Bold Mission Launched to Rescue NASA’s Fallen Telescope: A New Hope for Space Exploration

Posted on July 3, 2026 by Igor Mitreski

NASA’s Neil Gehrels Swift Observatory

NASA Goddard Space Flight Center

The Neil Gehrels Swift Observatory, one of NASA’s advanced space telescopes, faces a critical situation, as its mission to save and extend its operational life has commenced. Currently on a path to return to Earth in a few months, a successful rescue could allow it to continue its astronomical observations for many more years.

Like all satellites, Swift is experiencing orbital decay, having been launched in 2004. Originally at an altitude of around 600 kilometers, it now hovers at just 375 kilometers above the Earth’s surface. Recent solar flares intensified atmospheric drag, causing this unexpected decline in altitude.

NASA sought innovative solutions to keep the Swift operational, ultimately selecting a plan proposed by Catalyst Space Technologies, a small startup in Arizona, aimed at enhancing the observatory’s orbit.

This ambitious rescue mission involves a satellite named Link, equipped with three robotic arms designed to securely grasp Swift and elevate it back to safety. Though Link measures less than two meters tall and is about one-third the size of Swift, its large solar panels are well-equipped to power the necessary thrusters and grappling arm.

Launched on July 3 atop a Northrop Grumman Pegasus XL rocket, Link represents the final mission for this rocket before its retirement. Over the next two months, it will secure Swift and gradually elevate it for several weeks of testing in space before releasing it at its original altitude. If successful, this operation could extend Swift’s operational lifespan by up to 10 years.

Initially designed to study gamma-ray bursts—the most powerful explosions in the universe—Swift has detected approximately 1,800 of these events and made significant discoveries concerning other celestial phenomena, including comets, planets, supernovae, and black holes.

While the orbital boost will allow for continued observations, it will also serve as a pivotal demonstration of how to potentially salvage space telescopes. “Swift was never intended for servicing,” stated Ghonhee Lee, CEO of Katalyst. According to a statement, “By showing that rapid and economical life extension is possible, we are establishing a prototype for servicing spacecraft not designed for in-orbit maintenance.” This approach could present a cost-effective method for prolonging the lifespan of other satellites, including the Hubble Space Telescope, which is projected to cease operations in the 2030s unless proactive measures are taken.

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Source: www.newscientist.com

NASA’s Mission to Rescue Sinking Space Telescope: Orbital Rendezvous Plans Unveiled

Posted on June 30, 2026 by Igor Mitreski

NASA is gearing up for an exciting mission set to launch this Tuesday aimed at rescuing one of its flagship space telescopes.

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The Neil Gehrels Swift Observatory, launched over two decades ago, has been essential in studying gamma-ray bursts—some of the universe’s most powerful explosions. These phenomena occur during events such as black hole formations or when dense stars collide at the end of their life cycles.

Currently, Swift is facing serious threats, as NASA’s models indicate a potential orbital drop to dangerously low altitudes by October, below 185 miles, risking re-entry and disintegration.

Dr. Sean Domagal Goldman, head of NASA’s astrophysics division, emphasized the importance of Swift at a June 17 press conference. “This observatory excels at quickly identifying transient events in the night sky, making it unique. Thus, we’ve concluded that it deserves to be saved.”

In a bid to rescue the observatory, NASA is slated to launch a robotic spacecraft designed to elevate Swift’s orbit. Last year, the agency allocated $30 million to Arizona-based Catalyst Space Technologies for spacecraft development, while Northrop Grumman will supply the aircraft and rockets for launch.

The operation aims to have Northrop Grumman’s Stargazer aircraft lift off from the Marshall Islands around 6:23 a.m. Tuesday. Once at 40,000 feet, the Stargazer will release the Pegasus XL rocket carrying the LINK spacecraft, which stands 6 feet tall and weighs 880 pounds.

Following its launch, the LINK spacecraft will enter orbit, where it will capture the Swift Observatory and work to increase its altitude over several months.

All satellites in low Earth orbit gradually descend due to atmospheric drag. Swift is currently affected by this, compounded by an intense solar cycle experienced in 2024, known as solar maximum, which increases drag as the atmosphere heats up during heightened solar activity.

Digital illustration of NASA’s Swift Observatory.Conceptual Imagery Lab at NASA’s Goddard Space Flight Center

John Nosek, an astronomy and astrophysics professor at Penn State University, noted that salvaging Swift could offer broader benefits beyond just extending observation capabilities.

“The capability of recovering satellites that weren’t intended for in-orbit servicing could revolutionize NASA’s approach to spacecraft management,” Nousek stated. “If the LINK mission succeeds, it will only cost about $30 million (in 2026 dollars) to restore the functionality of a $300 million (2004 dollars) satellite.”

Kieran Wilson, vice president of technology at Catalyst Space Technologies, expressed optimism that the Swift Boost mission will reshape astronomers’ perspectives on satellite longevity.

“Traditionally, satellites are launched, complete their missions, and then are either discarded, re-entered, or put into graveyard orbits,” he stated at a June 17 press conference. “We need to be able to refuel, reposition, and upgrade satellites, even if they weren’t designed for such tasks.”

Since its launch in 2004, Swift Observatory has significantly contributed to our understanding of over 1,400 gamma-ray bursts and other high-energy cosmic phenomena, including the farthest known object detected, originating from an exploding star nearly 13 billion light-years away.

NASA has entrusted Katalyst Space Technologies with the task of building and launching the LINK spacecraft, slated for September 2025. Although the timeline appears feasible, Wilson warned that successfully rendezvousing with Swift in orbit and stabilizing its altitude remains a daunting challenge. Swift wasn’t designed for orbital operations and lacks thrusters to adjust its own position or accompany other spacecraft.

“Operational success in space is notoriously difficult,” Wilson acknowledged. “Rendezvousing with Swift will be particularly challenging, but we are prepared for the task ahead.”

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Source: www.nbcnews.com

Next-Generation Sensitive Radio Telescope Array to Launch in Nevada Desert

Posted on June 21, 2026 by Igor Mitreski

A remote region in the Nevada desert within the Great Basin is set to host the world’s most advanced radio telescope array.

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The California Institute of Technology is spearheading the project and announced its intention to initiate construction of the telescope after securing adequate funding. This project, known as the Deep Synoptic Array, consists of 1,650 individual radio antennas that will collectively study supermassive black holes, pulsars, and fast radio bursts — brief, powerful emissions of radio waves that often originate in deep space.

Greg Hallinan, an astronomy professor at Caltech and the principal investigator for the Deep Synoptic Array, commented, “The vast number of antennas distinguishes this telescope from any existing ones.”

Radio telescopes capture naturally occurring radio waves emitted by various celestial bodies, enabling astronomers to analyze these signals for insights into their structure, composition, and temperature.

While radio telescopes do not capture images like optical observatories, they can convert radio signals into data for imaging.

Hallinan stated that the Deep Synoptic Array will surpass all previous ground-based radio telescopes in performance, observing the sky 100 times faster while producing exceptionally high-quality radio images.

Regarding radio-emitting cosmic objects, he remarked, “Collectively, all telescopes built over the last century have identified approximately 20 million radio sources in the universe. This telescope will double that in just the first 24 hours.”

Each dish in this project is designed to measure about 20 feet in diameter. Together, they will form one of the largest radio telescope arrays ever constructed, covering over 123 square miles managed by the Bureau of Land Management in White Pine County, Nevada.

Hallinan indicated that the project is currently in the permitting phase, aiming to start construction next year and complete it by 2029.

For ground-based radio astronomy, two types of telescopes are commonly utilized: the Green Bank Telescope in West Virginia, which boasts a diameter of 328 feet, and the extensive array of small dishes like the Very Large Array in New Mexico, featuring 27 dishes arranged in a Y-shape.

Single-dish telescopes are generally more sensitive and capable of detecting faint radio waves from deep space, while large arrays of multiple dishes tend to yield clearer images. Hallinan noted that deep synoptic arrays have the potential to achieve both.

Members of the Caltech Deep Synoptic Array Team.
Katie Jameson / California Institute of Technology / DSA Project

The Deep Synoptic Array is engineered to detect radio emissions from millions of stars, galaxies, and additional celestial entities emitting radio light.

“Radio astronomy is transforming from sketches to high-resolution imagery,” said Vikram Ravi, Caltech astronomy professor and co-principal investigator of the Deep Synoptic Array, as stated in a recent announcement. “The DSA will scan a significantly larger celestial area more frequently than any other telescope.”

Researchers plan to utilize the array for at least five sky surveys, seeking captivating radio emission pulses for additional study.

“We will pinpoint the exact location of any detected radio source, enabling optical, infrared, and X-ray observatories to target that area for further exploration,” Hallinan explained.

Funding for the initiative has been provided by Schmidt Science, a philanthropic organization established by former Google CEO Eric Schmidt and his wife, Wendy. Schmidt has also recently taken the helm at rocket company Relativity Space, which secured a key NASA contract this week to deliver scientific instruments to Mars in 2028.

As a preliminary step, two prototype plates were recently constructed near Bishop, California, serving as technology demonstrations, according to Hallinan.

To identify a suitable location for the Deep Synoptic Array, Hallinan and his team evaluated sites throughout the western United States, including California, Nevada, New Mexico, and Utah. An ideal setting would be remote, minimizing interference from radio frequencies generated by devices like cell phones and Wi-Fi.

“This telescope is so sensitive that it can detect cell phones from the distance of the Sun,” Hallinan remarked.

The Great Basin in Nevada serves as a natural barrier against unwanted interference.

“The quiet valleys here have minimal population,” he added. “This site in White Pine County is the quietest location we evaluated, making it exceptionally suitable for radio astronomy.”

Source: www.nbcnews.com

NASA Launches Nancy Grace Roman Space Telescope for Record-Breaking Space Scans

Posted on June 16, 2026 by Igor Mitreski

In contrast to many of NASA’s flagship missions, the Roman Telescope was successfully delivered on budget and ahead of schedule. However, achieving this milestone was not without its challenges, according to Benford.

“Bringing this observatory to life in space has been a significant focus of my professional journey, and throughout the years, it felt like a relentless struggle,” he stated.

The Roman Telescope project has faced significant interruptions, including the COVID-19 pandemic and two long government shutdowns in U.S. history. Initially, NASA aimed for a launch by May 2027 at the latest.

The observatory is scheduled to launch atop a SpaceX Falcon Heavy rocket. Following its launch, the Roman Telescope will journey for over three months to reach its orbital destination. Upon arrival, mission controllers will test the observatory’s instruments before commencing scientific observations.

NASA employees and guests view the Nancy Grace Roman Telescope in the clean room.
Jason Andrew, NBC News

If all goes according to plan, Benford anticipates that the telescope’s first images will be revealed by the end of this year.

“It could be around Christmas time; hopefully, it will make for a delightful present,” he remarked.

Currently, NASA has no major space telescope initiatives in the pipeline. The agency is considering a mission called the Habitable World Observatory aimed at discovering signs of life on exoplanets, but this project won’t launch until the 2040s.

The impending launch of the Roman Telescope holds special significance for Goddard Space Flight Center employees, many of whom also contributed to the Hubble and Webb missions.

“The excitement is overwhelming; I’ve dedicated a substantial part of my career to this project,” shared mission systems engineer Mark Melton. He anticipates shedding tears upon the telescope’s deployment.

“It started as a concept, and now it’s a reality,” he concluded.

Source: www.nbcnews.com

Webb Telescope Uncovers Strongest Evidence Yet of Early Universe Black Hole

Posted on June 15, 2026 by Igor Mitreski

Astronomers have long been captivated by a mysterious cluster of faint red objects known as “little red dots,” discovered by the NASA/ESA/CSA James Webb Space Telescope. Recently, Vasily Kokolev, an astronomer at the University of Texas at Austin, and his team utilized the Webb’s NIRCam and NIRSpec instruments to capture the deepest spectrum of a tiny red dot, named GLIMPSE-17775, ever recorded. The findings reinforce the theory that this object is a supermassive black hole enveloped in a thick cocoon of partially ionized gas, aligning with the BH* (black hole star) model.

This web image depicts the small red dot GLIMPSE-17775 behind galaxy cluster Abel S1063. Credit: NASA / ESA / CSA / Vasily Kokorev, UT Austin / Alyssa Pagan, STScI.

“There is a growing consensus in the scientific community that this little red dot can be explained by the black hole star model,” said Kokolev.

“However, none of the other little red dots have presented all the necessary evidence together until now.”

