Kyoto, Japan — Down here on Earth we don’t usually notice, but the Sun is frequently ejecting huge masses of plasma into space. These are called coronal mass ejections (CMEs). They often occur together with sudden brightenings called flares, and sometimes extend far enough to disturb Earth’s magnetosphere, generating space weather phenomena including auroras or geomagnetic storms, and even damaging power grids on occasion.

Scientists believe that when the Sun and the Earth were young, the Sun was so active that these CMEs may have even affected the emergence and evolution of life on the Earth. In fact, previous studies have revealed that young Sun-like stars, proxies of our Sun in its youth, frequently produce powerful flares that far exceed the largest solar flares in modern history.

Huge CMEs from the early Sun may have severely impacted the early environments of Earth, Mars, and Venus. However, to what extent explosions on these young stars exhibit solar-like CMEs remains unclear. In recent years, the cool plasma of CMEs has been detected by optical observations on the ground. However, the high velocity and expected frequent occurrence of strong CMEs in the past have remained elusive.

In order to resolve this problem, an international team of researchers, including Kosuke Namekata of Kyoto University, sought to test whether young Sun-like stars produce solar-like CMEs.

“What inspired us most was the long-standing mystery of how the young Sun’s violent activity influenced the nascent Earth,” says Namekata. “By combining space- and ground-based facilities across Japan, Korea, and the United States, we were able to reconstruct what may have happened billions of years ago in our own solar system.”

The team’s analysis included simultaneous ultraviolet observations by the Hubble Space Telescope and optical observations by ground-based telescopes in Japan and Korea. Their target was the young solar analogue EK Draconis. Hubble observed far-ultraviolet emission lines sensitive to hot plasma, while the three ground-based telescopes simultaneously observed the hydrogen Hα line, which traces cooler gases. These simultaneous, multi-wavelength spectroscopic observations allowed the research team to capture both the hot and cool components of the ejection in real time.

These observations led to the first evidence of a multi-temperature coronal mass ejection from EK Draconis. The team found that hot plasma of 100,000 degrees Kelvin was ejected at 300 to 550 kilometers per second, followed about ten minutes later by a cooler gas of about 10,000 degrees ejected at 70 kilometers per second. The hot plasma carried much greater energy than cool plasma, suggesting that frequent strong CMEs in the past could drive strong shocks and energetic particles capable of eroding or chemically altering early planetary atmospheres.

Theoretical and experimental studies support the critical role that strong CMEs and energetic particles can play in initiating biomolecules and greenhouse gases, which are essential for the emergence and maintenance of life on an early planet. Therefore, this discovery has major implications for understanding planetary habitability and the conditions under which life emerged on Earth, and possibly elsewhere.

The research team noted that the success of this study was achieved through international teamwork and precise coordination between space- and ground-based observatories.

“We were happy to see that, although our countries differ, we share the same goal of seeking truth through science,” says Namekata.

###

The paper “Discovery of multi-temperature coronal mass ejection signatures from a young solar analogue” appeared on 27 October 2025 in Nature Astronomy, with doi: 10.1038/s41550-025-02691-8

About Kyoto University

Kyoto University is one of Japan and Asia’s premier research institutions, founded in 1897 and responsible for producing numerous Nobel laureates and winners of other prestigious international prizes. A broad curriculum across the arts and sciences at undergraduate and graduate levels complements several research centers, facilities, and offices around Japan and the world. For more information, please see: http://www.kyoto-u.ac.jp/en

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Kyoto University
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Researchers have achieved a breakthrough in solar physics by providing the first direct evidence of small-scale torsional Alfvén waves in the Sun’s corona – elusive magnetic waves that scientists have been searching for since the 1940s.

The discovery, published today in Nature Astronomy, was made using unprecedented observations from the world’s most powerful solar telescope, the U.S. National Science Foundation (NSF) Daniel K. Inouye Solar Telescope in Hawaii.

The findings could finally explain one of the Sun’s greatest mysteries – how its outer atmosphere the corona, reaches temperatures of millions of degrees while its surface is only around 5,500°C.

Alfvén waves, named after Nobel Prize winner Hannes Alfvén who predicted their existence in 1942, are magnetic disturbances that can carry energy through plasma.

Scientists have spotted larger, isolated versions of these waves before – normally related to solar flares. However, this is the first time that the small twisting type, that are present all the time and could power the Sun, have been directly observed.

