Discover PicII-503: A Protostar in the Ancient Pictor II Dwarf Galaxy
This striking image of PicII-503 highlights a second-generation star with the lowest iron content ever recorded outside our Milky Way galaxy. Image credits: CTIO / NOIRLab / DOE / NSF / AURA / University of Alaska Anchorage TA Chancellor and NSF NOIRLab / M. Zamani and D. de Martin, NSF NOIRLab / Anirudh Chiti / Alex Drlica-Wagner.
“This marks the first definitive detection of element formation in protogalaxies,” stated Dr. Aniru Chitty, a postdoctoral researcher at the University of Chicago, now at Stanford University.
“This discovery fills a crucial gap in understanding the origin of elements during the universe’s formative years.”
In the primordial epochs following the Big Bang, the cosmos was relatively simple, comprised almost entirely of hydrogen, helium, and lithium, giving rise to giant stars primarily formed by these elements.
More complex elements, like calcium and gold, were scarce since they had to be synthesized within stars themselves.
At the cores of these massive stars, nuclear fusion processes created increasingly heavier elements.
When these stars eventually exploded, they contributed to the formation of new stars, perpetuating this cycle until a diverse array of elements emerged, forming the universe we know today.
“To track elemental formation, we must search for stars with minimal heavy elements, as these accumulate over time,” explained University of Chicago astronomer Alexander Gee.
Using the Magellan Telescope at Las Campanas Observatory and ESO’s Very Large Telescope, astronomers identified a significant candidate star within the ultrafaint dwarf galaxy Pictor II.
This star, identified as PicIII-503, exhibits a remarkable structure, with an iron content approximately 1/100,000 times lower than that of our Sun.
This extraordinary finding not only generates excitement but also offers insights into the enigmatic origins of these early stars.
Consequently, since PicIII-503 remains within its original protogalaxy, astronomers have uncovered vital information regarding its formation theory, particularly related to the star’s explosive death.
“Upon the demise of a massive star, it possesses an ‘onion-skin’ structure: lighter elements like carbon reside in outer layers while heavier elements are found inside,” Gee noted.
“A weak explosion may only eject the outer layers, allowing the heavier inner materials to coalesce with neighboring gas and dust, which can form future generations of stars.”
“However, a vigorous explosion could propel these materials far beyond the small galaxies that existed during that era,” he added.
This exciting discovery provides context for the abundance of carbon-rich stars observed in our Milky Way, illuminating their origin, Dr. Chitty emphasized.
For more on the discovery of PicIII-503, refer to the research paper published in Nature Astronomy.
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A. Chitty et al. Enrichment by the first stars of relic dwarf galaxies. Nat Astron published online on March 16, 2026. doi: 10.1038/s41550-026-02802-z
Stunning Close-Ups of Triangular Galaxies Captured by ESO’s Very Large Telescope (VLT) Illuminate the Gas and Dust That Fuel Star Birth and Galaxy Evolution.
This VLT/MUSE image showcases the Triangulum Galaxy, a spiral galaxy approximately 3 million light-years away in the constellation Triangulum. Image credit: ESO / Feltre et al.
The Triangulum Galaxy, also referred to as Messier 33 or NGC 598, is a spiral galaxy located roughly 3 million light-years from Earth.
Visible as a faint haze in the Triangulum constellation under optimal dark sky conditions, this galaxy has long captivated astronomers.
It stands as one of the most significant members of the Local Group, a gravitationally bound assembly of over 50 galaxies, including the Milky Way and Andromeda. Though third largest in the group, it is the smallest spiral galaxy in this collection.
Spanning about 60,000 light-years, the Triangulum Galaxy is substantially smaller than Andromeda, which measures around 200,000 light-years, and the Milky Way, estimated at 100,000 light-years in diameter.
Dr. Anna Feltre and her colleagues from the INAF Astrophysical Observatory in Arcetri emphasized, “Stars do not exist in isolation; they thrive in rich, complex environments where they actively form.”
“Investigating these cosmic interactions enhances our understanding of star formation and the influence of their radiation on surrounding matter, which is crucial for unraveling how galaxies evolve,” they added.
In their research, astronomers utilized data collected by the VLT’s Multi-Unit Spectroscopic Explorer (MUSE).
“MUSE’s unique capability allows it to disperse light into a spectrum of colors, enabling us to analyze the chemical makeup of the interstellar medium across the entire field,” the team elaborated.
The vivid colors in the images signify various elements: blue, green, and red represent oxygen, hydrogen, and sulfur, respectively.
“Thanks to MUSE, we have mapped the distribution and motion of numerous elements, crucial for understanding the connections between stars and their environments.”
“These cosmic interactions create a visually stunning and dynamic landscape, revealing that star birthplaces are more intricate and beautiful than we ever envisioned,” concluded Dr. Feltre.
For in-depth insights, refer to the team’s paper published in the journal Astronomy and Astrophysics.
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A. Feltre et al. 2026. M3D: Mosaicking M33 using the MUSE datacube. I. Elucidating the Diversity of the H II Region of M33 Using MUSE. A&A 706, A367; doi: 10.1051/0004-6361/202557122
Globular cluster NGC 1850 lies within the Large Magellanic Cloud, our Milky Way’s satellite galaxy.
Copyright: NASA, ESA, and P. Goudfrooij (Space Telescope Science Institute). Processing: Gladys Kober (NASA/Catholic University of America)
What distinguishes a collection of stars from an entire galaxy? This seemingly simple inquiry poses a significant challenge to astronomers today.
Most casual stargazers view galaxies as distinct entities, akin to completed masterpieces. When peering through a backyard telescope, one can observe billions of stars or even more than 100 billion, radiating in a spiral formation of vibrant light. My experiences as a theoretical particle cosmologist reveal that galaxies are enveloped by an unseen dark matter halo, stretching far beyond the visible sphere. It’s also crucial to note that not all galaxies conform to the spiral design; some take on oval shapes, resembling a flattened sphere, making the classification of galaxies more complex than it appears.
As I’ve noted in previous discussions, our classification of galaxies continues to evolve. Clearly defining an object with a distinct spiral formation and vast star count is straightforward, but what about those that appear spheroidal yet possess millions of stars? Some of these may be categorized as globular clusters—collections of tens to millions of stars bound by gravity within a mere few light years.
These globular clusters are exclusively found within galaxies, indicating a fundamental difference between them and galaxies themselves. Globular clusters exhibit compactness, in contrast to galaxies, which expand more diffusely throughout space. The same holds true for dwarf spheroidal galaxies, which, despite being smaller than our Milky Way, still exhibit a relatively vast reach and often contain a more diverse stellar population. Moreover, while dwarf spheroidals are surrounded by their own dark matter halos, globular clusters typically are not.
Visualize a nested structure of galaxies enveloped by dark matter: at the center lies the Milky Way, encircled by a substantial halo, featuring a small quasi-spheroid and then an even smaller subhalo. This framework assists astronomers in distinguishing between galaxies and globular clusters, as the presence of dark matter identifies an object as a galaxy.
The understanding of these classifications was relatively clear until 2005, when the Sloan Digital Sky Survey (SDSS) released its initial data set. This monumental project aimed to document a quarter of the night sky, revealing numerous celestial entities never before observed. Among these findings was a faint cluster of stars near the Milky Way, dubbed ultra-faint satellites, which blurred the lines separating globular clusters from galaxies.
Further investigations into these enigmatic objects have unveiled some to be galaxies saturated with dark matter, yet the challenge persists, as these satellites remain elusive and hard to detect, living in what is described as the “valley of uncertainty.” A 2018 study by Blair Conn and colleagues noted these peculiar entities—neither clearly galaxies nor definitively not.
Ursa Major III has an astonishingly low count of only 60 stars.
CFHT/Unions/S. Gwin
Despite our anticipation for data to clarify these obscure classifications, recent sky surveys have unveiled even fainter clusters of celestial objects. We have learned to hesitate before declaring what is or isn’t a galaxy. A recent 2023 study led by Simon Smith from the University of Victoria has reported the discovery of Ursa Major III, labeled as “the least luminous known satellite of the Milky Way.” While this assertion instills confidence, the supporting evidence comprises merely 60 stars—an extraordinarily small number.
Ursa Major III might seem diminutive, yet its implications could resonate widely. A study last year asserted that, if it qualifies as a galaxy, it could help eliminate certain dark matter models. Determining whether Ursa Major III and its counterparts are genuinely galaxies could significantly impact astrophysics, cosmology, and particle physics.
Progress continues on this front. Recently, William Cerny and his team at Yale University published findings from an extensive study on a large group of these mysterious objects. Their conclusion? A diverse array exists among these entities, though further investigation is essential. We may not have definitive answers yet, but we sit at an exciting crossroads—firmly engaging in the pursuit of knowledge and further discoveries.
Your reading list:
Special collection: Poets, particularly Courtney Lamar Charleston and Comeonfune Felix’s Manifesto: Let the poets rule.
What are you currently viewing?
Too Much Alfred Hitchcock!
What are you presently working on?
Prepping for the U.S. release of my book, The End of Space and Time, on April 7th!
Chanda Prescod-Weinstein is an associate professor of physics and astronomy at the University of New Hampshire. She is the author of Turbulent Universe and her forthcoming book The Ends of Space and Time: Particles, Poetry, and the Boogie of Cosmic Dreams.
Unraveling Cosmic Mysteries in Cheshire, England
Join some of the brightest scientific minds for an insightful weekend delving into the universe’s enigmas, inclusive of a tour of the iconic Lovell Telescope.
Utilizing archival data from NASA’s NEOWISE mission alongside information from various space and ground-based observatories, astronomers have uncovered a remarkable observational record of a massive star’s transition into a black hole—a phenomenon previously theorized but seldom witnessed.
The location and disappearance of M31-2014-DS1. Image credit: De et al., doi: 10.1126/science.adt4853.
In their final stages, massive stars often undergo instability, expanding and exhibiting significant fluctuations in brightness that can be observed by humans.
Typically, these stars meet their end in spectacular supernova explosions, which are incredibly luminous and readily detectable.
However, it is theorized that not all massive stars culminate in such explosive deaths.
In some cases, a star’s core collapses, causing the outer materials to fall inward, leading to the creation of a black hole.
These failed supernovae are particularly challenging to identify due to their weak energy signatures, often appearing as stars that simply vanish from sight.
Columbia University astronomer Kisharai De and colleagues leveraged lengthy infrared observations from the NEOWISE mission to investigate variable stars within the Andromeda Galaxy, leading to the discovery of the rare supergiant star M31-2014-DS1.
During 2014, this star brightened in mid-infrared light; however, from 2017 to 2022, it dimmed by around 10,000 times in optical light (rendering it undetectable) and about tenfold in total light.
Subsequent observations using Hubble and large terrestrial telescopes revealed faint red remnants detectable in near-infrared light, indicating the star is now heavily obscured by dust, or a shadow of its former supergiant self from years past.
Researchers interpret these findings as evidence of a failed supernova explosion, resulting in the birth of a stellar-mass black hole.
“The star’s dramatic and sustained dimming is extremely unusual, indicating the core did not explode as a supernova but collapsed directly into a black hole,” stated Dr. De.
“It was long assumed that stars of this mass always explode as supernovae.”
Their observations challenge the belief that stars of equivalent mass either necessarily explode or fail to do so, likely influenced by chaotic interactions between gravity, gas pressure, and powerful shockwaves within a dying star.
Dr. De and his fellow scientists identified M31-2014-DS1, another giant star that may have met a similar fate as NGC 6946-BH1.
This study advances our understanding of the fate of the star’s outer layers post-supernova failure and collapse into a black hole.
Interaction among these elements, particularly convection influenced by temperature variances within a star, plays a crucial role.
The internal regions are extremely hot compared to the cooler outer areas, resulting in gas movement from hotter to cooler zones.
Even after a star’s core collapse, gases in the outer layers continue to move rapidly due to convection currents.
Theoretical models suggest that these currents prevent most outer layers from plunging directly into the core. Instead, the innermost layer orbits the black hole, allowing for the ejection of the outermost layers in the convective region.
As the ejected material cools while moving from the surrounding heat of the black hole, it forms dust as atoms and molecules condense.
This dust obscures the hot gas orbiting the black hole, warming it and creating brightness observable at infrared wavelengths.
This lingering red glow remains visible long after the star has vanished.
“The accretion rate is significantly slower than if the stars collided directly,” asserted Andrea Antoni from the Flatiron Institute.
“This convective material possesses angular momentum, causing it to rotate in a circular motion around the black hole.”
“Consequently, the process takes decades instead of months or years to unfold.”
“All these factors contribute to a brighter source than otherwise anticipated, leading to a prolonged delay in the dimming of the original star.”
For further insights, refer to this paper. The findings are published in this week’s edition of Science.
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Kisharai De et al. (2026). Massive stars in the Andromeda Galaxy vanish due to black hole formation. Science 391(6786): 689-693; doi: 10.1126/science.adt4853
The recently discovered dark galaxy candidates, particularly Candidate Dark Galaxy-2 (CDG-2), are primarily composed of dark matter and emit minimal light. This intriguing object features four globular clusters and is part of the Perseus galaxy cluster. The identification of CDG-2 presents significant implications for astronomers’ understanding of galaxy formation and evolution within the cosmic web, offering fresh insights into dark matter—an elusive substance that significantly outweighs ordinary matter yet remains invisible.
CDG-2 (dashed red circle) showcases its dominance in dark matter with only a sparse scattering of stars. Image credit: NASA/ESA/Dayi Li, Toronto/Joseph DePasquale, STScI.
“In the expansive fabric of the universe, most galaxies emit brilliant light across cosmic time and space,” stated University of Toronto astronomer David Lee and his research team.
“However, a rare subset of galaxies remains mostly hidden: those with low surface brightness, primarily dominated by dark matter and containing only a sparse collection of faint stars.”
“Detecting dark galaxies of this nature poses significant challenges.”