“GLIMPSE-17775 provides an exceptional opportunity to test these models due to its remarkable spectrum,” Kokolev added.

With a cosmological redshift of 3.5, GLIMPSE-17775 existed approximately 1.8 billion years after the Big Bang.

This intriguing object came into view serendipitously during Webb’s observations of the galaxy cluster Abel S1063, which aimed to identify Population III stars and faint early galaxies.

Positioned behind the star cluster, the brightness of the small red dot is enhanced through the phenomenon of gravitational lensing.

“When I first examined the spectrum, it felt like I had scattered puzzle pieces on the floor,” Dr. Kokolev remarked.

“We meticulously measured the lines, fitting the pieces together to form a cohesive picture.”

“Some initial fragments that appeared insignificant suddenly revealed a deeper connection.”

The spectroscopic data gathered by Webb contains multiple lines of evidence confirming the interpretation of GLIMPSE-17775 as a black hole star. This phenomenon occurs when a rapidly accreting black hole is shielded by a dense gas cocoon, which modifies the light emitted near the black hole, producing distinct spectral features.

“Everything aligns perfectly, and this adds depth to our understanding of the universe,” Kokolev expressed.

“In the future, I aspire to delve deeper into what powers the core of this little red dot.”

“While we believe it is a black hole, alternative theories are also intriguing and deserve consideration.”

“We anticipate that, within a year or two, we will have a definitive understanding of the energy sources that drive these phenomena.”

Details from the team’s findings will be published in the Astrophysical Journal.

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Vasily Kokolev and colleagues. 2026. Insights into the dense gas cocoon surrounding GLIMPSE-17775. APJ 1004, 153; doi: 10.3847/1538-4357/ae4ed7.

Source: www.sci.news

Webb Space Telescope Discovers Methane in Interstellar Comet 3I/ATLAS

Posted on June 2, 2026 by Igor Mitreski

Utilizing spectral data from the Mid-Infrared Instrument (MIRI) on the NASA/ESA/CSA James Webb Space Telescope, astronomers have successfully detected methane in the interstellar object 3I/ATLAS. This marks the first direct observation of methane in such an object.

Hubble captured this image of 3I/ATLAS on July 21, 2025, when the comet was 446 million kilometers (277 million miles) from Earth. Image credits: NASA/ESA/David Jewitt, UCLA/Joseph DePasquale, STScI.

“Interstellar objects (ISOs) are planetesimals that originate around distant stars and are subsequently ejected from their formation systems,” explained Matthew Belyakov, an astronomer at the California Institute of Technology.

“During its brief passage through our solar system, 3I/ATLAS provides a unique insight into a population of small extrasolar objects, serving as a valuable reference for understanding the processes of planetesimal formation throughout the galaxy.”

3I/ATLAS is now recognized as the third confirmed interstellar object, following 1I/’Oumuamua and 2I/Borisov, featuring an estimated core diameter of 2.6 km (1.6 miles).

Unlike 1I/’Oumuamua, which appeared inactive, 3I/ATLAS has persisted in a comatose state for some time.

“Concerted efforts are currently underway to analyze the chemical composition of the 3I/ATLAS coma,” the astronomers noted.

“Ground-based spectroscopy has identified gaseous cyanide and atomic nickel, while radio observations with ALMA have detected methanol and hydrogen cyanide in the molecular inventory.”

“Near-infrared space-based observations before perihelion with Webb and SPHEREx have revealed fluorescence signatures from water, carbon dioxide, and carbon monoxide.”

“Post-perihelion SPHEREx measurements indicated a notable increase in carbon monoxide production along with additional emission features in the 3.2-3.4 μm range, likely linked to organic material.”

“Further indicators of evolving activity in 3I/ATLAS include a bluish hue and noticeable asymmetry between pre-perihelion and post-perihelion water production trends.”

This image displays 3I/ATLAS, as captured by Webb’s MIRI instrument, with contour lines illustrating the presence of various gases. Water vapor, predominantly from comatose ice particles, extends beyond the core, while carbon dioxide and methane are concentrated closer to it. The spectrum below labels the signature gases escaping from the comet. Image credits: NASA/ESA/CSA/STScI/M. Belyakov, Caltech/I. Wong, STScI/A. Pagan, STScI.

The recent observations from Webb were conducted using the MIRI instrument on two separate occasions, capturing 3I/ATLAS as it orbited the Sun and subsequently retreated from the solar system.

The initial observation occurred between December 15 and 16, 2025, when the comet was approximately 329 million km (205 million miles) from the Sun. A second observation followed on December 27, when the comet had retreated to around 379 million km (236 million miles).

“Methane is highly volatile, transitioning from solid ice to gas with ease,” the researchers stated.

“The late emergence of methane in Comet 3I/ATLAS indicates that the substance is likely buried beneath a surface layer, shielded from sublimation until the comet’s proximity to the Sun warms the deeper icy layers.”

“The ratio of methane relative to water found is unexpectedly high and shares few parallels in our solar system.”

3I/ATLAS was already noted for its unusual carbon-rich composition, and Webb’s observations have confirmed it remains distinct.

This comet consistently exhibits significantly higher levels of carbon dioxide compared to water, in contrast to typical comets in our solar system.

The presence of methane and carbon dioxide suggests a different origin narrative than those formed around the Sun.

“Additionally, Webb’s observations revealed a rapid decrease in gas production as Comet 3I/ATLAS moved away from the Sun, with water showing the most considerable decline,” the scientists explained.

“Such behavior is expected for an object like this. As the comet receives less solar heat, its surface cools, resulting in diminished ice evaporation.”

A study detailing these findings is set to be published on April 8, 2026, in the Astrophysical Journal Letter.

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Matthew Belyakov et al. 2026. Volatile inventory of 3I/ATLAS as observed by JWST/MIRI. APJL 1001, L11; doi: 10.3847/2041-8213/ae5700

Source: www.sci.news

Webb Telescope Uncovers Supermassive Black Hole Older than Its Host Galaxy

Posted on May 29, 2026 by Igor Mitreski

Astronomers utilizing NASA/ESA/CSA’s James Webb Space Telescope have made a groundbreaking discovery of a massive black hole in the early universe, which intriguingly appears to be older than its host galaxy. This revelation raises significant questions about the formation of the universe’s first supermassive black holes.

This Webb/NIRCam image captures the small red dot Abell2744-QSO1, magnified and triple-imaged by the galaxy cluster Abell 2744. Image credits: NASA / ESA / CSA / Lukas Furtak, Ben-Gurion University / Alyssa Pagan, STScI.

Abel 2744-QSO1 (commonly referred to as QSO1) is a typical “little red dot” existing just 700 million years post-Big Bang.

Though QSO1 spans only 1,300 light-years and its light has traveled over 13 billion years, it offers a more accessible study compared to other small red dots due to its gravitational lensing by the galaxy cluster Abel 2744.

QSO1 is uniquely magnified and appears in three locations in the sky, thanks to this lensing effect.

Dr. Roberto Maiorino from the University of Cambridge stated, “This is a remarkable discovery that represents a paradigm shift in understanding black hole formation and growth.”

Initial studies suggest QSO1 may consist of a cloud of glowing hydrogen and helium gas orbiting a supermassive black hole approximately 40 million times the mass of our Sun.

However, uncertainty lingered regarding the true scale of this black hole, similar to other early black holes discovered by Webb.

Dr. Francesco Deugenio of the University of Cambridge remarked, “Until now, measurements of black hole masses in the early universe have been indirect, based on established knowledge of local black holes.”

Researchers have employed the Integral Field Unit (IFU) of Webb’s NIRSpec instrument to effectively map the movement of hydrogen gas around this black hole.

They observed that gas exhibited Keplerian motion, indicating it orbits a central point much like planets orbit the Sun in our solar system.

Ignas Giouojuvaris, a graduate student at the University of Cambridge, added, “This finding indicates that most of QSO1’s mass is concentrated in the central black hole.” If the mass were dispersed like many stars, the gas wouldn’t exhibit such precise Keplerian rotation.

Using these gravity-driven Keplerian motions, researchers could directly calculate the black hole’s mass through gas velocity measurements, a feat previously unattainable.

The black hole was found to be around 50 million solar masses, astonishingly accounting for two-thirds of QSO1’s total mass—thousands of times larger than proportions found in nearby galaxies, where supermassive black holes typically comprise only a small fraction of their host galaxies.

The IFU configuration map supported these observations, revealing that QSO1’s gas is primarily hydrogen and helium, with minimal heavy elements like oxygen, expected in a star-rich galaxy.

With less than 0.5% of the Sun’s metallicity, QSO1 stands as one of the most pristine galactic environments ever analyzed.

Dr. Cosimo Marconcini, an astronomer at the University of Florence, proclaimed, “This is an extraordinary result—marking the first direct measurement of a black hole’s mass within the first billion years post-Big Bang, aligning with prior indirect measurements.”

The extraordinary mass of QSO1 relative to its host galaxy implies it could not have formed gradually through the merging and feeding of smaller stellar-mass black holes.

Giouojuvaris noted, “We might be witnessing a black hole that lacks a substantial host galaxy and predates stellar processes.” This offers compelling evidence for the existence of primordial black holes and direct collapse black holes, concepts previously theorized but not substantiated.

Whether the black hole in QSO1 originated as a massive seed shortly after the Big Bang or emerged later from the collapse of a giant gas cloud, it likely formed large and may be in the initial stages of cultivating a galaxy around it.

These findings are documented in two research papers: the journal Nature and Royal Astronomical Society Monthly Notices.

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I. Juojubaris et al. 2026. Direct measurements of black hole masses in small red dots at high redshifts. Nature 653, 1017-1021; doi: 10.1038/s41586-026-10579-4

Roberto Maiorino et al. 2026. A black hole in a nearly primordial galaxy 700 million years post-Big Bang. MNRAS 548 (1): staf2109;doi: 10.1093/mnras/staf2109

Source: www.sci.news

Webb Telescope Identifies Methane in Exoplanet Saturn TOI-199b’s Atmosphere

Posted on May 26, 2026 by Igor Mitreski

Astronomers have harnessed spectral data from the Near Infrared Spectrometer (NIRSpec) on board the NASA/ESA/CSA James Webb Space Telescope to investigate the atmosphere of TOI-199b, a distant Saturn-mass exoplanet that is neither frigid nor scorching.

Artist’s impression of a gas giant exoplanet. Image credit: Sci.News.

TOI-199, a G-type star situated approximately 330 light-years away in the constellation Sera, hosts at least two massive planets: TOI-199b and TOI-199c.

The inner planet, TOI-199b, orbits its host star, receiving 2.5 times more radiation than Earth every 105 days, resulting in an estimated temperature of 352 K (79 degrees Celsius, or 174 degrees Fahrenheit).

With a mass of 0.17 times that of Jupiter and a radius of 0.81 times that of Jupiter, TOI-199b is inferred to have a Saturn-like internal structure and a hydrogen-rich atmosphere.

“TOI-199b is one of the most promising cold giant planets for atmospheric characterization,” stated Penn State astronomer Renyu Hu and colleagues.

Astronomers employed transmission spectroscopy to scrutinize light emitted from the star as it traversed the planet’s atmosphere, enabling the characterization of TOI-199b’s atmospheric composition.

“Our analysis revealed that the wavelengths of starlight absorbed by methane were blocked by the atmosphere,” explained Dr. Aaron Bello Alfe, a postdoctoral researcher at NASA’s Jet Propulsion Laboratory.

“Compositional models for temperate gas giant exoplanets indicated the likely presence of methane, so confirming this theory is a significant milestone.”

Webb’s observations also indicated that TOI-199b’s atmosphere contains ammonia and carbon dioxide in addition to methane.

“Further observations will enhance our understanding of the relative abundances of these gases,” noted Dr. Hu.

A comprehensive examination of temperate gas giants could refine our models and deepen our understanding of planetary formation and atmospheric evolution, including that of Earth.

“The success of this preliminary investigation encourages us to allocate more observational resources to study similar planets,” added the team.

This will enable us to determine whether TOI-199b is unique or if shared characteristics exist among planets of this type.

The team’s results were published in the May 20th issue of astronomy magazine.

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Aaron Bello-Alfe et al. 2026. Methane from the temperate exoplanet Saturn TOI-199b. A.J. 171,354; doi: 10.3847/1538-3881/ae4fba

Source: www.sci.news

Gemini North Telescope Explores the Mysteries of the Crystal Ball Nebula

Posted on May 22, 2026 by Igor Mitreski

Stunning new images captured by the 8.1-meter Gemini North telescope on Mauna Kea, Hawaii, showcase the Crystal Ball Nebula in remarkable detail. This glowing, lumpy mass of gas is intricately shaped by a pair of stars.

