supermassive stars; however, this particular cloud presents an intriguing mystery for astronomers.”
“This cloud of ejected material is the most expansive discovered around a giant star, spanning an impressive 1.4 light-years.”
“Stephenson 2 DFK 52 is quite similar to Betelgeuse, another renowned red supergiant, so we anticipated observing a comparable cloud surrounding it.”
“If Stephenson 2 DFK 52 is as close to us as Betelgeuse, the surrounding cloud would appear about one-third the size of the full moon.”
Recent observations from ALMA have enabled astronomers to quantify the mass of material enveloping the star and analyze its velocity.
“Regions moving towards us appear in blue, while those receding are represented in red,” they stated.
“The data suggests that the star experienced a significant mass loss event about 4,000 years ago, followed by a slow-down in its current mass loss rate.”
The team estimates that Stephenson 2 DFK 52 has a mass between 10-15 solar masses and has already lost 5-10% of its mass.
“The rapid expulsion of such materials within a brief time frame poses a mystery,” the researchers commented.
“Could an unusual interaction with a companion star be responsible? Why does the cloud exhibit such a complex shape?”
“Understanding why Stephenson 2 DFK 52 has expelled so much material can illuminate insights into its eventual fate.
Mark A. Sheebert et al. 2025. Discovery of the extraordinary red supergiant Stephenson 2 DFK 52 within the expansive stellar cluster RSGC2. A&A in press; Arxiv: 2507.11609
Labeled L 98-59F, this exoplanet is an ultra-terrestrial with a minimum mass of 2.8 times that of Earth, orbiting within the habitable zone of the small red dwarf star L 98-59 every 23 days.
Artistic impressions of the L 98-59 Planetary System, with the habitable zone Super Earth L 98-59F in the foreground. Image credit: Benoît Gougeon/Udem.
L 98-59, also known as TOI-175 and TIC 307210830, is an M-type star with roughly one-third the mass of the Sun.
This stellar system is located approximately 34.5 light years away in the southern constellation of Volans.
It contains three transiting exoplanets discovered by TESS in 2019, along with an outer planet confirmed in 2021 using the ESO’s ESPRESSO spectrograph, with orbital periods of 2.25, 3.7, and 7.45 days.
The planets vary in size (0.8-1.6 times Earth’s radius), mass (0.5-3 times Earth’s mass), and potential compositions, likely leaning towards being water-rich.
In a recent study, astronomer Charles Cadigg and colleagues reanalyzed data from TESS, ESPRESSO, HARPS, and the Webb Space Telescope at the University of Montreal and the Exoplanetary Institute.
They achieved unprecedented accuracy in determining the sizes and masses of the planets.
“We refined the radii of L 98-59B, C, and D to 0.84, 1.33, and 1.63 Earth radii, respectively,” they reported.
“Our updated mass estimates are 0.46 Earth mass for L 98-59B, 2.0 for L 98-59C, and 1.64 for L 98-59D, with a minimum mass of 2.82 for L 98-59F.”
Astronomers confirmed the existence of a fifth planet, L 98-59F, located within the habitable zone of the star, where liquid water could exist.
“This discovery is particularly thrilling as we uncover temperate planets within such a compact system,” Dr. Cadiw remarked.
“It emphasizes the remarkable diversity of planetary systems and bolsters the argument for studying potentially habitable worlds around low-mass stars.”
“These new findings provide the most comprehensive view of the intriguing L 98-59 system to date,” he added.
“This exemplifies the potential of combining data from space telescopes and precision instruments, creating a crucial target for future atmospheric studies with the NASA/ESA/CSA James Webb Space Telescope.”
Precise measurements revealed the almost circular orbit of the innermost planet, a configuration conducive for future atmospheric detection.
“The varied rocky worlds and range of planetary compositions make L 98-59 a unique laboratory to explore some of the field’s most pressing questions. Do Super-Earths and Sub-Neptunes form differently around low-mass stars?” queried Professor Renée Doyon of Montreal University, director of the Trottier Institute for Exoplanet Research.
Charles Caddy et al. 2025. Detailed architecture of the L98-59 system and confirmation of the fifth planet in the habitable zone. AJ in press; Arxiv: 2507.09343
Utilizing the speckle imager Alopeke from the Gemini North Telescope, part of the NSF’s International Gemini Observatory, astronomers captured direct images of Betelgeuse.
Betelgeuse (right) and its remarkable companions (left). Image credits: International Gemini Observatory/Noirlab/NSF/Aura/M. Zamani, Noirlab of NSF.
Betelgeuse is an 8-million-year-old red supergiant located about 724 light years away on the shoulder of the Orion constellation.
It ranks among the largest known stars, with a radius approximately 1,400 times greater than that of the Sun.
Also referred to as Alpha Orionis or Alpha Ori, Betelgeuse is one of the brightest stars in the sky, radiating more light than 100,000 suns.
The star is nearing the end of its life cycle, and when it eventually explodes, the event will shine brightly, becoming visible for weeks even during daylight.
Betelgeuse experiences a major variability period of roughly 400 days, accompanied by a longer secondary period of about six years.
In 2019 and 2020, a significant drop in Betelgeuse’s brightness occurred, known as the “big dimming” event.
This led to speculation about an imminent supernova explosion, but astronomers later found that a large cloud of dust ejected during the dimming was the true cause.
Although the “big dim” mystery has been resolved, it rekindled interest in studying the red supergiant, prompting new analyses of existing archival data.
One analysis suggested that the presence of companion stars might be responsible for Betelgeuse’s six-year brightness fluctuations.
However, searches conducted by the NASA/ESA Hubble Space Telescope and the NASA Chandra X-ray Observatory did not detect these companions.
Dr. Steve Howell and his colleagues at NASA’s Ames Research Center investigated potential companions of Betelgeuse, referred to as Alpha Ori B or The Betelbuddy, using the Speckle Imager ‘Alopeke at the Gemini North Telescope.
“Speckle Imaging is an astronomical technique that employs very short exposure times to mitigate image distortion caused by Earth’s atmosphere,” they explained.
“This method allows for high resolution, and when combined with the light-gathering power of Gemini North’s 8.1m mirror, it enables the direct detection of faint companions of Betelgeuse.”
Analyzing the light from the companion stars allowed astronomers to identify their characteristics.
The companions appear to be A or B-type main-sequence stars, approximately six magnitudes fainter than Betelgeuse, with an estimated mass of around 1.5 solar masses.
The companion is situated relatively close to Betelgeuse, at about four times the distance between the Earth and the Sun.
This discovery marks the first detection of a close stellar companion orbiting a supergiant star.
Even more remarkably, the companions are within the extensive outer atmosphere of Betelgeuse, demonstrating the exceptional resolution capabilities of “Alopeke.”
“The speckle capabilities provided by the International Gemini Observatory prove to be a vital tool for astronomers across a wide range of applications,” stated Dr. Martin, NSF Program Director at the International Gemini Observatory.
“Providing solutions to the Betelgeuse mystery, which has persisted for centuries, is an exciting achievement.”
Survey results will appear today in the Astrophysical Journal Letters.
____
Steve Howell et al. 2025. Possibility of direct imaging discovery of the stellar companion to Betelgeuse. apjl in press; doi: 10.3847/2041-8213/adeaaf
Identified during a significant survey of a large sloping object (lido) and classified as 2020 VN40, this TransNeptunian entity is the first confirmed object that completes one orbit around the Sun for every ten orbits of Neptune. This discovery, detailed in a paper published in the Journal of Planetary Science, aids researchers in comprehending the behavior of distant objects in the outer solar system and their formation. It lends support to the theory that various remote objects are momentarily “captured” by the gravitational pull of Neptune as they traverse space.
Artist’s impressions of the Transneptunian object. Image credits: NASA/ESA/G. Bacon, stsci.
“This marks a major advancement in our understanding of the outer solar system,” remarked Dr. Rosemary Pike, an astronomer at the Harvard & Smithsonian Center for Astrophysics.
“It demonstrates that even the most remote areas influenced by Neptune can harbor objects, offering fresh insights into the evolution of the solar system.”
“This is merely the beginning,” commented Dr. Katherine Bolk, an astronomer at the Institute of Planetary Science.
“We are opening new windows into the history of the solar system.”
The discovery of 2020 VN40 was facilitated by the Lido Survey, which focused on identifying unusual objects in the outer solar system.
This research utilized the Canadian French Hawaii Telescope for primary observations, with supplemental observations conducted by the Gemini Observatory and Magellan Bird.
The study aimed to locate remnants with orbits extending well above and below the plane of Earth’s orbit around the Sun—an area of the outer solar system that has not been thoroughly examined.
“We’ve witnessed considerable effort and extensive results,” stated Dr. Samantha Lawler, an astronomer at the University of Regina and a member of the Lido team.
The average distance of VN40 in 2020 is approximately 139.5 times that of Earth’s distance from the Sun, following a notably tilted trajectory around the solar system.
The object becomes even more intriguing when considering its relationship with Neptune.
Unlike most objects that, based on their orbital duration ratios, are nearest to the Sun when Neptune is distant, the 2020 VN40 reaches its closest point to the Sun when Neptune is relatively nearby, based on its positional perspective above the solar system.
The inclination of the object’s orbit indicates that it is not positioned closely, as the 2020 VN40 is significantly lower than the general level of the solar system.
All other known resonant TransNeptunian objects have orbits that prevent such alignment when approaching the Sun, even from a flat perspective.
“This new discovery is like uncovering hidden rhythms in familiar songs,” expressed Dr. Ruth Murray Clay, an astronomer at the University of California, Santa Cruz.
“It has the potential to alter our understanding of the movement of distant objects.”
____
Rosemary E. Pike et al. 2025. Lido: Discovery of a 10:1 resonator with a new, obsolete state. Planet. SCI. J 6, 156; doi:10.3847/psj/addd22
Astronomers have, for the first time, been able to witness the early stages of solar system formation, discovering small entities that would eventually evolve into planets orbiting a distant young star.
This represents the earliest phase of planetary formation ever documented, giving us insight into our own solar system’s appearance shortly after the Sun ignited.
“We observe signs of planetary development – the transformation of tiny dust particles into slightly larger grains – and in some systems, this provides insight into earlier phases. Professor Merel Van ‘T Hoff, a co-author of the new study, elaborated on these findings. BBC Science Focus.
“This can be likened to researchers studying human evolution who, for the first time, can observe infants by examining young children.”
The Baby Planetary System is coming to life around a young star known as Hops-315, located 1,300 light years from Earth.
Stars in this early stage are thought to closely resemble our Sun, making them ideal subjects for uncovering the secrets of our solar system’s inception and Earth’s genesis.
Young stars like Hops-315 are enveloped by hot disks of gas and dust termed “protoplanetary discs.” Initially, these disks are extremely hot, causing silicon and iron – crucial planetary components – to be in gaseous form. However, as the disk cools, these elements begin to solidify.
Evidence from ancient meteorites in our solar system suggests that the first solid materials were formed from these discs, specifically crystalline minerals containing silicon monoxide (SiO).
These images illustrate how hot gas condenses into solid minerals around Baby Star Hops-315. The left image captures Hops-315 and its surroundings as seen by the Atacama Large Millimeter/Submillimeter Array (Alma). Two insets depict an artist’s representation of silicon monoxide molecules condensing into solid silicates – credit: ESO/L. Calsada/Alma (ESO/NAOJ/NRAO)/M. McClure et al.
Using the James Webb Space Telescope (JWST) and Atacama Large Millimeter/Submillimeter Array (Alma), international teams identified SiO in its gaseous form and as a newly formed crystalline mineral surrounding Hops-315, strongly indicating that solidification is just beginning.
“The first tiny minerals we observe clump together to form ‘pebbles,’ roughly the size of thumbnails,” Professor Melissa McClure, who led the research, stated. BBC Science Focus. “If they cluster closely enough, they can naturally collapse under their own gravity, forming bodies similar in size to kilometer-sized asteroids.
“Eventually, these will collide and merge, creating a planetary embryo, a full-sized rocky planet, or even the core of a gas giant like Jupiter.”
The research team plans to continue its observations of Hops-315 while also looking for other systems at this nascent stage of planetary evolution.
However, don’t expect to witness planetary formations in real-time. As Van’T Hoff remarked, “The timescale for disk evolution spans hundreds of thousands of years.”
Merrell van T. Hoff is an assistant professor at Purdue University in the United States. His research aims to understand how planets form and how frequently Earth-like planets exist in the Milky Way and other galaxies. Before joining Purdue, Professor Van’T Hoff was a postdoctoral researcher with the Michigan Fellows Association at the University of Michigan.
Melissa McClure is an assistant professor at Leiden Observatory in the Netherlands and a Beni Prize laureate. Her research employs observations and models to trace how solid building blocks of life (such as “dust” grains like ice and rocks) are incorporated from the formation of dense molecular clouds to the evolution of planets within protoplanetary discs and young exoplanets.
Research conducted by astronomer Matthew Hopkins and his team at Oxford University suggests that 3i/Atlas, the second interstellar comet discovered near our solar system, may have been on its trajectory over 3 billion years ago.
Top view of the Milky Way displaying the predicted orbits of our Sun and 3i/Atlas. Comets are represented by dashed red lines, while the sun is indicated by a dashed yellow line. The comet’s route to the outer thick disc is mostly clear, whereas the sun remains close to the nucleus of the galaxy. Image credit: M. Hopkins / Otautahi Oxford Team / ESA / Gaia / DPAC / Stefan Payne-Wardenaar / CC-SA 4.0.