UKRI Future Leader Fellow Professor Richard Morton,  a Professor within Northumbria University’s School of Engineering, Physics and Mathematics, led the research, He said: “This discovery ends a protracted search for these waves that has its origins in the 1940s. We’ve finally been able to directly observe these torsional motions twisting the magnetic field lines back and forth in the corona.”

The breakthrough was made possible by the unique capabilities of the Daniel K. Inouye Solar Telescope’s Cryogenic Near Infrared Spectropolarimeter (Cryo-NIRSP), the most advanced coronal instrument of its kind.

This cutting-edge spectrometer can see incredibly fine details in the corona and is highly sensitive to changes in the movement of plasma.

With its four-meter-wide mirror – four times larger than previous solar telescopes – the Daniel K. Inouye Solar Telescope, built and operated by the NSF National Solar Observatory, represents two decades of international planning and development.

Northumbria University has played a crucial role in its development as part of a UK consortium that designed cameras for the telescope’s Visible Broadband Imager, building on the University’s established reputation in observations of the solar atmosphere.

Professor Morton won time to use the telescope while it was still being tested and used the instrument to track the movement of iron, heated to 1.6 million degrees Celsius, in the corona.

The key breakthrough came from Professor Morton developing entirely new analytical techniques to separate different types of wave motion in the data. As he explains: “The movement of plasma in the sun’s corona is dominated by swaying motions. These mask the torsional motions, so I had to develop a way of removing the swaying to find the twisting.”

While the more familiar ‘kink’ waves cause entire magnetic structures to sway back and forth and are visible in film captured of the Sun, the newly detected torsional Alfvén waves cause a twisting motion that can only be detected through spectroscopic analysis – measuring how plasma moves toward and away from Earth, creating characteristic red and blue shifts on opposite sides of magnetic structures.

The discovery has profound implications for understanding how the Sun works. The corona, the Sun’s outermost atmosphere visible during solar eclipses, is heated to temperatures exceeding one million degrees Celsius – hot enough to accelerate plasma away from the Sun as the solar wind that fills our entire solar system.

The research represents a major international collaboration, with co-authors from Peking University in China, KU Leuven in Belgium, Queen Mary University of London, the Chinese Academy of Sciences, and the NSF National Solar Observatory in Hawaii and Colorado.

Understanding these fundamental processes has practical importance for space weather prediction. The solar wind carries magnetic disturbances that can disrupt satellite communications, GPS systems, and power grids on Earth. Alfvén waves may also be the source of ‘magnetic switchbacks’ – significant carriers of energy in the solar wind that have been observed by NASA’s Parker Solar Probe.

“This research provides essential validation for the range of theoretical models that describe how Alfvén wave turbulence powers the solar atmosphere,” added Professor Morton. “Having direct observations finally allows us to test these models against reality.”

The team anticipates this discovery will spark further investigations into how these waves propagate and dissipate energy in the corona. The ability of the Daniel K. Inouye Solar Telescope’s Cryo-NIRSP instrument to provide high-quality spectra opens new possibilities for studying wave physics in the solar atmosphere.

The research was supported by UKRI Future Leaders Fellowships, the National Natural Science Foundation of China, and the European Union’s Horizon Europe programme.

This is the third paper Professor Morton has published this year in relation to his research into Alfvén waves. In April 2025 the paper High-frequency Coronal Alfvénic Waves Observed with DKIST/Cryo-NIRSP was published in The Astrophysical Journal, followed by the paper On the Origins of Coronal Alfvénic Waves, published in June 2025 in The Astrophysical Journal Letters.

FURTHER INFORMATION:

• The paper Evidence for small-scale torsional Alfvén waves in the solar corona was published in Nature Astronomy on XX October 2025.  DOI: 10.1038/s41550-025-02690-9
• Visit the Northumbria University Research Portal to find out more about Professor Richard Morton’s work.

RELATED NEWS:

• Northumbria to help build world’s biggest solar telescope in £220 million project
• Researchers find evidence for a new fundamental constant of the Sun
• Global magnetic field of the solar corona measured for the first time
• £1.2 million awarded to improve our understanding of the Sun
• Recognition for Northumbria physicist’s solar discoveries
• First successful routine measurements of Sun’s magnetic field in the corona

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Because the object does not emit any light or other radiation, it was detected by the way its gravity distorts light passing through or near it. This effect is called gravitational lensing. Based on the distortion, astronomers can infer the amount of matter in the unseen object.