This captivating image of the Crystal Ball Nebula was taken by the International Gemini Observatory’s 8.1 m Gemini North Telescope. Image credit: J. Miller & M. Rodriguez, International Gemini Observatory & NSF’s NOIRLab / TA Rector, University of Alaska Anchorage & NSF’s NOIRLab / D. de Martin & M. Zamani, NSF’s NOIRLab.

The Crystal Ball Nebula, located approximately 1,500 light-years away in the constellation Taurus—near the border of Perseus—is officially designated as NGC 1514.

Discovered on November 13, 1790, by the renowned German-British astronomer William Herschel, this nebula is a breathtaking example of celestial beauty.

Utilizing the Gemini Multi-Object Spectrograph (GMOS), the latest images of the Crystal Ball Nebula were captured by the Gemini North Telescope, part of the International Gemini Observatory funded by the NSF and operated by NSF’s NOIRLab.

NOIRLab astronomers classify the Crystal Ball Nebula as a planetary nebula, a term first introduced by Herschel himself. He recognized the spherical shape of these objects in the 1700s, coining the term due to their resemblance to planets—despite the fact that they are entirely unrelated.

Planetary nebulae are formed when a low- or intermediate-mass star expels its outer layers towards the end of its life, creating a spherical gas cloud.

Unlike many planetary nebulae, which typically have smoother shapes, the Crystal Ball Nebula is characterized by its uniquely bumpy gas shells.

As the central star releases this gas, its inner core becomes exposed, with radiation from the core energizing the gas to scorching temperatures, resulting in a colorful glow. For instance, the Crystal Ball Nebula’s temperature is estimated to be around 15,000 K.

Herschel was captivated by the nebula’s dimly lit shell; before his discovery, he believed nebulae to be merely distant collections of stars.

The bright spot at the center of the gaseous shell contradicted this theory. Herschel noted, in 1791: ‘Our judgment, we may venture to say, and it will be, is that the nebula around this star is not of a stellar nature.’

He theorized that the light emanating from the Crystal Ball Nebula originated from a single star, rather than a group of distant stars.

Although the new images may depict a singular bright source at the center—similar to Herschel’s observations—the Crystal Ball Nebula actually harbors two stars.

These two stars form a binary pair that orbits each other with a period of approximately nine years, marking it as the longest known binary star pair within a planetary nebula, according to the astronomers.

Source: www.sci.news

Hubble Space Telescope Explores Galaxy After Starburst Event

Posted on May 19, 2026 by Igor Mitreski

NGC 1266 is a fascinating cosmic object frozen between two identities, offering astronomers insights into the cessation of star formation.

This Hubble image illustrates lenticular galaxy NGC 1266, showcasing reddish-brown dust clumps that obscure its surface while distant galaxies radiate red, blue, and orange light. Image credits: NASA/ESA/K. Alatalo, STScI/G. Kober, NASA, and The Catholic University of America.

Located approximately 100 million light-years away in the constellation Eridanus, NGC 1266 is a distinguished lenticular galaxy.

Astronomers classify NGC 1266 as a transitional galaxy, serving as an evolutionary bridge between spiral and elliptical galaxies.

“The lenticular shape features a bright central bulge with a spiral-like disk, yet lacks spiral arms and minimal elliptical star formation,” Hubble experts explained.

“While its structure and classification are intriguing, they are not the galaxy’s most remarkable attributes.”

“NGC 1266 is identified as a rare post-starburst galaxy, positioned in the transition between galaxies that have experienced significant star formation and quieter elliptical galaxies,” the researchers noted.

Post-starburst galaxies, which comprise about 1% of the local galaxy population, boast young stars but few active star-forming regions.

Approximately 500 million years ago, NGC 1266 experienced a minor merger with another galaxy.

“This merger triggered new star formation and injected gas into the supermassive black hole, thus augmenting the mass of the galaxy’s central bulge,” astronomers reported.

“The influx of material heightened the activity of the black hole, leading to the formation of an active galactic nucleus.”

“This increased black hole activity likely generated powerful winds and jets of gas along its rotation axis.”

Over time, the explosive formation of new stars and the black hole’s powerful jets depleted the galaxy’s star-forming gas, while turbulence from these processes impeded further star formation.

Through observations from Hubble and other telescopes, astronomers discovered strong gas outflows from NGC 1266 and significant disturbances in its interstellar space.

Their findings revealed that star nurseries are concentrated in the galaxy’s center, with little to no star formation occurring beyond that region.

“These observations imply that supermassive black holes at galaxy centers may inhibit star birth by stripping or ejecting star-forming gas,” the researchers concluded.

“The shock waves produced by this activity generate turbulence that disrupts the interstellar gas and dust, preventing the remaining material from condensing into new stars.”

Source: www.sci.news

Webb Space Telescope Uncovers Early Universe’s Slow-Rotating Galaxies

Posted on May 5, 2026 by Igor Mitreski

In the vastness of today’s universe, galaxies predominantly exhibit ordered rotation. However, among the largest star systems, those that do not form new stars are often influenced by chaotic stellar motion. Astronomers refer to these galaxies as slow-rotators. While fast-rotating systems are frequently observed, slow-rotators are believed to be rare, especially in the early universe. Recent findings from the NASA/ESA/CSA James Webb Space Telescope have illuminated a slowly rotating giant galaxy known as XMM-VID1-2075, located at redshift z = 3.449, which means we are observing a galaxy that is approximately 12 billion years old.

The Webb/NIRSpec/IFU image depicting the slowly rotating galaxy XMM-VID1-2075. Credit: Forest et al., doi: 10.1038/s41550-026-02855-0.

Current astronomical theories indicate that the first galaxies formed through the acquisition of angular momentum from inflowing gas, coupled with gravitational forces causing them to rotate.

Over billions of years, many galaxies—particularly those within clusters—undergo numerous mergers. These interactions lead to their combined rotations either enhancing or partially countering each other.

This phenomenon explains why some galaxies nearest to Earth display minimal overall rotation, yet contain considerable random stellar movement.

The discovery of XMM-VID1-2075 as a slow rotator is surprising, especially considering it reached this state when the universe was less than 2 billion years old.

“This invariant characteristic can typically only be observed in the most massive, mature galaxies closer to us in space and time,” stated Ben Forrest, an astronomer from the University of California, Davis.

“It was particularly striking that we found this galaxy exhibiting no indications of rotation, which raises intriguing questions.”

Ben Forrest and his team, part of the MAGAZ3NE (z>3 NEar-Infrared Giant Ancient Galaxies) survey, had previously conducted observations of XMM-VID1-2075 at the WM Keck Observatory in Hawaii.

“Earlier MAGAZ3NE observations confirmed that this galaxy ranks among the most massive in the early universe, possessing several times the number of stars as the Milky Way and not forming any new stars, making it an exceptional candidate for further study,” Dr. Forrest added.

Astronomers utilized the NASA/ESA/CSA James Webb Space Telescope to evaluate the relative motion of matter within XMM-VID1-2075, along with two other similarly aged galaxies.

“Conducting this type of analysis is standard for nearby galaxies due to their proximity and size, allowing for ground-based studies. Nevertheless, it’s challenging with high-redshift galaxies since they appear much smaller from our vantage point,” Dr. Forrest explained.

“The Webb Telescope is pioneering new research frontiers in this field.”

“Among the three galaxies we examined, one displayed clear rotation, one exhibited a somewhat chaotic pattern, while one showed no rotation but random stellar movement.”

“This pattern aligns with the characteristics of some of the most massive galaxies in our local universe, yet the early discovery of this slow rotator is quite unexpected.”

What led to the formation of this slow-rotating galaxy in under 2 billion years?

One hypothesis is that XMM-VID1-2075’s slow rotation may not stem from multiple mergers, but rather a singular collision between two galaxies rotating in nearly opposite directions, a notion supported by the team’s observations.

“In this galaxy, we observe a significant excess of light on one side,” Dr. Forrest noted.

“This suggests that an additional entity may be interacting with the system, potentially altering its dynamics.”

This groundbreaking research is detailed in the following paper published in Nature Astronomy.

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B. Forrest et al.. Discovery of a massive, slowly rotating galaxy from the early universe. Nat Astron, published online May 4, 2026. doi: 10.1038/s41550-026-02855-0

Source: www.sci.news

NASA Telescope Reveals 10,000 New Planets: A Groundbreaking Discovery

Posted on April 27, 2026 by Igor Mitreski

Stunning Artist’s Impression of a Star with Two Exoplanets Transiting

Credit: NASA, ESA, and G. Bacon (STScI)

Artist's impression of a star with two planets transiting it — Stunning Artist’s Impression of a Star with Two Exoplanets Transiting

Credit: NASA, ESA, and G. Bacon (STScI)

Astronomers have discovered over 10,000 candidate planets using data from NASA’s telescopes, representing the largest number ever noted in a single observation.

NASA’s Transiting Exoplanet Survey Satellite (TESS), launched in 2018, specializes in searching for exoplanets—planets orbiting stars outside our solar system. Exoplanets are detected by observing temporary decreases in brightness from stars, indicating that an orbiting planet has moved in front of the star.

To date, TESS has confirmed more than 750 exoplanets, with thousands more candidates awaiting validation. The aggregate number of confirmed exoplanets by various telescopes has now surpassed 6,000.

Joshua Roth and researchers at Princeton University reported an even higher potential count by re-evaluating TESS’s first year of data. By merging images from different telescopes, they identified planets that are less luminous, whether due to their smaller size or greater distance from Earth. This effort has uncovered 11,554 candidate exoplanets, 10,091 of which weren’t previously acknowledged.

“Predictions indicated there were likely thousands of undiscovered planets within TESS data,” says Roth. “We simply hadn’t searched thoroughly enough yet.”

These newly identified planets extend up to 6,800 light-years from Earth, reaching deeper into the galaxy than TESS previously could. More than 90% of these new findings are categorized as ‘hot Jupiters’, gas giants orbiting extremely close to their stars in just a few days. TESS is particularly adept at detecting such worlds. Smaller variants, including Neptune-like planets and super-Earths, are also among the findings.

However, not all candidates are confirmed exoplanets. Each must be monitored using additional telescopes, as some signals may be false positives due to factors like binary stars. “The false positive rate for TESS is typically around 50%,” Roth states, estimating there could be a maximum of 5,000 genuine planets, but cautions that perhaps only 3,000 truly exist.

Nonetheless, this wealth of data could effectively double the known exoplanet count in the universe. Jesse Christiansen, the lead scientist at NASA’s Exoplanet Science Institute, emphasizes the importance of these discoveries for understanding exoplanet formation. “The more exoplanets we have, the better we can analyze and differentiate them,” she notes, highlighting the diverse types of ‘Jupiters’ different stars produce. “These are essential questions we can address with a sizable sample.”

Additionally, there are many more planets in the TESS data that await discovery, including around 8,000 previously identified candidates still under investigation. “We always anticipated that eventually thousands of planets would be revealed,” Christiansen predicted, suggesting that TESS could ultimately confirm between 12,000 and 15,000 planets. “I’ve eagerly awaited a document like this for quite some time.”

Topics Covered:

Source: www.newscientist.com

Webb Telescope Unveils Ice Clouds on Distant Jupiter-Like Exoplanet

Posted on April 24, 2026 by Igor Mitreski

Astronomers utilizing NASA/ESA/CSA’s James Webb Space Telescope have discovered swirling clouds of water ice in the atmosphere of Epsilon Indi Ab, a cold super-Jupiter that challenges current models of giant planetary atmospheres.

An artist’s impression of Epsilon Indi Ab with water clouds above an ammonia-based atmosphere. Image credit: EC Matthews, MPIA / T. Müller, HdA.

Epsilon Indi A, a K5V star located about 12 light-years from Earth in the southern constellation Indus, is home to Epsilon Indi Ab.

This star, also known as HD 209100 or HIP 108870, is estimated to be between 3.7 and 5.7 billion years old.

Slightly less massive and cooler than the Sun, Epsilon Indi A is orbited by Epsilon Indi Ab, a gas giant planet several times more massive than Jupiter.

Epsilon Indi Ab has a surface temperature ranging from 200 to 300 K (approximately -70 to 20 degrees Celsius).