“All comets formed alongside our solar system, like Halley’s comets, are up to 4.5 billion years old,” Dr. Hopkins explained.
“In contrast, interstellar visitors can be significantly older. Our statistical analyses indicate that 3i/Atlas is very likely to be the oldest comet we’ve observed thus far.”
Unlike 1i/Oumuamua and 2i/Borisov, the two previous interstellar objects that passed through our solar system, 3i/Atlas appears to be on a more inclined path through the Milky Way.
A recent study forecasts that 3i/Atlas is likely to be rich in water ice, as it probably formed around the star of the ancient, thick disc.
“This is an aspect of the galaxy that we’ve never encountered before,” said Chris Lintot, a professor at Oxford University and host of The Sky at Night.
“I believe there is a two-thirds chance that this comet predates the solar system and has been drifting through interstellar space ever since.”
As it nears the Sun, the heat from sunlight activates 3i/Atlas, generating a coma and tail composed of steam and dust.
Initial observations indicate that the comet is already active and may even be larger than any of its interstellar predecessors.
If this is validated, it could influence the detection of similar objects by future telescopes, such as the upcoming Vera C. Rubin Observatory.
Furthermore, it could offer insights into the role that ancient interstellar comets play in the formation of stars and planets throughout the galaxy.
“We’re in an exciting phase. 3i/Atlas is already displaying signs of activity,” remarked Dr. Michele Bannister, an astronomer at the University of Canterbury.
“The gases we might observe in the future, as 3i/Atlas is heated by the Sun, will help us evaluate our models.”
“Some of the world’s largest telescopes are currently monitoring this new interstellar entity. One of them may make a significant discovery!”
Jupiter’s surrounding space is among the most unique in our solar system, and the plasma present is equally remarkable, exhibiting unprecedented wave patterns.
Robert Lysak, from the University of Minnesota, explores Aurora phenomena. These captivating displays of green and blue light on Earth are accompanied by nearly undetectable ultraviolet rays near Jupiter’s poles.
To comprehend the auroras on this distant planet, it’s vital to grasp the intricacies of the plasma that generates these lights—a mix of charged particles and atomic components that envelopes the planet. Insights gathered from NASA’s Juno spacecraft have led Lysak and his team to identify that Jupiter’s Auroral Plasma resonates with a novel type of wave.
This newly identified wave is a combination of two well-characterized types of plasma waves: the Alfven wave, which arises from the motion of charged particles, and the Langmuir wave, which corresponds to electron movement. Lysak points out that since electrons are much lighter than charged particles, these two kinds of waves typically oscillate at vastly different frequencies.
However, the environment near Jupiter’s poles possesses conditions ideal for both waves to oscillate together. This is enabled by the low density of the plasma in that region and the strong magnetic field exerted by the planet.
“The plasma characteristics observed are truly unique when compared to those in other parts of our solar system,” states John Leif Jorgensen at the Institute of Technology Denmark. With Juno’s data uncovering new wave patterns, he believes we can learn more about the magnetic attributes of distant exoplanets by looking for similar signals.
Juno is currently in orbit around Jupiter, with Lysak noting that if its mission is extended, it could provide unparalleled insights into the giant planet and its complexities. This mission, however, is one among several that may face cuts due to proposed NASA budget reductions.
“Discontinuing missions while they are yielding valuable data would be a significant setback for our field,” concludes Lysak.
It seems that something might have struck Saturn. If so, amateur astronomers could play a crucial role in validating this potential historical event for the gas giant.
Approximately seven asteroids or comets are predicted to collide with Saturn each year, yet these instances often go unnoticed. Currently, NASA employee and amateur astronomer Mario Lana is capturing images that may reveal such an occurrence.
Lana is part of a project called Detect, which employs software to scrutinize images of Jupiter and Saturn, aiming to identify any brief flashes caused by impacts. If these flashes are detected through various telescopes, it can help eliminate the chance of a glitch and confirm the impact.
Ricardo Fuso from the University of Basque Country in Spain is also engaged in detection efforts, but Lana’s flashes are described as “a faint shock signature or just a bright pixel on the camera.” Specifically, astronomers are interested in footage of Saturn taken on July 5th UTC between 9:00 AM and 9:15 AM.
“If only one person witnessed this flash, then it might be an overstatement. Lee Fletcher at the University of Leicester, UK, commented, “If others also witnessed the flash, that’s fantastic; we confirmed an impact.”
Mark Norris, at the University of Central Lancashire in the UK, notes that the rising popularity of amateur astronomy and advances in telescope technology are beneficial. “There’s a good chance that someone has captured something they haven’t noticed yet or dismissed as a technical issue,” he notes.
That said, even if the impact is confirmed, the scientific value of the data may be limited due to insufficient information about the impacting object. Ideally, knowing its speed and mass in advance would facilitate observations, allowing us to assess the impact on known variables. This was the case in 1994 when Comet Shoemaker-Levy 9 impacted Jupiter.
3i/Atlas is only the third celestial object ever detected, following the interstellar asteroid 1i/Oumuamua in 2017 and the interstellar comet 2i/Borisov in 2019.
Images of 3i/Atlas captured by the Atlas telescope. Image credit: University of Hawaii.
The 3i/Atlas is currently about 670 million km (420 million miles) from the Sun and is expected to make its closest approach in October 2025, moving just within Mars’ orbit.
It is estimated to be up to 20 km (12 miles) in diameter, traveling at around 60 km (37 miles) per second relative to the Sun.
This comet poses no threat to Earth, remaining within a distance of 240 million km (150 million miles), which is more than 1.5 times the distance between the Earth and the Sun.
3i/Atlas is an active comet. As it approaches the Sun, the heat causes frozen gases to turn into vapor, releasing dust and ice particles into space and initiating the formation of a glowing coma and tail.
However, by the time it reaches its closest point to Earth, it will be obscured by the Sun. It is expected to be visible again by early December 2025, providing astronomers with an opportunity for further research.
“Finding possible interstellar objects is extremely rare, and it’s thrilling to see the Atlas telescope catch this asteroid,” said a representative.
“These interstellar visitors allow us to glimpse something intriguing from solar systems beyond our own.”
“3i/Atlas is the largest ever observed, yet numerous such objects traverse our inner solar system each year.”
“The likelihood of an impact with Earth is minimal, occurring less than once in 10 million years, but Atlas is consistently scanning the sky for potentially hazardous objects.”
Astronomers across Hawaii, Chile, and other nations are tracking the comet’s progression.
They seek to learn more about the composition and behavior of this interstellar visitor.
“It is precisely their foreign nature that makes interstellar objects like 3i/Atlas so remarkable,” an ESA astronomer stated.
“While all planets, moons, asteroids, comets, and life forms in our solar system share a common origin, our interstellar visitors are genuine outsiders.”
“They are remnants from other planetary systems, providing clues about the formation of worlds beyond our own.”
“It may take thousands of years before humans visit planets in another solar system, and interstellar comets give us the chance to stimulate our curiosity as we interact with something from another world.”
“These icy nomads offer a rare, tangible link to the broader galaxy. This material is fundamentally different from our own and is formed in unique environments.”
“Visiting such objects connects humanity with the universe on a grander scale.”
Following the interstellar asteroid 1i/Oumuamua and comet 2i/Borisov, 3i/Atlas is the third identified object and the second comet from outside the solar system.
This image was captured on July 2, 2025, with an Itemescope.net T72 telescope in Riojartad, Chile, depicting the interstellar comet 3i/Atlas. Image credit: Filipp Romanov/CC by-sa 4.0.
3i/Atlas was discovered by a NASA-funded research telescope dedicated to the Atlas (Asteroid Surface Impact Last Altar System) project on July 1, 2025, in Riojartad, Chile.
The interstellar comet approached from the direction of constellations and is currently about 670 million km (420 million miles) away.
“Since the initial report, pre-discovery observations have been gathered from archives of three different Atlas telescopes globally and from Zwicky’s transitional facility at Palomar Observatory in San Diego County, California,” a NASA astronomer wrote in a statement.
“These pre-discovery observations date back to June 14th, 2025.”
Known as 3I/ATLAS, C/2025 N1 (ATLAS), and A11PL3Z, it currently measures approximately 4.5 AU (670 million km, or 416 million miles) away.
Comets pose no threat to Earth, maintaining a safe distance of at least 1.6 AU (240 million km, or 150 million miles).
It is predicted to reach its closest approach to the Sun around October 30th, 2025, at a distance of 1.4 AU (210 million km, or 130 million miles).
Its size and physical characteristics are being studied by astronomers worldwide.
This diagram illustrates the trajectory of 3i/Atlas as it traverses the solar system. Image credit: NASA/JPL-Caltech.
If the brightness of 3i/Atlas is attributed to reflecting sunlight at a typical albedo of 10%, its diameter would be approximately 100-200 times greater than the estimated length of 20 km for Oumuamua and about 50-100 times larger than the estimated size of Borisov.
“If all three objects are indeed rocky, the mass of 3i/Atlas is more than 10 million times greater than that of Oumuamua and at least 100,000 times the core mass of Borisov.”
“This is remarkable because we expect high-mass objects to be exceedingly rare.”
“Based on data from the major asteroid belts of the solar system, we would expect millions of objects like Oumuamua for each object with the mass of 3i/Atlas.”
3i/Atlas should remain visible to ground telescopes until September 2025.
It is anticipated to reappear on the opposite side of the Sun by early December, enabling further observations.
“Based on its trajectory, 3i/Atlas seems to enter in a retrograde orbit, inclined at 175 degrees relative to Earth’s orbital plane from the thin disc of stars in the Milky Way,” explains Professor Roeb.
“In the upcoming months, we will gain further insights into the properties of 3i/Atlas based on data from various ground-based telescopes and the NASA/ESA/CSA James Webb Space Telescope, including the NSF/DOE Vera C. Rubin Observatory in Chile.”
The primordial stars, known as group III, likely formed from the abundant gases present in the young universe. These stars were responsible for generating the first heavier elements, illuminating the universe, bringing an end to the cosmic dark ages, and ushering in the era of reionization. Due to the challenges of direct observation, the characteristics of these early stars are still largely unknown. Professor Anastasia Fialkov from Cambridge University and her team suggest that astronomers can infer the masses of these stars by analyzing the cosmological 21 cm signal produced by hydrogen atoms located between the regions where the stars formed.
Artist’s impression of a field of Population III stars that would have existed hundreds of millions of years post-Big Bang. Image credits: noirlab/nsf/aura/J. da silva/SpaceEngine.
“This presents a unique opportunity to understand how the universe’s first light emerged from darkness,” stated Professor Fialkov.
“We are beginning to unravel the narrative of the transition from a cold, dark cosmos to one filled with stars.”
Studies focused on the universe’s ancient stars rely on the faint 21 cm signal, an energy signature emanating from over 13 billion years ago.
This signal, influenced by the radiation from nascent stars and black holes, offers a rare glimpse into the universe’s formative years.
Professor Fialkov leads the Leach theory group dedicated to radio experiments analyzing space hydrogen.
“Leach is a radio antenna and one of two key projects designed to enhance our understanding of the dawn and reionization phases of the universe, when the first stars reactivated neutral hydrogen atoms,” explained the astronomer.
“While our abilities to capture radio signals are presently undergoing calibration, we remain dedicated to unveiling insights about the early universe.
“Conversely, the Square Kilometer Arrays (SKAs) chart variations in cosmic signals across extensive areas of the sky.”
“Both initiatives are crucial for probing the masses, brightness, and distribution of the universe’s earliest stars.”
In their current research, Professor Fialkov and co-authors formulated a model to predict the 21 cm signal for both REACH and SKA, discovering that the signal is sensitive to the mass of the first stars.
“We are the first group to accurately model how the 21 cm signal correlates with the mass of the first stars, factoring in ultraviolet starlight and x-ray emissions resulting from the demise of the first stars,” stated Professor Fialkov.
“Our findings stem from simulations integrating the primordial conditions of the universe, such as the hydrogen and helium composition formed during the Big Bang.”
In developing their theoretical framework, researchers examined how the 21 cm signal responds to the mass distribution of Population III stars.
They discovered that earlier studies underestimated this relationship as they failed to account for both the quantity and luminosity of x-ray binaries among Population III stars and their impact on the 21 cm signal.
While REACH and SKA cannot photograph individual stars, they do provide comprehensive data on stars, x-ray binary systems, and entire galactic populations.
“Connecting radio data to the narrative of the first stars requires some imagination, but its implications are profound,” remarked Professor Fialkov.
“The predictions we present hold significant value in enhancing our understanding of the universe’s earliest stars,” noted Dr. Eloi de Lera Acedo from Cambridge University.
“We offer insights into the masses of these early stars, suggesting that the light they emitted may have been drastically different from today’s stars.”
“Next-generation telescopes like REACH are set to unlock the secrets of the early universe. These predictions are vital for interpreting radio observations being conducted from Karu, South Africa.”
The research paper was published online today in the journal Nature Astronomy.