Dr. Li and his collaborators employed advanced statistical techniques to uncover 10 previously known galaxies with low surface brightness, in addition to identifying two new dark galaxy candidates by analyzing concentrated groupings of globular clusters.
These clusters may reveal the existence of faint stellar populations that are not easily observed.
To validate one of the dark galaxy candidates, they utilized NASA/ESA’s Hubble Space Telescope, ESA’s Euclid Space Observatory, and the ground-based Subaru Telescope in Hawaii.
High-resolution images captured by Hubble unveil four globular clusters closely packed within the Perseus Cluster—a large galaxy cluster located approximately 240 million light-years away in the constellation Perseus.
Further follow-up surveys using Hubble, Euclid, and Subaru revealed a faint, diffuse glow surrounding the cluster, providing compelling evidence of the underlying galaxy.
“This marks the first detection of a galaxy identified solely through its globular cluster population,” remarked Dr. Lee.
“Under conservative assumptions, these four clusters represent the entirety of the CDG-2 globular cluster.”
Preliminary assessments indicate that CDG-2 possesses brightness equivalent to about 6 million Sun-like stars, with globular clusters constituting 16% of its visible content.
Remarkably, approximately 99% of its mass is believed to be dark matter, encompassing both visible and dark constituents.
Much of the normal matter that facilitates star formation may have been stripped away due to gravitational interactions with neighboring galaxies in the Perseus cluster.
“CDG-2 stands out as the most globular cluster-dominated galaxy and may be among the most dark matter-dominated galaxies ever discovered,” the astronomers concluded.
Read their research paper published in June 2025. Astrophysics Journal Letter.
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Dai (David) Lee et al. 2025. Dark galaxy candidate-2: Verification and analysis of nearly dark galaxies in the Perseus cluster. APJL 986, L18; doi: 10.3847/2041-8213/adddab
NASA/ESA/CSA’s James Webb Space Telescope has made groundbreaking observations of a galaxy featuring gaseous “tentacles” within a galaxy cluster at a redshift of 1.156. This remarkable finding allows us to observe the universe as it was approximately 8.5 billion years ago.
This web image highlights the jellyfish galaxy COSMOS2020-635829, with dashed circles marking four out-of-plane sources in its tail. Image credit: Roberts et al., doi: 10.3847/1538-4357/ae3824.
“The jellyfish galaxy derives its name from the long, tentacle-like streams trailing behind it,” explained Dr. Ian Roberts of the University of Waterloo and his team.
“As it travels quickly through the hot, dense galaxy cluster, the gas within the cluster acts like a powerful wind, pushing the jellyfish galaxy’s gas backward and forming a visible trail.”
“This phenomenon is referred to as ram pressure stripping.”
The research team discovered a new jellyfish galaxy through deep-space data captured by the Webb Telescope.
Named COSMOS2020-635829, this galaxy resides in the COSMOS field, a well-explored area of the sky studied extensively by various telescopes.
“While sifting through vast amounts of data from this thoroughly investigated region, we aimed to uncover previously undocumented jellyfish galaxies,” Dr. Roberts noted.
“Early in our analysis, we stumbled upon a distant, uncharted jellyfish galaxy that piqued our interest.”
COSMOS2020-635829 exhibits a typical galactic disk coupled with bright blue nodes in its trajectory, indicative of very young stars.
The ages of these stars suggest they formed in gas trails stripped from their host galaxy, a behavior characteristic of jellyfish galaxies.
Insights from this study challenge established beliefs regarding the conditions in deep space during that era.
Scientists previously thought the galaxy cluster was still in formation and that ram pressure stripping was a rare occurrence.
Dr. Roberts and his co-authors identified three further discoveries that could reshape our understanding of the cosmos.
“The first discovery indicates that the cluster environment was already intense enough to strip galaxies away. Second, the cluster can significantly alter galaxy properties sooner than anticipated,” Roberts explained.
“Finally, these dynamics might play a crucial role in forming the populations of inactive galaxies we observe in today’s galaxy clusters.”
“These findings offer pivotal insight into the evolution of galaxies in the early universe.”
For more details on this discovery, check out the paper published in the Astrophysical Journal.
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Ian D. Roberts et al. 2026. JWST reveals candidate jellyfish galaxy at z = 1.156. APJ 998, 285; doi: 10.3847/1538-4357/ae3824
At the galactic center lies the enigmatic supermassive black hole, Sagittarius A*. Some researchers propose that this may not be a black hole at all, but rather clusters of dark matter.
Dark matter, which comprises about 85% of the universe’s matter, does not interact with light or normal matter outside of gravitational forces. Despite its significance, our understanding of dark matter is limited. As Valentina Crespi from the National University of La Plata (UNLP) notes, “While we know dark matter exists at the galaxy’s edge, the core remains a mystery.”
Crespi and her team developed a model of a galactic nucleus made of dark matter consisting of light particles called fermions. Their findings suggest that fermion dark matter can clump in ways that resemble supermassive black holes from afar.
“From Earth, this scenario appears akin to what one would expect from a black hole; however, a spacecraft could pass through without any issues,” explains Carlos Arguelles, part of the UNLP research team. “Even if you were swallowed by a black hole, you wouldn’t perish; you would pass through safely.”
The researchers base their model on the orbit of a star near Sagittarius A* and a small gas cloud, aligning with observations of galaxy rotation and imagery from the Event Horizon Telescope (EHT) from 2022. This imaging reveals a glowing ring of superheated matter around Sagittarius A*, potentially influenced by a dark matter core.
However, observation support for the dark matter theory does not confirm its validity. Gaston Gillibet from New York University stresses, “While this simple explanation aligns with the evidence, I still believe the central object is likely a black hole.” He emphasizes the necessity of remaining open to all possibilities in this fascinating debate.
Concerns arise regarding the model’s applicability to observations near the event horizon. Shep Doeleman from Harvard University notes that the distinctive spiral pattern of the magnetic field in this region corresponds closely with black hole characteristics.
Moreover, fermion dark matter’s clumping is limited to about 10 million times the Sun’s mass. Although this could explain the majestic size of supermassive black holes, images of M87*—a black hole substantially larger than Sagittarius A*—complicate this theory as M87* closely resembles Sagittarius A* despite its size of approximately 6.5 billion solar masses.
Researchers admit that both dark matter and black hole theories hold equal plausibility. Crespi notes, “While we have enhanced tools today, confirming the nature of these phenomena is still not foolproof.” Achieving the necessary image resolution for this identification would extend far beyond the capabilities of even the next-generation EHT, indicating that definitive answers may be decades away.
If Sagittarius A* is indeed a manifestation of dark matter, it would profoundly impact our understanding of the universe. Fermion dark matter, which current cosmological models do not predict, could revolutionize not only our comprehension of black holes but also our entire cosmic paradigm.
Explore the Mysteries of the Universe: Cheshire, England
Join leading scientists for a weekend of exploration into the universe’s mysteries, with an engaging program that includes a visit to the iconic Lovell Telescope.
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Astronomers utilizing the NASA/ESA/CSA James Webb Space Telescope have identified an extraordinary presence of small gas-phase hydrocarbons—such as benzene, triacetylene, diacetylene, acetylene, methane, and methyl radicals—within the concealed core of the ultra-bright infrared galaxy IRAS 07251-0248.
Hydrocarbons are influential in shaping the chemistry of the interstellar medium. However, definite observational constraints on their enrichment and relationship with carbonaceous particles and polycyclic aromatic hydrocarbons remain elusive. García Bernete et al. report Webb infrared observations of the Local Ultraluminous Infrared Galaxy (ULIRG) IRAS 07251-0248, revealing extragalactic detections of small gas-phase hydrocarbons. Image credit: García-Bernete et al., doi: 10.1038/s41550-025-02750-0.
The core of IRAS 07251-0248 (also known as 2MASS J07273756-0254540) is obscured by significant amounts of gas and dust.
This dense material absorbs most radiation emitted by the central supermassive black hole, complicating studies with traditional telescopes.
However, the infrared spectrum can penetrate this dust, providing unique insights about these regions and illuminating vital chemical processes in this heavily obscured core.
Dr. Ismael García Bernete and his team employed spectroscopic observations using Webb’s NIRSpec and MIRI instruments, covering wavelengths from 3 to 28 microns.
These observations reveal chemical signatures of gas-phase molecules alongside signatures from ice and dust particles.
These data empowered astronomers to characterize the abundance and temperature of various chemical species within the core of this concealed galaxy.
Remarkably, they discovered an exceptionally high abundance of small organic molecules such as benzene, methane, acetylene, diacetylene, and triacetylene—the first such detections outside our Milky Way, including the methyl radical.
Additionally, substantial amounts of solid molecular materials, including carbonaceous particles and water ice, were identified.
“We uncovered unexpected chemical complexity, showcasing abundances far exceeding current theoretical models,” stated Dr. García Bernete, an astronomer at the Astrobiology Center.
“This suggests a continuous source of carbon within these galactic nuclei, fueling this rich chemical network.”
“These molecules may serve as vital building blocks for complex organic chemistry, relevant to processes that pertain to life.”
Professor Dimitra Rigopoulou from the University of Oxford remarked, “Small organic molecules may not exist in living cells, yet they could play a pivotal role in prebiotic chemistry—a crucial step toward forming amino acids and nucleotides.”
These findings were published in a recent issue of Nature Astronomy.
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I. Garcia-Bernete et al. Abundant hydrocarbons within buried galactic nuclei with evidence of processing of carbonaceous particles and polycyclic aromatic hydrocarbons. Nat Astron, published online on February 8, 2026. doi: 10.1038/s41550-025-02750-0
Astronomers utilizing the NASA/ESA Hubble Space Telescope have captured stunning new images of the lenticular galaxy NGC 7722.
This captivating Hubble image showcases NGC 7722, a lenticular galaxy located approximately 187 million light-years from Earth in the constellation Pegasus. Image credits: NASA / ESA / Hubble / RJ Foley, UC Santa Cruz / Dark Energy Survey / DOE / FNAL / DECam / CTIO / NOIRLab / NSF / AURA / Mehmet Yüksek.
NGC 7722, also known by its alternate names IRAS 23361+1540, LEDA 71993, and UGC 12718, was first discovered on August 12, 1864, by German astronomer Heinrich Louis d’Arest.
This intriguing lenticular galaxy is part of the NGC 7711 group, which comprises seven prominent galaxies.
“Lenticular galaxies represent a unique classification that exists between the well-known spiral and elliptical galaxies,” Hubble astronomers stated.
“These galaxies are less common as their ambiguous morphology makes it challenging to classify them definitively as spiral, elliptical, or a hybrid of both.”
“Many known lenticular galaxies, including NGC 7722, exhibit features of both spiral and elliptical types.”
“Although NGC 7722 lacks the prominent arms characteristic of spiral galaxies, it showcases a magnificent glowing halo and a bright central bulge reminiscent of elliptical galaxies,” the researchers explained.
“Unlike elliptical galaxies, NGC 7722 possesses a visible disk featuring concentric rings swirling around a luminous core.”
“One of its most remarkable attributes is the long lanes of dark red dust that elegantly curl around the outer disk and halo.”
Recent images of NGC 7722 taken with Hubble’s Wide Field Camera 3 (WFC3) bring the galaxy’s striking dust lanes into sharp focus.
“Dust bands are common among lenticular galaxies and create a stunning contrast against the smooth, luminous halo typically surrounding such galaxies,” the astronomers added.
“The distinctive dust lane of NGC 7722, like many other lenticular galaxies, is believed to result from a past merger with another galaxy.”
“While the exact formation processes of lenticular galaxies remain elusive, mergers and gravitational interactions are thought to play a critical role in altering their shapes and influencing their gaseous and dusty content.”
New research led by Rohan Naidu from the Massachusetts Institute of Technology’s Kavli Institute for Astrophysics and Space Studies reveals that the galaxy MoM-z14 existed a mere 280 million years after the Big Bang.
This image depicts MoM-z14, a galaxy that emerged shortly after the Big Bang. Image credit: NASA/ESA/CSA/STScI/Rohan Naidu, MIT/Joseph DePasquale, STScI.
“Thanks to the Webb Space Telescope, humanity can now explore deeper into the universe than ever before, challenging our previous predictions,” stated Dr. Naidu.
Using Webb’s NIRSpec instrument, Dr. Naidu and colleagues confirmed that MoM-z14 possesses a cosmological redshift of 14.44. This indicates that for approximately 13.5 billion years—out of the universe’s estimated age of 13.8 billion years—the light has been elongated and “shifted” to red wavelengths as it travels through space.
Dr. Pascal Oesch from the University of Geneva emphasized, “While we can estimate a galaxy’s distance from images, it’s crucial to follow up with detailed spectroscopy to accurately understand what we are observing.”
MoM-z14 is part of an increasing number of unexpectedly bright galaxies in the early universe, outnumbering theoretical predictions before the Webb’s launch by 100 times.
“The disparity between theoretical models and observational data regarding the early universe is expanding, prompting intriguing questions for future exploration,” said Dr. Jacob Shen, a postdoctoral researcher at MIT.
One potential avenue for research lies in the oldest stars within the Milky Way, where a small number exhibit high nitrogen levels, mirroring some of Webb’s observations of early galaxies, including MoM-z14.
“We can examine ancient stars in our galaxy like fossils from the early universe, and thanks to Webb, we have direct insights into galaxies at that epoch, revealing shared features such as unusual nitrogen enrichment,” remarked Dr. Naidu.
Interestingly, MoM-z14 emerged only 280 million years post-Big Bang, a brief time span that shouldn’t have allowed for ample nitrogen production from stellar generations.
Researchers propose that the dense early universe environment might have facilitated the formation of supermassive stars, capable of producing more nitrogen than any stars observed nearby.
Additionally, MoM-z14 appears to be clearing the surrounding universe of the dense primordial hydrogen fog characteristic of early cosmic history.
The Webb was designed to chart this cleansing period known as reionization, where early stars broke through dense hydrogen gas and emitted enough high-energy light to reach us today.