This planet is warmer than Jupiter (140 K, -133 degrees Celsius) due to residual heat from its formation.

Over millions of years, Epsilon Indi Ab is expected to cool further, eventually dropping below Jupiter’s temperature.

“With a mass of 7.6 times that of Jupiter, Epsilon Indi Ab is significantly more massive, yet its diameter is comparable to Jupiter,” stated Dr. Bhavesh Rajput, a student at the Max Planck Institute for Astronomy.

Rajput et al. utilized Webb’s Mid-Infrared Instrument (MIRI) to capture direct images of Epsilon Indi Ab.

They also estimated the ammonia content in its atmosphere.

“For Jupiter, both ammonia gas and clouds dominate the observable upper atmosphere,” the researchers noted.

“Epsilon Indi Ab was presumed to have large amounts of ammonia gas; however, clouds consisting of ammonia were not detected.”

“Intriguingly, our photometric analysis revealed lower ammonia levels than anticipated.”

A likely explanation is the presence of thick yet patchy clouds of water ice, akin to high-altitude cirrus clouds on Earth.

“This discovery poses significant implications and highlights the advancements being made with Webb,” commented Dr. James Mang, an astronomer at the University of Texas at Austin.

“What was once invisible is now within our view, offering insights into atmospheric structures, including cloud formations.”

“This new complexity adds layers to our atmospheric models, allowing for further detailed analyses of these cold, distant exoplanets.”

These findings will be published in the Astrophysics Journal Letter.

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Elizabeth C. Matthews et al. 2026. JWST’s second examination of Epsilon Indi Ab: New photometric data confirms ammonia presence and suggests thick cloud layers in the exoplanet’s atmosphere. APJL 1002, L5; doi: 10.3847/2041-8213/ae5823

Source: www.sci.news

Hubble Space Telescope Captures Stunning Images of IC 486

Posted on April 3, 2026 by Igor Mitreski

The Hubble team has unveiled a stunning close-up image of the barred spiral galaxy IC 486.

This captivating Hubble image portrays IC 486, a barred spiral galaxy approximately 380 million light-years away in the constellation Gemini. Image credits: NASA / ESA / Hubble / MJ Koss / AJ Barth.

IC 486 is situated in the constellation Gemini and lies about 380 million light-years from Earth.

This galaxy, recognized by other designations such as LEDA 22445, IRAS 07572+2645, and UGC 4155, was discovered on March 6, 1891, by Austrian astronomer Rudolf Ferdinand Spitaler.

IC 486 features a striking central rod-like structure, from which spiral arms extend and wrap around the core in a cohesive, ring-like formation.

According to Hubble astronomers, “Hubble’s advanced imaging technology reveals subtle color variations throughout IC 486.”

The core displays a blue-white hue dominated by older stars, while faint bluish areas within the surrounding disk indicate regions of more recent star formation.

“Dust lanes weave through the galaxy, gently obscuring light and pinpointing areas enriched with molecular gas where new stars are likely to emerge,” they noted.

The center of the galaxy emanates a distinctive white glow, which surpasses the surrounding stellar light. This glow originates from IC 486’s active galactic nucleus (AGN), powered by a supermassive black hole that is over 100 million times the mass of the Sun.

“All sufficiently large galaxies harbor supermassive black holes at their cores, but some are particularly voracious, consuming significant amounts of gas and dust, forming swirling accretion disks from which they derive their energy,” the astronomers elaborated.

“The immense heat generated by the orbiting material produces intense radiation, including X-rays, that can outshine the entire galaxy.”

Such galaxies, characterized by their central AGN, are referred to as active galaxies.

Despite IC 486’s orderly appearance, “it is a dynamic system shaped by gravitational forces and the evolution of stars,” they concluded.

“Over millions of years, stars are born, age, and perish, contributing to the ongoing narrative of galactic evolution in our universe.”

Source: www.sci.news

Hubble Space Telescope Returns to the Famous Crab Nebula: A New Look at an Iconic Astronomical Marvel

Posted on March 24, 2026 by Igor Mitreski

By analyzing new observations from Hubble alongside images captured in 1999, astronomers have successfully tracked the continuing expansion of one of the sky’s most studied supernova remnants, the Crab Nebula. This expansion is fueled by a rapidly spinning pulsar at its core.

This captivating image of the Crab Nebula was taken by the NASA/ESA Hubble Space Telescope in 2024. Image credit: NASA/ESA/STScI/William Blair, JHU/Joseph DePasquale, STScI.

In 1054, astounded Chinese astronomers witnessed a remarkably bright nova, the second brightest object in the night sky after the moon, visible even during the daytime for a remarkable 23 days. Observations of this supernova were also documented by Japanese, Arabian, and Native American astronomers.

Today, the luminous Crab Nebula, also known as Messier 1, M1, NGC 1952, or Taurus A, occupies the position of that brilliant star, situated approximately 6,500 light-years away in the constellation Taurus.

This nebula’s brightness makes it visible even through amateur telescopes, making it a popular object for stargazers.

Initially identified in 1731 by the English physicist and astronomer John Beavis, the Crab Nebula was later rediscovered in 1758 by French astronomer Charles Messier.

The name “Crab Nebula” derives from its resemblance in an 1844 painting by Irish astronomer Lord Rose.

At its center lies the remnant core of the original star, known as the Crab Pulsar (PSR B0531+21).

“We often perceive the sky as a static body,” remarked Dr. William Blair, an astronomer at Johns Hopkins University. “However, the enduring journey of the NASA/ESA Hubble Space Telescope has shown us that the Crab Nebula continues to evolve and expand from the explosion that occurred nearly 1,000 years ago.”

In the latest images, Hubble revealed the nebula’s intricate filament structure, demonstrating substantial outward movement over a 25-year period at an astonishing rate of 5.6 million kilometers per hour (3.4 million miles per hour).

“Hubble possesses the unique longevity and resolution necessary to capture these intricate changes,” the astronomers noted.

To facilitate comparisons with new images, Hubble’s 1999 image of the Crab Nebula has undergone reprocessing.

“The color variations observed in both Hubble images signal changes in the gas’s local temperature, density, and chemical composition.”

“Even after extensive work with Hubble, I’m continually amazed by the detailed structure and improved resolution revealed by Hubble’s Wide Field Camera 3 (WFC3) compared to 25 years ago,” Dr. Blair commented.

“WFC3 was installed in 2009, marking the last time Hubble’s instrument was upgraded by astronauts.”

“The filaments at the edges of the nebula seem to be moving more rapidly than those at the center and appear to be expanding outward instead of stretching over time.”

This phenomenon is attributed to the pulsar’s nature as a pulsar wind nebula, driven by synchrotron radiation generated from interactions between the pulsar’s magnetic field and the surrounding nebula material.

In contrast, other notable supernova remnants typically expand in a manner influenced by shock waves from the initial explosion, which erode the outer shell of gas ejected by the dying star.

The new high-resolution observations from Hubble also offer deeper insights into the Crab Nebula’s three-dimensional structure, challenging to assess from two-dimensional images.

In an intriguing observation, shadows of some filaments are reflected in the haze of synchrotron radiation within the nebula.

Interestingly, some bright filaments in the latest Hubble images do not display shadows, suggesting they are located behind the nebula.

“The true significance of Hubble’s observations of the Crab Nebula is yet to unfold,” the researchers asserted.

“Data from Hubble can be integrated with recent findings from other telescopes observing the Crab Nebula across varying wavelengths of light.”

“NASA/ESA/CSA’s James Webb Space Telescope is set to release infrared light observations of the Crab Nebula in 2024.”

Comparing Hubble’s images with modern multiwavelength observations will provide scientists with a comprehensive understanding of the ongoing aftermath of supernovae, continuing to intrigue astronomers long after new stars first appeared in the sky.

Find more findings published in January 2026. Astrophysical Journal.

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William P. Blair et al. 2026. Revisiting the Crab Nebula using HST/WFC3. APJ 997, 81; doi: 10.3847/1538-4357/ae2adc

Source: www.sci.news

Stunning Telescope Capture: Mysterious Comet’s Collapse Revealed After Serendipitous Breakthrough

Posted on March 23, 2026 by Igor Mitreski

Stunning Capture of Comet K1 by Hubble

Image Credit: NASA, ESA, Dennis Bodewits (Australia)

Comet K1 captured by the Hubble Space Telescope — Stunning Capture of Comet K1 by Hubble

Image Credit: NASA, ESA, Dennis Bodewits (Australia)

Recently, we were fortunate to observe Comet K1 just after it fragmented into four pieces. This event could offer crucial insights into the formation and evolution of our solar system.

John Noonan and researchers from Auburn University in Alabama had initially aimed to study a different comet using the Hubble Space Telescope. However, due to the spacecraft’s limitations in high-speed orbiting, they redirected their focus to a new target—comet C/2025 K1 (ATLAS). Upon directing Hubble towards K1, they were surprised to find it had already split into four distinct fragments.

“While we have observed comets break apart before, this was the first time we didn’t anticipate it occurring during our observations,” Noonan shared. “The ability to capture these images was incredibly fortunate.”

These unprecedented images of a freshly shattered comet provide invaluable data. Typically, it is challenging to predict when a comet will begin to splinter, let alone align a space telescope to capture the moment. However, the high-resolution images acquired allowed researchers to estimate that K1 began to fracture approximately a week prior to the images being taken.

Observations of Comet K1 Over Three Days

Image Credit: NASA, ESA, Dennis Bodewits (Australia)

Comets consist of primordial ice from the early solar system, yet their surfaces erode over time due to solar radiation and other cosmic effects. To uncover this primordial ice and gain insights into planetary formation, we must delve beneath the surface—a task that shattered comets facilitate.

As a comet disintegrates, it releases ice that transitions into gas, diffusing into space. “These extremely cold ice remnants are suddenly exposed to warmth for the first time in billions of years and should rapidly subliminate,” Noonan explained. Surprisingly, in the case of K1, it took about two days post-fragmentation for brightness to emerge, typically indicating sunlight interacting with sublimated gases and dust.

The reason for this unexpected delay remains unclear. Noonan and his team are currently analyzing the remaining data from K1, which is anticipated to clarify the delay in brightening and reveal the comet’s internal composition. “We are poised to embark on groundbreaking research regarding this comet and early solar system dynamics,” he stated.

Topic:

Source: www.newscientist.com

Webb Telescope Discovers Progenitor Star of NGC 1637 Supernova

Posted on February 24, 2026 by Igor Mitreski

Astronomers utilizing the NASA/ESA/CSA James Webb Space Telescope have made a groundbreaking discovery: they have identified a nearby supernova, specifically a red supergiant star, that was obscured by a thick layer of dust and remained invisible to prior observatories.

This striking image combines observations from both the James Webb Space Telescope and Hubble, focusing on spiral galaxy NGC 1637. It captures the evolutionary stages of the red supergiant star and reveals its transformation following the supernova event SN 2025pht. Image credit: NASA/ESA/CSA/STScI/C. Kilpatrick, Northwestern/A. Suresh, Northwestern/J. DePasquale, STScI.

The supernova event, designated SN 2025pht, was first identified in NGC 1637 on June 29, 2025.

In response, astronomers dedicated substantial resources to investigating this supernova.

However, Northwestern University’s astronomer Charlie Kilpatrick and his team chose to explore archival data, analyzing pre-supernova images to determine which star exploded.

A 2024 image of NGC 1637 captured with Webb’s MIRI (Mid-Infrared Instrument) and NIRCam (Near-Infrared Camera) highlights a distinct red supergiant star positioned precisely where SN 2025pht is currently visible.

“We anticipated this moment, hoping for a supernova to occur in a galaxy that Webb was already monitoring,” stated Dr. Kilpatrick.

“By integrating the Hubble and Webb datasets, we unveiled the star’s complete characteristics for the first time.”

“This red supergiant represents the dustiest star we have ever observed transitioning into a supernova,” noted Aswin Suresh, a graduate student at Northwestern University.

This dust anomaly may help solve a persistent mystery in astronomy: the absence of certain red supergiant stars.

Astronomers expect that the most massive stars should explode as the brightest supernovae, making their identification in pre-explosion images straightforward. However, this has not been the case.

One possible explanation is that these massive, aging stars are often heavily surrounded by dust, rendering their light invisible.

Observations from Webb regarding SN 2025pht seem to support this hypothesis.

“I have advocated for this interpretation, but I didn’t expect the outcome to be as pronounced as in the case of SN 2025pht,” commented Dr. Kilpatrick.