____
T. Gessey-Jones et al. Determination of the mass distribution of the first stars from a 21 cm signal. Nature Astronomy Published online on June 20th, 2025. doi:10.1038/s41550-025-02575-x
Polycyclic aromatic hydrocarbons (PAHs) are believed to be the most prevalent class of organic compounds in the universe, yet their lifecycle in interstellar media remains poorly understood. Recently, astronomers using NSF’s Green Bank telescopes identified cyanocoronene (C24H11CN), the largest PAH discovered in space, located within the starless cloud core TMC-1.
Cyanocoronene, composed of seven interconnected benzene rings and cyano groups, is a region known for its abundant chemistry and was discovered in the cold, dark molecular cloud TMC-1, recognized as a new cradle for star formation. Image credits: NSF/AUI/NSF/NRAO/P.VOSTEEN.
Cyanocoronene is a derivative of coronene, often regarded as a prototype compact PAH due to its stability and distinctive structure.
PAHs are thought to play a crucial role in the chemistry that captures a significant portion of the universe’s carbon and contributes to star and planet formation.
Until this discovery, only smaller PAHs had been identified in space, making this finding a significant leap in understanding size limits.
“Each new detection brings us closer to understanding the origins of the complex organic chemistry in the universe, and possibly the building blocks of life,” says Dr. Gabi Wentzel, an astronomer at the Center for Astrophysics at MIT and Harvard & Smithsonian.
Dr. Wentzel and her team first synthesized cyanocoronene in the laboratory and recorded its unique microwave spectrum using advanced spectroscopic methods.
Equipped with this molecular fingerprint, the astronomers searched data from the Green Bank telescope, the primary instrument for the Gotham project (GBT observations of TMC-1: GBT observations of aromatic molecules).
They identified several spectral lines of cyanocoronene, confirming its presence with a statistical significance of 17.3 sigma, a robust detection by astronomical standards.
Cyanocoronene is currently the largest individual PAH molecule found in interstellar space, featuring 24 carbon atoms in its core structure (excluding the cyano group).
The quantity of cyanocoronene detected is comparable to that of smaller PAHs previously identified, challenging the notion that larger molecules are rare in the universe.
This indicates that even more complex aromatic molecules may be prevalent in the cosmos.
“The presence of such a large, stable PAH lends support to the idea that these molecules can serve as significant reservoirs of carbon and potentially facilitate the formation of new planetary systems throughout their lifecycle,” the researchers stated.
“The quantum chemical analysis in this study reveals that the reaction between coronene and CN radicals enables the efficient formation of cyanocoronene in cold space conditions.
“This implies that even prior to star formation, there can be chemical processes that establish complex organic matter.”
“The discovery of cyanocoronene not only adds new chapters to the narrative of astrochemistry but also reinforces the PAH hypothesis. It suggests that these molecules are responsible for the enigmatic infrared emission zones scattered throughout the universe.”
“Additionally, it establishes a direct link between interstellar clouds, meteoroids, and asteroid chemistry, implying that organic molecules present in our solar system might have originated in similar environments long before the Sun was born.”
Astronomers are making significant strides in comprehending how matter behaves and interacts in space utilizing fast radio bursts (FRB). They have found that over three-quarters of the universe’s ordinary material is concealed within sparse intergalactic gases, and they have also identified the furthest FRB event recorded to date.
This artist’s concept illustrates the density regions and red blank areas of the universe’s web in blue. Image Credit: Jack Madden/Illustristng/Ralf Konietzka/Liam Connor, CFA.
For many years, it has been established that at least half of the normal, predominantly proton-based baryonic material in the universe has gone unaccounted for.
Previous approaches by astronomers employed methods like X-ray and ultraviolet observations to gather significant clues regarding this missing mass, which manifests as extremely thin warm gases between galaxies.
The challenge arises from the high-temperature, low-density gas that remains mostly invisible to most telescopes, leaving scientists unable to assess its presence or distribution.
This is where FRBs come into play – brief, intense radio signals emitted by distant galaxies that researchers have recently demonstrated could measure baryonic matter in space, although its location remained a mystery until now.
In the latest study, scientists examined 60 FRBs, with the most distant FRB recorded at 1,174 million light-years (FRB 20200120E) from Messier 81 and reaching up to 9.1 billion light-years (FRB 20230521b).
This enabled them to pinpoint the missing material within intergalactic spaces or the intergalactic medium (IGM).
“The ‘baryon problem’ was never in doubt,” stated Dr. Liam Connor, an astronomer at the Harvard & Smithsonian Center for Astrophysics. “The issue has always been about its location. Now with FRBs, we’ve established that three-quarters of it exists between galaxies in the cosmic web.”
By analyzing the delays in each FRB signal as it traveled through space, Dr. Connor and his colleagues tracked the gaseous medium along its path.
“FRBs function like flashlights in space, illuminating the intergalactic medium. By accurately gauging how the light slows down, we can assess this medium, whether it’s starkly visible or barely detectable,” Dr. Connor explains.
The findings are revealing—approximately 76% of the universe’s baryonic matter resides within the IGM.
Additionally, about 15% is found in galaxy halos, with a minor fraction embedded within stars and cool galactic gases.
This distribution aligns with predictions made by advanced cosmological simulations, yet this is the first instance of direct confirmation.
“This marks a triumph for contemporary astronomy,” noted Dr. Vikram Ravi, an astronomer from California.
“Thanks to FRBs, we are now approaching a new understanding of the universe’s structure and composition.”
“These brief flashes enable us to trace the invisible baryonic matter filling the expansive voids between galaxies,” he added.
“Baryons are pulled into galaxies by gravity; however, supermassive black holes and supernova explosions can expel them back into the IGM, cooling cosmic temperatures when they spiral out of control,” commented Dr. Connor.
“Our findings indicate that this feedback mechanism is effective, suggesting gas must be displaced from galaxies into the IGM.”
The team’s results are published today in the journal Nature Astronomy.
____
L. Connor et al. Gas-rich cosmic web unveiled by the partition of missing baryons. Nature Astronomy Published online on June 16th, 2025. doi:10.1038/s41550-025-02566-y
Astronomers utilizing ESO’s Extremely Large Telescope (VLT) have captured stunning images of a highly structured planetary formation disc surrounding the star Rik 113.
This image, captured with a very large telescope at ESO in Chile, illustrates the RIK113 system. Image credits: ESO/Ginski et al.
RIK 113 is located approximately 431 light-years away in the constellation Scorpio.
Also referred to as 2MASSJ16120668-3010270, this star hosts a structured protoplanetary disc.
“In a study published last year, the intricate nature of this protoplanetary disc was first unveiled by the Atacama Large Millimeter/sub-millimeter Array (ALMA),” remarked Galway astronomer Christian Ginsky and colleagues.
“These findings indicated the presence of gaps, suggestive of planet-like objects within them.”
“This prompted the team to conduct follow-up observations using ESO’s Very Large Telescope (VLT).”
Employing VLT’s Sphere Instrument, Dr. Ginski and co-authors obtained a new image of the system, revealing an appealing spiral feature in the inner ring.
“Our team is currently examining nearly 100 planet-forming discs around nearby stars, and these images are exceptional,” Dr. Ginsky noted.
“It is rare to find a system exhibiting both rings and spiral arms. This aligns almost perfectly with predictions regarding how planets form from the parent disk, according to theoretical models.”
“Such detections bring us a step closer to comprehending how planets, in general, formed and the origins of our solar system in the far past.”
A detailed analysis of the VLT/Sphere data hinted at two potential signals, as well as two possible signals from a protoplanet orbiting Rik 113, close to the original detection by ALMA.
At this stage, these signals serve more as proposals than definitive confirmations.
Nonetheless, these results are highly promising for future explorations, with both ALMA and VLT studies indicating the presence of at least one planet.
“We identified an inner disc (up to 40 AU) with two spiral arms, which are separated by a gap from the outer ring extending to 115 AU,” the astronomer stated.
“Comparing with unique and hydrodynamic models from the literature, we found that these structures are consistent with the existence of embedded gas giants, with masses ranging from 0.1 to 5 Jupiter masses depending on the model and its underlying assumptions.”
“The RIK 113 system is one of the few that displays this remarkable form of spiral arms amidst the scattered gaps of light and the ring,” they added.
“We hypothesize that this could be linked to higher disk viscosity compared to other systems, such as PDS 70.”
“If a planet in the disk is confirmed, RIK 113 will become a focal point for studying planetary disk interactions.”
Study published online in the journal Astronomy and Astrophysics.
____
C. Ginsky et al. 2025. Disk evolution studies with imaging of nearby young stars (Destinys): 2MassJ16120668-3010270 Evidence of planetary disk interaction in the system. A&A in press; doi: 10.1051/0004-6361/202451647
A potential new dwarf planet has been identified at the distant fringes of our solar system, taking approximately 25,000 years to complete one orbit around the Sun.
This celestial object, designated 2017, was discovered by a team from the Advanced Research Institute and Princeton University who were searching for a “Planet 9,” a hypothesized planet larger than Earth that is believed to orbit beyond Neptune. Some astronomers suspect that this elusive Ninth planet could shed light on the peculiar clustering of various objects and other oddities observed in the outer solar system.
While in pursuit of the elusive Planet Nine, researchers instead came across another resident of our cosmic neighborhood.
“It’s similar to the way Pluto was discovered,” remarked Sihao Cheng, a member of the Advanced Research Institute that spearheaded the research team. “This endeavor was a real adventure.”
If validated, the newly found dwarf planet could be what Chen refers to as Pluton’s “extreme cousin.” The findings were published on the Preprint site arXiv and have yet to undergo peer review.
Cheng and his colleagues estimate that 2017 measures approximately 435 miles in diameter.
Dwarf planets are categorized as celestial bodies orbiting the Sun that possess enough mass and gravity to be nearly round, yet unlike typical planets, they do not clear their orbital paths of asteroids and other objects.
Eritayan, a co-author of the study and a graduate student at Princeton University, noted that one fascinating characteristic of 2017 is its highly elongated orbit. At its most distant points from the Sun, it lies over 1,600 times farther than Earth does from the Sun.
The potential dwarf planets were discovered through a meticulous examination of a vast dataset from a Chilean telescope that was scanning the universe for signs of dark energy. By compiling observations over time, the researchers identified moving objects exhibiting clear patterns.
While 2017 may be one of the most distant known objects in the solar system, its discovery suggests that other dwarf planets may exist in that vast region of space.
“We used public data that had been available for some time,” explained Jiaxuan Li, a graduate student and co-author of the research at Princeton University. “It was just hiding in plain sight.”
Li mentioned that the object is currently located near the Sun, necessitating a wait of about a month for researchers to conduct follow-up observations using ground-based telescopes. They also hope to eventually study the object with the Hubble Space Telescope or the James Webb Space Telescope.
In the meantime, Chen stated he remains committed to the quest for Planet Nine. However, new findings may complicate long-held theories about the existence of such a planet.
The hypothesis surrounding Planet Nine suggests that planets several times Earth’s size in the outer solar system might clarify why certain groups of icy objects seem to have unusually clustered orbits.
“Under the influence of Planet Nine, any object lacking a specific orbital geometry would eventually become unstable and be expelled from the solar system,” Yang explained.
Despite 2017’s long orbit leading it away from clustered objects, Yang’s calculations indicate that its path will remain stable for the next billion years.
In essence, if Planet Nine existed, 2017 would not persist. Yet, Yang emphasized that further research is essential, and the discovery of a new dwarf planet candidate does not definitively rule out Planet Nine’s existence.
For one thing, the simulations currently utilize a single hypothetical location for Planet Nine, and scientists do not all agree on the locations of these planets.
Konstantin Batygin, a planetary science professor at the California Institute of Technology, first proposed the existence of Planet Nine in a 2016 study co-authored with Mike Brown from Caltech.
He remarked that the discoveries related to 2017 neither confirm nor deny the theory. Batygin noted that outer solar system objects that might demonstrate gravitational influences of Planet Nine must have their closest points of orbit remain sufficiently distant and not interact significantly with Neptune.
“Unfortunately, this object does not fall into that category,” Batygin told NBC News. “It’s in a chaotic orbit, so the implications are not significant, as it complicates the scenario.”
Batygin expressed excitement about the new research for providing additional context regarding how objects evolve in the outer solar system, praising the researchers’ efforts in mining public datasets as “heroic.”
Chen, however, remains optimistic about finding Planet Nine.
“The entire project commenced as a search for Planet Nine, and I’m still in that mindset,” he remarked. “This, however, is an enthralling tale of scientific discovery. Whether or not Planet Nine exists, the pursuit is a captivating venture.”
The recently identified Transneptunian object, which was named in 2017, stands out as one of the most prominent objects in our solar system, measuring approximately 700 km in diameter, thus qualifying as a dwarf planet.
All cut-out images of 19 detections for 2017 2017. Image credits: Chen et al, arxiv: 2505.15806.
Transneptunian Objects (TNOs) are small celestial bodies that orbit the Sun at distances greater than that of Neptune.
In the 30 years following the discovery of the first TNO outside Pluto, numerous research initiatives have been launched to explore the expansive regions of the outer solar system, resulting in the identification of over 5,000 TNOs to date.
The newly discovered TNO is significant for two main reasons: its unique trajectory and substantial size.
“The object’s aphelion—the furthest point in its orbit from the Sun—is over 1,600 times the distance of Earth’s orbit,” states Dr. Sihao Chen, an astronomer at the Institute of Advanced Research and Boundary Research.