MoM-z14 serves as a key clue in mapping the reionization timeline, a task previously unattainable before Webb unveiled this epoch of the universe.
“We require further information to understand the early universe better. More detailed observations from Webb and additional galaxies will help identify common features, and NASA’s next Nancy Grace Roman Space Telescope is expected to contribute significantly,” noted Yijia Li, a graduate student at Penn State.
“This is an exhilarating time as the Webb reveals the universe’s earliest epochs, showcasing the vastness of uncharted territory still to explore.”
Rohan P. Naidu et al. 2026. Cosmic Miracle: Confirmed in JWST, an extremely bright galaxy with zspec=14.44. Open Astrophysics Journal in press. arXiv: 2505.11263
Webb astronomers have unveiled a breathtaking image captured by the NASA/ESA/CSA James Webb Space Telescope, showcasing MACS J1149.5+2223 (MACS J1149), a cosmic collection of hundreds of galaxies situated about 5 billion light-years from Earth in the constellation Leo. The latest images not only highlight the cluster’s brilliant galaxies but also illustrate how their immense gravitational forces uniquely affect the fabric of space-time.
The stunning image of the galaxy cluster MACS J1149.5+2223. Image credits: NASA / ESA / CSA / Webb / C. Willott, National Research Council Canada / R. Tripodi, INAF-Astronomical Observatory of Rome.
The latest Webb image of MACS J1149 dramatically showcases light from background galaxies, which is bent and magnified in a remarkable phenomenon known as gravitational lensing. This creates elongated arcs and distorted shapes, revealing the mass of both clusters.
“The immense gravity of this galaxy cluster does more than hold the galaxies adrift in the universe,” the Webb astronomers explained in a statement.
“As light from galaxies beyond the cluster travels toward our telescope over billions of years, its trajectory through space-time is warped by the gravitational forces of the intervening galaxies.”
This gravitational lensing effect is evident throughout the image of MACS J1149, with galaxies appearing stretched into narrow streaks and others morphing into unusual shapes. A prime example of gravitational lensing can be seen near the image’s center, just below the prominent white galaxy.
In this area, a galaxy with spiral arms has been transformed into a shape resembling a pink jellyfish. This peculiar galaxy once harbored the farthest single star ever identified and a supernova that appeared four times simultaneously.
“This program employs Webb’s advanced instruments to explore the evolution of low-mass galaxies in the early Universe, shedding light on their star formation, dust content, and chemical makeup,” the astronomers stated.
The data collected will also assist researchers in studying the epoch of reionization, when the first stars and galaxies illuminated the universe, mapping mass distributions in galaxy clusters, and understanding how star formation diminishes within cluster environments.
Exploring ‘Small Red Dots’ Unveiled by the James Webb Space Telescope
Credit: NASA, ESA, CSA, STScI, and D. Kocevski (Colby U.)/Space Telescope Science Institute Public Extension Office
The remarkable bright galaxies uncovered by the James Webb Space Telescope (JWST) may not be as brilliant as initially thought. These celestial bodies once posed a challenge to our cosmic understanding, implying they were home to supermassive black holes and an unexpected abundance of stars. However, new insights suggest these galaxies may harbor “baby” black holes.
During its initial years surveying the early Universe, JWST serendipitously discovered numerous bright and red galaxies, referred to as “little red dots” (LRDs).
The light emitted by these galaxies indicates the presence of far more mass than previously recognized in any other galaxy. They exhibit star densities that challenge existing models or host black holes larger than expected considering the size of their parent galaxies.
Both scenarios would necessitate a substantial overhaul of our galaxy formation and black hole growth theories in the early Universe.
Initial assumptions posited that the red hue of LRDs was due to copious dust surrounding the black holes or stars. This notion has come under scrutiny, as researchers find little evidence of dust in these extraordinary galaxies.
Jenny Green, a researcher at Princeton University, posits that this discovery warrants a reevaluation of LRD characteristics. “We were confident that if red coloration was due to dust, we’d detect dust emissions. However, we found none,” Green stated. “This suggests our initial assumption about their dust content was flawed.”
Previous analyses gauged the total brightness of the LRDs by assessing specific wavelengths of light linked to hydrogen, calibrated against a model of how dust impacts this light.
In their recent study, Green and her team measured the total light output from two LRD galaxies across various light frequencies, including X-rays and infrared. They discovered that, except for visible light, these galaxies emitted significantly less light than the typical galaxy—implying that LRDs are at least ten times dimmer than earlier estimates. This revelation holds critical implications for the nature of black holes within LRDs.
“If the emitted light is substantially less than we’ve believed, the mass of the black holes is likely much more modest,” Green remarked. “This reduces the tensions that have perplexed us since the black holes no longer need to be exceedingly massive or possess substantial mass initially.”
The new emission patterns imply the black holes may harbor less mass compared to standard black holes. Rohan Naidu from the Massachusetts Institute of Technology describes them as “baby black holes.” He further noted these findings align with the emerging perspective that LRD black holes could be categorized as black hole stars—a unique type of black hole encased in gas.
“In a typical black hole, what we observe is merely a fraction of the total energy emitted by the system. However, we should reconsider the little red dots as bulging black hole stars,” Naidu explained. “Most of their energy appears to be emitted at wavelengths we can detect, suggesting that what we see accurately reflects their output.”
Conversely, Roberto Maiorino from the University of Cambridge emphasizes that one cannot definitively ascertain the black hole’s mass within an LRD, as the emitted light reveals its growth rate rather than its total mass.
Green asserts that the notion of baby black holes holds merit. “If the photon count is significantly lower,” she noted, “this indicates a downward shift in the entire mass scale. On average, they possess lesser masses than previously assumed when we incorrectly categorized them as regular accreting black holes enshrouded in dust.”
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Astronomers utilizing NASA’s James Webb Space Telescope have captured the most detailed infrared images of the Circus Galaxy’s core, making it one of the closest known active galaxies to the Milky Way. Webb’s observations indicate that much of the hot dust surrounding supermassive black holes in galaxies is being drawn into the black holes themselves, contrary to previous models that suggested powerful outward streams.
The Hubble image showcases the Circinus Galaxy, a spiral galaxy located approximately 13 million light-years away in the southern constellation Circinus. A close-up from Webb reveals the core’s glow in infrared light, highlighting the intricate features obscured by dust. Image credits: NASA / ESA / CSA / Webb / Hubble / Enrique Lopez-Rodriguez, University of South Carolina / Deepashri Thatte, STScI / Alyssa Pagan, NOIRLab / CTIO at STScI / NSF.
The Circus Galaxy, also known as ESO 97-G13 or LEDA 50779, is situated about 13 million light-years from Earth, nestled south of the constellation Circinus. This galaxy has fascinated astronomers due to its center being enveloped in a dense cloud of gas and dust.
Traditional ground-based telescopes have faced challenges in isolating regions near the central black hole, where matter spirals inwards and emanates intense infrared light. However, Webb’s state-of-the-art technology enabled Dr. Julien Girard and his team at the Space Telescope Science Institute to pierce through this dust veil with extraordinary clarity.
This remarkable breakthrough was achieved by employing Webb’s Near-Infrared Imager and Slitless Spectrometer (NIRISS) in a specialized high-contrast mode known as aperture masking interferometry.
This innovative technique transforms the instrument into a compact interferometer, merging light captured through various small apertures to generate precise interference patterns.
By examining these patterns, astronomers were able to reconstruct a finely detailed image of the Circus Galaxy’s central engine, revealing that the majority of infrared radiation originates from the donut-shaped torus of dust encircling the black hole, rather than from materials being ejected outward.
Dr. Girard remarked, “This is the first instance where Webb’s high-contrast mode has been employed to observe an extragalactic source.” He expressed hope that their findings will inspire fellow astronomers to leverage aperture masking interferometry to study faint but relatively small, dusty structures surrounding bright objects.
The supermassive black hole remains active, continuously consuming surrounding matter. Gas and dust conglomerate in a torus around the black hole, forming a rotating accretion disk as material spirals inward. This disk generates heat through friction, releasing light across diverse wavelengths, including infrared.
New data from Webb indicate that most of the infrared emissions near the center of the Circus Galaxy stem from the innermost region of this dusty torus, challenging previous assumptions that outflow dominated emissions.
This pioneering technique lays the groundwork for more profound investigations of black holes in other galaxies. By applying Webb’s high-contrast imaging to subsequent targets, researchers aim to establish a broader catalog of emission patterns, which could ascertain whether the behavior observed in the Circus Galaxy is typical among active galactic nuclei or a distinct case.
Their discoveries not only present a clearer perspective on the feeding mechanisms of black holes but also underscore the escalating power of interferometry in space-based astronomy.
More observations are forthcoming, as Webb continues to redefine what can be observed from the most concealed regions of the universe.
Dr. Enrique López Rodríguez, an astronomer at the University of South Carolina, noted, “We will likely require a statistical sample of a dozen or two dozen black holes to comprehend how the mass of the accretion disk and its outflow correlate with the black hole’s power.”
For further details, refer to the results published in today’s edition of Nature Communications.
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E. Lopez Rodriguez et al. 2026. JWST interferometry imaging reveals a dusty torus obscuring the Circinus Galaxy’s supermassive black hole. Nat Commun 17, 42; doi: 10.1038/s41467-025-66010-5
Using high-resolution images, NIRCam, a near-infrared camera aboard the NASA/ESA/CSA James Webb Space Telescope, has led astronomers to discover COSMOS-74706, one of the earliest known barred spiral galaxies. This discovery is pivotal in shaping our understanding of cosmic evolution.
COSMOS-74706: Unsharp mask overlaid on F200W, F277W, and F356W filter configurations. The white lines represent logarithmic spirals along the galaxy’s arm structure while the lines indicate the north-south bar structure. Image credit: Daniel Ivanov.
The barred spiral galaxy COSMOS-74706 existed approximately 11.5 billion years ago.
“This galaxy developed its bar just two billion years after the universe’s inception,” stated Daniel Ivanov, a graduate student at the University of Pittsburgh.
“Stellar bars are linear features found at the centers of galaxies, confirming their namesakes.”
COSMOS-74706’s bar comprises a dense collection of stars and gas, appearing as a bright line bisecting the galaxy when viewed perpendicularly to its plane.
Stellar bars significantly influence a galaxy’s evolution, funneling gas from the outskirts into the center, which feeds the supermassive black hole and can inhibit star formation within the galactic disk.
While previous reports identified barred spiral galaxies, their analyses were inconclusive due to the less reliable optical redshift methods compared to the spectroscopy used for COSMOS-74706 verification.
In some instances, a galaxy’s light was distorted by a massive object, leading to a phenomenon known as gravitational lensing.
“Essentially, COSMOS-74706 is the most redshifted spectroscopically confirmed lensless barred spiral galaxy,” Ivanov noted.
“We were not surprised to find barred spiral galaxies so early in the universe’s timeline.”
“In fact, some simulations suggest the bar formed at redshift 5, or roughly 12.5 billion years ago.”
“However, I believe we shouldn’t expect to find many of these galaxies just yet.”
This discovery helps refine the timeline for bar formation, making it a significant finding.
Revolutionary findings from the Atacama Large Millimeter/Submillimeter Array (ALMA) have uncovered scorching intracluster gas in the young galaxy cluster SPT2349-56, just 1.4 billion years post-Big Bang. This groundbreaking discovery challenges existing models of galaxy cluster evolution.
Artist’s impression of the forming galaxy cluster SPT2349-56, showcasing radio jets from active galaxies within a hot intracluster atmosphere. Image credit: Lingxiao Yuan.
The SPT2349-56 galaxy cluster is located approximately 12.4 billion light-years away, providing a glimpse into the universe when it was only 1.4 billion years old, or about ten percent of its current age.
This compact protocluster hosts multiple actively growing supermassive black holes and over 30 starburst galaxies.
These starburst galaxies are forming stars at a staggering rate—1,000 times faster than the Milky Way—and are densely packed within a space only three times larger than the Milky Way itself.
“We were not prepared to discover such a hot stellar atmosphere at this early stage in the universe’s history,” remarked Dazhi Zhou, a Ph.D. candidate at the University of British Columbia.
Astronomers utilized a unique observation methodology known as thermal observation, particularly employing the Sunyaev Zeldovich (tSZ) Effect.
This approach identifies faint shadows cast by hot electrons in galaxy clusters against the faint cosmic microwave background, rather than the light emitted directly by the gas.
Previously, astronomers believed that galaxy clusters lacked the maturity required for their gas to heat up and evolve during the early cosmic era.
The discovery of hot cluster atmospheres had never been recorded within the initial 3 billion years following the Big Bang.
“SPT2349-56 reshapes our understanding,” stated Professor Scott Chapman, a researcher at Dalhousie University and the University of British Columbia.
“Our findings indicate that the cluster’s atmosphere is superheating remarkably early—just 1.4 billion years after the Big Bang—during a period when we anticipated the gas to be cooler and accumulating slowly.”
“This raises the possibility that the formation of large clusters could heat their gas much more efficiently and intensely than our current models suggest.”
The intense explosion from SPT2349-56’s supermassive black hole, identified as a bright radio galaxy, may be an efficient mechanism for superheating the surrounding gas, according to the study.
This discovery implies that energetic phenomena, such as outbursts from supermassive black holes or violent starbursts, might have played significant roles in rapidly heating the gas in early galaxy clusters within the first billion years of the universe.
This superheating may be crucial for transforming these young, cold galaxy clusters into the vast, hot galaxy clusters observed today.
Current models may require reassessment regarding our understanding of how galaxies and their environments evolve.
This finding marks the earliest direct detection of hot cluster gases, pushing the boundaries of astronomical research into these environments.
The identification of a significant reservoir of hot plasma at such an early cosmic epoch forces scientists to reconsider the sequence and pace of galaxy cluster evolution.
It also generates new inquiries about the interplay between supermassive black holes and galaxy formation in shaping the universe.