In fact, the new object is so small that it was detected by inducing a small pinch in the distorted image caused by a much larger object, like a flaw in a funhouse mirror.

“It’s an impressive achievement to detect such a low mass object at such a large distance from us,” said Chris Fassnacht, professor in the Department of Physics and Astronomy at the University of California, Davis, who is a co-author on the Nature Astronomy paper. “Finding low-mass objects such as this one is critical for learning about the nature of dark matter.”

The mystery object has a mass about 1 million times that of our Sun. Its nature is unknown: It could be a clump of dark matter 100 times smaller than any previously detected, or it might be a very compact, inactive dwarf galaxy.

Although imperceptible except for its gravitational effects, dark matter is thought to shape the distribution of galaxies, stars and other visible bodies across the sky. A key question for astronomers is whether dark matter can exist in small clumps without any stars. This could confirm or refute some theories about the nature of dark matter.

Using telescopes worldwide

The team used instruments including the Green Bank Telescope (GBT), West Virginia; the Very Long Baseline Array (VLBA), Hawaiʻi; and the European Very Long Baseline Interferometric Network (EVN), which includes radio telescopes in Europe, Asia, South Africa and Puerto Rico to create an Earth-sized super-telescope, to capture the subtle signals of gravitational lensing by the dark object.

It is by a hundred-fold the lowest mass object yet found by this technique, suggesting that the method could be used to find other, similar objects.

“Given the sensitivity of our data, we were expecting to find at least one dark object, so our discovery is consistent with the so-called ‘cold dark matter theory’ on which much of our understanding of how galaxies form is based,” said lead author Devon Powell at the Max Planck Institute for Astrophysics (MPA), Germany. “Having found one, the question now is whether we can find more and whether the numbers will still agree with the models.”

The team is further analyzing the data to better understand the nature of the dark object, and also looking for more examples of such dark objects in other parts of the sky.

Additional authors are: John McKean, University of Groningen, the Netherlands, South African Radio Observatory and University of Pretoria; Simona Vegetti, MPA; Cristiana Spingola, Istituto di Radioastronomia, Bologna; and Simon D. M. White, MPA.

The work was supported in part by the European Research Council, the Italian Ministry of Foreign Affairs and International Cooperation and the National Research Foundation of South Africa. The National Radio Astronomy Observatory is a facility of the U.S. National Science Foundation.

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Published today in Nature Astronomy, this discovery further strengthens the case for a dedicated European Space Agency (ESA) mission to orbit and land on Enceladus.

In 2005, Cassini found the first evidence that Enceladus has a hidden ocean beneath its icy surface. Jets of water burst from cracks close to the moon’s south pole, shooting ice grains into space. Smaller than grains of sand, some of the tiny pieces of ice fall back onto the moon’s surface, whilst others escape and form a ring around Saturn that traces Enceladus’s orbit.

Lead author Nozair Khawaja explains what we already knew: “Cassini was detecting samples from Enceladus all the time as it flew through Saturn’s E ring. We had already found many organic molecules in these ice grains, including precursors for amino acids.

The ice grains in the ring can be hundreds of years old. As they have aged, they may have been ‘weathered’ and therefore altered by intense space radiation. Scientists wanted to investigate fresh grains ejected much more recently to get a better idea of what exactly is going on in Enceladus’s ocean.

Fortunately, we already had the data. Back in 2008, Cassini flew straight through the icy spray. Pristine grains ejected only minutes before hit the spacecraft’s Cosmic Dust Analyzer (CDA) instrument at about 18 km/s. These were not only the freshest ice grains Cassini had ever detected, but also the fastest.

The speed mattered. Nozair explains why:

“The ice grains contain not just frozen water, but also other molecules, including organics. At lower impact speeds, the ice shatters, and the signal from clusters of water molecules can hide the signal from certain organic molecules. But when the ice grains hit CDA fast, water molecules don’t cluster, and we have a chance to see these previously hidden signals.”

It took years to build up knowledge from previous flybys and then apply it to decipher this data. But now, Nozair’s team has revealed what kind of molecules were present inside the fresh ice grains.

They saw that certain organic molecules that had already been found distributed in the E ring were also present in the fresh ice grains. This confirms that they are created within Enceladus’s ocean.