“Conversely, its perihelion—the closest point in its orbit to the Sun—is 44.5 times that of Earth’s orbit, akin to Pluto’s orbit.”
“This extreme trajectory takes around 25,000 years to complete, suggesting a complex gravitational history,” he adds.
“We likely experienced a close encounter with a massive planet, compelling us into this wide orbit,” comments Princeton University astronomer Dr. Elitas Yang.
“There may have been multiple phases in this transition.”
“The object might have initially been ejected into the Oort Cloud, the outermost region of the solar system, which is home to numerous comets.”
“Many extreme TNOs appear to follow similar trajectories, but 2017 OF201 stands out as an anomaly,” remarks Dr. Jiaxuan Li, also from Princeton University.
“This clustering is interpreted as indirect evidence suggesting the presence of another celestial body, often referred to as Planet X or Planet Nine, which could be influencing these objects through gravitational forces.”
“The existence of 2017 OF201 as an outlier in this clustering could potentially challenge this hypothesis.”
Astronomers estimate the diameter of 2017 OF201 to be 700 km, making it the second-largest object on such an extensive orbit.
“2017 OF201 can only be detected about 1% of the time when it is relatively close to us,” Dr. Chen notes.
“The presence of this solitary object implies that there may be around 100 other similar objects with comparable trajectories and sizes.”
Researchers discovered 2017 OF201 as part of an ongoing initiative to identify TNOs and potential new planets in the outer solar system.
The detection involved identifying bright spots in astronomical image databases from the Victor M. Blanco Telescope and the Canada France Hawaii Telescope (CFHT), as well as attempting to trace groups of possible spots that indicate TNO movement across the sky.
Scientists identified 2017 OF201 in 19 different exposures collected over a span of seven years.
“Although advancements in telescopic technology have allowed us to explore distant realms of the universe, much remains to be uncovered within our own solar system,” concludes Dr. Chen.
The team’s paper has been published online at arxiv.org.
____
Sihao Cheng et al. 2025. Discovery of new planet candidates in extremely wide orbits: 2017 OF201. arxiv: 2505.15806
A new “coronal adaptive optics” system has been developed by astronomers at the NSF’s National Solar Observatory and New Jersey Institute of Technology to generate high-resolution images and films by eliminating atmospheric blurring.
This image captures a 16-minute time-lapse film that illustrates the formation and collapse of a complex plasma stream measuring approximately 100 km per 100 km in front of a coronal loop system. This marks the first observation of such flows, referred to as plasmoids, raising questions about the dynamics involved. The image, taken by a Good Solar Telescope at Big Bear Solar Observatory with the new coronal adaptive optics system CONA, showcases hydrogen α light emitted by the solar plasma. While the image is artificially colored, it reflects the real color of hydrogen alpha light, with darker colors indicating bright light. Image credit: Schmidt et al. /njit /nso /aura /nsf.
The solar corona represents the outermost layer of the solar atmosphere, visible only during a total solar eclipse.
Astronomers have long been fascinated by its extreme temperatures, violent eruptions, and notable prominence.
However, Earth’s atmospheric turbulence has historically caused blurred images, obstructing the observation of the corona.
“Atmospheric turbulence, similar to the sun’s own dynamics, significantly degrades the clarity of celestial observations through telescopes. Fortunately, we have solutions,” stated Dr. Dark Schmidt, an adaptive optics scientist at the National Solar Observatory.
CONA, the adaptive optics system responsible for these advancements, corrects the atmospheric blurring affecting image quality.
This cutting-edge technology was funded by the NSF and implemented at the 1.6-meter Good Solar Telescope (GST) located at Big Bear Solar Observatory in California.
“Adaptive optics function similarly to autofocus and optical image stabilization technologies found in smartphone cameras, fixing atmospheric distortions rather than issues related to user instability,” explained Dr. Nicholas Golsix, optical engineer and lead observer at Big Bear Solar Observatory.
The second film depicts the rapid creation and collapse of a finely detailed plasma stream.
“These observations are the most detailed of their kind, highlighting features that were previously unobserved, and their nature remains unclear,” remarked Vasyl Yurchyshyn, a professor at the New Jersey Institute of Technology.
“Creating an instrument that allows us to view the sun like never before is incredibly exciting,” Dr. Schmidt commented.
Another film captures the dynamic movements across the solar surface, influenced by solar magnetism.
“The new Collar Adaptive Optical System closes the gap from decades past, delivering images of coronal features with resolution down to 63 km. This is the theoretical limit achievable with the 1.6 m Good Solar Telescope,” Dr. Schmidt stated.
“This technological leap is transformative. Discoveries await as we improve resolution tenfold,” he emphasized.
The team’s findings are detailed in a published paper in today’s issue of Nature Astronomy.
____
D. Schmidt et al. Observation of fine coronal structures with higher order solar adaptive optics. Nature Astronomy Published online on May 27, 2025. doi:10.1038/s41550-025-02564-0
Analysis from the ESO’s Very Large Telescope (VLT) and ALMA data indicates that intense radiation from a quasar within these galaxies affects the gas properties of other galaxies, reducing their ability to form new stars.
Artistic impression of a galaxy merger where the right galaxy hosts a quasar at its core. This quasar, containing a supermassive black hole, emits a powerful radiation cone that affects neighboring galaxies. This interaction can destroy gas and dust clouds, leaving behind only denser regions that may struggle to form stars. Image credit: ESO/M. Kornmesser.
“In the far reaches of the universe, two galaxies are entangled in an exhilarating conflict,” remarked Dr. Paschier Notardem, an astronomer affiliated with the Paris Astronomical Institute.
“On a collision course at speeds of 500 km/s, they collide multiple times, only to push one another away before gearing up for another round.”
“Thus, we refer to this system as the ‘space joust.’ However, these galactic contenders don’t fight fairly, utilizing quasars to strike with beams of radiation.”
Quasars are the luminous cores of certain distant galaxies powered by supermassive black holes, emitting substantial amounts of radiation.
The combination of a quasar with a galaxy was significantly more common during the universe’s first billion years, allowing astronomers to glimpse the remote past using powerful telescopes.
The light from this “joust of the universe” traveled over 11 billion years to reach us, providing a snapshot of the universe when it was merely 18% of its current age.
ALMA image showcasing the molecular gas content of two galaxies involved in a collision. Image credits: ALMA/ESO/NAOJ/NRAO/Balashev et al.
“According to Dr. Sergei Balashev from the Ioffe Institute,
the observations from the new VLT/ALMA indicate that radiation from the quasar J012555.11-012925.00 obliterates the normal gas and dust clouds in the surrounding galaxy, leaving only the densest regions.
These regions are likely too limited for star formation, causing a significant decline in stellar nurseries within the affected galaxy.
However, the transformed galaxies are not the only ones undergoing changes.
“These mergers are believed to funnel substantial amounts of gas into the supermassive black holes at the galaxies’ centers,” Dr. Balashev mentioned.
“In this cosmic arena, fresh supplies of fuel come within reach of black holes that power the quasar.”
“As these black holes are nourished, the quasar can persist in its destructive assault.”
A paper detailing these findings was published today in the journal Nature.
____
S. Balashev et al. Quasar radiation transforms gas in a merged companion galaxy. Nature Published online on May 21, 2025. doi:10.1038/s41586-025-08966-4
Recently identified by astronomers, this newly discovered molecular cloud is one of the largest structures in the sky and is among the closest to the Sun and Earth ever detected.
The EOS Cloud is situated at the boundary of your local bubble—a region populated by large gases within the solar system. Image credits: Thomas Müller, HDA & MPIA/Thavisha Dharmawardena, NYU.
Molecular clouds consist of gas and dust, primarily composed of hydrogen, the most prevalent molecule in the universe and essential for the formation of all known stars and planets.
Additionally, these structures harbor other molecules, including carbon monoxide.
Traditional detection methods for molecular clouds often involve wireless and infrared observations, which readily capture the chemical signatures of carbon monoxide.
However, Blakely Burkhart, an astrophysicist from Rutgers University in New Brunswick, and his team took a different approach.
“This is the first molecular cloud discovered by directly seeking out the distant ultraviolet radiation of molecular hydrogen,” Dr. Burkhart stated.
“Our data revealed glowing hydrogen molecules detected through fluorescence in distant ultraviolet light. This cloud truly shines in the dark.”
The new molecular cloud, named EOS, was located approximately 300 light-years from Earth and can be viewed here.
It resides at the periphery of a local bubble, a region filled with gases surrounding the solar system.
Astronomers estimate that these crescent clouds are immense, spanning about 40 months across the sky and having a mass approximately 3,400 times that of the Sun.
They are projected to dissipate within 6 million years.
According to the research team, the EOS cloud poses no threat to Earth or the solar system.
Its proximity offers a unique opportunity to explore the properties of structures within the interstellar medium.
The interstellar medium, composed of gas and dust, fills the space between stars in the galaxy and is a key source for new star formation.
“When you look through a telescope, you observe the solar system in its formative phase, but the exact process remains unclear,” Dr. Burkhart explained.
“The discovery of EOS is thrilling because it allows us to directly measure how molecular clouds form and dissolve, as well as how galaxies transform interstellar gas and dust into stars and planets.”
“Utilizing distant UV fluorescence technology could redefine our understanding of the interstellar medium, uncover hidden clouds across the galaxy, and even push our exploration further back to the very edge of the universe’s inception.”
The findings are reported in a study published today in the journal Nature Astronomy.
____
B. Burke Hart et al. Dark molecular clouds near local bubbles revealed via H2 fluorescence. Nature Astronomy. Published online on April 28, 2025. doi:10.1038/s41550-025-02541-7
One of the most immense singular formations observed in the cosmos, these expansive hydrogen gas clouds, have been found surprisingly close to Earth.
Naming it EOS, after the Greek goddess of dawn, the cloud was discovered through the faint ultraviolet light emitted by hydrogen molecules.
Referred to as molecular clouds, these colossal structures of gas and dust serve as nurseries for new stars.
Historically, astronomers have depended on radio and infrared telescopes to locate these clouds, detecting the carbon monoxide signature. However, scientists took a distinct approach to uncover EOS.
“This marks the first molecular cloud identified through the direct search for distant ultraviolet emissions of molecular hydrogen,” stated Professor Blakesley Burkhart, the leading researcher on the project.
“The data revealed glowing hydrogen molecules detected through fluorescence in distant ultraviolet rays. This cloud truly shines in the dark.”
https://c02.purpledshub.com/uploads/sites/41/2025/04/eos.mp4Scientists have identified potential star-forming clouds, designated EO. It ranks among the largest single structures in the sky and is one of the nearest formations to the sun and earth ever observed.
Situated just 300 light years from Earth at the confines of a gas-rich area known as the local bubble, EOS spans a region of sky comparable to a full moon width of 40 and possesses approximately 3,400 times the sun’s mass.
Despite its size and proximity, it remained concealed due to being “co-dark,” which indicates a deficiency of carbon monoxide that traditional detection methods rely on.
“The discovery of EOS is thrilling because it allows us to directly observe the formation and dissociation of molecular clouds and how galaxies transform interstellar gases and dust into stars and planets,” Burkhart commented.
Dr. Thavisha Dharmawardena noted, “During my graduate studies, I was informed that observing molecular hydrogen wasn’t straightforward.”
The data was acquired using a Faltraviolet spectrometer installed on the Korean satellite STSAT-1. Published in 2023, Burkhart quickly unearthed a concealed structure.
“The story of the cosmos is one of billions of years of atomic transformation,” Burkhart explained.
“The hydrogen found in the EOS cloud dates back to the Big Bang and eventually fell into our galaxy, merging near the sun. Thus, these hydrogen atoms have traveled a remarkable 13.6 billion-year journey.”
The recently identified planet orbits a binary system comprising two equal brown dwarf stars positioned at a 90-degree angle from 2mass J15104786-2818174 (hereafter referred to as 2M1510).
This diagram illustrates exoplanets orbiting two brown dwarfs. Image credit: ESO/M. Kornmesser.
Cardiovascular planets represent the realm of diabetes found within a binary star system.
These planets generally have orbits aligned with the planes in which their host stars revolve around one another.
Previously, there were indications that planets might exist in vertical or polar orbits. Theoretically, these orbits were stable, and disc formations observed suggested potential planets around polar orbits of stars.
However, astronomers have now obtained clear evidence of the existence of these polar planets.
“We are thrilled to have played a role in finding robust evidence for this configuration,” stated PhD candidate Thomas Beycroft from the University of Birmingham.
The newly discovered exoplanet, 2M1510B, orbits a unique pair of young brown dwarfs.
These brown dwarfs undergo mutual solar eclipses as viewed from Earth, a characteristic that qualifies them within what astronomers refer to as a binary system.
This configuration is exceptionally rare, marking only the second identified pair of brown dwarfs and the first solar system discovered at a right angle relative to the orbit of its two host stars.
Artist’s impression of the unusual trajectory of 2M1510B around the brown dwarf. Image credit: ESO/L. Calsada.
“The planet revolving around the binary brown dwarfs in a polar orbit is remarkably thrilling,” commented Amalie Triaudo, a professor at the University of Birmingham.
Astronomers discovered 2M1510B by refining the trajectories and physical characteristics of the two brown dwarfs using UV and Visual Echelle Spectroscopy (UVES) at ESO’s Very Large Telescope.