“SPT2349-56 serves as an intriguing laboratory,” Zhou commented.
“We are witnessing intense star formation, energetic supermassive black holes, and this superheated atmosphere all confined within young, dense star clusters.”
“There remains a considerable observational gap between this chaotic initial phase and the more tranquil clusters observed later in cosmic history.”
“Mapping the evolution of the universe’s atmosphere over time will be a compelling avenue for future exploration.”
For further reading, see the published results in the journal Nature dated January 5, 2026.
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Zhou D. et al. Detection of hot intracluster gas at redshift 4.3 via Sunyaev Zeldovich. Nature, published online January 5, 2026. doi: 10.1038/s41586-025-09901-3
Stunning image from the James Webb Space Telescope revealing an Einstein Ring formed by two distant galaxies.
Image Credit: ESA/Webb, NASA & CSA, G. Mahler
As we approach 2026, we’re stepping into a year rich with galactic exploration.
We’ll witness the beginning of the Vera C. Rubin Observatory’s deep dive into the space-time legacy, alongside a potential launch of NASA’s Nancy Grace Roman Space Telescope.
Both observatories are pivotal for galaxy observation, aimed at cataloging and unraveling the complexities of galaxy structures and behavior. Expect significant updates on galactic findings in the upcoming months!
As excitement grows for the wealth of information we’ll receive on galaxies, it’s notable that my early interest skewed towards active galactic nuclei (AGNs)—galaxies boasting supermassive black holes that release immense energy as they consume matter near the event horizon. Admittedly, I was drawn to AGNs primarily for their black hole attributes.
During my PhD journey, my curriculum mandated multiple courses on galaxies, which initially overwhelmed me. Galaxies are classified by shape, each category diving into further sub-categories, revealing a perplexing web of classifications. This complexity often felt devoid of mathematical logic, highlighting a possible divide between theorists and experimentalists.
If only I could rewind time and tell my younger self that the challenges in galaxy classification were what deserved my attention.
One of the core challenges in this research realm is that galaxies only manifest as 2D images in the night sky; we lack the ability to perceive them in three dimensions or to observe their rotation due to their enormity. Thus, we rely on these frozen snapshots in time, interpreting their classification based on scientific judgment and taste.
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The shape of a galaxy offers fascinating insights into its evolutionary history – elliptical galaxies typically harbor older stars. “
Historically, Edwin Hubble devised a classification system for galaxies that remains influential today. He defined three fundamental shapes: elliptical, spiral, and irregular. Notably, lenticular galaxies, while appearing spiral, lack an actual spiral structure.
Gérard de Vaucouleurs expanded this classification by incorporating subcategories to identify patterns within galaxy shapes. However, the efficacy of these classifications hinges on the quality of the underlying dataset. A century ago, during Hubble’s time, the datasets were rudimentary, lacking knowledge of dark matter—a critical component now understood to inhabit galaxies.
Galaxy shapes serve as indicators of evolutionary history; for instance, elliptical galaxies often house older stars and lie closer in proximity to galaxy clusters. Furthermore, the assembly and evolution history of these galaxies relates intricately to the configuration of their surrounding dark matter halos.
Additionally, galaxy shapes can unveil secrets about dark energy, which accelerates the universe’s expansion. The Roman Space Telescope aims to deepen our understanding in this regard.
The Vera Rubin Observatory will extend its observational prowess, particularly focusing on dwarf spheroidal galaxies—dim, circular galaxies devoid of substantial star mass. These dwarf galaxies frequently accompany larger counterparts, helping to illuminate the evolutionary structure of the universe.
Excitingly, the scientific teams behind the Rubin and Roman telescopes are collaboratively strategizing on how best to utilize the forthcoming data. As we honor the legacies of Vera C. Rubin and Nancy Grace Roman, 2026 heralds a new generation dedicated to exploring galaxies in extraordinary detail.
What I’m currently reading: Twilight novel series.
What I see: Correct, the Twilight movie series.
What I’m working on: I’m diligently finishing the draft of my third book: Cosmos is a Black Aesthetic.
Chanda Prescod-Weinstein is an associate professor of physics and astronomy at the University of New Hampshire. She is the author of Turbulent Universe and upcoming works The Ends of Space and Time: Particles, Poetry, and the Boogie of Cosmic Dreams.
Astronomers have made significant strides in understanding how the most prevalent type of planet in our galaxy, known as super-Earths, forms. A new study highlights that these planets begin life as “bloated” infants, rapidly shedding much of their thick atmospheres.
This groundbreaking research, published in Nature, observed four youthful exoplanets within the V1298 Tau system. Remarkably, their host star is merely 20 million years old—akin to a 5-month-old baby in cosmic terms.
Currently, these planets boast radii 5 to 10 times larger than Earth, but their masses only range from 5 to 15 times that of Earth, resulting in a density similar to that of Styrofoam.
This “bloated” state occurs as the young star’s heat and light cause the planet’s atmosphere to expand dramatically. Consequently, these planets are losing significant amounts of gas into space, eventually leading to a reduction in size to somewhere between that of Earth and Neptune.
Super-Earths and sub-Neptunes, as they are often called, have been detected around numerous other stars, establishing them as the most ubiquitous type of planet known today. However, they remain absent in our solar system.
Lacking nearby examples to study these intermediate worlds in detail has made them a “missing link” in our understanding of planetary formation and evolution.
“V1298 Tau is a crucial link between star- and planet-forming nebulae visible across the sky and the mature planetary systems we are currently discovering in abundance,” stated Dr. Eric Pettigura from the University of California, who was involved in the research.
Astronomers had speculated about this growth pattern for infant planets based on their sizes, but this marks the first instance of direct observation of the phenomenon.
“These planets have already experienced rapid changes, significantly losing their original atmospheres and cooling more swiftly than traditional models predict,” noted James Owen, a co-author from Imperial College London.
“Their evolution is ongoing. Over the next few billion years, they will continue to shed atmospheres and reduce in size, eventually forming a compact system of super-Earths and sub-Neptunes widely observed throughout the galaxy.”
A Stroke of Luck
As with many astronomical breakthroughs, this discovery resulted from both serendipity and diligent effort.
The researchers analyzed the planets by monitoring their transits—temporary declines in a star’s brightness when a planet moves in front of it. The depth of this dip indicates the planet’s radius, while the timing offers insights into its orbit.
Planets block only a small fraction of a star’s light, typically around 1%, making their detection a challenging endeavor. – Credit: ESA
While scientists were aware that these planets were on the larger side, part of the transits for the two outer planets was missed, leaving uncertainties about their orbits.
“We used computer models and educated guesses to narrow down hundreds of possibilities,” Pettigura explained.
Fortunately, their predictions proved accurate. Upon searching for the planets again using ground-based telescopes, they successfully located them on the first attempt.
“I was thrilled,” Pettigura remarked. “Given the uncertain timing, I anticipated needing at least six attempts. It felt like hitting a hole-in-one in golf.”
Once the orbits were confirmed, the team conducted a detailed analysis to determine the planets’ masses.
As planets move past each other, their gravitational forces subtly alter their orbits, affecting transit timings. The greater a planet’s mass, the stronger its gravitational pull. This enabled the researchers to differentiate timing variations to ascertain the planets’ masses.
“The unexpectedly large radii of these young planets led to the hypothesis of very low densities, which had not been previously measured,” stated Trevor David of the Flatiron Institute, who was a co-author on the first discovery of this system.
“By measuring the masses of these planets for the first time, we have provided crucial observational evidence that validates their ‘bulgy’ characteristics, establishing a significant benchmark for planetary evolution theory.”
Astronomers unveiled a remarkable giant galaxy cluster known as RM J130558.9+263048.4 on December 31, 2020. Due to its bubble-like appearance and superheated gas, they aptly named it the Champagne Cluster. The stunning new composite image of this galaxy cluster features X-ray data from NASA’s Chandra X-ray Observatory combined with optical information from the Legacy Survey.
The Champagne Cluster appears as a luminous array of galaxies amidst a vibrant neon purple cloud. The cluster reveals over 100 galaxies split into two groups, with notable variations among them. Foreground stars display diffraction spikes surrounded by a subtle haze. Many small galaxies showcase blue, orange, or red tones and exhibit varied shapes. This indicates a multifaceted nature, while the central purple gas cloud emitted by Chandra signals a high-temperature region, indicative of two colliding clusters. Image credit: NASA / CXC / UCDavis / Bouhrik others. / Legacy Survey / DECaLS / BASS / MzLS / SAO / P. Edmonds / L. Frattare.
Recent research led by astronomer Faik Bourik from the University of California, Davis, utilized instruments from NASA’s Chandra X-ray Observatory and ESA’s XMM Newton Observatory to investigate the Champagne Cluster.
The team also analyzed data from the DEIMOS multi-object spectrometer located at the W. M. Keck Observatory.
“Our new composite image indicates that the Champagne Galaxy Cluster consists of two galaxy clusters merging to form a larger cluster,” the astronomers stated.
“In typical observations, multimillion-degree gas is roughly circular, but in the Champagne Cluster, it spans from top to bottom, highlighting the collision of two clusters.”
“Distinct clusters of individual galaxies are prominently visible above and below the center,” they added.
“Remarkably, the mass of this hot gas exceeds that of all 100 or more individual galaxies within the newly formed cluster.”
“This cluster is also abundant in invisible dark matter, a mysterious substance that pervades the universe.”
The Champagne Cluster is part of a rare category of merging galaxy clusters, akin to the well-known Bullet Cluster, where the hot gas from each cluster collides, slows, and creates a clear separation from the heaviest galaxies.
By comparing this data with computer simulations, researchers propose two potential histories for the Champagne Cluster.
One theory suggests that the two star clusters collided over 2 billion years ago, followed by an outward movement due to gravity, leading them to a subsequent collision.
Alternatively, another link posits a single collision about 400 million years ago, after which the clusters have begun moving apart.
“Further studies on the Champagne Cluster could illuminate how dark matter reacts during high-velocity collisions,” the scientists concluded.
For more insights, refer to their published paper in July 2025, featured in the Astrophysical Journal.
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Faik Bourik others. 2025. New dissociated galaxy cluster merger: discovery and multiwavelength analysis of the Champagne Cluster. APJ 988, 166;doi: 10.3847/1538-4357/ade67c
Explore the stunning new image captured by the NASA/ESA Hubble Space Telescope, showcasing a section of the N159 star-forming complex located in the Large Magellanic Cloud, a dwarf galaxy approximately 160,000 light-years away from Earth.
This breathtaking Hubble image portrays N159, a vibrant star-forming complex in the Large Magellanic Cloud. Image credit: NASA / ESA / Hubble / R. Indebetouw.
N159 stands as one of the most colossal molecular clouds within the Large Magellanic Cloud, making it a noteworthy member of our cosmic neighborhood – the Milky Way galaxy.
Positioned at the southwestern edge of the renowned Tarantula Nebula, N159 spans over 150 light-years across.
The newly released Hubble image captures only a fraction of the expansive N159 complex.
“A dense cloud of cold hydrogen gas predominates the scene, creating a complex array of ridges, cavities, and luminescent filaments,” stated Hubble astronomers.
“Within these thick clouds, newly formed stars begin to blaze, their intense radiation illuminating the surrounding hydrogen in a striking crimson hue.”
“The brightest zones signify the presence of hot, massive young stars whose vigorous stellar winds and energetic light reshape the surrounding space.”
“These powerful forces carve out bubble-like formations and hollow cavities within the gas, clearly illustrating the effects of stellar feedback.”
“Dark clouds in the foreground glow thanks to a new star shining from behind.”
“The illuminated clouds and intricate bubbles reveal the dynamic interplay between star formation and the primordial matter from which stars arise, capturing the perpetual cycles of creation and transformation within this neighboring galaxy.”
Astronomers utilizing the NASA/ESA Hubble Space Telescope have captured a remarkable image of the barred spiral galaxy NGC 1511.
This Hubble image features the barred spiral galaxy NGC 1511, located approximately 50 million light-years away in the constellation Hydra. Image credit: NASA / ESA / Hubble / D. Tilker.
NGC1511 resides in the constellation Hydra, about 50 million light-years from our planet.
This spiral galaxy was discovered by British astronomer John Herschel on November 2, 1834.
NGC 1511, also known as ESO 55-4, IRAS 03594-6746, or LEDA 14236, is a principal member of a small galaxy group known as the NGC 1511 Group.
“Like many galaxies, NGC 1511 doesn’t navigate through space alone,” stated Hubble astronomers.
“Instead, it exists alongside a pair of smaller galactic companions known as NGC 1511A and NGC 1511B. Both companions lie outside the scope of this Hubble image.”
“NGC 1511B is the nearest neighbor to NGC 1511, and the two galaxies have likely collided in the past,” researchers remarked.
“A thin filament of hydrogen gas links them, and NGC 1511B is elongated and warped due to this collision.”
Astronomers have also discovered signs indicating that NGC 1511 once had another small companion galaxy that has since been completely annihilated.
“These disruptions have impacted NGC 1511 as well,” the researchers added.
“This galaxy has undergone explosive star formation, and its disk displays unusual loops and plumes that may suggest previous interactions with nearby galaxies.”
“We are utilizing Hubble’s precise observations of NGC 1511 to analyze star clusters nestled within its dusty gas, aiming to comprehend how material circulates from interstellar clouds to stars and back.”
A cosmic network is disrupting a galaxy’s star-forming abilities. Galaxies require gas to generate stars, and a distant dwarf galaxy, nearly 100 million light-years away, is being deprived of this essential material by an expansive web of cosmic constituents.
While one half of the galaxy known as AGC 727130 seems relatively normal, its opposite side shows gas stretching well beyond its perimeter, being torn apart by unseen forces. Researchers from Columbia University in New York identified this collapsing galaxy utilizing the Very Large Array, a radio observatory situated in New Mexico Nicholas Luber.