They also found totally new molecules that had never been seen before in ice grains from Enceladus. For the chemists reading, the newly detected molecular fragments included aliphatic, (hetero)cyclic ester/alkenes, ethers/ethyl and, tentatively, nitrogen- and oxygen-bearing compounds.

On Earth, these same molecules are involved in the chains of chemical reactions that ultimately lead to the more complex molecules that are essential for life.

“There are many possible pathways from the organic molecules we found in the Cassini data to potentially biologically relevant compounds, which enhances the likelihood that the moon is habitable,” says Nozair.

“There is much more in the data that we are currently exploring, so we are looking forward to finding out more in the near future.”

Co-author Frank Postberg adds: “These molecules we found in the freshly ejected material prove that the complex organic molecules Cassini detected in Saturn’s E ring are not just a product of long exposure to space, but are readily available in Enceladus’s ocean.”

Nicolas Altobelli, ESA Cassini project scientist adds: “It’s fantastic to see new discoveries emerging from Cassini data almost two decades after it was collected. It really showcases the long-term impact of our space missions. I look forward to comparing data from Cassini with data from ESA’s other missions to visit the icy moons of Saturn and Jupiter.”

Returning to Enceladus

Discoveries from Cassini are valuable for planning a future ESA mission dedicated to Enceladus. Studies for this ambitious mission have already begun. The plan is to fly through the jets and even land on the moon’s south polar terrain to collect samples.

A team of scientists and engineers is already considering the selection of modern scientific instruments that the spacecraft would carry. This latest result made using CDA will help guide that decision.

Enceladus ticks all the boxes to be a habitable environment that could support life: the presence of liquid water, a source of energy, a specific set of chemical elements and complex organic molecules. A mission that takes measurements directly from the moon’s surface, seeking out signs of life, would offer Europe a front seat in Solar System science.

“Even not finding life on Enceladus would be a huge discovery, because it raises serious questions about why life is not present in such an environment when the right conditions are there,” says Nozair.

Notes for editors

‘Detection of Organic Compounds in Freshly Ejected Ice Grains from Enceladus’s Ocean’ by N. Khawaja et al. is published today in Nature Astronomy. DOI: 10.1038/s41550-025-02655-y

Lead author Nozair Khawaja conducted the research at Freie Universität Berlin and the University of Stuttgart, both in Germany. Frank Postberg is also affiliated with Freie Universität Berlin.

Cassini-Huygens was a cooperative project of NASA, ESA and the Italian Space Agency. It comprised two elements: the Cassini orbiter and the Huygens probe.

Cassini’s Cosmic Dust Analyzer (CDA) was led by the University of Stuttgart in Germany.

For more information please contact:

media@esa.int

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Nicole Shearer
European Space Agency
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European Space Agency
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Neural Radiance Fields (NeRF) is a fascinating technique that creates three-dimensional (3D) representations of a scene from a set of two-dimensional (2D) images, captured from different angles. It works by training a deep neural network to predict the color and density at any point in 3D space. To do this, it casts imaginary light rays from the camera through each pixel in all input images, sampling points along those rays with their 3D coordinates and viewing direction. Using this information, NeRF reconstructs the scene in 3D and can render it from entirely new perspectives, a process known as novel view synthesis (NVS).

Beyond still images, a video can also be used, with each frame of the video treated as a static image. However, existing methods are highly sensitive to the quality of the videos. Videos captured with a single camera, such as those from a phone or drone, inevitably suffer from motion blur caused by fast object motion or camera shake. This makes it difficult to create sharp, dynamic NVS. This is because most existing deblurring-based NVS methods are designed for static multi-view images, which fail to account for global camera and local object motion. In addition, blurry videos often lead to inaccurate camera pose estimations and loss of geometric precision.

To address these issues, a research team jointly led by Assistant Professor Jihyong Oh from the Graduate School of Advanced Imaging Science (GSIAM) at Chung-Ang University (CAU) in Korea, and Professor Munchurl Kim from Korea Advanced Institute of Science and Technology (KAIST), Korea, along with Mr. Minh-Quan Viet Bui, Mr. Jongmin Park, developed MoBluRF, a two-stage motion deblurring method for NeRFs. “Our framework is capable of reconstructing sharp 4D scenes and enabling NVS from blurry monocular videos using motion decomposition, while avoiding mask supervision, significantly advancing the NeRF field,” explains Dr. Oh. Their study was made available online on May 28, 2025, and was published in Volume 47, Issue 09 of the IEEE Transactions on Pattern Analysis and Machine Intelligence on September 01, 2025.