The researchers observed strange forces acting on the trajectory of the brown dwarf, leading to speculation about a unique formation with an unusual orbital angle.
“After considering all plausible scenarios, the only explanation consistent with our data is that the planet within this binary is in polar orbit,” Beycroft noted.
“This discovery was fortuitous, as our observations weren’t initially aimed at studying the composition or orbit of such a planet, making it an exciting surprise,” Professor Triaud explained.
“Overall, I believe this not only showcases our astronomers’ capabilities but also illuminates the possibilities within the intriguing universe we inhabit.”
This image depicts the triple system 2M1510. Image credits: Centre Donna Astromyk destrasbourg/Sinbad/Panstars.
This discovery was made possible due to innovative data analysis developed by Dr. Larita Sylum of Cambridge University.
“We can derive their physical and orbital parameters from the variation in speed between the two brown dwarfs, although these measurements were previously uncertain,” Dr. Sairam remarked.
“This improvement has revealed that the interactions between the two brown dwarfs are intricately influenced.”
Study published in the journal Advances in Science.
____
Thomas A. Baicroft et al. 2025. Evidence of polar drainage bulges orbiting a pair of brown dwarfs. Advances in Science 11 (16); doi:10.1126/sciadv.adu0627
Using data from NASA’s transit exoplanetary survey satellite (TESS), MIT astronomers discovered a rocky exoplanet orbiting the bright K-Dwarf Star BD+05 4868A and observed variable transport depths, a feature of comet-like tails formed by the dusty effects expressing the distemination planet. This exoplanet-specific is the presence of a dust tail that is prominent in both subsequent and major directions, contributing to the extinction of starlight from the host star.
Impressions of the collapsed exoplanet artists around a giant star. Image credits: Jose-Luis Olivares, MIT.
BD+05 4868A also known as TIC 466376085 or hip 107587, is about 140 light years away from the Pegasus constellation.
A new descattering named BD+05 4868AB approaches the star towards the sun at about 20 times the mercury, completing its orbit every 30.5 hours, but about the mass of mercury.
In close proximity to BD+05 4868A, the planet is roasted at about 1,600 degrees Celsius (3,000 degrees Fahrenheit) and may be covered in boiling magma in space.
Just as planets bubble around the stars, it strips off a huge amount of surface minerals and effectively evaporates.
MIT astronomer Marc Hon and colleagues discovered BD+05 4868AB using NASA’s Exoplanet Survey Satellite (TESS).
The signal that turned the astronomer over was a unique transport with a dip that all orbits were deeply fluctuating.
They confirmed that the signal is a tough orbital planet that has long been chasing comet-like fragments.
“The tail range is huge, extending up to 9 million km long, or about half the entire planet’s orbit,” Dr. Hong said.
“The planets collapse at a dramatic rate, and each time a star orbits the star, it appears to be throwing away the amount of material equivalent to Mount Everest.”
Researchers predict that the planet could completely collapse within about 1 to 2 million years.
Dr. Avi Shporer, an astronomer at MIT, said:
Of the almost 6,000 planets astronomers have discovered so far, scientists know only three other collapsed planets beyond our solar system.
Each of these crumbling worlds was discovered over a decade ago using data from NASA’s Kepler Space Telescope. All three planets were found with similar comet-like tails.
The BD+05 4868AB has the longest tail to date and has the deepest transits from four known collapsed planets.
“That means that its evaporation is the most devastating and disappears much faster than other planets,” Dr. Hong said.
Impressions of the artists of Planet K2-18B and its host star
ESA/Hubble, M. Kornmesser
Astronomers claim they have seen the most powerful evidence ever for living on another planet. However, other astronomers are cautioning until the findings are verified by other groups, allowing alternative, nonbiological explanations to be excluded.
“These are the first hints we see about the alien world we probably live in.” Nick Madhusdan We held a press conference at Cambridge University on March 15th.
Astronomers first discovered the Exoplanet K2-18B in 2015, quickly establishing it as a promising place for searching for life. Planets orbiting stars about eight times more than Earth, 124 light years away from us, sit in a habitable zone of stars where liquid water is present. Further observations in 2019 found evidence of water vapor. This led to the suggestion that, although not all astronomers agreed, the planet could be covered in oceans sitting under a hydrogen-rich atmosphere.
In 2023, Madhusudhan and his colleagues used James Webb Space Telescope (JWST) instruments to examine the atmosphere of the near-infrared light K2-18B, again finding evidence of water vapor and methane. However, they also found appetizing hints for dimethyl sulfide (DMS), a molecule that is produced exclusively by organisms on Earth, primarily by marine phytoplankton. However, the signs of DMS were very weak and many The astronomers argued Stronger evidence is needed to be certain about the existence of molecules.
Currently, Madhusudhan and his colleagues use different instruments to observe the K2-18b than the mid-infrared camera JWST. They discovered a much stronger signal against DMS and a molecule that could be called dimethyldisulfide (DMDS).
“What we’re finding is a line of independent evidence in different wavelength ranges with different equipment that can potentially biological activity on the planet,” Madhusdan said.
The team argues that detection of DMS and DMD is at three sigma levels of statistical significance. This corresponds to a 1/100 chance that a pattern of data like this will become absorption. In physics, the standard threshold for accepting something as a true discovery is five sigmas, which corresponds to 1-3.5 million chances that data is a coincidence.
Nicholas Wargan The NASA Ames Research Center in California says the evidence is more convincing than the 2023 results, but it should be verified by other groups. When data is published next week, other researchers can begin to review the findings, but this could take weeks or months as JWST data is difficult to interpret. “It’s not just about downloading data and checking if there’s a DMS. It’s this extremely complicated process,” says Wogan.
Other scientists are more skeptical of the findings. “These new JWST observations do not provide compelling evidence that DMS or DMD exists in the atmosphere of K2-18B.” Ryan McDonald At the University of Michigan. “We have a juvenile chase wolf situation in the K2-18B, where multiple previous 3-sigma detections have completely disappeared when subjected to closer scrutiny.
Madhusudhan and his team estimate that further 16 to 24 hours of further observations at the JWST will help reach 5-sigma levels, but observing the planet’s atmosphere means that this cannot be guaranteed.
“The relative size of the atmosphere compared to the planet’s size is pretty close to the thickness of the apple’s skin on top of the apple, which is what we’re trying to measure.” Thomas Beatty At the University of Wisconsin-Madison, where I was not part of the learning team. Wogan adds that reaching five sigmas may be fundamentally impossible due to the amount of noise in the data.
But if further observations prove that this is a real discovery, it would be a “risqué progress,” says Beatty. “Ignoring whether it was actually being produced for a moment, I said that ten years ago it is evidence of life in a planetary atmosphere that can certainly host it.”
Madhusudhan and his colleagues calculate that the potential concentration of DMS and DMD in K2-18B appears to be over ten parts, thousands of times more than the concentrations in the Earth’s atmosphere. This could show far more biological activity than Earth if the signal turns out to be correct, but establishing that chemicals have biological origins requires more work, he says.
“We need to be very careful,” Madhusdan said. “At this stage, when you detect DMS and DMD, you can’t claim it’s for life. Let’s be very clear about that.
It could take some time to eliminate another mechanism, Wogan says. “This kind of thing hasn’t been studied in practice. In a hydrogen-rich atmosphere, DM doesn’t know tons about it. It requires a lot of work.”
The difficulty in proving that it has no nonbiological explanations is that it could potentially put K2-18B in the category of viable biosignature candidates over a long period of time. Sarah Seager At Massachusetts Institute of Technology. “It could remain in that category for decades, because the problem will not be completely solved by providing limited data deplanets,” she says.
However, Madhusudhan says this discovery is important whether it comes from life or not. “This was a revolutionary moment, and we were able to come from a single cell life, not just as astronomers, but also for our species, from a single cell life billions of years ago, to a highly technological civilization where we could peer into the atmosphere of another planet and find evidence of actual biological activity,” he said.
The Mystery of the Universe: Cheshire, England
Spend a weekend with some of the brightest minds of science. Explore the mystery of the universe in an exciting program that includes an excursion to see the iconic Lovell telescope.
SGR 0501+4516 is the most likely candidate for Magnetaru’s Milky Way galaxy, which was not born from the supernova explosion, as originally predicted. The object may be very strange and may provide clues to the mechanism behind the fast radio bursts.
Impressions of Magneter artists. Image credit: ESA.
“A magnetor is a neutron star made up entirely of neutrons. What makes Magnetar unique is the extreme magnetic fields,” says Dr. Ashley Chris, an astronomer at the European Center for Space Research and Technology.
The strangeness of SGR 0501+4516 was identified with the help of ESA’s Gaia spacecraft with the help of a sensitive instrument mounted on the NASA/ESA Hubble Space Telescope.
Initially, Magnetar was discovered in 2008 when NASA’s Swift Observatory discovered a fierce flash of gamma rays from the outskirts of the Milky Way.
As magnetors are neutron stars, the natural explanation for their formation is that they are born in Supernova, where stars can explode and even collapse into ultra-density neutron stars.
This looked like the case of SGR 0501+4516, located near the supernova remnants called HB9.
The separation between the sky magnetor and the center of the supernova remnants is only 80 arcs, or slightly wider than the pinky finger, when seen at the edge of the extended arm.
However, a decade of research with Hubble questions Magnetall’s birthplace.
After the initial observation using ground-based telescopic tunables shortly after the discovery of SGR 0501+4516, astronomers used Hubble’s exquisite sensitivity and stable points to find the faint infrared glow of Magnetaral in 2010, 2012, and 2020.
Each of these images was arranged in a reference frame defined by observations from Gaia Spacecraft. GaiaSpacecraft has created a highly accurate 3D map of almost 2 billion stars in the Milky Way.
This method revealed subtle movements of magnets as they crossed the sky.
“All of this movement we measure is smaller than a pixel in a Hubble image,” said Dr. Joe Lyman, an astronomer at Warwick University.
“The ability to perform such measurements robustly is truly a testament to Hubble’s long-term stability.”
By tracking the magnetor’s location, astronomers were able to measure the apparent movement of the object across the sky.
Both the velocity and direction of movement of SGR 0501+4516 indicated that the magnetor was not associated with the remains of nearby supernova.
Tracking the magnetor’s trajectory thousands of years in the past showed that there were no other supernova remnants or large star clusters that it could be associated with.
If SGR 0501+4516 was not born on a supernova, the magnetors must be older than the estimated age of 20,000, or they may have been formed in a different way.
Magnetors can also be formed through a process called amalgamation or accretion-induced decay of two low-mass neutron stars.
Acceleration-induced decay requires a binary star system containing white dwarves.
When a white dwarf pulls gas from its companions, it grows too large to support itself, leading to an explosion, or perhaps a magnet.
“This scenario usually leads to a nuclear reaction ignition and a white d star explosion, leaving nothing behind,” said Dr Andrew Levan, an astronomer at Ladboo University and Warwick University.
“However, it is theorized that under certain conditions, white dwarfs may instead collapse into neutron stars. I think this is how SGR 0501+4516 was born.”
SGR 0501+4516 is currently the best candidate for galaxy magnetarals and may have been formed by a merger or an adductive decay.
The magnets formed through accretion-induced decays can provide some explanation for the mystical fast radio bursts, which are short but powerful flashes of radio waves.
In particular, this scenario may explain the origins of fast radio bursts that emerge from a group of stars that are too old to recently create a huge star to explode as a supernove.
“The magnetor’s fertility and formation scenarios are one of the most pressing issues of high-energy astrophysics, affecting many of the most powerful temporary events in the universe, including gamma-ray bursts, superilluminating supernovas and fast radio bursts.”
Survey results It will be displayed in the journal Astronomy and Astrophysics.
____
aa chrime et al. 2025. Magnetor SGR 0501+4516 infrared support and proper movement. A&A 696, A127; doi: 10.1051/0004-6361/202453479
Using advanced statistical modeling, a team of researchers from ETH Zurich, Seti Institute, and University ‘Tor Vergata’ Yonversity investigated how many exoplanets should be observed and understood before declaring that life beyond Earth is common or rare.
Future telescopes will investigate mild terrestrial exoplanets to estimate the frequency of habitable or inhabited worlds. Angerhausen et al. It aims to determine the minimum number of exoplanets required to draw statistically significant conclusions. Particularly for null results (i.e., no detection). Image credit: Sci.News.
In science, not being able to find anything can bring important insights.
When scientists look for life on exoplanets, they often focus on certain characteristics, such as water, gases like oxygen and methane, which may exhibit biological activity.
But what if scientists can’t find these features? Can we learn meaningful things about how ordinary life exists in the universe?
“Even one positive detection changes everything, but up until then we need to make sure we are learning as much as possible from what we can’t find,” said Dr. Daniel Angerhausen, researcher at ETH Zurich and SETI Institute.
New research shows that if scientists look at 40-80 planets and can’t find any signs of life, they can confidently conclude that less than 10-20% of similar planets have life.
However, this depends heavily on how certain we are for each observation.
These discoveries allow scientists to set meaningful caps on the prevalence of living in the universe.
Furthermore, if there is only 10% of planets in the Milky Way alone that have some form of life, it could still be more than 10 billion planets.
“This kind of outcome would be a turning point,” Dr. Angerhausen said.
“Even if life is not found, ultimately we can quantify planets that are truly rare or common with planets with detectable biosignatures.”