“This might clarify the absence of these heavier supergiant stars, as they tend to be engulfed in more dust.”

The team also discovered that the dust enveloping the star is likely rich in carbon—an unexpected finding, as silicate-rich dust is typically anticipated in these environments.

They speculate that this carbon may have been released from the star’s core shortly before the explosion.

“Mid-infrared observations were crucial in identifying the specific type of dust present,” Suresh added.

For more in-depth details on this discovery, view the team’s research paper published in October 2025 in the Astrophysics Journal Letter.

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Charles D. Kilpatrick et al. 2025. Type II SN 2025pht of NGC 1637: Detection of a red supergiant star with carbon-rich circumstellar dust, marking the first acknowledgment of a supernova progenitor star via JWST. APJL 992, L10; doi: 10.3847/2041-8213/ae04de

Source: www.sci.news

Chandra Telescope Unveils Newborn Star Cluster in the Cocoon Nebula

Posted on February 22, 2026 by Igor Mitreski

The Chandra team has unveiled a stunning new composite image of the Cocoon Nebula, a fascinating reflection and emission nebula located in the constellation Cygnus. This image artfully combines high-energy X-rays with optical and infrared light, showcasing a vibrant population of newborn stars emerging from the surrounding clouds of dust and gas.

This composite image of the Cocoon Nebula highlights a heart-shaped formation. X-ray data from Chandra reveals a new cluster of stars, complemented by optical light from astrophotographers Michael Adler and Barry Wilson, as well as infrared data from the WISE mission. Image credits: NASA / CXC / SAO / JPL / Caltech / WISE / M. Adler / B. Wilson / L. Frattare.

The Cocoon Nebula is located approximately 2,650 light-years away in the constellation Cygnus.

This nebula, also known as IC 5146 or Colinder 470, spans 15 light-years across.

The object was first discovered by American astronomer Edward Emerson Barnard on October 11, 1893.

Chandra astronomers noted, “This image depicts the Cocoon Nebula as a vibrant, glowing heart-shaped cloud amidst a backdrop of millions of stars in the Milky Way.”

“The core of this nebula features warm reds, oranges, and golds, forming a luminous cocoon of gas and dust, with soft, uneven edges that gradually fade into the surrounding darkness.”

“Within this illuminated cloud lies a multitude of young stars, some visible as bright white or bluish dots, while others remain hidden or only detectable through X-ray light captured by NASA’s Chandra X-ray Observatory.”

“These X-rays trace a population of newly formed, highly active stars clustered near the center of the nebula,” the researchers explained.

“The heart-shaped nebula glows from a combination of light emitted by these young stars and starlight reflected by the surrounding dust.”

“Optical data from two astrophotographers, along with infrared observations from NASA’s Wide Field Infrared Surveyor (WISE), add depth and texture, unveiling a shimmering starry landscape and the dense, dusty regions where new stars are continuously forming.”

Source: www.sci.news

Webb Telescope Detects Hydrogen Sulfide Gas in Three Super-Jupiter Exoplanets

Posted on February 22, 2026 by Igor Mitreski

For the first time, astronomers utilizing NASA/ESA/CSA’s James Webb Space Telescope have detected hydrogen sulfide gas in the atmospheres of three gas giant exoplanets orbiting the star HR 8799, located in the Pegasus constellation and approximately 30 million years old. This significant finding indicates that the sulfur originated from solid materials in the protoplanetary disk where the planets formed.

Artist’s rendering of the HR 8799 planetary system during its early evolutionary stages, featuring a gas and dust disk around planet HR 8799c (Dunlap Institute for Astronomy and Astrophysics/Media Farm).

HR 8799 lies about 129 light-years away from Earth and hosts a substantial debris disk alongside four super-Jupiter planets (HR 8799b, c, d, and e).

The smallest of these gas giants is five times the mass of Jupiter, while the largest exceeds ten times Jupiter’s mass.

These exoplanets reside far from their star, with the nearest planet being situated 15 times farther from its star than Earth is from the Sun.

Unlike many exoplanets discovered through indirect data analysis, the planets in the HR 8799 system can be directly observed using ground-based telescopes.

“HR 8799 is unique as the only imaged stellar system containing four gas giant planets, although other systems have one or two larger companion stars with formation processes yet to be understood,” explained Dr. Jean-Baptiste Ruffio, an astronomer at the University of California, San Diego.

Utilizing Webb’s unprecedented sensitivity, Dr. Ruffio and colleagues conducted detailed studies of the chemical compositions of the planets HR 8799c, d, and e.

Due to the faintness of these planets—approximately 10,000 times dimmer than their host star—the researchers developed innovative data analysis techniques to isolate weak signals in the Webb data.

“Prior studies of carbon and oxygen on these planets, conducted from Earth, could originate from ice, solids, or gas in the disk, making them unreliable indicators of solid material,” noted Dr. Jerry Xuan, a postdoctoral researcher at UCLA and Caltech.

“In contrast, sulfur is distinctive because, away from the star, these planets should harbor sulfur in solid form.”

“It’s impossible for these planets to accumulate sulfur in gaseous form.”

The identification of hydrogen sulfide indicates that sulfur was gathered in solid form from materials that existed in the disk surrounding the star during the planets’ formation. These solids were assimilated as the planet formed, and the intense heat of the young planet’s core and atmosphere caused them to vaporize into the sulfur gas present today.

Notably, the sulfur-to-hydrogen and carbon-to-oxygen-to-hydrogen ratios on these planets are significantly higher than those found in stars, hinting at a distinct planetary composition.

This puzzling consistency in the enrichment of heavy elements is also observed in Jupiter and Saturn.

“The uniform enhancement of carbon, oxygen, sulfur, and nitrogen in Jupiter is complex, but observing this in another star system suggests a universal trend in planet formation, where planets naturally integrate heavy elements in nearly equal proportions,” Dr. Xuan commented.

The findings could advance the search for Earth-like exoplanets.

“The techniques used here allow for the optical and spectral separation of planets from stars, enabling detailed studies of exoplanets located far from Earth,” Dr. Xuan stated.

“While currently limited to gas giants, as telescope technology and instruments improve, scientists aim to apply these methods to Earth-like planets.”

“Locating an Earth analog is the ultimate goal of exoplanet research; however, achieving this may take decades.”

“Nevertheless, within the next 20 to 30 years, we might obtain the first spectra of an Earth-like planet, allowing us to investigate biological markers such as oxygen and ozone in its atmosphere.”

Findings detailed in the Journal of Natural Astronomy on February 9, 2026.

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J.B. Ruffio et al. “Jupiter-like homogeneous metal enrichment in a system of multiple giant exoplanets,” Nat Astron published online on February 9, 2026. doi: 10.1038/s41550-026-02783-z

Source: www.sci.news

Webb Telescope Uncovers Most Distant Jellyfish Galaxy Discovered to Date

Posted on February 22, 2026 by Igor Mitreski

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

Source: www.sci.news

Webb Telescope Uncovers Hidden Layers of Uranus’ Upper Atmosphere

Posted on February 21, 2026 by Igor Mitreski

Astronomers have successfully mapped the vertical structure of Uranus’ ionosphere for the very first time, uncovering unexpected temperature peaks, a decline in ion density, and enigmatic dark regions influenced by the planet’s unique magnetic field. These groundbreaking findings, achieved through nearly a full day of observations using the NIRSpec instrument aboard NASA/ESA/CSA’s James Webb Space Telescope, confirm a decades-long cooling trend in Uranus’ upper atmosphere and offer an unprecedented look at how this ice giant interacts with its surrounding space differently than other celestial bodies in our solar system.

Tiranti et al. mapped the vertical structure of Uranus’s upper atmosphere, revealing variations in temperature and charged particles across different heights. Image credits: NASA / ESA / CSA / Webb / STScI / P. Tiranti / H. Melin / M. Zamani, ESA & Webb.

Uranus’s upper atmosphere remains one of the least understood components in our solar system, despite its critical role in elucidating the interactions between the giant planet and its space environment.

Astronomer Paola Tiranti from Northumbria University and her team dedicated nearly an entire day to observing Uranus with Webb’s NIRSpec instrument.

They successfully measured the vertical structure of the ionosphere, the electrically charged layer of the atmosphere where auroras occur.

“This is the first time we’ve been able to visualize Uranus’s upper atmosphere in three dimensions,” Tiranti remarked.

“Utilizing Webb’s sensitivity, we can investigate how energy migrates upward through the planet’s atmosphere, even observing the effects of polarized magnetic fields.”

Measurements revealed temperature peaks at approximately 3,000 to 4,000 km above the surface, while ion density peaked around 1,000 km, significantly weaker than previously modeled predictions.

Webb also identified two bright bands of auroral emission located near Uranus’s magnetic poles, along with an unexpected area of depleted emission and density, likely tied to the planet’s unusual magnetic field geometry.

These discoveries confirm a long-term cooling trend in Uranus’ upper atmosphere and highlight new structures shaped by its magnetic environment.

These findings offer critical benchmarks for future missions and enhance our comprehension of how giant planets—both within and beyond our solar system—maintain the energy balance in their upper atmospheres.

“Uranus’ magnetosphere is one of the most peculiar in the solar system,” Tiranti emphasized.

“Its tilt and offset from the planet’s rotational axis cause its auroras to be distributed in a complex fashion across the surface.”

“Webb has provided insights into how deeply these effects penetrate into the atmosphere.”

“By detailing Uranus’s vertical structure so thoroughly, Webb aids in our understanding of the energy balance of the ice giant.”

“This represents a significant step toward characterizing giant planets beyond our solar system.”

For further details, refer to the results published in the journal Geophysical Research Letters.

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Paola I. Tiranti et al. 2026. JWST uncovers the vertical structure of Uranus’ ionosphere. Geophysical Research Letters 53 (4): e2025GL119304; doi: 10.1029/2025GL119304

Source: www.sci.news

Event Horizon Telescope Discovers Potential Origin of Messier 87 Black Hole’s Jet

Posted on February 3, 2026 by Igor Mitreski

Astronomers utilizing the groundbreaking Event Horizon Telescope—a global network of eight advanced radio telescopes—have pinpointed the likely origin of a massive space jet emanating from the core of Messier 87.

This Webb/NIRCam image showcases the extraordinary space jet of Messier 87. Image credits: Jan Röder, Maciek Wielgus, Joseph B. Jensen, Gagandeep S. Anand, R. Brent Tully.

Messier 87, a colossal elliptical galaxy situated approximately 53 million light-years away in the Virgo constellation, is of great scientific interest.

Also known as M87, Virgo A, and NGC 4486, this galaxy hosts a supermassive black hole, approximately 6 billion times the mass of our Sun.

This supermassive black hole generates a striking, narrow jet of particles that extends roughly 3,000 light-years into the cosmos.

To investigate such distant regions, astronomers are combining radio telescopes from around the world to create a virtual Earth-sized observatory known as the Event Horizon Telescope (EHT).

Using EHT observations of M87 conducted in 2021, researchers assessed the brightness of radio emissions at various spatial scales.

They discovered that the luminous ring surrounding the black hole does not account for all radio emissions, identifying an additional compact source approximately 0.09 light-years from the black hole that aligns with the predicted location of the jet’s base.

“By pinpointing where the jet originates and how it connects to the black hole’s shadow, we are adding significant insights into this cosmic puzzle,” stated Saurabh, a student at the Max Planck Institute for Radio Astronomy and a member of the EHT Collaboration.

“The newly collected data is currently undergoing analysis with contributions from international partners and will soon incorporate additional telescopes, improving our understanding of this area,” remarked Dr. Sebastiano von Fehrenberg, an astronomer at the Canadian Institute for Theoretical Astrophysics.

“This will provide us with a much clearer view of the jet’s launch region.”

“We’re transitioning from merely calculating the positions of these structures to aiming for direct imaging,” he added.

“The jet is postulated to be launched using the rotational energy of the black hole through electromagnetic processes, presenting a unique laboratory where general relativity and quantum electrodynamics intersect,” explained Professor Bert Lipperda, also from the Canadian Institute for Theoretical Astrophysics.

“Studying how jets are launched in proximity to a black hole’s event horizon is a crucial advancement in our comprehension of these cosmic titans.”

“The observational data will empower scientists to test theories regarding the interplay between gravity and magnetism in the universe’s most extreme environments, bringing us closer to understanding the ‘engines’ that shape entire galaxies.”

Find more details in the result published in the Journal on January 28, 2026, in Astronomy and Astrophysics.