Even though AGC 727130 is in proximity to two other dwarf galaxies, the researchers concluded that it isn’t close enough to engage with them in a way that would create turbulent gas. Their findings imply that the gas is expelled through a mechanism known as ram pressure stripping. This occurs when a galaxy traverses an intragalactic cloud—in this case, part of the cosmic web—leaving behind its gas. Without this gas, galaxies become “quenched” and are unable to create new stars.
The filamentous structures in the cosmic web are so slender that it would likely take more than one filament to strip gas from a galaxy, yet AGC 727130 resides at the junction of multiple filaments. “The concept that a cosmic web could extract gas from galaxies through collisional pressure is not surprising and likely happens frequently, but it’s challenging to confirm,” states Luber. “We were fortunate to observe this phenomenon.”
Identifying such galaxies poses a challenge because the gas removal is a gradual process, and galaxies that have already lost their gas tend to be exceedingly faint. “What’s intriguing about this outcome is that low-mass extinguished dwarf galaxies are exceptionally rare; only a few, less than 0.06 percent, are believed to exist without a substantial host galaxy,” comments Julia Blue Bird, a radio astronomer based in New Mexico.
Even among that limited number of extinguished dwarf galaxies, only a scant few have had their gas stripped by the cosmic web rather than through interactions with other galaxies. “This might be… the first definitive case of such an occurrence,” remarks Jacqueline Van Gorcom from Columbia University. Several large radio telescopes are poised to unveil new gas maps across extensive regions of the universe, which could provide additional insights regarding these galaxies.
This discovery is crucial in addressing a cosmological dilemma known as the missing satellite problem. Current cosmological models suggest there should be significantly more dwarf galaxies orbiting larger ones than we currently observe. “We struggle to find many quenched dwarfs; is it because they’re hard to detect, or are they simply not present? This suggests that quenching may also be occurring far from larger galaxies,” states team member Sabrina Stierwalt from Occidental College in California. Uncovering additional galaxies quenched by the cosmic web could help reconcile discrepancies between model predictions and actual observations.
Remarkably, Segue 1, an extremely faint dwarf galaxy, is positioned at the center of this image.
CDS, Strasbourg, France/CDS/Aladdin
Astoundingly, a supermassive black hole appears to reside at the heart of a nearby galaxy previously believed to be dominated by dark matter. Segue 1 is scarcely a galaxy, hosting merely around 1,000 stars compared to the Milky Way’s vast hundreds of billions. Yet, it seemingly contains a black hole with a mass approximately 10 times greater than the combined total of all its stars.
Segue 1 and similar dwarf galaxies lack sufficient stars to generate the gravitational force needed to hold them intact. To address this anomaly, physicists have long speculated that dark matter—a mysterious, invisible substance—fills the universe, contributing additional gravity.
Recently, Nathaniel Lujan and colleagues at the University of Texas at San Antonio began exploring computer models of Segue 1. They anticipated that the model yielding the best fit would be one characterized by dark matter. “After running hundreds of thousands of models, we were unable to find a viable solution,” Lujan remarks. “Eventually, we decided to experiment with the black hole mass, and that dramatically changed the results.”
The model that closely aligned with the observations of Segue 1 featured a black hole with a mass around 450,000 times that of the Sun. This discovery was particularly unexpected—not only due to the galaxy’s scarcity of stars but also considering its age. With so few stars, Segue 1 is estimated to have formed merely 400 million years following the universe’s initial star formation. Time constraints make it challenging for such a massive black hole to develop, especially since the much larger Milky Way likely consumed most of the gas that could have nourished Segue 1 shortly after its inception.
“This suggests there may be far more supermassive black holes than previously assumed,” Lujan states. If true, this could clarify some of the gravitational effects formerly attributed to dark matter, though it remains uncertain whether Segue 1 is typical of all dwarf galaxies. The quest for additional supermassive black holes continues.
Gamma rays are detected in unusually high amounts at the center of the Milky Way galaxy
The center of our galaxy is exhibiting unusual behavior, potentially linked to dark matter. In 2009, observations from the Fermi Gamma-ray Space Telescope uncovered unexpectedly high levels of gamma ray emissions from the Milky Way’s center, a phenomenon termed galactic central gamma-ray excess (GCE). Simulations suggest these gamma rays could arise from the annihilation of dark matter particles.
The discussion surrounding the origins of GCE has intensified since its initial discovery, leading to two main theories. The first posits that it may stem from a previously unobserved population of pulsars, rapidly spinning neutron stars that emit considerable radiation.
Alternatively, it could be linked to weakly interacting massive particles (WIMPs), long considered primary candidates for dark matter. These particles seldom interact with normal matter, but a collision between two can lead to annihilation and consequently, a burst of gamma rays.
However, the dark matter explanation has lost traction recently, especially after searches for WIMPs yielded no results. “The dark matter interpretation demands greater proof due to insufficient direct evidence of its existence despite thorough investigations,” notes Jeff Grube from King’s College London.
Another factor contributing to this skepticism is that dark matter in galaxies is expected to be evenly distributed, while GCEs display a flattened distribution. Yet, new simulations by Joseph Silk and his colleagues at Johns Hopkins University in Maryland indicate that this discrepancy may not be significant.
These new simulations carefully considered the Milky Way’s history in relation to GCEs. “We know from history that our galaxy merged with smaller galaxies billions of years ago, which contributed to the formation of dark matter,” noted Silk. “No one would have anticipated that the galaxy’s center would exhibit spherical symmetry due to this history.”
The results confirmed this notion, resulting in a distorted dark matter distribution aligned with the shape of GCE, reviving the dark matter theory. However, the mystery remains unresolved, as pulsars continue to be a viable explanation. “At best, the situation is still ambiguous,” added Grube.
The current gamma-ray observatories do not possess the capability to distinguish between these two theories; however, the Cherenkov Telescope Array observatories, under construction in the Canary Islands and Chile and expected to begin operations in 2026, could provide clarity.
“In many ways, there’s a 50 percent chance that we may have discovered significant dark matter, but we require new telescopes to confirm this,” stated Silk. If GCE is indeed the result of dark matter, it could offer the best insight yet into this enigmatic substance that underpins the universe.
NGC 7496 is a barred spiral galaxy situated roughly 24 million light-years away in the Taurus constellation.
This Hubble image captures barred spiral galaxy NGC 7496 in the constellation Hyuri, located approximately 24 million light-years away. Image credits: NASA / ESA / Hubble / R. Chandar / J. Lee / PHANGS-HST team.
NGC 7496 was discovered by British astronomer John Herschel on September 5, 1834.
The galaxy is also identified as ESO 291-1, LEDA 70588, and IRAS 23069-4341, and spans approximately 70,000 light-years in diameter.
NGC 7496 belongs to the NGC 7582 group, which comprises about 10 large galaxies.
This galaxy is classified as a Type II Seyfert galaxy, notable for a high star formation rate.
At its center lies an active galactic nucleus containing a supermassive black hole primarily consuming gas.
According to Hubble astronomers, “Hubble observed NGC 7496 for the first time as part of the Physics at High Angular Resolution of the Nearby GalaxieS (PHANGS) program.”
“Alongside the NASA/ESA Hubble Space Telescope, this initiative utilizes the capabilities of various powerful observatories, including the Atacama Large Millimeter/Submillimeter Array, ESO’s Very Large Telescope, and the NASA/ESA/CSA James Webb Space Telescope.”
“NGC 7496 was the inaugural galaxy in the PHANGS sample to be observed by Webb.”
“Each of these observatories offers a unique perspective on this extensively studied galaxy.”
“With its exceptional ultraviolet capabilities and high resolution, Hubble’s observations reveal young star clusters emitting high-energy radiation.”
“Hubble’s insights into NGC 7496 will assist in determining the ages and masses of these young stars, as well as the degree to which their light is obscured by dust.”
“Previous Hubble images of NGC 7496 were released in 2022,” they noted.
“Today’s image incorporates fresh data showcasing the galaxy’s star clusters amid glowing red clouds of hydrogen gas.”
The Hubble team has unveiled stunning images captured by the NASA/ESA Hubble Space Telescope, showcasing half of the Barred Spiral Galaxy NGC 6000.
This Hubble image reveals NGC 6000, a barred spiral galaxy located around 102 million light years away in the constellation Scorpius. Image credits: NASA/ESA/Hubble/A. Filippenko/MHözsaraç.
NGC 6000 is approximately 102 million light years distant from the constellation Scorpio.
Also known as ESO 450-20, IRAS 15467-2914, or LEDA 56145, this spiral galaxy spans nearly 67,000 light years.
It was first observed by British astronomer John Herschel on May 8, 1834.
Classified as a Seyfert II Galaxy, NGC 6000 is the brightest galaxy in the constellation of Scorpio.
“The NGC 6000 showcases a luminous yellow center surrounded by a sparkling blue region,” stated Hubble astronomers.
“These colors signify variations in the average age, mass, and temperature of the stars within the galaxy.”
“In the galaxy’s core, the stars tend to be older and smaller.”
“Interestingly, fewer giant stars are cooler compared to their larger counterparts; cooler stars appear red, while hotter stars take on a blue hue.”
“Along the spiral arm of NGC 6000, the Brilliant Star cluster is home to a young, massive star that distinctly looks blue.”
Hubble’s instruments gathered data from new images of NGC 6000 while investigating the site of a recent supernova explosion in a nearby galaxy.
“NGC 6000 has witnessed two supernovas: SN 2007CH in 2007 and SN 2010 in 2010,” noted the astronomer.
“We were able to detect the faint glow of the supernova several years post the initial explosion.”
“These observations assist in determining the star mass of supernova progenitor cells and whether they possess stellar companions.”
“If you zoom in on the right side of the galaxy disc in this image, you may notice other yellow and blue formations, which are four thin lines.”
“These represent asteroids from our solar system transit across Hubble’s field of vision while observing NGC 6000.”
“The four streaks arise from varying exposures captured sequentially with brief pauses in between, which we merged to create this final image.”
“The colors appear in this manner: each exposure captures specific red and blue wavelengths, as we used filters to isolate light at very particular wavelengths.”
“Collecting these individual exposures is vital for studying and comparing star colors, though it makes inter-agency intrusions quite apparent.”
A potentially newly discovered galaxy from the James Webb Space Telescope
NASA, ESA, CSA, CEERS, G. Gandolfi
Astronomers might have found galaxies that formed very early in the universe, approximately 200 million years apart from their closest counterparts, but they caution that alternative explanations could exist.
Giovanni Gandolfi from the University of Padua, along with his team, examined data from the James Webb Space Telescope (JWST) in search of distant cosmic formations from the universe’s 13.8 billion-year timeline.
The greater the distance of a galaxy from Earth, the longer it takes for its light to reach us, and it will be redshifted due to the universe’s expansion.
Until now, the earliest confirmed galaxy identified by JWST, named Mom-Z14, has a redshift of 14.4, indicating that it has been moving toward us since the universe was just 280 million years old. Gandolfi and his colleagues, however, have reported finding 32 intriguing objects with redshifts, placing them at a time when the universe was merely 90 million years old. They have named this discovery Capotauro after the Italian mountains.
“Capotauro could represent the most distant galaxy we’ve encountered,” states Gandolfi.
The team derived their conclusion from observing minor fluctuations in a deep JWST survey of the sky that resemble a distant galaxy. By utilizing various filters on the telescope, they were able to determine the redshift of the light emitted by the galaxy, arriving at a count of 32.
If validated, this object might represent a very young galaxy in formation, or potentially a primitive black hole enveloped by a dense atmosphere.
Nonetheless, this presumed galaxy appears uncommonly bright, akin to those observed in later redshift instances like Mom-Z14, suggesting it has a mass approximating a billion times that of the Sun.
For a galaxy to reach such mass, its efficiency in converting gas into stars must be near 100%, according to Nicha Reese Chawarit from the National Institute of Astronomy in Thailand, indicating that the stars cannot explode. Modelling, however, suggests that achieving 10-20% or even lower is plausible. “I believe there’s something amiss,” she remarks.
If this is not a galaxy, Gandolfi and his team propose that the object could alternatively be a brown dwarf (a star that didn’t ignite). These alternative theories are also compelling, Gandolfi notes, particularly if it is a cold brown dwarf or distant planet, possibly 6000 light years away and at room temperature.
“It could represent one of the first substellar objects ever formed in our galaxy,” adds Gandolfi.
To confirm this, the team requires additional observing time on the JWST to precisely analyze the light from the object. Leethochawalit supports the notion that it may not be a galaxy but also states that such follow-up research could still be worthwhile.
“If it turns out to be a galaxy with a redshift of 32, then a lot of our previous assumptions might be entirely wrong,” she states.
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Using the Widefield Camera 3 (WFC3) mounted on the NASA/ESA Hubble Space Telescope, astronomers have captured a breathtaking new image of the Spiral Galaxy NGC 7456.
This Hubble image showcases NGC 7456, a spiral galaxy located 51 million light-years away in the constellation of Grus. Image credits: NASA/ESA/Hubble/D. Thilker.
NGC 7456 was discovered by British astronomer John Herschel on September 4, 1834.
This galaxy is approximately 51 million light-years from Earth, in the constellation Grus.
Also referred to as ESO 346-26, IRAS 22594-3950, or LEDA 70304, it spans a diameter of 117,100 light-years.
The NGC 7456 belongs to the LDC 1547 Galaxy Group, which includes 16 large galaxies.
“In Hubble’s image, one can observe the intricate, swirling arms of this galaxy in exquisite detail, complemented by a dark, diffuse mass of dust,” remarked an astronomer from Webb.
“The bright pink regions signify gas-rich areas where new stars are emerging, illuminating the surrounding clouds, as this gas emits transmitted red light.”
“The Hubble program has been gathering these data to study stellar activity, tracking new star-forming clouds, hydrogen, star clusters, and gaining insights into galaxy evolution over time,” they further explained.
“With its capability to capture visible ultraviolet and some infrared light, Hubble isn’t the only observatory focused on NGC 7456.”