The findings will have a direct impact on future missions such as NASA’s Habitable World Observatory (HWO) and European-led large-scale interferometers on exoplanets searching for life.
These missions will study dozens of Earth-like planets by analyzing the planet’s atmosphere for water, oxygen, and even more complex biosignature signs.
Research shows that the number of observed planets is large enough to draw critical conclusions about the likelihood and prevalence of life in the galaxy.
However, this study points out that even with advanced equipment, these studies should carefully account for uncertainty and bias, and develop frameworks to ensure statistically meaningful results.
One important insight from this study is that uncertainty in individual observations, such as false negatives, can significantly impact conclusions.
“It’s not just the number of planets we observe. It’s about how confident we are to see what we’re looking for or not,” Dr. Angerhausen said.
“If we are not careful and confident in our ability to identify life, even large-scale research can lead to misleading consequences.”
The study will be published in today’s Astronomy Journal.
____
Daniel Engerhausen et al. 2025. What if nothing is found? Bayesian analysis of null statistics in future exoplanet habitability and biosignature investigations. AJ 169, 238; doi:10.3847/1538-3881/adb96d
Astronomers using the Muse Instrument with ESO’s extremely large telescope (VLT) detected ultra-large black hole-driven winds with the Burred Spiral Galaxy NGC 4945.
This image shows NGC 4945, a spiral galaxy that exceeds 12 million light-years in the constellation of Centaurus. The super-large black hole-driven wind of the NGC 4945 is shown in red in the inset. Image credits: ESO/Marconcini et al.
NGC 4945 It is more than 12 million light years away from Earth, the constellation of Centaurus.
Otherwise known as the Caldwell 83. That’s what this galaxy was like I discovered it by James Dunlop, the Sottsch astronomer in 1826.
NGC 4945 hosts one of the closest active, ultra-large black holes to Earth.
“At the heart of almost every galaxy, they are very large black holes,” the ESO astronomer explained in a statement.
“Some people are not particularly hungry, as they are in the heart of our own Milky Way.”
“However, the super-large black hole in NGC 4945 is greedy and consumes a huge amount of problems.”
Astronomers have studied the ultra-high Massive black holes of the NGC 4945 using the Muse Instrument, an ESO’s extremely large telescope (VLT).
“Contrary to the all-consuming reputation typical of black holes, this messy eater is blowing away the powerful winds of ingredients,” they said.
“This cone-shaped wind is shown in red in the inset and is covered in a wider image taken with La Silla’s MPG/ESO telescope.”
“In fact, this wind moves so fast that it completely escapes the galaxy, giving in to space in intergalactic space.”
“This is part of a new study measuring how the wind moves in several nearby galaxies,” they added.
“Muse’s observations show that these incredibly fast winds show strange behavior. They actually speed up far from the central black hole, and accelerate even further on their journey to the outskirts of the galaxy.”
“This process suggests that black holes control the fate of the host galaxy by ejecting potential star-forming material from the galaxy and attenuating the star’s fertility.”
“It also shows that more powerful black holes can hamper their own growth by removing the gas and dust they feed, bringing the entire system closer to a kind of galactic equilibrium.”
“Now, these new results bring us one step closer to understanding the mechanisms of wind acceleration that are responsible for galaxy evolution and the history of the universe.”
Survey results It will be displayed in the journal Natural Astronomy.
____
C. Marconcini et al. Evidence of rapid acceleration of AGN-driven winds at the Kiloparsec scale. Nut Athlonreleased on March 31, 2025. doi:10.1038/s41550-025-02518-6
The rotation period for Uranus was estimated at 17.24 hours from radio auroral measurements by NASA’s Voyager 2 spacecraft in 1986. Using long-term tracking of Uranus’ poles between 2011 and 2022 from Hubble images of UV light, astronomers now have an updated independent, highly accurate rotation period of 17.247864 hours, or 28 seconds longer than the estimated Voyager 2.
This image of the Uranus aurora was photographed by Hubble on October 10th, 2022. Image credit: NASA/ESA/Hubble/L. Ramie/L. Slomovsky.
“Our measurements not only provide essential references to the planetary science community, they solve long-standing problems. Previous coordinate systems based on outdated rotation periods quickly become inaccurate, making it impossible to track Uranus’ magnetic poles.
“With this new longitude system, we can compare nearly 40 years of observations of the Aurora and even plan future Uranus missions.”
This breakthrough was possible thanks to long-term surveillance of Hubble’s Uranus.
For over a decade, telescopes have regularly observed their ultraviolet emissions, allowing astronomers to generate magnetic field models that match changes in the position of magnetic poles with time.
“The continuous observation from Hubble was extremely important,” Dr. Lammy said.
“Without this rich data, it would not have been possible to detect periodic signals at the level of accuracy achieved.”
Unlike Earth, Jupiter, or Saturn’s aurora, Uranus’ aurora behaves in a unique and unpredictable way.
This is due to the highly tilted magnetic field of the planet, which is significantly offset from the axis of rotation.
The findings not only help astronomers understand Uranus’ magnetosphere, but also help to provide important information for future missions.
“These discoveries set a stage for further research that will deepen our understanding of one of the most mystical planets in the solar system,” the author said in a statement.
“The ability to monitor objects for decades has allowed Hubble to remain an essential tool for planetary science, paving the way for the next era of exploration on Uranus.”
result It was published in the journal this week Natural Astronomy.
____
L. Ramie et al. A new rotation period and longitude system for Uranus. Nut AthlonPublished online on April 7th, 2025. doi:10.1038/s41550-025-02492-z
It’s similar to how paleontologists use certain known fossils Indexed Fossil Until assessing rock formations and ancient environments so far, astronomers look for specific patterns of light emissions from space to mark the age of space history. For example, early galaxies give the UV rays that originate from electrons in hydrogen atoms to the type of ultraviolet rays that exert from the second lowest to the lowest energy state. Lyman Alphaor ly⍺ Emission.
For decades, astronomers have associated ly⍺ emissions with periods within billions of years of a big bang called the Big Bang. The era of reionizationwhen the average speed of star formation in galaxies was much higher than today. When they find a galaxy that emits light strongly, they classify it into ly⍺Emitter or Lae And we can be sure that it goes back to the era of reionization. Observing Laes, astronomers talk more about the history of the Milky Way and other galaxies like us.
However, researchers face confounding factors when looking for Laes. The expansion of the universe distorts light in a process called Cosmological redshift. However, more prominently Dustboth Intergalacticcovers the light. While astronomers can analyze the full light of light from the galaxy to find evidence of ly⍺ emissions, it would be much faster to develop tools to predict whether a galaxy is likely to be a LAE based on more readily available measurements.
One team of astronomers developed a model for this problem only Machine Learning A technique known as a Neural Networks. This technique replicates how neurons in the brain function, with several interconnected layers receiving and transmitting signals based on initial inputs and generating final outputs.. The trick is that the programmer knows what inputs to input and what output they expect in the end. The algorithm itself needs to know how best to set up a central connection, what to look for, and how to rank the importance of each input.
The team began with data from two surveys of light sources in space: 926 galaxies VanderOf these, only 520 are laes, starting from 507 Musethey were all laes. They trained the algorithm using 80% of this data to explicitly communicate which sources are actual LAES and which sources are not. They saved the remaining 20% of the data for testing.
Through this initial test, the team identified six parameters of neural networks to focus on evaluating galaxies for LAE potential. These parameters were the rate of star formation, total star mass, UV brightness, UV emission patterns, age, and dust. They programmed the network to output an estimate of the probability that a particular galaxy is a LAE, and thought that what was above 70% meant that the algorithm classified it as an LAE.
When we created a neural network using training data, the team tested several additional rounds. Using early test data, their networks found that they correctly identified the network in 77% of the time, as there was only a 14% chance of false positives. When they looked at what their network prioritized to make these predictions, they found that the most important factors were the galaxy’s UV emission pattern, its UV brightness, and the mass of its star.
Following this initial success, the team applied the network to another investigation. cosmos2020and a subset of that raise, SC4Kwith fewer details than the training data survey. From these datasets, the team’s neural network identified true Laes for 72% of the time.
The team’s final results came when they applied neural networks to data from NASA’s new telescope. jwst. The ultimate goal in their model is to study the distant past of the universe, and JWST aims to see better-looking sources than ever before, so the success of the test is Already checking the results of LAE from JWST It will be a good sign of future success. They found a true positive rate of 91% in JWST data, showing the validity of their approach and illuminated the path to know more about the history of the universe.
The mass of the ultra-large black hole in the heart of the large Magellan cloud, a small milky satellite galaxy, is approximately 600,000 solar mass.
Impressions of the Hyper Belt Lattist artist ejected from the large Magellan cloud (shown on the right). If the binary star system gets too close to an ultra-large number of black holes, intense gravity will tear the pair apart. One star is captured in tight orbits around a black hole, while the other is thrown outward at extreme speeds – often exceeding thousands of kilometers per second, making it a high-speed star. The inset diagram illustrates this process. The orbital path of the original binary is displayed as an interwoven line, one star is captured by a black hole (near the center of the inset), and the other is ejected into space (bottom right). Image credit: CFA/Melissa Weiss.
“Our Milky Way galaxy halo includes a few stars running faster than local escape speeds in orbit that carry them into intergalactic space,” said Dr. Jesse Han, Ph.D. of the Harvard & Smithsonian Center for Astrophysics and Colleagues.
“One mechanism for generating such ultrafast stars is the Hills mechanism. When a close binary star wanders near an ultrahigh Massive black hole, one star can be captured, while the other is ejected at a rate that reaches more than a second.”
In their new study, astronomers followed the path with ultrafine accuracy of 21 superfast stars in halos outside the Milky Way.
They confidently categorized these stars, finding that seven of them coincided with those born out of the center of the Milky Way.
However, the other nine stars coincided with those born from the centre of the large Magellan cloud, about 160,000 light years away from us.
“Cosmologically speaking, it's amazing to notice another super-large black hole just below the block,” Dr. Han said.
“Black holes are so stealthy that this has been under our noses this time.”
Researchers discovered a large Magellanic Cloud black hole using data from ESA's Gaia Mission.
They also used improved understanding of the orbital of the d-star galaxies around the Milky Way, which was recently obtained by other astronomers.
“We knew these superfast stars had been around for a while, but Gaia provided us with the data we needed to figure out where they actually came from,” says Dr. Kareem El-Badry, an astronomer at Caltech.
“Combining these data with a new theoretical model of how these stars move, we made this incredible discovery.”
“The only explanation we can come up with for these data is the presence of a monster black hole in the next Galaxy,” said Dr. Scott Lucchini, an astronomer at the Harvard & Smithsonian Center for Astrophysics.
As our solar system orbits the Milky Way, we encounter a variety of environments, including dense regions of interstellar media. These encounters can increase the flow of interstellar dust into the solar system and the Earth's atmosphere, exposing parts of the solar system to interstellar mediums. The discovery of new galactic structures, such as the Radcliffe waves over the 9,000 Wright years, raises the question of whether the Sun encountered any of them. New research shows that the solar system trajectories intersected with the waves of Radcliffe in the Orion star-forming region 15 to 12 million years ago (Miocene era). In particular, this period coincides with the mid-Miocene climate transition on Earth, providing an interdisciplinary connection with paleoclimatology.
When the solar system brings the Milky Way into orbit, we encounter a variety of galactic environments with different interstellar densities, including hot voids, fronts of supernova blasts, and cold gas clouds.
The passage of the sun through dense regions of interstellar media can affect the solar system in several ways.
For example, pressure enhancement compresses the heliosphere and exposes parts of the solar system to cold, dense interstellar media.
Furthermore, the amount of interstellar dust mounted on the Earth's atmosphere can increase, potentially enhancing the delivery of radioactive isotopes such as iron-60 through dust grains.
Radcliffe's waves are narrow sinusoidal gas structures and consist of many known star-forming cloud complexes, including CMA, Orion, Taurus, Perseus, Cephaus, North American Nebula, and Cygnus.
With an estimated mass of 3 million people, this gas structure appears to vibrate consistently like a moving wave and is thought to be part of the Milky Way spiral structure.
Dr. Efrem Macconi, a doctoral student at the University of Vienna, said:
“Our Sun encountered a higher gas density region as it passed through the waves of Radcliffe in the Orion constellation.”
Using data from ESA's Gaia mission and spectroscopic observations, Dr. Maconi and his colleagues identified the passage of the solar system through the Radcliffe Wave in the Orion area.
“The findings are based on previous works identifying Radcliffe's waves,” said Professor Joanne Albes of the University of Vienna.
“We passed the Orion area as well as famous star clusters like NGC 1977, NGC 1980 and NGC 1981.”
“The area is easily visible in the winter sky in the Northern Hemisphere and in the summer in the Southern Hemisphere.”
“Look for Orion Constellation and Orion Nebula (Messier 42) – our solar system has come from that direction!”
“The increased dust from this galaxy encounter may have had some effects.”
“It could potentially leave traces of radioactive elements from supernovas in the geological record that permeate the Earth's atmosphere.”
“Current technologies may not be sensitive enough to detect these traces, but future detectors may make it possible.”
This study shows that the solar system passing through the Orion region occurred around 18.2 to 11.5 million years ago, with the most likely time between 148 and 12.4 million years ago.
This time frame is in good agreement with the mid-Miocene climate transition, and is a major shift from warm variable climate to cool climates, leading to the establishment of a continental-scale prototype Antarctic ice sheet composition.