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Saurabh et al. 2026. Investigation of the jet-based ejection from M87* with 2021 Event Horizon Telescope observations. A&A 706, A27; doi: 10.1051/0004-6361/202557022

Source: www.sci.news

Hubble Space Telescope Discovers Stunning Lenticular Galaxy NGC 7722

Posted on February 3, 2026 by Igor Mitreski

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.”

Source: www.sci.news

Webb Telescope Uncovers Most Distant Galaxy Yet: Meet MoM-z14

Posted on January 29, 2026 by Igor Mitreski

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.”

For more details on the discovery of MoM-z14, refer to the upcoming publication in Open Astrophysics Journal.

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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

Source: www.sci.news

Webb Telescope Unveils Most Detailed Dark Matter Map to Date

Posted on January 28, 2026 by Igor Mitreski

Utilizing the ultra-sharp images from the NASA/ESA/CSA James Webb Space Telescope, astronomers have successfully crafted a highly detailed, wide-area mass map of the Universe. This groundbreaking map reveals the intricate interweaving of dark matter and ordinary matter, stretching from the filaments of galaxies to the dense clusters. Developed as part of the COSMOS-Web survey, this new map boasts more than double the resolution of previous efforts and delves deeper into the early universe’s evolution.

This web image shows about 800,000 galaxies, overlaid with a dark matter map in blue. Image credit: NASA / STScI / J. DePasquale / A. Pagan.

Dark matter constitutes roughly 85% of the universe’s total matter, yet it’s challenging to detect since it neither emits nor absorbs light, rendering it invisible to standard telescopes.

However, its gravitational influence alters the trajectory of light from far-off galaxies.

By examining subtle distortions in the shapes of numerous distant galaxies, scientists can ascertain how this unseen mass is distributed, irrespective of its nature.

When compared with known luminous structures, researchers can pinpoint the locations of dark matter.

Previous mass maps generated using the NASA/ESA Hubble Space Telescope and other observatories suffered from limited resolution, sensitivity, and area coverage, restricting their views to only the largest cosmic structures.

Dr. Diana Scognamiglio from NASA’s Jet Propulsion Laboratory and her team harnessed Webb’s imaging capabilities to analyze the shapes of approximately 250,000 galaxies, reconstructing the most detailed mass map of a contiguous universe region to date.

“This is the most extensive dark matter map produced in conjunction with Webb, boasting clarity unmatched by any prior dark matter maps from other observatories,” stated Dr. Scognamiglio.

“Previously, we only glimpsed blurred images of dark matter.”

“With Webb’s extraordinary resolution, we can now observe the universe’s invisible framework in unprecedented detail.”

This new map uncovers substantial galaxy clusters along with intricate networks of dark filamentary bridges and low-mass galaxies, too faint or too distant to be spotted by conventional telescopes.

These formations align with major cosmological models, suggesting that galaxies emerge at dense points between the dark matter filaments spreading throughout the universe.

Dr. Gavin Leroy, an astronomer at Durham University, remarked: “By illustrating dark matter with unparalleled precision, our map demonstrates how the unseen elements of the universe shaped visible matter, facilitating the creation of galaxies, stars, and ultimately, life itself.”

“This map highlights the crucial role of dark matter, the universe’s true architect, which gradually organizes the structures we observe through our telescopes.”

Professor Richard Massey of Durham University added, “Wherever normal matter exists in the universe today, dark matter is also present.”

“Every second, billions of dark matter particles pass through your body. They are harmless and continue on their paths unnoticed.”

“However, the entire cloud of dark matter surrounding the Milky Way possesses enough gravity to keep our galaxy intact. Without dark matter, the Milky Way would disintegrate.”

For more information, refer to the published results in this week’s edition of Nature Astronomy.

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D. Scognamiglio et al. Ultra-high resolution map of (dark) matter. Nat Astron published online on January 26, 2026. doi: 10.1038/s41550-025-02763-9

Source: www.sci.news

Webb Telescope Explores a Lenticular Galaxy Cluster in the Leo Constellation

Posted on January 27, 2026 by Igor Mitreski

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 remarkable image of MACS J1149 is part of the Canadian NIRISS Unbiased Cluster Survey (CANUCS) program.

“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.

Source: www.sci.news

Exploring the Fascinating Heart of the Circus Galaxy: Insights from Webb Telescope

Posted on January 14, 2026 by Igor Mitreski

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

Source: www.sci.news

Stunning Close-Up of Arp 4 Captured by Hubble Space Telescope

Posted on December 23, 2025 by Igor Mitreski

Discover the latest stunning image captured by the NASA/ESA Hubble Space Telescope, showcasing Arp 4, an intriguing visual pair of galaxies located in the constellation Cetus.

The Hubble image captures the galaxy pair Arp 4. Image credits: NASA / ESA / Hubble / J. Dalcanton, Dark Energy Survey / DOE / FNAL / DECam / CTIO / NOIRLab / NSF / AURA.

For more details, explore Arp 4, which features the bright spiral galaxy MCG-02-05-050a alongside the larger spiral galaxy MCG-02-05-050.

Located within the constellation Cetus, this galaxy pair was first discovered by Dutch-Canadian astronomer Sidney van den Bergh in 1959.

Arp 4 stands as the fourth entry in Halton Arp’s Atlas of Peculiar Galaxies and belongs to the section focusing on “Galaxies with Low Surface Brightness.”

“The term ‘Arp 4’ derives from the Atlas of Peculiar Galaxies compiled by astronomer Halton Arp during the 1960s,” Hubble astronomers explained.

“These ‘unusual galaxies’ were chosen for photography to illustrate their distinct and non-standard shapes, providing insights into galaxy evolution.”

Hubble’s mission has transformed our understanding of galaxies, revealing captivating examples from Arp’s Atlas, including Arp 4.

The initial galaxies in this catalog, including Arp 4, exhibit low surface brightness, rendering them faint and challenging to observe.

“The larger galaxy, cataloged as MCG-02-05-050, features fragmented arms and a dim disk, perfectly fitting this description,” the astronomers noted.

“In contrast, its smaller counterpart, MCG-02-05-050a, is considerably brighter and more dynamic as a spiral galaxy.”

“Crucially, these galaxies are not in close proximity,” the researchers emphasized.

“The prominent blue galaxy, MCG-02-05-050, lies 65 million light-years from Earth.”

“Meanwhile, the brighter, smaller galaxy MCG-02-05-050a is positioned at an impressive 675 million light-years, over ten times farther away.”

This positioning likely suggests that MCG-02-05-050a is the more substantial of the two, while MCG-02-05-050 is relatively smaller.

“This visual pairing is simply an unlikely coincidence,” the astronomers added.

“Despite the absence of a physical connection, we can enjoy the unique sight of Arp 4 as an enthralling duo adorning our night sky.”

Source: www.sci.news

Hubble Space Telescope Revisits NGC 4388

Posted on December 16, 2025 by

The NASA/ESA Hubble Space Telescope has captured breathtaking new images of the intriguingly tilted spiral galaxy NGC 4388.

This Hubble image showcases spiral galaxy NGC 4388, located about 59 million light-years away in the constellation Virgo. Image credits: NASA / ESA / Hubble / S. Veilleux / J. Wang / J. Greene.

NGC 4388 is situated roughly 59 million light-years away in the constellation Virgo.

This galaxy was first identified by British astronomer Sir Wilhelm Herschel on April 17, 1784.

Also referred to as LEDA 40581 and IRAS 12232+1256, it has a diameter of 120,000 light-years.

NGC 4388 is among the brightest galaxies in the Virgo Cluster, which comprises over 2,000 galaxies.

Classified as an active galaxy, NGC 4388 features a bright and energetic core.

“NGC 4388 is tilted at a steep angle relative to our viewpoint, appearing almost face-on,” Hubble astronomers mentioned in a statement.

“This angle allows us to observe intriguing features that were not visible in earlier Hubble images of the galaxy released in 2016. A gas plume is seen emanating from the galaxy’s core, extending outward from the galaxy’s disk towards the bottom right corner of the image.”

“But where did this outflow originate? What causes it to shine?”

“The answer seems to lie in the vast spaces that separate the galaxies within the Virgo Cluster.”

“Though it may seem like the void between galaxies is empty, this area is actually filled with clusters of hot gas known as the intracluster medium.”

“As NGC 4388 traverses the intracluster medium, it punches through this gas.”

“The pressure from the hot intracluster gas forces material out of NGC 4388’s disk, trailing it as the galaxy moves.”

“The origin of the energy that ionizes this gas cloud and produces its glow remains uncertain,” the researchers observed.

“We suspect that some energy may originate from the galaxy’s center, where a supermassive black hole accelerates the surrounding gas to create a superheated disk.”

“The intense radiation emitted from this disk could ionize the gas nearest to the galaxy, while shock waves could cause filaments of gas farther out to become ionized.”

Source: www.sci.news

Gemini North Telescope Unveils New Images of 3I/ATLAS

Posted on December 13, 2025 by

On November 26, 2025, astronomers utilized the Gemini Multi-Object Spectrograph (GMOS) on the Gemini North Telescope located on Mauna Kea, Hawaii, to capture images of the interstellar comet 3I/ATLAS. Recent observations demonstrate how this comet has evolved since its closest approach to the Sun.

This image, taken with GMOS on the Gemini North Telescope, depicts 3I/ATLAS traveling among stars and galaxies. Operating as part of the International Gemini Observatory, it is funded in part by NSF and managed by NSF’s NOIRLab. Image credit: International Gemini Observatory / NOIRLab / NSF / AURA / B. Bolin / J. Miller & M. Rodriguez, International Gemini Observatory & NSF’s NOIRLab / TA Rector, University of Alaska Anchorage & NSF’s NOIRLab / M. Zamani, NSF’s NOIRLab.

3I/ATLAS reached its closest approach to the Sun, termed perihelion, on October 30, 2025.

Having emerged from behind the Sun, this interstellar body was observed near Zania, a triple star system situated in the Virgo constellation.

On November 26, 2025, researcher Bryce Bolin from Eureka Scientific, along with colleagues, obtained new images of the comet as part of a public outreach initiative by NSF NOIRLab in partnership with Shadow the Scientist.

“Providing the public with a viewing experience under optimal conditions allows for a genuine front-row glimpse of interstellar visitors,” Dr. Bolin stated.

“Offering the public insight into our work as astronomers and our methodologies also serves to demystify science and the data collection process, enhancing transparency in the study of this captivating astronomical entity.”

The 3I/ATLAS image, captured using GMOS, highlights the comet’s coma—a cloud of gas and dust that forms around its icy center when approaching the Sun. Image credit: International Gemini Observatory / NOIRLab / NSF / AURA / B. Bolin / J. Miller & M. Rodriguez, International Gemini Observatory & NSF’s NOIRLab / TA Rector, University of Alaska Anchorage & NSF’s NOIRLab / M. Zamani, NSF’s NOIRLab.

The recent GMOS image comprises exposures taken through four different filters: blue, green, orange, and red.

“During the exposure, the comet remains stationary in the center of the telescope’s field of view,” the astronomers explained.

“However, the background stars shift in relation to the comet, creating colorful streaks in the final image.”

“Initial images of the comet from the Shadow the Scientist session at Gemini South, Chile, exhibited a red hue.”

“In contrast, the new images released today display a subtle greenish glow.”

“This phenomenon results from light emitted by gases in the comet’s coma containing diatomic carbon, a reactive molecule made of two carbon atoms that emits light at green wavelengths. This gas evaporates as the comet heats up.”

“What remains uncertain is how comets behave as they move away from the Sun and cool down.”

“Many comets respond slowly to the Sun’s heat, as it takes time for the warmth to penetrate the comet’s interior.”

“Such delays could accelerate the evaporation of new compounds or potentially lead to the comet’s disintegration.”

Source: www.sci.news

Hubble Space Telescope Focuses on Markarian 178

Posted on December 9, 2025 by

Astronomers utilizing the NASA/ESA Hubble Space Telescope have captured breathtaking new images of the blue, compact dwarf galaxy Markarian 178.

This Hubble image showcases the blue compact dwarf galaxy Markarian 178. Image credit: NASA / ESA / Hubble / F. Annibali / S. Hon.

Markarian 178 is situated roughly 13 million light years away in the constellation Ursa Major.

This galaxy, commonly referred to as Mrk 178, LEDA 35684, and UGC 6541, spans a diameter of 5,700 light years.

“MRK 178 is one of over 1,500 Markarian galaxies,” stated Hubble astronomers.