“ESA’s XMM-Newton satellite has imaged X-rays from galaxies multiple times and discovered what is known as a hyper-luminous X-ray source.”
“These compact objects emit significantly more powerful X-rays than one would expect for their size.”
“We are still investigating what drives these extreme objects. NGC 7456 contributes several examples to this research.”
“Additionally, the area surrounding the galaxy’s supermassive black hole is incredibly bright and energetic, making NGC 7456 an active galaxy.”
“Whether viewed in visible light or X-rays, there’s always something intriguing about this galaxy, whether focusing on its core or its outer regions.”
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Q&A Section: This month’s questions include: Can animals engage with video games? Why do my eyelids twitch unexpectedly? What does “clubbed finger” refer to? Are there particles related to time? Will relocating near a golf course improve my health? Is breakfast cereal genuinely nutritious? Should I give up on high-intensity interval training? Can clothing chemicals disrupt my hormones? What are the most dangerous fish? Can we detect animals in infrared? And much more…
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The glow within the cluster is the soft luminosity of stars that have been stripped from their galaxy amidst the layers of galaxy clusters.
Abell 3667 is depicted in this Decam image. Image credits: CTIO/NOIRLAB/NSF/AURA/ANTHONY ENGLERT, Brown University/TA Rector, Noirlab/M. Zamani & D of University of Alaska Anchorage & NSF. De Martin, NSF’s Noirlab.
Galaxy clusters comprise thousands of galaxies, varying widely in age, shape, and size.
Typically, they have a mass about 10 billion times that of the Sun.
Historically, galactic clusters were regarded as the largest structures in the universe, spanning hundreds of millions of light-years and including numerous galactic clusters and groups, until superclusters were discovered in the 1980s.
Nonetheless, galaxy clusters still hold the title of the largest gravitationally bound structure in the universe.
“The study of galaxy clusters not only informs us about the formation of the universe, but it also places constraints on the characteristics of dark matter,” stated Brown University astronomer Anthony Englat and his team.
One significant clue astronomers seek to grasp the history of galactic clusters is the light within the cluster. This faint glow is emitted by stars that have been stripped from their original galaxy due to the immense gravitational forces of the forming galaxy cluster.
These stars provide evidence of past galactic interactions, although most current telescopes and cameras face challenges in detecting them.
The subtle intra-cluster light from the galaxy cluster Abel 3667 shines vividly in new images created from a total of 28 hours of observation at 570 megapixels using the Dark Energy Camera (Decam) at NSF’s M. Blanco 4-M Telescope, a program of NSF’s Noirlab at Cerro Tololo Inter-American Observatory.
“Abell 3667 is located over 700 million light-years away from us,” the astronomer mentioned.
“Most of the faint light sources in this image are distant galaxies, not foreground stars from our own Milky Way.”
“In Abell 3667, two small galaxy clusters are currently merging, as evidenced by the luminous bridge (yellow) of stars extending toward the center of this image.”
“This bridge is formed from material stripped off from the merging galaxies, forming one massive conglomerate known as the brightest cluster galaxy.”
“Not only does this sparkling sky encompass distant galaxies, but it also highlights faint foreground features due to the prolonged exposure.”
“The Milky Way’s hair follicles, or integrated flux nebula, consist of faint clouds of interstellar dust that appear as soft bluish chains crossing the image.”
“These structures are patches of dust that are illuminated by the light of the stars within our own galaxy.”
“They present as diffuse, filamentous formations that can span extensive areas of the sky.”
Survey results will be published in the Astrophysics Journal Letter.
____
Anthony M. Engrat et al. 2025. Announcing optical bridges in Abel 3667 in-cluster light: LSST precursor data. apjl 989, L2; doi: 10.3847/2041-8213/ade8f1
Utilizes data from 10m space-based wireless telescopes, including Radioastron. Astronomers have formed a network of 27 ground observation stations focused on OJ 287, a galaxy approximately 5 billion light-years distant from the Cancer constellations.
This image of OJ 287 reveals the sharply curved ribbon-like structure of the plasma jet emitted from its center. Image credits: Efthalia Traianou / Heidelberg University / IWR.
“Among the different types of active galactic nuclei, BL Lacertae (BL LAC) objects are notable for their rapid, large-amplitude variability and significant polarization across multiple wavelengths due to relativistic jets aligned closely with our line of sight.”
“A standout example of this subclass is OJ 287, characterized by a redshift of z = 0.306.”
Optical observations of OJ 287 have yielded an extensive light curve extending back to the 1880s, covering nearly 150 years.
This comprehensive dataset has uncovered periodic brightness variations, featuring marked 60-year cycles and notable high-brightness flares with recurrent double peaks occurring approximately every 12 years.
These periodic changes can be attributed to the presence of a binary supermassive black hole system, where secondary supermassive black holes follow eccentric precession paths around the more massive primary.
“The level of detail in the new images allows us to see the structure of the OJ 287 Galaxy like never before,” stated Dr. Traianou.
“The images penetrate deep into the galaxy’s center, revealing the jet’s sharply curved ribbon-like structure.”
“This also provides new insights into the composition and dynamics of plasma jets.”
“Certain regions exceed temperatures of 10 trillion Kelvin, indicating the release of extreme energy and movement near the black hole.”
Astronomers have also monitored the development, dispersion, and interactions of new shock waves along the jet, linking them to energies in the range of trillions of electron volts from rare gamma-ray observations made in 2017.
Using Radioastron and 27 terrestrial observatories, they captured images of OJ 287 across the radio spectrum.
The imaging relies on measurement techniques that utilize overlapping waves related to the properties of light waves.
“Interference measurement images bolster the hypothesis that a binary supermassive black hole resides within OJ 287,” the researchers commented.
“This also offers critical insights on how these black holes influence the shape and direction of the emitted plasma jet.”
“These unique characteristics position the galaxy as an ideal candidate for further studies on black hole mergers and associated gravitational waves.”
Survey results will be published in the journal Astronomy and Astrophysics.
____
E. Traianou et al. 2025. Reveal ribbon-like jets on OJ 287 via Radioastron. A&A 700, A16; doi: 10.1051/0004-6361/202554929
Samsung’s 7th generation flip phone sheds unnecessary features, boasting an expansive cover screen outside and a spacious folding display within, yet it doesn’t drastically change the existing formula.
The Galaxy Z Flip 7 will join the Book Style Z Fold 7 as Samsung’s two flagship folding devices in 2025. Similar to its predecessor, the Flip’s main allure is the ability to fold one of Samsung’s largest screens in half, making it ideal for pocket transport.
Prices starting at £1,049 (€1,199/$1,099/$1,799) align closely with the standard S25+ and Super Thin S25 Edge, yet offer slightly larger displays.
The Flip 7 operates just like a standard Android device, showcasing a flexible OLED screen and a generous 6.9-inch OLED main display. Photo: Samuel Gibbs/The Guardian
The Flip 7 is a touch taller than its predecessor, supporting a larger 6.9-inch inner screen. Additionally, it’s thinner by 1.2mm when folded. However, unlike the noticeable upgrades introduced with this year’s Fold 7, the changes may not be readily apparent.
The new outer cover display envelops the camera and LED flash at the top half of the Flip 7. It accommodates more text from notifications and widgets, significantly enhancing its appearance compared to prior iterations. Selecting an appealing wallpaper can make the dark metallic blue shade especially striking.
The hinge offers a reassuringly robust closure, though operating the Flip 7 with one hand can be quite challenging. Photo: Samuel Gibbs/The Guardian
The Flip 7 features a glass exterior, but the inner screen is shielded with a softer material that tends to collect fingerprints, exhibit glare, and show marks easily. It demands more care than a conventional flat phone. While the Flip is water-resistant, it’s not dust-proof, meaning the hinge should be safeguarded from tiny particles that could cause issues.
Specifications
Main screen: 6.9in FHD+ 120Hz AMOLED INFINITY FLEX Display (397PPI)
Water resistance: IP48 (up to 1.5 meters for 30 minutes)
Folded dimensions: 85.5 x 75.2 x 13.7mm
Expanded dimensions: 166.7 x 75.2 x 6.5mm
Weight: 188g
Performance and Battery Life
The Flip 7 charges fully in approximately 90 minutes, utilizing a power adapter of 25W or greater (not included) to reach 50% in 30 minutes. It also supports 15W wireless charging. Photo: Samuel Gibbs/The Guardian
Equipped with the Samsung Exynos 2500 chip, the Flip 7 features a high-end processor comparable to the Qualcomm Snapdragon 8 Elite found in other flagship devices from Samsung. Although it may not claim top performance accolades, the Flip 7 delivers a solid gaming experience, even if the phone heats up during extended sessions.
Battery performance falls slightly short compared to its predecessor, typically lasting around 36 hours between charges while utilizing a mix of 5G and Wi-Fi, and supports roughly 6 hours of screen time. This aligns closely with the base S25 model, implying that most users will likely need to charge the Flip 7 nightly, especially considering that prolonged 5G usage leads to greater battery depletion than on Qualcomm-powered Samsung devices.
One UI 8
In Flex Mode, tools such as the trackpad, scroll wheel, playback, and camera controls appear on the upper half of the screen. Photo: Samuel Gibbs/The Guardian
Alongside the Z Fold 7, the Flip 7 is among the initial Samsung devices running One UI 8 (based on Android 16) at launch. It’s a robust Android version offering extensive customization and stable performance.
The interface closely resembles that of the standard S25 series software, featuring multiple AI capabilities for tasks like lighting adjustments, image modification and generation, transcription, and translation. Additional Google AI services such as Gemini and Circle to Search are also present. The Now Bar is a fantastic feature that displays current activities such as sports scores, music playback, timers, alarms, and more.
The Flip 7 includes various tools specifically for foldable devices. A convenient “flex mode” allows content, websites, or applications to shift to the top half of the screen while folding the Flip into an L shape, placing controls on the lower half.
Currently playing music album art displays beautifully on the Flip 7’s external cover screen. Photo: Samuel Gibbs/The Guardian
Numerous tools for utilizing external screens are available. You can view notifications, reply to texts, manage music and system settings, access a range of widgets like audio recorders and calculators, and interact with Gemini without needing to open the phone. Some applications like Google Maps, Messages, WhatsApp, Netflix, and YouTube can also be accessed on the external screens. However, to run additional apps on the cover screen, downloading Samsung’s MultiStar plugin from the Galaxy Store is necessary—though this should ideally be a built-in feature.
Samsung pledges to provide Android and security updates until July 31, 2032.
Camera
Flex mode encourages creativity in photography, allowing for diverse angles and configurations. Photo: Samuel Gibbs/The Guardian
Cameras are a less impressive aspect of the Flip 7. It includes a 50-megapixel main camera, a 12MP ultra-wide lens, and a 10MP selfie camera on the inside.
While the selfie camera performs adequately, it’s not exceptional and struggles in low-light conditions for video calls. Instead, you might opt to use the main camera for selfies, utilizing the cover screen as a viewfinder for improved results.
The main camera shines outdoors, capturing detailed and vibrant colors, although indoor shots can suffer from murkiness and graininess due to lower lighting. The ultra-wide camera is decent for landscapes but struggles significantly in dim conditions.
The camera comes loaded with playful modes, including features for taking photos or videos in a traditional handicam style, which supports hands-free selfies.
Overall, the Flip 7 captures acceptable photos, but its camera quality falls short compared to traditional flagship devices.
Sustainability
Although there is a small gap near the hinge, the rest of the phone is sealed shut to prevent dust and fluff from entering. Photo: Samuel Gibbs/The Guardian
The battery is designed to retain at least 80% of its original capacity over a maximum of 2,000 complete charging cycles.
The device is generally repairable, with internal screen repairs estimated at around £294. Samsung also provides CARE+ insurance for accidental damage, reducing repair costs to £119.
The Flip 7 utilizes recycled materials such as aluminum, cobalt, copper, glass, gold, lithium, plastic, rare earth elements, and steel, accounting for 18.2% of the device’s weight. Samsung operates trade-in and recycling programs for older devices and documents the environmental impact of its phones in reports (PDFs).
Price
The Samsung Galaxy Z Flip 7 starts at £1,049 (€1,199/$1,099/$1,799).
For comparison, the Z Fold 7 is priced at £1,799, the S25 Edge at £1,099, the S25+ at £999, the Z Flip 7 FE at £849, the Motorola Razr 60 Ultra at £1,099, and the Xiaomi Mix Flip at £640.
Verdict
The Flip 7 stands as Samsung’s most appealing flip device, with the most notable enhancement being its larger outer screen.
Most other features mirror those of its predecessor. While the interior folding display is impressive, it is also delicate and requires careful handling. The side-mounted power button fingerprint scanner is functional yet somewhat inconveniently positioned. The camera quality is decent but does not compete with standard flagship models, and the battery life leaves much to be desired. However, the software is robust, with 7 years of updates promised. Overall, it feels somewhat repetitive.
The Flip 7 is an excellent choice for those wanting a substantial display in a compact form factor, yet it lacks the transformative redesign seen in its larger Fold 7 counterpart released this year.
Strengths: Bigger outer screen, ample inner display, IP48 water resistance, 7 years of updates, a variety of AI features, attractive design, enjoyable software.
Drawbacks: High price point, less durable than conventional phones, repairs may be costly, no dust resistance, camera lacks telephoto zoom, and its performance does not reach flagship standards, coupled with a lack of significant updates.
The Flip 7 offers stunning aesthetics and can perform numerous tasks while closed, though most functions are better executed on the main internal display. Photo: Samuel Gibbs/The Guardian
NASA, ESA, Jennifer Lotz, Matt Mountain, Anton M. Koekemoer, HFF Team (STScI)
In the vast expanse of the universe, galaxies that exhibit peculiar contours are surprisingly filled with ancient stars. This offers astronomers an initial peek into a unique type of stellar body that emerged soon after the universe’s inception.