This study raises the possibility of a link between past crossings of the solar system through galaxy neighbours and Earth's climate through interstellar dust, but the authors need further investigation of the causal relationship. It emphasizes that there is.
“The basic processes responsible for the mid-Miocene climate transition have not been fully identified, but available reconstructions are most likely to be long-term reductions in atmospheric greenhouse gas carbon dioxide concentrations. It suggests that it is a high explanation.
“However, our research highlights that interstellar dust associated with the crossing of Radcliffe's waves has affected the Earth's climate and may have played a potential role during this climate change. Masu.”
“To change the Earth's climate, the amount of extraterrestrial dust on Earth needs to be much larger than what previous data suggests.”
“Future research explores the importance of this contribution. This past climate change and current climate change is comparable as this past climate change is unfolding over a timescale of hundreds of thousands of years. It is important to note that we do not do that.”
“In contrast, the evolution of global warming today has been happening at an unprecedented rate for decades to centuries due to human activity.”
study Published in the journal Astronomy and Astrophysics.
____
E. Machoni et al. 2025. Passing through the solar system through the waves of Radcliffe in the mid-Miocene. A&A 694, A167; doi: 10.1051/0004-6361/202452061
An extreme class of planets not found in our solar system, Ultrahot Jupiters offers a unique window into atmospheric processes. Using four telescope units in ESO’s extremely large telescopes, astronomers are currently being investigated deep into the atmosphere of the Ultra Hot Jupiter ExoPlanet WASP-121B, revealing separate powerful winds in separate layers, We have formed a map of the 3D structure of the atmosphere.
This diagram shows the atmospheric structure and movement of the WASP-121B. Image credit: ESO/M. Kornmesser.
The WASP-121B is a gas giant exoplanet 1.87 times larger than Jupiter and 1.18 times larger.
First discovered in 2016, this alien world takes just 1.3 days to traverse the parent F6 star WASP-121 (TYC 7630-352-1).
The WASP-121 system is approximately 881 light years away from the puppy’s constellations.
The WASP-121B is what is called “Ultra Hot Jupiter” and takes only 1.3 days to get the WASP-121 into orbit. It’s so close to the parent star, that when it gets closer, the star’s gravity begins to tear it apart.
Astronomers estimate the planet’s temperature is about 2,500 degrees Celsius (4,600 degrees Fahrenheit), high enough to boil some metals.
“The WASP-121B atmosphere behaves in a way that challenges understanding of how the weather works not only on Earth, but on all planets,” says the astronomer at Lagrange Laboratory, an astronomer at ESO. said Dr. Julia Victoria Seidel. Cote d’Azur.
“It feels like something from science fiction.”
“What we found was amazing. The Jet River rotates material around the planet’s equator, and another flow at a lower level in the atmosphere moves the gas from the hot side to the cool side. “
“We’ve never seen this kind of climate on any planet.”
“The observed jet stream spans half the planet, gaining speed and thrusts the air in the sky hard as it crosses the hot side of the WASP-121B.”
“Even the strongest hurricanes in the solar system seem milder in comparison.”
Dr. Seidel and colleagues to reveal the 3D structure of the atmosphere of the WASP-121B Used Espresso equipment located in ESO’s extremely large telescopes (VLTs) combines the light from four large telescope units into a single signal.
This combination mode of VLT collects 4 times the light of an individual telescope unit and reveals the details of the feinder.
Espresso was able to detect signatures of multiple chemical elements by observing the planet’s complete passage in front of the host star, resulting in different layers of the atmosphere.
“The VLT has led to three different layers of the Exoplanet atmosphere falling on one side,” said Dr. Leonardo A. dos Santos, an astronomer at the Institute of Space Telescope Science.
Astronomers were able to track the movement of iron, sodium and hydrogen, and track winds in the deep, central and shallow layers of the Earth’s atmosphere, respectively.
“It’s a very challenging observation for space telescopes and highlights the importance of ground-based observations on exoplanets,” Dr. Dos Santos said.
Interestingly, observations are also It was revealed Titanium is present just below the jet stream.
This was another surprise, as previous observations of the planet showed that this element was absent, and perhaps hidden deep within the atmosphere.
“It’s truly amazing to be able to study the details of such vast distances such as the chemical composition and weather patterns,” said PhD Viviana Prinos. A student at Lund University.
____
JV Seidel et al. Vertical structure of the atmospheric jet stream of the exporanet. NaturePublished online on February 18th, 2025. doi:10.1038/s41586-025-08664-1
Three layers of the atmosphere of a giant tyro gas
ESO/m. Cone Messer
The atmosphere of a distant world is mapped in detail for the first time, revealing a strange, dizzy weather system, and the fastest winds ever blew inexplicably around the Earth's stratosphere.
Astronomers have been studying the WASP-121B, also known as Tylos, since 2015. A planet 900 light years away is a vast ball of gas twice the size of Jupiter, and the stars orbit very closely and complete their perfect orbit. Only 30 Earth Time. This close orbit heats the planet's atmosphere to a temperature of 2500°C, and is hot enough to boil iron.
now, Julia Seidel Chile and her colleagues' observatory in southern Europe use a very large telescope at the observatory to see in the burnt, hot atmosphere of Tyros, with at least three different layers of gas in different directions around the planet. I found out there. I've seen it before. “It's absolutely crazy, it's a science fiction-like pattern and behavior,” Seidel says.
The atmosphere of our solar system planets is driven by the internal temperature difference, whereas the winds in the upper layers are more affected by the temperature difference, and the strong wind flows are more affected by the temperature difference. shares a similar structure to Created by the heat of the sun, it warms the daylight side of the planet, while the other warms.
However, in the atmosphere of Tyros, it is driven by heat from the planetary stars, and it is the lower wind that moves away from the warm surface, but the jetstream is primarily in the middle layer of the atmosphere, surrounding the equator of Tyros. It looks like it's moving. In the direction of the planet's rotation. The upper layer also exhibits jetstream-like characteristics, but hydrogen gas floats outward from the planet. This is difficult to explain using current models, Seidel says. “What we're looking at now is actually the opposite of what comes out of theory.”
Furthermore, Tylos' jetstream is the most powerful ever, blasting at about 70,000 km/h on half the planet. This is almost twice as much as the previous record holder. It is unknown what exactly drives this velocity, but researchers believe it is caused by the planet's strong magnetic field or by ultraviolet rays from the stars. “This could change the flow pattern, but this is all very speculative,” Seidel says.
Astronomers have imaged planetary belts of 74 planetary systems as part of resolved ALMA and SMA observations in nearby star (reason) investigations (reason).
The gallery contains 74 images of different star systems with exoconterry belts taken at the Sub-Millimeter Array (SMA) and Atacama's Large Millimeter/Sub-Millimeter (ALMA) Wireless Telescope Facility. Image credit: Luca Matrà.
To find evidence of comets outside our solar system, astronomers have turned to two facilities that detect specific bands of radio waves: sub-millimeter arrays (SMAs) and large millimeters/sub-millimeters in Atacama Meter array (ALMA).
Due to the dust and rock size of these belts, this type of light is especially good for finding and imaging these structures.
The stars in this study ranged from very young to middle-aged ages like our Sun.
“The joint programme between SMA and Alma Dubbed reasons presents a significant milestone in the Exometallibelt study, as its images and subsequent analysis reveal where the pebbles and exomets are located. is”
“In these regions, it's very cold (minus 250 to minus celsius), so most compounds, including water, are frozen like ice from these exomets.”
“Exocomet is a rock and ice rock of at least 1 kilometre in size, and it collides together within these belts, and here produces pebbles that are observed in an array of telescope Alma and SMA,” says Dr. Matra. said.
“The Exometallibelt is located in at least 20% of our planetary systems, including our solar system.”
“The Kuiper Belt is an example of the comet belt of our own solar system.”
“Far beyond Pluto's orbit, some scientists believe the Kuiper belt is the source of the internal solar system where Earth was located, delivered through comets billions of years ago.”
The new image shows a significant diversity of structures within the belt. Some are narrow rings, while others are wider and may be classified as discs rather than belts.
Additionally, some of the 74 Exocomet systems have multiple rings or discs, some of which are eccentric. In other words, it's more like an elliptical shape, not a circular orbit.
This provides evidence that there are still undetectable planets or possibly moons, and that their gravity affects the distribution of pebble in these systems.
“The arrays like Alma and SMA used in this work are extraordinary tools that continue to give us incredible new insights into the universe and how it works,” says Harvard & Smithsonian Astrophysics. said Dr. David Wilner, an astrophysicist at the Center for Science.
“The research requires extensive community effort and has incredible legacy value with multiple potential pathways for future research.”
“The dataset of belt and planetary systems properties enables research into the birth and evolution of these belts, as well as the study of tracking observations across next-generation wavelength ranges from the NASA/ESA/CSA James Webspace Telescope. “The huge telescope and future plans for Alma are plans to zoom further into the details of these belts.”
a paper The explanation of the results was published in the journal Astronomy and Astrophysics.
____
L. Matra et al. 2025. Reasons for the nearby stars Alma and SMA: population resolved 74 planetary belts at millimeter wavelengths. A&A 693, A151; doi: 10.1051/0004-6361/202451397
Candidate planetary systems detected by microlens method are thought to travel at least 540 km (1.2 million mph) per 540 km.
Impressions of the superniputin exoplanet artist orbiting a low-mass star near the center of our Milky Way galaxy. Image credits: NASA/JPL-Caltech/R. Hurt, Caltech-IPAC.
“I think this is the so-called Super Neptune world orbiting a low-mass star at the distance between Venus and Earth's orbit,” University of Maryland, College Park, NASA Goddard. At the Space Flight Center.
“The star is so weak that it is outside its habitable zone. If so, it will be the first planet ever discovered orbiting a fast star.”
The system was first discovered indirectly in 2011 thanks to the microlens event MOA-2011-BLG-262.
“Microlenses occur because a large amount of presence distorts the fabric of space-time,” the astronomer explained.
“Whenever an intervening object appears to drift near a background star, light from the star curve passes through space-time, distorted around nearby objects.”
“If the alignment is particularly close, the distortion around the object behaves like a natural lens and can amplify the light of the background star.”
In MOA-2011-BLG-262, microlens signals revealed pairs of celestial bodies.
Astronomers have determined relative masses (one is about 2,300 times heavier than the other), but their exact mass depends on how far they are from the Earth.
“It's easy to determine the mass ratio,” said Dr. David Bennett, a senior research scientist at the Goddard Space Flight Center at the University of Maryland, College Park and NASA.
The MOA-2011-BLG-262 Discovery Team has a microlens object that is about 20% of the stars, about 29 times heavier than Earth, or Jupiter's mass with Exomoon. They suspected it was one of roughly four times more illicit planets.
To understand which explanations were more likely, Dr. Terry, Dr. Bennett and his colleagues searched data from the Keck Observatory in Hawaii and the Gaia satellite at the ESA.
If the pair are illegitimate Exoplanets and Exomoons, they will not look effective – dark objects lost in the black space of the universe.
Researchers discovered a strong suspect about 24,000 light years away and put it in the bulge of the Milky Way galaxy.
By comparing the position of the stars in 2011 and 2021, they calculated its speed.
But that's its 2D motion. If it's heading towards us or away from us, it must be moving even faster.
Its true speed may increase to the galaxy's escape speed exceeding 600 km/s (1.3 million mph) per second.
If so, the planetary system is destined to traverse intergalactic space for millions of years to come.
“To make sure the newly identified star is part of the system that caused the 2011 signal, we looked again in another year and it moved the right amount and moved in the right direction. And I want to see where it is. We've detected a signal,” Dr. Bennett said.
“If a high-resolution observation indicates that the stars remain in the same position, it can be sure that it is not part of the system that caused the signal,” says Aparna Bhatacharya at the University of Maryland. The doctor said. College Park and NASA's Goddard Space Flight Center.
“That means the Rogue Planet and the Exomoon model are preferred.”
Team's paper It was released this week Astronomy Journal.
____
Sean K. Terry et al. 2025. A candidate high-speed peeling system for galaxy swelling. AJ 169, 131; doi:10.3847/1538-3881/ad9b0f
Einstein rings (also known as Einstein – Chuworson rings or Chuworson rings) pass through very large masses such as galaxy clusters and giant galaxies as light from distant objects, such as galaxies.
Close-up of Einstein rings around NGC 6505. Image credits: ESA/Euclid/Euclid Consortium/NASA/J.-C. Cuillandre / G. Anselmi / T. Li.
This is the first powerful gravitational lens discovered in Euclidean, and the first powerful lens in the NGC object of investigation.
In the Galaxy-Galaxy's strong gravitational lens, light from the distant source galaxy is distorted and enlarged by the gravitational field of the foreground lens galaxy, forming multiple images of the source galaxy.
When the source is resolved, that is, not like a point, but close to the projection center of the lens of the source plane, a so-called Einstein ring is formed.
Both Einstein rings and lensed sources have enormous scientific value and are used in a variety of applications.
“The Einstein ring is an example of a strong gravity lens,” says Dr. Conor O'Riordan, an astronomer at the Max Planck Institute for Astrophysics.
“All powerful lenses are special because they are very rare and very scientifically useful.”
“This is especially special because it's very close to the Earth and makes the alignment very beautiful.”