“These galaxies are named after Benjamin Markarian, an Armenian astrophysicist who compiled a catalog of galaxies that exhibit unusual brightness in ultraviolet light.”

“While most galaxies appear blue due to a plethora of young, hot stars and minimal dust, Mrk 178 presents a reddish hue. This concentration of massive stars is particularly abundant in the brightest, reddish areas near the galaxy’s edge.”

“This azure nebula houses numerous unique entities known as Wolf Rayet stars.”

“A Wolf-Rayet star is a massive star whose atmosphere is expelled by intense stellar winds,” the astronomers clarified.

“Mrk 178 features such an abundance of Wolf-Rayet stars that vivid emission lines from the hot stellar winds of these stars are inscribed into the galaxy’s spectrum.”

“In this image, captured using some of Hubble’s specialized optical filters, ionized hydrogen and oxygen are notably represented as red in Mrk 178.”

“Massive stars transition into the Wolf-Rayet stage immediately before collapsing into a black hole or neutron star.”

“We understand that some event must have instigated Mrk 178’s recent surge in star formation, as Wolf-Rayet stars have lifespans of merely a few million years.”

“At first glance, it remains uncertain what is instigating this phenomenon. Mrk 178 does not appear to have any neighboring galaxies that could disrupt its gas and promote new star formation.”

“Instead, we hypothesize that either a gas cloud collided with Mrk 178, or that the gas was affected as the galaxy traversed through the intergalactic medium, energizing this small galaxy with waves of brilliant new stars.”

Source: www.sci.news

Upcoming Satellite Launch May Distort Hubble Space Telescope Images

Posted on December 4, 2025 by

Simulated representation of satellite trails contaminating images from future space telescopes

NASA/Boruff, Markham, Howell

Should space companies proceed with plans to deploy hundreds of thousands of satellites, up to a third of the images captured by the Hubble Space Telescope may be compromised.

In the last five years alone, over 75% of the approximate 14,000 satellites now orbiting Earth have been launched, many as part of megaconstellations, notably Elon Musk’s Starlink. Proposals indicate that we could see the deployment of as many as 500,000 satellites by the end of the 2030s, according to submissions to the US Federal Communications Commission (FCC).

Astronomers have long raised concerns regarding the potential impact of these satellites on ground-based telescopes. However, research by Alejandro Borlaf and his team at NASA’s Ames Research Center indicates that space telescopes are at risk as well.

“A telescope in space benefits from an unblemished environment; there’s no atmosphere or city lights,” Borlaf explains. “For the first time, we’re facing the issue of a man-made object contaminating our observations. This discovery was startling.”

By analyzing filings from the FCC and the International Telecommunication Union, Borlaf’s team estimated the anticipated number of satellites and their orbits over the next decade. They simulated the effect of these satellites blocking observations from four space observatories, including Hubble and China’s Shuntian telescope, as well as the Arrakis dark matter telescope set to launch in 2030, and the already launched SPHEREx galaxy telescope.

The researchers found that if 560,000 satellites are launched as projected, Hubble photos may capture an average of two satellite orbits, while Xuntian images could have approximately 90 satellite orbits due to a broader field of view and orbital altitude.

They validated their simulations by demonstrating that with the existing number of satellites, 4% of Hubble’s images would be influenced by the trajectories of these satellites, consistent with analyses of actual images.

These predictions could materialize if satellite launches proceed as planned. According to John Valentine from Dark Sky Consulting, a Tucson-based firm, it’s uncertain how many satellites will ultimately launch. “Many experts believe that over the next 15 years, the number of operational satellites could stabilize between 50,000 and 100,000.”

If the final number turns out to be only a fraction of the proposed figures, Valentine suggests, the impact on space telescopes would be notably reduced. “The number of trajectories per image would increase only slightly for ARRACHIS and Xuntian, while remaining relatively unchanged for SPHEREx and HST.”

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Source: www.newscientist.com

Hubble Space Telescope Reveals Stunning New Image of NGC 1792

Posted on December 2, 2025 by

Located in the southern part of the constellation Columba, NGC 1792 is a tempestuous and highly energetic spiral galaxy.

This Hubble image highlights the active spiral galaxy NGC 1792. Image credits: NASA / ESA / Hubble / D. Thilker / F. Belfiore / J. Lee / PHANGS-HST Team.

NGC 1792 is approximately 36.4 million light-years away from Earth, positioned to the south of the constellation Columba, bordering Caelum.

This galaxy, also known as AGC 24019 or LEDA 16709, was identified by Scottish astronomer James Dunlop on October 4, 1826.

The chaotic appearance of NGC 1792 features dust interspersed throughout its disk.

This galaxy is abundant in neutral hydrogen gas, leading to a high rate of new star formation.

“Astronomers find NGC 1792 intriguing, as its tumultuous appearance implies,” stated Hubble astronomers.

“Classified as a starburst galaxy, it serves as a dynamic site for star formation, with spiral arms rich in star-forming regions.”

“Surprisingly, it is quite luminous for its mass,” they added.

“This galaxy is approaching its larger neighbor, NGC 1808. The intense gravitational interaction between the two is believed to have stirred the gas reserves of the galaxy.”

“Consequently, star formation is more concentrated on the side where the gravitational pull is stronger.”

“This makes NGC 1792 an ideal subject for astronomers aiming to comprehend the intricate interactions among gas, star clusters, and supernovae within galaxies.”

In 2020, astronomers utilized Hubble’s Wide Field Camera 3 (WFC3) to observe NGC 1792.

The recent images incorporate additional WFC3 data collected in 2025, enriching our understanding of the turbulent astrophysical activity in the galaxy.

“The red light radiating in the arms signals H-alpha emission from a dense cloud of hydrogen molecules,” remarked the astronomers.

“Stars are born within these clouds and emit strong ultraviolet light.”

“This process ionizes the surrounding gas, causing it to emit light at a distinctive red wavelength, a clear indicator of a new star.”

Source: www.sci.news

Gemini South Telescope Shines Light on the Butterfly Nebula

Posted on November 29, 2025 by

In celebration of the 25th anniversary of the International Gemini Observatory’s completion, students in Chile chose the Gemini South Telescope to capture an image of NGC 6302, also known as the Bug Nebula or Butterfly Nebula (Caldwell 69).

This image captured by the Gemini South Telescope showcases the planetary nebula NGC 6302. Image credit: International Gemini Observatory / NOIRLab / NSF / AURA / J. Miller & M. Rodriguez, International Gemini Observatory & NSF’s NOIRLab / TA Rector, University of Alaska Anchorage & NSF’s NOIRLab / M. Zamani, NSF’s NOIRLab.

NGC 6302 is a planetary nebula situated 2,417 light-years away in the constellation Scorpius.

“Planetary nebulae are a type of emission nebula formed by a massive star at the end of its lifecycle, shedding material and surrounded by an expanding, glowing shell of ionized gas,” stated astronomers at the International Gemini Observatory.

“These intriguing structures usually have a circular, planet-like appearance, which is how they earned the name ‘planetary nebulae’ from early astronomers who observed them through telescopes.”

While various dates are associated with the discovery of NGC 6302, a 1907 study by American astronomer Edward E. Barnard is commonly credited, though it could have been discovered earlier in 1826 by Scottish astronomer James Dunlop.

This nebula is characterized by an extremely complex dipolar morphology, highly excited gases, elevated molecular weight, and the presence of crystalline silicate dust.

Its butterfly shape extends over two light-years, roughly half the distance from the Sun to Proxima Centauri.

“In recent images obtained from the Gemini South Telescope, the glowing ‘wings’ of the Butterfly Nebula appear to emerge from the interstellar medium,” the astronomers explained.

“This visually stunning object was chosen by Chilean students for the 8.1-meter telescope as part of the Gemini First Light Anniversary Image Contest.”

“This competition engaged students at the Gemini telescope site, honoring the legacy established by the International Gemini Observatory since its first light in November 2000.”

In 2009, astronomers utilized the Wide Field Camera 3 on the NASA/ESA Hubble Space Telescope to identify the central star of NGC 6302 as a white dwarf. This star shed its outer layers over 2,000 years ago and now possesses about two-thirds the mass of the Sun.

It ranks as one of the hottest known stars, with a surface temperature exceeding 250,000 degrees Celsius (450,000 degrees Fahrenheit), indicating it must have formed from a substantially large star.

Further investigation of NGC 6302 uncovers a dramatic formation history.

Before its transformation into a white dwarf, the star was a red giant approximately 1,000 times the diameter of the Sun.

This massive star expelled its outer gas layer, moving outward from the equator at a relatively slow rate, forming a dark donut-shaped band still observable around the star.

Other gases were expelled perpendicular to this band, restricting outflow and creating the bipolar structure visible today.

As the star evolved, it released strong stellar winds that pierced its “wings” at speeds exceeding 3 million kilometers per hour (1.8 million miles per hour).

This combination of slow and fast-moving gases further sculpted the “wings,” revealing a vast terrain of cloudy ridges and pillars.

Now, as a white dwarf, the star emits intense radiation that elevates the temperature of NGC 6302’s “wings” to over 20,000 degrees Celsius (approximately 35,000 degrees Fahrenheit), causing the gas to glow.

“Dark red areas in the image represent regions of energized hydrogen gas, while deep blue spots indicate regions of energized oxygen gas,” the researchers mentioned.

“These materials, alongside other elements like nitrogen, sulfur, and iron discovered in NGC 6302, are critical for forming the next generation of stars and planets.”

Source: www.sci.news

Hubble Space Telescope Unveils Stunning New Image of NGC 4535

Posted on November 17, 2025 by

Astronomers utilizing the NASA/ESA Hubble Space Telescope have captured astonishing new images of the barred spiral galaxy NGC 4535.

This Hubble image depicts spiral galaxy NGC 4535, situated approximately 52.6 million light-years away in the constellation Virgo. Image credits: NASA / ESA / Hubble / F. Belfiore / J. Lee / PHANGS-HST team.

NGC4535 is located in the Virgo constellation, roughly 52.6 million light-years distant.

This galaxy, also referred to as LEDA 41812 and UGC 7727, spans about 115,000 light-years.

First observed by German-British astronomer William Herschel on December 28, 1785.

When viewed through smaller telescopes, NGC 4535 appears hazy and ethereal, prompting prominent amateur astronomer Leland S. Copeland to name it the “Lost Galaxy” in the 1950s.

“This galaxy is so faint when seen through small telescopes that it has been nicknamed the ‘Lost Galaxy,'” noted Hubble astronomers.

“With its 2.4-meter-diameter mirror, Hubble is ideally equipped to observe faint galaxies like NGC 4535 and reveal features such as its magnificent spiral arms and central bar of stars.”

NGC 4535 ranks among the largest galaxies in the Virgo Cluster, a massive assembly of 2,000 galaxies located near the prominent elliptical galaxy Messier 87.

The nearly circular shape of the galaxy suggests that we are viewing it almost face-on.

Its center features a distinct bar structure with a dust lane that sharply curves before branching into the spiral arm.

“The young star clusters of NGC 4535 are vividly visible in the Hubble images, scattered throughout the galaxy’s spiral arms,” the astronomers stated.

“Many clusters of bright blue stars are enveloped by glowing pink clouds.”

“These clouds, known as H II regions, indicate that this galaxy is home to particularly young, hot, and massive stars emitting high-energy radiation.”

“Massive stars significantly impact their environment by heating the clouds they are born from, producing powerful stellar winds, and ultimately exploding as supernovae.”

The new Hubble images include data from an observational program cataloging around 50,000 H II regions in nearby star-forming galaxies.

“Previous images of NGC 4535 were released in 2021,” the researchers mentioned.

“Both the 2021 images and the latest ones include observations from around the globe. The PHANGS program aims to understand the relationship between young stars and cold gas.”

“Today’s images provide a new perspective on NGC 4535 by highlighting the bright red glow of the nebula surrounding the massive star during its initial few million years of existence.”

Source: www.sci.news

Hubble Space Telescope Reveals Stunning New Image of NGC 4102

Posted on November 4, 2025 by

The Hubble Space Telescope, operated by NASA and ESA, unveils the radiant galactic core and stunning spiral arms in this fresh perspective of NGC 4102.

This Hubble image illustrates NGC 4102, an intermediate spiral galaxy located 55.4 million light-years away in the constellation Ursa Major. Image credit: NASA / ESA / Hubble / G. Fabbiano.

NGC 4102 is positioned to the north of Ursa Major, approximately 55.4 million light-years distant.