Although the James Webb Space Telescope (JWST) has allowed scientists to revisit regions of the early universe, pinpointing the first stars remains elusive. These primordial stars, termed Population III stars, are primarily colossal hydrogen spheres believed to have formed in the universe’s infancy. As the very first stars, they left behind an environment largely devoid of heavier elements following their demise.
While there have been theories hinting at the existence of such stars, definitively proving their existence in the early universe has been challenging, as galaxies appeared to have become tainted with heavier elements merely a few hundred million years post-Big Bang.
Recently, Morihara Highlands from the California Institute of Technology and his team found a galaxy almost entirely composed of hydrogen, indicating the presence of Population III stars. However, this galaxy emerged later than expected, approximately a billion years after the universe began.
Dubbed Amore6, it was initially identified within the Abell 2744 galaxy cluster. Upon measuring the light from Amore6 using the JWST, Morishita and his colleagues noted the complete absence of common oxygen ions. This suggests that the galaxy harbors less than 0.2% of the oxygen present in our sun, indicating a lack of contamination by heavier elements.
As the universe evolves, the likelihood of encountering such pristine galaxies diminishes. In images captured by the JWST, Amore6 appears somewhat isolated, which Morishita posits could be a factor in its untouched state. “This seclusion might mean that this galaxy has not yet encountered sufficient gas to trigger star formation, implying that it could evolve slowly,” he mentions.
“If these findings are validated, it would be truly astonishing, as we did not anticipate discovering such an untarnished galactic environment later in the universe’s development,” says Fabio Pacucci of the Harvard Smithsonian Astrophysics Center in Massachusetts.
This discovery has implications for observing “direct collapse” black holes. Unlike the conventional pathway of collapsed stars, these black holes form from massive clouds of untainted gas. While astronomers had predicted their existence, they have never actually formed as it was believed that primitive gas was only available for a limited period, up to 100 million years after the Big Bang. However, if this untainted gas can persist for an extended duration, the potential for observing such phenomena increases, Pacucci argues.
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Galaxies are groups of stars held together by gravitational forces. Most galaxies originated in the first 200 million years after the Big Bang and have transformed over approximately 14 billion years. Early galaxies formed as aggregates of stars that clustered around the center of mass. In the youth of the universe, galaxies were in close proximity, exerting gravitational pull on one another. As the universe expands, the distances between galaxies have grown, reducing their interactions. They have remained far apart, allowing for internal development over billions of years.
Astronomers categorize galaxies based on their current shapes. Those resembling the Milky Way are termed spiral, while circular or oval-shaped ones are called elliptical. Galaxies that fall between spiral and elliptical forms are referred to as lenticular, and any that do not fit into these categories are labeled irregular. Over 75% of galaxies identified by astronomers are spiral in nature. If a spiral galaxy features prominent bars of stars and dust through its center, researchers classify it further as a barred spiral galaxy.
About 60% of spiral galaxies, including the Milky Way, exhibit galactic bars, designating them as barred spiral galaxies. These bars also serve as nurseries for star formation and are catalysts for the galaxy’s evolution. However, astronomers understand that galaxies do not inherently begin with these bars, prompting further investigation into the formation processes and timelines of these features.
This diagram illustrates the galactic classification system developed by 20th-century astronomer Edwin Hubble. The galaxy marked with the “E” label represents elliptical galaxies, while S0 indicates lenticular galaxies. The other “S” labels refer to spiral galaxies, with those labeled “SB” denoting a spiral structure. “Hubble tuning fork diagram” by cosmogoblin is licensed under CC0 1.0.
An international team of scientists researched the formation of bars in 20 galaxies near the Milky Way using advanced analytical techniques developed over the last four years. They gathered data from the TIMER space investigation, focused on the light emission patterns known as spectra from stars near the centers of these galaxies. The TIMER survey utilized the Very Large Telescope in Chile, equipped with a multi-unit spectroscopic explorer called MUSE.
The team initially struggled to obtain spectra for individual stars within these galaxies. As a reference, the closest galaxy studied was 7 megaparsecs away, approximately 23 million light years, or 130 million miles. Individual stars are too diminutive to distinguish at such distances, even with the most precise instruments.
To overcome this challenge, the team analyzed the spectra of stars within two concentric rings representing different regions at the centers of these galaxies. The inner ring comprised stars strictly within the bars of the galaxy, corresponding to an area known as the nuclear disk, while the outer ring included both inner and outer stars of the bar, referred to as the main disk.
They subtracted the spectrum of the stars in the inner ring from that of the outer ring, yielding two distinct light patterns: one for stars within the bar and another for stars outside of it. By treating the combined patterns of each ring as representative of typical stars in those regions, they could estimate the age of individual stars and ascertain when they formed. Past astrophysical models suggest that galaxy bars enhance the star formation rate around their centers. Hence, the team inferred the formation timing of galaxy bars as stars began to form more rapidly within those structures.
With this innovative approach, they estimated the age range for the 20 galaxies studied, with an error margin of approximately 1.5 billion years. Among their sample, the galaxy that formed bars most recently was 800 million years old. Out of the 20 galaxies, 14 formed bars approximately 7.5 billion years ago or later, while the remaining six galaxies established bars around 9.5 billion years ago, with the oldest estimates dating back 13.5 billion years. In contrast to earlier predictions, they found that larger galaxies do not necessarily possess older bars.
From the diverse ages of the bars observed, the team concluded that the formation of galaxy bars is an ongoing process in the cosmos. Their methodology provides astrophysicists with a means of gaining deeper insights into the dynamics of the early universe and the interactions between ancient galaxies, which connect to their present forms. By doing so, future research teams can establish a refined timeline for the universe and identify changes in how dominant forces have shaped galaxies, from their interactions to their internal structuring.
Samsung’s newest flagship folding phone appears to have shed some weight. The outcome is one of the sleekest and lightest devices on the market, significantly enhancing its portability.
The Galaxy Z Fold 7 measures 8.9mm in thickness when closed. Excluding the camera bump at the back, its profile is comparable to that of a typical smartphone, making it easy to fit into your pocket, but it unfolds to a folding tablet at just 4.2mm thick.
However, priced at £1,799 (€2,099/$2,000/$2,899), this device comes at a steep cost. It represents an expensive, cutting-edge solution that potentially replaces your phone, tablet, or PC within one compact device.
The ultra-slim design results in a notable camera bump that extends approximately 5.5mm from the rear. Photograph by Samuel Gibbs/The Guardian
The seventh iteration of Samsung’s folding technology addresses many of the issues found in its predecessors. Weighing only 215g—24g lighter than last year’s edition—it resembles a typical large smartphone when closed.
It fits comfortably in your pocket. Sending messages, making calls, navigating, and taking photos feels just like using a conventional phone. Even the front 6.5-inch screen is vibrant, colorful, and smooth with a 120Hz refresh rate. The enhancements to the fingerprint scanner on the power button are quick and precise.
When opened like a book, the Fold 7 is impressively thin, only slightly thicker than the USB-C port itself. Its lightweight feel is deceptive; it’s solidly built. One wonders how the device can achieve such thinness without forgoing the charging port. The flexible 8-inch OLED screen is smooth, bright, and almost square, capable of running two apps side by side.
The exterior screen and back are shielded by the latest tempered glass technology, while the inner screen features a layer that is softer than standard glass, making it prone to fingerprints and a bit shiny. The crease along the fold is nearly invisible, visible mainly under glare.
With Flex Mode, you can enjoy viewing content on the Fold 7 in a half-folded position, resembling a mini laptop setup. Photograph by Samuel Gibbs/The Guardian
Specifications
Main screen: 8-inch QXGA+ 120Hz (368PPI) AMOLED Flexible Display
Water Resistance: IP48 (1.5 meters for 30 minutes)
Folded Dimensions: 158.4 x 72.8 x 8.9mm
Expanded Dimensions: 158.4 x 143.2 x 4.2mm
Weight: 215g
Power for Multitasking
The Fold 7 achieves a full charge in 82 minutes and reaches 60% in under 30 minutes utilizing a USB-C power adapter of 25W or higher (not included). Photograph by Samuel Gibbs/The Guardian
The Fold 7 is equipped with the same flagship Qualcomm Snapdragon 8 Elite processor and 12GB of RAM as the S25 Ultra and S25 Edge. This setup ensures excellent performance for daily tasks and high-end gaming, outpacing competitors like the Google Pixel 9 Pro fold.
Its battery reliably lasts about two days, with each screen being used for around four hours and several hours spent on 5G. This performance level mirrors its predecessor and functions similarly to a standard smartphone. Depending on usage, many find they need to recharge every other day.
One UI 8 for Android 16
The Fold 7 can run two apps in full size, and allows for a total of up to 8 apps using split-screen and floating windows. Photograph by Samuel Gibbs/The Guardian
The Fold 7 stands out as one of the first devices to ship with One UI 8 (Android 16). While it hasn’t seen drastic changes since last year’s software, it still offers an impressive suite of features. This includes the handy Now Valle Bar at the bottom of the lock screen, showcasing live sports scores, music, timers, and other commonly used tools.
Samsung effectively leverages the multitasking capabilities afforded by the folding format better than its competitors. Up to 8 apps can be accessed concurrently on the internal screen, with each having its own unique home screen layout. Users can adjust app sizes and shapes, use apps in a partially folded state, and move them seamlessly between screens.
Moreover, the Fold 7 integrates all the AI features from the S25 series, including Google Gemini, Circle to Search, Writing and Drawing tools, Transcription, and Audio Editing capabilities. While some of these are useful, others tend to be superfluous, much like many trendy AI offerings. Notably, Samsung commits to providing Android and security updates until July 31, 2032.
Camera
Capturing photos is simple with the Fold 7, whether closed or opened slightly for hands-free shots. Photograph by Samuel Gibbs/The Guardian
The prominent camera system on the back includes a 200MP main camera, a 12MP ultra-wide, and a 10MP telephoto camera with 3x zoom. There’s also a pair of 10MP selfie cameras on either screen.
The main 200MP camera excels in a range of lighting conditions, delivering high-quality photos and representing a significant improvement over its predecessor’s capabilities.
The 12MP Ultra Wide Camera offers commendable performance and can achieve good macro shots, while the 3x telephoto camera produces pleasing portraits, albeit with some softness in low-light scenarios, lacking the 5x zoom found on some higher-end models. Similar limitations apply to the selfie camera, as it can be grainy in dim lighting. However, users can utilize the outer screen as a viewfinder when taking selfies with the main camera, leading to better results.
The camera app is user-friendly, boasting numerous shooting modes and solid video recording capabilities. Overall, the Fold 7 presents a robust camera system that competes well against flagship slab phones, delivering impressive results.
Sustainability
The Fold 7 closely resembles a standard smartphone from both the front and back. Photograph by Samuel Gibbs/The Guardian
The battery is expected to retain at least 80% of its original capacity over 2,000 full charge cycles.
The phone is generally reparable, with internal screen repairs estimated at around £500. Samsung also offers a self-repair program similar to CARE+ that can bring repair costs down to £139.
The Fold 7 incorporates recycled materials such as aluminum, cobalt, copper, glass, gold, lithium, plastic, rare earth elements, and steel, which make up 13.7% of its total weight. Additionally, Samsung has trade-in and recycling programs for older devices, aiming to mitigate the environmental impact of smartphones as outlined in their sustainability reports.
Price
The Samsung Galaxy Z Fold 7 begins at £1,799 (€2,099/$1,999.99/$2,899).
For comparison, the Galaxy Z Flip is priced at £1,049, the Galaxy S25 Edge at £1,099, the S25 Ultra at £1,249, and the Google Pixel 9 Pro Fold at £1,399.
Verdict
The Galaxy Z Fold 7 is a remarkably high-tech device that represents a significant improvement over its predecessor, addressing many of the typical issues associated with folding smartphones.
When closed, it feels significantly thinner and lighter, akin to a traditional phone. Upon opening, the internal screen is still flexible, with creases that are almost imperceptible, paired with vibrant visuals that enhance multitasking capabilities.
The camera, while effective, doesn’t overshadow the device’s overall utility, but it can cause the phone to wobble when placed flat on a surface. In addition, the Fold 7 features the same advanced processors as Samsung’s top-tier regular smartphones, alongside good battery life and solid software support.
However, the fragile nature of the folding mechanism, lack of proper dust resistance, the delicate inner screen, and hefty price tag remain notable drawbacks. If your primary aim is to have a compact device that serves as both phone and tablet, this model may not sway you.
Nevertheless, the Fold 7 stands out as the finest folding phone on the market, presenting the major upgrades that Samsung has been striving for in recent years.
Pros: Combines phone and tablet functionality, feels like a standard phone when closed, boasts exceptional software with robust multitasking features, impressive tablet display, top-notch performance, reliable battery life, water resistance, and extended software support.
Cons: Expensive, lacks dust resistance, potentially more fragile than standard devices, costly repairs, and limited zoom capabilities compared to traditional smartphones.
You might easily forget that the Fold 7 can be unfolded, as it functions and feels like a standard smartphone when using the external display. Photograph by Samuel Gibbs/The Guardian
The NASA/ESA Hubble Space Telescope has captured a stunning image of the Barred Spiral Galaxy NGC 3285b.
This Hubble image reveals NGC 3285B, a spiral galaxy approximately 137 million light years away in the Hydra constellation. The color images were generated from separate exposures in the ultraviolet and infrared regions using Hubble’s Wide Field Camera 3 (WFC3), based on data collected through seven filters. Image credits: NASA/ESA/Hubble/RJ Foley, UC Santa Cruz.
NGC 3285b is situated around 137 million light years from the Hydra constellation.
It is also referred to as Leda 31293, ESO 501-18, or IRAS 10322-2723, with a diameter of 100,000 light years.
NGC 3285B boasts a disc and multiple swirling arms, characterized by a large, bright, golden nucleus, while its spiral arms exhibit a light, faint reddish hue.
It is part of the NGC 3312 Galaxy Group (LGG 210) and is a member of the Hydra I Galaxy Cluster.
“NGC 3285B is a component of the Hydra I Cluster, one of the largest galactic clusters in the nearby universe,” stated Hubble astronomers.