The ring of light surrounding the NGC 6505, captured by ESA's Euclidean telescope, is a stunning example of the Einstein ring. Image credits: ESA/Euclid/Euclid Consortium/NASA/J.-C. Cuillandre / G. Anselmi / T. Li.
Not only are you on the ESA's Euclidean spacecraft using deep imaging data from visible cameras (VIS) and near-infrared spectrometers and photometers (NISP) equipment, but also Keck Cosmic Web Imager (kcwi) At the Wm Keck Observatory, astronomers discovered Einstein rings around the center NGC 6505An oval galaxy about 590 million light years from Earth.
The ring around the foreground NGC 6505 is made up of light from even brighter galaxies.
The galaxy in the background is 4.42 billion light years away, and the light is distorted by the force of gravity on its way towards us.
“I think it's very interesting to see this ring within the famous galaxy, first discovered in 1884,” says Dr. Valeria Pettorino, scientist of the ESA Euclid project.
“The galaxy has been known to astronomers for a very long time. Still, this ring has not been observed before.”
“This shows how powerful Euclidean is and we're finding new things in places we thought we knew well.”
“This discovery is extremely encouraging and demonstrates its incredible capabilities for the future of the Euclidean Mission.”
The discovery of the Einstein ring on the NGC 6505 is paper Published in the journal Astronomy and Astrophysics.
____
CM Orioludan et al. 2025. Euclid: Complete Einstein Ring for NGC 6505. A&A 694, A145; doi: 10.1051/0004-6361/202453014
The astronomers have identified nine rings using NASA/ESA Hubble Space Telescope and WM KECK Observatory’s KECK COSMIC Web Imager (KCWI) data.
Pasha et al。 Nine rings around the Leda 1313424, a ring galaxy, about 567 million lights, have been detected around the constellation of Pisces. They also confirmed that the galaxy had pigeons and created these rings through the Reda 1313424. Image Credit: NASA / ESA / HUBBLE / IMAD PASHA & Pieter Van Dokkum, Yale University.
LEDA 1313424 A ring galaxy found in the image of Legacy Survey Dr9 in 2019.
The galaxy called Bulls Eye’s nickname has an reddish transition of Z = 0.0394 corresponding to the distance of 567 million light years.
The diameter of LEDA 1313424 is 250,000 light years. This is almost 2.5 times that of the Milky Way galaxy.
“This was an accidental discovery,” said Imado Pasha, a student in the Yale University doctoral course.
“I was looking at a ground -based imaging survey, but when I saw a galaxy with some transparent rings, I was immediately drawn to it. I had to stop to investigate it. did.”
Approximately 50 million years ago, a small blue dwarf galaxy moved like a dart that passed the core of LEDA 1313424.
With this collision, 10 rings were created around LEDA 1313424. This has detected nine unprecedented rings.
A thin gas trail links the pair, but is currently 130,000 light years away.
“We are catching Bulls Eye at a very special moment,” said Professor Peter Van Dockm of Yale University.
“When there are many rings in such a galaxy, there is a very narrow window after the impact.”
Researchers used Hubble’s clear vision to identify the eight rings of LEDA 1313424 and check another ring using KECK.
They also discovered a brilliant connection between Ring Galaxy and many years. The galaxy ring seems to have moved almost exactly as expected as the model predicted.
“The theory was developed on the day I saw a lot of rings,” said Professor Van Dokum.
“I am very pleased to confirm the predictions for these years in the Bulls Eye Galaxy.”
From the top, it is clear that the Galaxy ring is not evenly spaced like a Dart board. The image of Hubble shows the galaxy from a slight angle.
“If you look down on the galaxy directly, the ring looks circular, the ring will be bundled in the center, and will gradually be far away and gradually break away,” Pasha explained.
a paper Regarding this discovery, it was released today Astronomical physics journal letter。
______
Imad Pasha et al。 2025. Bullsia: HST, KECK/KCWI, and the characteristics of the giant 9 -ring dragon fly. APJL 980, L3; DOI: 10.3847/2041-8213/AD9F5C
New data from a very large telescope between NASA's CHANDRA X-Ray Observatory and ESO provides evidence that explosions from ultra-large black holes can help you cool the gas and feed yourself.
These images indicate two galaxy clusters of research, Perseus cluster and Centaul scraster. The chandradata represented by blue reveals X -rays from hot gas filaments, and VLT data indicates a red cooler filament. Image Credit: NASA / CXC / SAO / OLIVARES et al. / dss / cfht / sitelle / ESA / STSCI / ESO / VLT / MUSE / N. wolk.
In a new study, Dr. Valeria Olibales and her colleagues of Santiago De Chile University analyzed the deep observations of seven galaxy clusters, which indicate a remarkable poly-phase filament structure: Perseus, M87, Centaur, Abel 2597, Abel 1795, Hydra-A, Hydra, and Hydra PKS 0745-191.
“At the center of the galaxy cluster is the huge galaxy in the universe. This galaxy has a huge black hole with millions to billion times a mass of the sun.” I said.
“The jet from these black holes is driven by the black hole that exhales gas.”
Their results support a model in which the explosion from the black hole causes hot gases and cools down a narrow gas filament.
Gas turbulence also plays an important role in this trigger process.
According to the model, some of these warm gases in these filaments should flow into the center of the galaxy and supply them to black holes, causing explosions.
The explosion cools more gas, supplies black holes, and leads to further explosions.
The model predicts that it is related to the bright gas and warm gas filament at the center of the galaxy cluster.
More specifically, in areas where hot gas is bright, warm gases need to be brightened.
“Our results provide a new understanding of filament filled with these gases. This is important not only for feeding black holes, but also for forming new stars.” The person said.
“This progress has been made possible by innovative technology that separates hot filaments of Chandra X -ray data from other structures, including a large cavity of hot gas created by a black hole jet.”
“The newly discovered relationship of these filaments indicates the remarkable similarity of what is found in the tail of the jellyfish. These are peeled off when moving the surrounding gases and the long tail. It was formed.
“This similarity means that the universe connection between the two objects is revealed and that these objects have a similar process.”
Team paper Published in the journal Natural astronomy.
______
V. Olivary et al. Hα-X-ray surface gaze correlation of the cooling flow cluster filament. Nut asron Released online on January 27, 2025. Doi: 10.1038/S41550-02473-8
G-Dwarf is one of these outside planets, HD 20794D, which is likely to be a rocky planet where the parent’s star can live. HD 20794。
This image shows a resident zone around HD 20794 (green) and three planets in the system. Image credit: Gabrielpérezdíaz / smm / IAC.
“HD 20794 is not a normal star in HD 20794D,” said UNIGE ASTRONOMER XAVIER DUMUSQUE.
“Due to its lightness and proximity, it becomes an ideal candidate for the future telescope, and its mission is to directly observe the atmosphere of the outside planet.”
The HD 20794 is a bright G6V star in 6.04 % (19.7 light year) on the constellation of Ellidanus.
Stars, also known as LHS 19 or ERI, host at least three large -scale outside planets: HD 20794B, C, and D.
They have a track period of 18.3, 89.7, and 647.6 days, along with 2.2, 3, and 5.8 global quality.
“The interest of Super Earth Planet The HD 20794D is located in a zone where the stars can live and the place where liquid water can exist.
“Instead of tracing a relatively circular orbit like the Earth or Mars, the HD 20794D trains an elliptical trajectory with a large change in the distance to the star during the revolution.”
“Therefore, the planet vibrates between the inner ends of the star -free zone (0.75 au) and the track (2 au).”
“If there is water in the HD 20794D, it will promote the appearance of life from ice state to liquid state during the Earth revolution around the stars.”
Astronomer monitored the HD 20794 system with the ESO’s very large telescope (VLT) in the paranal of Chile, the Echelle branch device of the rocky planet and the stable spectrum observation (espresso) device.
They participated in espresso data along with the data of the high -precision radial speed planetary searcher (HARPS) device installed in the 3.6 -meter telescope of Chile, including archive data and new measurements from recent archives and new measurements.
“The HD 20794 system is a high -priority target for future air characteristics evaluation with direct imaging facilities,” said researchers.
Their paper Published in the journal Astronomy and astronomical physics。
______
N. Nari et al。 2025. Review of nearby star HD 20794 multi -planet system A & A 693, A297; DOI: 10.1051/0004-6361/202451769
Astronomers have discovered a blazar — a quasar with a jet aligned along our line of sight — at redshift of 7. Named VLASS J041009.05-013919.88, this object is the most distant blazar ever identified, providing a rare glimpse into the epoch of reionization when the Universe was less than 800 million years old.
An artist's impression of a blazar. Image credit: DESY / Science Communication Lab.
VLASS J041009.05-013919.88 (J0410-0139 for short) is powered by a black hole with a mass of 700 million solar masses.
Multi-wavelength observations show that its radio variability, compact structure, and X-ray properties identify it as a blazar with a jet aligned toward Earth.
The discovery of J0410-0139 implies the existence of a much larger population of similar jetted sources in the early Universe.
These jets likely enhance black hole growth and significantly affect their host galaxies.
“The fact that J0410–0139 is a blazar, a jet that by chance happens to point directly towards Earth, has immediate statistical implications,” said Dr. Eduardo Bañados, an astronomer at the Max Planck Institute for Astronomy.
“As a real-life analogy, imagine that you read about someone who has won $100 million in a lottery.”
“Given how rare such a win is, you can immediately deduce that there must have been many more people who participated in that lottery but have not won such an exorbitant amount.”
“Similarly, finding one active galactic nucleus with a jet pointing directly towards us implies that at that time, there must have been many active galactic nuclei in that period of cosmic history with jets that do not point at us.”
“Where there is one, there's one hundred more,” said Dr. Silvia Belladitta, also from the Max Planck Institute for Astronomy.
Observations with instruments such as NSF's Very Large Array, NSF's Very Long Baseline Array, NASA's Chandra X-ray Observatory, and the Atacama Large Millimeter/submillimeter Array (ALMA) indicate that J0410-0139 exhibits radio emission amplified by relativistic beaming, a hallmark of blazers.
Its spectrum also confirms stable accretion and emission regions typical of active black holes.
This discovery raises questions about how supermassive black holes grow so rapidly in the Universe's infancy.
Models may need to account for jet-enhanced accretion or obscured, super-Eddington growth to reconcile this finding with the known black hole population at such high redshifts.
“This blazar offers a unique laboratory to study the interplay between jets, black holes, and their environments during one of the Universe's most transformative epochs,” said Dr. Emmanuel Momjian, an astronomer at NSF's National Radio Astronomy Observatory.
“The alignment of J0410-0139's jet with our line of sight allows astronomers to peer directly into the heart of this cosmic powerhouse.”
“The existence of J0410-0139 at such an early time suggests that current radio surveys might uncover additional jetted quasars from the same era.”
“Understanding these objects will illuminate the role of jets in shaping galaxies and growing supermassive black holes in the early Universe.”
The results appear in two papers (paper #1 and paper #2) in the journal Nature Astronomy and the Astrophysical Journal Letters.
_____
E. Bañados et al. A blazar in the epoch of reionization. Nat Astronpublished online December 17, 2024; doi: 10.1038/s41550-024-02431-4
Eduardo Bañados et al.2025. [C ii] Properties and Far-infrared Variability of az = 7 Blazar. ApJL 977, L46; doi: 10.3847/2041-8213/ad823b
A new study has provided the first definitive evidence that fast radio bursts can originate from the magnetosphere, the highly magnetic environment immediately surrounding very compact objects.
Artist's impression of a neutron star. Image credit: Sci.News.
Fast radio bursts (FRBs) are short, brilliant bursts of radio waves that originate primarily from extragalactic distances.
These phenomena release as much energy in one millisecond as the sun does in 10,000 years, but the physics that cause them are unknown.
Theories range from a highly magnetized neutron star exploded by a stream of gas near a supermassive black hole to proposals whose outburst characteristics match the signature of technology developed by an advanced civilization.
MIT astronomer Kenzie Nimmo and colleagues focused on the event, dubbed FRB 20221022A, in a new study.
This burst was first detected by the Canadian Hydrogen Intensity Mapping Experiment (CHIME) in 2022.
The event occurred in a galaxy about 200 million light years away and lasted about 2 milliseconds.
New research suggests that FRB 20221022A emerged from a region extremely close to the rotating neutron star, up to 10,000 km away.
At such close distances, the burst could have originated from the neutron star's magnetosphere, a highly magnetic region immediately surrounding the microstar.
“In a neutron star environment like this, the magnetic field is actually at the limit of what the universe can produce,” Dr. Nimmo said.
“There has been a lot of discussion about whether this bright radio emission can leak out of that extreme plasma.”
“Atoms cannot exist around these highly magnetic neutron stars, also known as magnetars. They are simply torn apart by the magnetic field,” added astronomer Kiyoshi Masui of the Massachusetts Institute of Technology.
“What's interesting here is that we found that the energy stored in magnetic fields gets twisted and rearranged near the source of the magnetic field and is emitted as radio waves visible on the far side of the universe.”
This website uses cookies so that we can provide you with the best user experience possible. Cookie information is stored in your browser and performs functions such as recognising you when you return to our website and helping our team to understand which sections of the website you find most interesting and useful.
Strictly Necessary Cookies
Strictly Necessary Cookie should be enabled at all times so that we can save your preferences for cookie settings.