This intermediate spiral galaxy was discovered on April 12, 1789, by the German-British astronomer William Herschel.

Also known as UGC 7096, NGC 4102 features an active galactic nucleus.

“Active galactic nuclei are luminous centers within galaxies, powered by supermassive black holes with masses millions to billions of times greater than that of the Sun,” stated Hubble astronomers.

“When these black holes attract surrounding gas, the intense gravitational forces cause the gas to heat up and emit light across various wavelengths, from X-rays to radio,” they added.

“NGC 4102 stands as a prime candidate for examining the interaction between active galactic nuclei and their host galaxies,” noted the researchers.

“These active galactic nuclei range from very powerful variants that consume significant amounts of matter and produce jets of charged particles to more subdued types that gently draw in gas and emit less intense light.”

“NGC 4102 is likely categorized among the latter; it falls within the Compton-thickness classification, indicating a dense gas environment surrounding its nucleus, and is identified as a low-ionization nuclear emission line region (LINER).”

“LINER galaxies are recognized by emission lines from weakly ionized elements and may be sustained by supermassive black holes gradually accumulating gas from their vicinity.”

Previous imaging of NGC 4102, derived from observations with Hubble’s Wide Field Planetary Camera 2 (WFPC2), was released in 2014.

“The latest imaging offers an enhanced view of the galaxy, utilizing data from Hubble’s Wide Field Camera 3 (WFC3), which replaced WFPC2 in 2009, providing improved resolution and a larger field of view,” according to the researchers.

“These new observations are part of a program that integrates visible-light imagery from Hubble with X-ray data from the Chandra X-ray Observatory, aimed at exploring NGC 4102 and its relationship with active galactic nuclei.”

Source: www.sci.news

US Withdrawal of Support for CMB-S4 Telescope is Catastrophic

Posted on October 30, 2025 by

South Pole telescope. CMB-S4 was meant to explore temperature and polarization changes in microwave light across vast areas of the sky.

Brad Benson, University of Chicago Fermilab

In the words of Robert Frost from The Road Not Taken, “Two roads diverged in a yellow wood / And sorry I could not travel both.”

This sentiment resonates as I reflect on the U.S. government’s July 9 announcement: CMB-S4 projects will no longer receive support. CMB-S4 (Cosmic Microwave Background Stage 4) was set to be the next groundbreaking multicontinental telescope system, promising unparalleled insights into the oldest light traversing the universe.

Initially, the universe was a turbulent mix of dense particles and plasma, so thick that photons (light particles) could scarcely move without colliding with something. This primordial environment was also extremely hot, hindering the formation of atoms. It wasn’t until cosmic inflation—a rapid expansion of spacetime lasting an imperceptibly short period—that temperatures fell sufficiently to allow the first hydrogen atoms to form, providing photons the freedom to zip across space.

Sixty-one years ago, we discovered the existence of these photons, known as cosmic microwave background radiation (CMB). What began as mere background noise in radio signals has been recognized as a link to the early universe, leading us to meticulously analyze the wavelengths, intensities, and variations of these photons.

The CMB offers a trove of information regarding the origins of all matter we observe, including stars that later create gold through supernovae. By surveying the entire sky for changes in photon temperatures, we can identify minute fluctuations in temperature. While their positions appear random, the magnitude of these variations is consistent across the board.

Our prevailing theory posits that these fluctuations arise from tiny quantum variations in matter density at the time the photons were released. Greater concentrations of matter served as the seeds for gas accumulation, which ultimately merged into protostars, leading to the formation of stars and galaxies. Thus, these CMB fluctuations mark our cosmic genesis.

“
The withdrawal from this project signifies a reckless retreat by the U.S. from global scientific cooperation.
“

One of the most significant measurements we’ve derived from the CMB is how its temperature fluctuations correlate with various physical scales. Understanding the distances over which particular phenomena manifest allows us to analyze the variation’s origins—whether from larger or smaller scales. Essentially, different epochs in cosmological history are imprinted within the CMB.

For instance, we can “detect” when the universe became transparent to matter and when hydrogen first formed, an epoch referred to as recombination. Although these events are beyond our visual perception, we can gauge the presence of dark matter and dark energy based on their influence on the CMB.

CMB-S4 aimed to advance our understanding of the lessons the CMB has to offer. An important objective was to seek evidence of primordial gravitational waves, ripples in spacetime associated with cosmic inflation. Although different inflationary models propose plausible physical descriptions of our universe, specific details remain elusive. The signatures of gravitational waves on the CMB may provide the most effective means of distinguishing among these models.

The cessation of government backing for CMB-S4 is akin to jamming a bike’s wheel, abruptly halting our exploration of the cosmos. The repercussions will be felt globally. Historically, the U.S. has made significant investments in cosmological science, which attracts students internationally to its educational institutions. U.S.-sourced experimental data typically serves as a critical global resource. The retreat from the project, which seemed likely under the former administration, is now part of a broader trend of the U.S. distancing itself from global collaboration.

Frost concludes his poem by reflecting on the implications of his chosen path. It is indeed regrettable that the United States has opted not to explore the less traveled road in scientific pursuits. It undoubtedly makes an impact, but unfortunately, not for the better.

A week in Chanda

What I am reading

I find the works of Niaesh Afsholdi and Phil Halper captivating. Their book, The Battle of the Big Bang: A New Story About the Origins of Our Universe, is particularly intriguing.

What I see

I keep rewatching DC Universe movies, especially those featuring my favorite character, Harley Quinn.

What I am working on

I’ve been attempting to capture stunning images of the Andromeda Galaxy from my backyard.

Topic:

Source: www.newscientist.com

Green Bank Telescope Maps Cold ‘Dark’ Gas in Cygnus X

Posted on October 30, 2025 by

An astronomer utilizing the Green Bank Telescope (GBT) has developed an extensive map of carbon monoxide (CO) and dark molecular gas in star-forming complexes, particularly in Cygnus X.

These images illustrate the location of CO-dark molecular gas within Cygnus X. Image credit: NSF/AUI/NSF’s NRAO/P.Vosteen.

For decades, scientists have recognized that most new stars are birthed in frigid clouds of molecular hydrogen gas.

A significant portion of this molecular hydrogen remains elusive to most telescopes as it fails to emit easily detectable light.

Astronomers have typically sought these clouds by examining carbon monoxide (CO), a molecule that serves as a glowing signal for star-forming regions.

However, it has been uncovered that CO houses a considerable amount of “non-glowing” gas conducive to star formation.

This concealed material, referred to as CO-dark molecular gas, has represented one of astronomy’s most significant blind spots.

In a fresh study, NRAO astronomer Kimberly Emig and her team mapped this hidden gas across extensive sections of the sky, using radio spectral lines from atomic recombination known as carbon radio recombination lines (CRRLs).

Their map encompasses Cygnus X, a star-forming region located approximately 5,000 light-years away in the constellation Cygnus.

“It’s akin to suddenly switching on a light in a room and discovering various structures that were previously unseen,” Dr. Emig remarked.

The newly constructed map unveils a sprawling network of arcs, ridges, and webs of dark gas permeating Cygnus X.

These formations indicate where star-forming materials accumulate and evolve before becoming noticeable as molecular clouds in CO.

The authors demonstrated that these faint carbon signals, observed at very low radio frequencies, serve as an extraordinarily powerful instrument for uncovering hidden gas that directly correlates ordinary matter with the birth of new stars.

They found that this dark gas is not static; instead, it flows, shifts, and moves at rates much faster than previously recognized. These dynamics influence the stellar formation rate.

Moreover, they discovered that the intensity of these carbon lines is directly connected to the intense starlight bathing the area, emphasizing the significant role radiation plays in galactic recycling.

“By illuminating the invisible, we can trace how the raw ingredients in our galaxy transform from simple atoms into complex molecular structures that will ultimately become stars, planets, and potentially life,” Dr. Emig stated.

“This marks merely the beginning of comprehending an otherwise unseen force.”

Find the results published in the October 17th edition of the Astrophysical Journal.

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Kimberly L. Emig et al. 2025. The cold dark gas of Cygnus X: the first large-scale mapping of low-frequency carbon recombination lines. APJ 992, 216; doi: 10.3847/1538-4357/adfa17

Source: www.sci.news

Hubble Space Telescope Reveals an Unexpected New Perspective of NGC 4571

Posted on October 28, 2025 by

This image captured by the NASA/ESA Hubble Space Telescope offers a fresh and detailed view of the star-filled spiral galaxy NGC 4571.

This Hubble image highlights NGC 4571, a spiral galaxy located about 60 million light-years away in the constellation Coma. Image credits: NASA / ESA / Hubble / F. Belfiore / J. Lee / PHANGS-HST team.

NGC 4571 is positioned 60 million light-years away in the constellation Taurus.

This galaxy was discovered by German-British astronomer William Herschel on January 14, 1787.

Also referred to as IC 3588, LEDA 42100, and UGC 7788, NGC 4571 is classified as a spiral galaxy with low surface brightness.

It belongs to the Virgo Cluster, which comprises over 1,000 galaxies.

This cluster is part of the more extensive Virgo supercluster, which encompasses a local group that includes our very own Milky Way galaxy.

“NGC 4571 captivates with its feather-like spiral structure and vibrant star clusters,” remarked Hubble astronomers regarding this new image.

“The galaxy’s dusty spiral arms are sprinkled with bright pink nebulae that contain massive young stars.”

“The star-forming clouds in this image are heated to about 10,000 K due to intense ultraviolet light from young stars at their centers, although stars form in much cooler conditions.”

“Stars emerge from giant molecular clouds that can span tens to hundreds of light-years, with temperatures only slightly above absolute zero.”

“The remarkable change from a frigid gas cloud to a blazing young star is driven by the immense gravitational force that compacts the gas into dense clumps within star-forming clouds.”

“As these clumps yield to gravity and collapse inward, they eventually reach sufficient heat and density to initiate nuclear fusion at their cores and begin to shine.”

“The luminous clouds depicted in this image enclose particularly massive stars that are hot enough to ionize the gas within their stellar nurseries.”

In 2022, the Hubble team captured intricate images of NGC 4571 as part of an observational initiative incorporating data from major observatories, including Hubble, NASA/ESA/CSA’s James Webb Space Telescope, and the Atacama Large Millimeter/Submillimeter Array.

“The newly released images today add data from a program aimed at understanding the impact of dust on observations of young stars obscured within their natal clouds,” the astronomers noted.

Source: www.sci.news

Hubble Space Telescope Captures NGC 3370 Observations

Posted on October 21, 2025 by

Astronomers utilizing the NASA/ESA Hubble Space Telescope have captured new images of the nearly face-on spiral galaxy NGC 3370.

This Hubble image illustrates spiral galaxy NGC 3370, located approximately 90 million light-years away in the constellation Leo. Image credits: NASA / ESA / Hubble / A. Riess / K. Noll.

NGC 3370 is situated in the constellation Leo, roughly 90 million light-years from Earth.

This galaxy, also known as the Silverado Galaxy, IRAS 10444+1732, LEDA 32207, and UGC 5887, is nearly comparable to our Milky Way in both diameter and mass.

Discovered on March 21, 1784, by German-British astronomer William Herschel, NGC 3370 was the first of its kind to be identified.

Together with NGC 3447 and NGC 3455, it forms part of the NGC 3370 galaxy group.

NGC 3370 contains two types of celestial objects that astronomers find valuable for measuring distances to far-off galaxies: Cepheid variable stars and Type Ia supernovae.

“Cepheid variable stars undergo changes in both size and temperature during their pulsations,” Hubble astronomers explained in a statement.

“Consequently, the brightness of these stars fluctuates over timescales of days to months.”

“This variation reveals a key relationship: the brighter a Cepheid variable star, the slower its pulsation.”

“By timing the pulsation cycle of a Cepheid variable star, we can ascertain its true brightness.”

“When combined with observations of its apparent brightness from Earth, this data enables us to calculate the distance to the star and its galaxy.”

“Type Ia supernovae allow for distance measurements through a single explosive event, as opposed to periodic brightness changes.”

“These explosions occur when a star’s dead core reignites due to a sudden surge of nuclear fusion.”

“They reach similar peak brightness levels, akin to those of Cepheid variable stars, and knowing the intrinsic brightness of a supernova allows us to determine its distance.”

“The observation of both Cepheid variable stars and Type Ia supernovae is crucial for accurately gauging how quickly our universe is expanding.”

Source: www.sci.news