“Galactic clusters consist of hundreds to thousands of galaxies held together by gravity.”
“The Hydra I cluster is centered around two massive elliptical galaxies.”
“Each of these galaxies spans about 150,000 light years, roughly 50% larger than our Milky Way.”
NGC 3285B lies on the outskirts of the Hydra I cluster, distanced from the colossal central galaxy.
“This galaxy captured Hubble’s interest as it hosted a Type Ia supernova in 2023,” the astronomer noted.
“Type Ia supernovae produce a condensed star core known as white dwarf explosives, igniting a sudden fusion burst approximately five billion times brighter than the sun.”
The supernova, labeled SN 2023XQM, appears as a blue dot on the far left side of the galaxy’s disc.
“Hubble observed NGC 3285B as part of a campaign focused on Type Ia supernovae.”
“We aim to address the effects of distance and dust by examining each of these supernovae in ultraviolet, optical, and near-infrared light.”
“This initiative will enhance cosmic distance measurements that depend on observations of Type Ia supernovae.”
J1025+1402, one of three small red dot galaxies up to 2.5 billion light years apart
Digital Legacy Survey/d. Lang (Permieter Institute)
A new analysis shows that peculiar galaxies, once only identified in early cosmic formations, have surfaced more recently, raising intriguing questions about their origins.
Recent observations made by astronomers utilizing the James Webb Space Telescope (JWST) have revealed compact red entities from the universe’s first billion years, dubbed Little Red Dots (LRD). These were initially believed to be associated with phenomena in the early universe, like the formation of supermassive black holes at the cores of galaxies, including our own.
Xiaojing Lin from China’s Tsinghua University, along with her research team, has discovered LRD in a much younger universe, about 12 billion years post-Big Bang. “This finding demonstrates that the conditions fostering small red dots are not solely confined to the early universe,” states Lin.
The researchers employed a telescope based in New Mexico to analyze images captured during the Sloan Digital Sky Survey. They pinpointed three objects that appeared as LRD, but significantly, they were merely 2.5 billion light years apart.
“They meet all criteria for classification as small red dots,” remarks Xiaohui Fan from the University of Arizona. “I believe there’s no doubt regarding their similarity.”
Each LRD is estimated to be approximately one million times the mass of the Sun, with dimensions comparable to the solar system. One of these LRDs is nicknamed the “egg” due to its elongated structure. The team also identified a few other potential LRD candidates awaiting confirmation.
These findings are exhilarating, says Anthony Taylor from the University of Texas at Austin, as they provide unique insights into the characteristics of LRDs. These objects are faint enough that telescopes like the JWST and Hubble can analyze them significantly easier than their early universe counterparts, potentially unveiling their true nature.
“They’re much closer to us, making them appear much brighter,” adds Taylor.
A schematic diagram showing what the local small red dots might be, depicting a black hole at the center, encircled by a significant gas envelope (yellow), streams of gas, clouds, and dust.
Xiaojing Lin with Cass Fan
A potential explanation for LRDs is that they signify the nascent phases of extraordinarily massive black holes maturing within the galaxy, possibly marking their initiation as they begin consuming matter voraciously.
It’s currently unclear whether local LRDs are dormant galaxies that have recently awakened or if they have just formed and are starting to consume significant amounts of material. “At this point, it is premature to discuss that aspect,” Taylor points out.
The team is eager to utilize Hubble and JWST to delve deeper into these local LRDs. “I have a proposal for Hubble pending approval,” Fan comments.
LRDs have the potential to exist not just in contemporary and ancient universes but throughout cosmic history. “They may have been lurking, camouflaged, amidst the cosmos,” Fan remarks. “People haven’t known what to look for.”
NASA astronomers have utilized data from multiple universes and ground-based telescopes to produce breathtaking new images of the Andromeda Galaxy, the nearest spiral galaxy to our Milky Way.
This new composite image of the Andromeda Galaxy features X-ray data from Chandra and XMM-Newton (depicted in red, green, and blue), ultraviolet data from Galex (blue), optical data from ground astrophotographers (Jakob Sahner and Tarun Kottary), as well as infrared data from Spitzer, Cobe, Planck, and Herschel (in red, orange, purple). Wireless data sourced from the Westerbork Synthesis Radio Telescope (red-orange). Image credit: NASA.
Also referred to as NGC 224, Messier 31, or M31, the Andromeda Galaxy is a spiral galaxy located approximately 2.5 million light-years from Earth.
With over 100 billion stars, it is comparable in size to our own Milky Way galaxy.
Visible as cigar-shaped patches of light high in the autumn sky, the Andromeda Galaxy’s enormous bubbles of high-temperature diffuse plasma make it appear 100 times the angular diameter of the full moon.
The galaxy is surrounded by a dark, invisible halo extending about a million light-years and is believed to contain half of its star mass.
Andromeda has significantly contributed to various fields of astrophysics, especially in the study and identification of dark matter.
In the 1960s, astronomer Dr. Vera Rubin and her team investigated Andromeda and identified invisible forces influencing the galaxy’s spiral arm rotations.
“This new image of the Andromeda Galaxy is released to honor Vera Rubin’s pioneering contributions that transformed our comprehension of the cosmos,” stated a NASA astronomer.
“Rubin’s meticulous measurements of Andromeda’s rotational curves provided some of the earliest and most convincing evidence that galaxies exist within vast halos of unseen material.”
“Her research reshaped long-standing assumptions and sparked a new era of inquiry into the structure and dynamics of the universe.”
“To celebrate her scientific achievements, the US Mint recently issued a quarter featuring Rubin as part of the American Women Quarters program in 2025.”
To create a new image of the Andromeda Galaxy, astronomers analyzed data from NASA’s Chandra X-Ray Observatory, XMM-Newton, Planck, and Herschel Telescopes from ESA, in addition to data from retired Galex and Spitzer telescopes. Information was also gathered from astrophotographers using ground-based telescopes and wireless data from the Westerbork Synthesis Radio Telescope.
“Each type of light provides unique insights into this neighboring galaxy as compared to the Milky Way,” the researchers noted.
“For instance, Chandra’s X-rays unveil high-energy radiation around the ultra-massive black holes at Andromeda’s core, alongside numerous small, dense objects scattered throughout the galaxy.”
“A recent publication on Chandra observations of the Andromeda Galaxy details the amount of X-rays emitted by the ultra-massive black holes at the galaxy’s center over the past 15 years.”
“One flare was detected in 2013, showcasing the typical X-ray amplification seen from a black hole.”
The lines of galaxies that emerged after the collision of the two dwarf galaxies, which tore gases from one another.
Keim et al./Decals
A curious dwarf galaxy may have originated from a bullet-like collision in the universe.
Michael Keim from Yale University and his team employed the Keck Observatory in Hawaii to examine the distinctive trails of 12 small dwarf galaxies located approximately 75 million light-years from the Milky Way.
The orientation and velocity of the galaxies indicate that they resulted from a head-on impact between two galaxies known as NGC 1052-DF2 and NGC 1052-DF4. This collision expelled gas, which eventually coalesced into a group of stars due to gravitational attraction.
“They’re exceptionally unique,” states Kayme. “This is the only known system of its kind.”
Keim and his colleagues named this system after a similar cluster of large galaxies referred to as Bullet Clusters.
It is believed that the two galaxies collided at a speed of 350 kilometers per second around 9 billion years ago. As they passed through one another, gas was stripped from each galaxy. “While it’s improbable for two stars to collide,” notes Kayme, “the same does not apply to gas clouds.”
Interestingly, the remnants of stars left after the collision appear to lack dark matter. This is quite unusual, as most galaxies contain a substantial amount of dark matter, often comprising over 90% of their total mass.
Keim and his team theorize that this anomaly may stem from dark matter’s inability to interact with regular matter during the gas stripping process or because it remained unaffected by the interaction.
This finding may challenge alternative theories regarding dark matter, which posit that discrepancies in stellar and galactic behavior stem from gravitational effects rather than the existence of dark matter particles. “This suggests that dark matter is indeed a particle that can be separated from a galaxy,” explains Kayme.
Images and videos from the Vera C. Rubin Observatory showcase over 10 hours of test observations before being revealed. The event was live streamed on Monday from Washington, DC.
Keith Bector, an associate professor from the University of Wisconsin-Madison physics department, has contributed to the Rubin Observatory for nearly a decade as a system verification scientist, ensuring that all components of the observation deck function properly.
He mentioned that the team was present as images streamed in real-time from the camera.
“In the control room, there was a moment when all engineers and scientists gazed at these images. We were able to observe more details about stars and galaxies,” Vector explained to NBC News. “Understanding this on an intellectual level is one thing, but on an emotional level, I realized I was part of something truly extraordinary, all happening in real-time.”
One of the newly released images enabled the Rubin Observatory to identify galaxies billions of light-years away, alongside asteroids in the solar system and stars in the Milky Way.
“In fact, most of the objects captured in these images exhibit light that was emitted before our solar system was formed,” highlighted Bechtol. “We are witnessing light that reflects billions of years of the universe’s history, and many of these galaxies have never before been observed.”
Astronomers are eagerly awaiting the first images from the new observatory, affirming that experts will aid in unraveling some of the universe’s greatest mysteries and revolutionizing our understanding.
“We are entering the golden age of American science,” stated Harriet Kang, acting director of the Energy Department of Science. She elaborated in a statement.
“We anticipate that the observation deck will provide profound insights into our past, future, and potentially the fate of the universe,” Kang remarked during a Monday event.
The Vera C. Rubin Observatory is collaboratively managed by the Energy Agency and the National Science Foundation.
Named after an American astronomer renowned for uncovering evidence of dark matter in space, the observatory is situated atop Cerro Pachon, a mountain in central Chile. It is designed to capture around 1,000 images of the southern hemisphere sky each night, covering the entire visible southern sky every three to four nights.
These early images stem from a series of test observations and mark the commencement of a bold decade-long mission to scan the sky continuously, capturing all visible details and changes.
“The entire observatory design is centered on this capability, enabling you to point, shoot, and repeat,” Bechtol noted. “Every 40 seconds, the view shifts to a new part of the sky. Imagine bringing the night sky back to life in a way we’ve never experienced before.”
By repeating this process nightly over the next decade, scientists aim to create extensive images of the visible southern sky, tracking bright stars, moving asteroids in the solar system, measuring supernova explosions, and observing other cosmic phenomena.
“Utilizing this groundbreaking scientific facility, we will delve into many mysteries of the universe, including the dark matter and dark energy that fills our cosmos,” stated Brian Stone, Chief of Staff of the National Science Foundation, in a statement.
Astronomers have identified the largest known cloud of energy particles encircling galaxy clusters, with around 20 million annual clouds around the galaxy cluster PLCK G287.0+32.9.
This new composite image, created using X-rays from NASA’s Chandra X-Ray Observatory (blue and purple), radio data from Meerkat Radio Telescope (orange and yellow), and optical images from Panstarrs (red, green, and blue), illustrates the giant galaxy cluster PLCK G287.0+32.9. Image credit: NASA/CXC/CFA/Rajpurohit et al. / panstarrs / sarao / meerkat / sao / n. wolk.
Located 5 billion light years from Earth in the Hydra constellation, PLCK G287.0+32.9 has garnered astronomers’ attention since its initial detection in 2011.
Prior research uncovered two bright relics, revealing a massive shock wave illuminating the cluster’s edges. However, the extensive, faint radio emissions filling the space between them went unnoticed.
Recent radio images have shown that the entire cluster is enveloped in a faint radio glow that is nearly 20 times the diameter of the Milky Way, suggesting an extraordinary and powerful phenomenon at play.
“We anticipated finding a bright pair of relics at the cluster’s edge. Found “The Harvard & Smithsonian Astrophysics Center” mentioned: “The Harvard & Smithsonian’s Astrophysics Center is a great way to help you get started,” Dr. Kamursh Rajprohit, an astronomer at the Harvard & Smithsonian Center for Astrophysics, noted.
“No energy particle clouds of this magnitude have been spotted in such galaxy clusters or anything comparable.”
Previous record holders, located around Abel 2255 in the Galaxy Cluster, spanned about 16.3 million light years.
In the central region of the cluster, Dr. Rajprohit and his team identified radio halos where frequencies of this scale are typically undetectable, marking the first discovery of size at 114 million light years at 2.4 GHz.
The findings posed questions for the team, providing compelling evidence of magnetic fields where cosmic ray electrons and magnetic fields extend throughout the cluster.
However, it remains uncertain how these electrons can accelerate over such vast distances.
“Very extended radio halos are seldom visible across most frequencies, as the electrons responsible for them tend to lose energy. They are aged and have cooled over time,” Dr. Rajpurohit stated.
“The discovery of this colossal halo has now led to a significant increase in radio emissions between the catastrophic impact and the rest of the cluster.”
“This suggests something is actively accelerating or re-accelerating the electrons, yet none of the usual explanations apply.”
“We suspect that extensive shock waves and turbulence may be contributing factors, but additional theoretical models are needed to arrive at a definitive conclusion.”
This discovery offers researchers a new pathway to investigate cosmic magnetic fields—one of the primary unanswered questions in astrophysics—helping to elucidate how magnetic fields shape the universe on the largest scales.
“We’re beginning to perceive space in ways we have never imagined,” Dr. Rajprohit emphasized.
“This necessitates a reevaluation of how energy and matter traverse through its grandest structures.”
“Observations from NASA’s Chandra X-ray Observatory, managed by the Smithsonian Astrophysical Observatory, reveal boxy structures, comet-like tails, and several other distinct features of the cluster’s hot gas, indicating that the cluster is highly disturbed.”
“Some of these X-ray features correspond with radio-detected structures, pointing to substantial shocks and turbulence driven by merging events, facilitating electron acceleration or re-acceleration.”
“In the core of a cluster, some of these features may arise from the merger of two smaller galaxy clusters, or an explosion triggered by an exceptionally large black hole, or a combination of both.”
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