MoBluRF consists of two main stages: Base Ray Initialization (BRI) and Motion Decomposition-based Deblurring (MDD). Existing deblurring-based NVS methods attempt to predict hidden sharp light rays in blurry images, called latent sharp rays, by transforming a ray called the base ray. However, directly using input rays in blurry images as base rays can lead to inaccurate prediction. BRI addresses this issue by roughly reconstructing dynamic 3D scenes from blurry videos and refining the initialization of “base rays” from imprecise camera rays.

Next, these base rays are used in the MDD stage to accurately predict latent sharp rays through an Incremental Latent Sharp-rays Prediction (ILSP) method. ILSP incrementally decomposes motion blur into global camera motion and local object motion components, greatly improving the deblurring accuracy. MoBluRF also introduces two novel loss functions, one that separates static and dynamic regions without motion masks, and another that improves geometric accuracy of dynamic objects, two areas where previous methods struggled.

Owing to this innovative design, MoBluRF outperforms state-of-the-art methods with significant margins in various datasets, both quantitatively and qualitatively. It is also robust against varying degrees of blur.

“By enabling deblurring and 3D reconstruction from casual handheld  captures, our framework enables smartphones and other consumer devices to produce sharper and more immersive content,” remarks Dr. Oh. “It could also help create crisp 3D models of shaky footages from museums, improve scene understanding and safety for robots and drones, and reduce the need for specialized capture setups in virtual and augmented reality.”

MoBluRF marks a new direction for NeRFs, enabling high quality 3D reconstructions from ordinary blurry videos recorded with everyday devices.

***

Reference

DOI: https://doi.org/10.1109/TPAMI.2025.3574644

About Chung-Ang University

Chung-Ang University is a leading private research university in Seoul, South Korea, dedicated to shaping global leaders for an evolving world. Founded in 1916 and achieving university status in 1953, it combines academic tradition with a strong commitment to innovation. Fully accredited by the Ministry of Education, CAU excels in fields such as pharmacy, medicine, engineering, and applied sciences, driving impactful discoveries and technological progress. Its research-intensive environment fosters collaboration and excellence, producing scholars and professionals who lead in their disciplines. Committed to global engagement, CAU continues to expand its influence as a hub for scientific advancement and future-driven education.

Website: https://neweng.cau.ac.kr/index.do

About Assistant Professor Jihyong Oh

Dr. Jihyong Oh is an Assistant Professor in the Department of Imaging Science, Graduate School of Advanced Imaging Science, Multimedia & Film (GSAIM) at Chung-Ang University (CAU; Seoul, South Korea), and has been leading the Creative Vision and Multimedia Lab (https://cmlab.cau.ac.kr/) since September 2023. Prior to this, he was a postdoctoral researcher at VICLAB at KAIST (Daejeon, South Korea). He received his B.E., M.E., and Ph.D. degrees in Electrical Engineering from KAIST in 2017, 2019, and 2023, respectively. His research primarily focuses on low-level vision, image/video restoration, 3D vision, and generative AI. He has published papers at CVPR, ICCV, ECCV, AAAI, TPAMI, TCSVT, Neurocomputing, and Remote Sensing, and serves as a reviewer for these conferences and journals, as well as for SIGGRAPH and IEEE TPAMI, TIP, TGRS, TMM and Access. He received Outstanding Reviewer Awards for ICCV 2021 and CVPR 2024.

Website: https://scholarworks.bwise.kr/cau/researcher-profile?ep=1528

Original Publication
Authors: Minh-Quan Viet Bui, Jongmin Park, Jihyong Oh and Munchurl Kim.
Journal: IEEE Transactions on Pattern Analysis and Machine Intelligence
DOI: 10.1109/TPAMI.2025.3574644
Method of Research: Computational simulation/modeling
Subject of Research: Not applicable
Article Title: MoBluRF: Motion Deblurring Neural Radiance Fields for Blurry Monocular Video
Article Publication Date: 1-Sep-2025
COI Statement: The authors declare no competing interests.

Original Source: https://neweng.cau.ac.kr/cms/FR_CON/BoardView.do?MENU_ID=920&CONTENTS_NO=&SITE_NO=3&BOARD_SEQ=14&BOARD_CATEGORY_NO=&BBS_SEQ=140

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Mapping Star Formation Hidden Behind Dust

Studying star-forming regions is challenging because thick clouds of gas and dust obscure them from view, and their distances are difficult to measure directly.

Gaia cannot see these clouds outright, but it can measure both the positions of stars and the “extinction” of starlight — how much light is dimmed by dust. Using this data, scientists created 3D maps that reveal the location of dust and, indirectly, how much ionised hydrogen gas is present — a key marker of active star formation.

Combining Data from Millions of Stars

The new 3D map draws on Gaia observations of 44 million ordinary stars and 87 massive O-type stars, covering space up to 4,000 light-years from the Sun.

O stars are rare, very hot, and extremely bright, shining intensely in ultraviolet light. Their energetic radiation strips electrons from hydrogen atoms, ionising the surrounding gas and leaving behind clouds of charged particles — known as HII regions. These regions are key indicators of where stars are currently forming.

While many telescopes have captured views of these areas from Earth’s perspective, Gaia now allows researchers to visualise their true three-dimensional structure — as if looking at the Milky Way from the outside.

A Bird’s-Eye View of the Milky Way

“Gaia provides the first accurate view of what our section of the Milky Way would look like from above,” explains Lewis McCallum, astronomer at the University of St Andrews, UK, and first author of two papers describing the new 3D model.

“There has never been a model of the distribution of the ionised gas in the local Milky Way that matches other telescope’s observations of the sky so well. That’s why we are confident that our top-down view and fly-through movies are a good approximation of what these clouds would look like in 3D.”

McCallum’s map features well-known star-forming regions such as the Gum Nebula, North America Nebula, California Nebula, and the Orion–Eridanus superbubble, now seen in fully navigable 3D for the first time.

Revealing a Giant Interstellar Cavity

This new perspective is already offering insights into how massive stars influence their environments. McCallum’s team noticed that some star-forming clouds appear to be venting gas and dust into a vast cavity within the interstellar medium.

“This map nicely shows how radiation of massive stars ionises the surrounding interstellar medium and how dust and gas interact with this radiation. The 3D model provides a detailed look at the processes that shape our local galactic environment and helps astronomers understand interactions between the warm and cold components of the local Universe,” explained Sasha Zeegers, ESA Research Fellow and an expert on interstellar dust.

Expanding the Map in Future Gaia Releases

“It required huge computational power to generate the map out to ‘just’ 4000 light-years from the Sun in high resolution [2]. We hope that the map can be expanded further out once Gaia has released its new set of data,” says Lewis McCallum.

“Gaia’s distance measurements of the nearby hot stars, and the 3D maps of dust – obtained from measuring the extinction and positions of millions of ordinary stars using Gaia data – are both crucial ingredients of this new map. Gaia’s fourth data release will contain data of even better quality and quantity, making it possible to further advance our knowledge of star-forming regions,” confirms Johannes Sahlmann, ESA’s Gaia Project Scientist.

Notes for Editors

• [1] Ionised hydrogen clouds are known as HII regions, which emit a distinct hydrogen-alpha (Hα) spectral line at a wavelength of 656.3 nm.
  
• [2] This new work builds on an earlier 2024 dust map of our local galaxy by Edenhofer et al., which McCallum’s team incorporated and combined with O-type star data to highlight ionised star-forming regions.
  
• Related papers by L. McCallum et al. are published in Monthly Notices of the Royal Astronomical Society:
  
  • Paper 1 (Letters)
    
  • Paper 2
    

Summary

• Gaia data produced the most accurate 3D map of star-forming regions in the Milky Way.
• Map covers 4,000 light-years around the Sun, based on 44 million ordinary stars and 87 O-type stars.
• O stars ionise hydrogen gas, marking sites of active star formation (HII regions).
• 3D views include the Gum Nebula, North America Nebula, California Nebula, and Orion–Eridanus superbubble.
• Some star-forming clouds are venting gas and dust into a large interstellar cavity.
• Future Gaia data releases will expand and refine this 3D map further.
  

Original Publication

Authors: Lewis McCallum, Kenneth Wood, Robert Benjamin, Dhanesh Krishnarao and Anna F McLeod.

Journal: Monthly Notices of the Royal Astronomical Society

DOI: 10.1093/mnras/staf1022

Article Publication Date: 21-Jun-2025

Source: https://www.esa.int/Science_Exploration/Space_Science/Gaia/Fly_through_Gaia_s_3D_map_of_stellar_nurseries

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